CREATE DATABASE IF NOT EXISTS `cnes-fuse` /*!40100 DEFAULT CHARACTER SET utf8 */; USE `cnes-fuse`; -- MySQL dump 10.13 Distrib 5.5.9, for Win32 (x86) -- -- Host: odysseus2 Database: cnes-fuse -- ------------------------------------------------------ -- Server version 5.1.41-3ubuntu12.10 /*!40101 SET @OLD_CHARACTER_SET_CLIENT=@@CHARACTER_SET_CLIENT */; /*!40101 SET @OLD_CHARACTER_SET_RESULTS=@@CHARACTER_SET_RESULTS */; /*!40101 SET @OLD_COLLATION_CONNECTION=@@COLLATION_CONNECTION */; /*!40101 SET NAMES utf8 */; /*!40103 SET @OLD_TIME_ZONE=@@TIME_ZONE */; /*!40103 SET TIME_ZONE='+00:00' */; /*!40014 SET @OLD_UNIQUE_CHECKS=@@UNIQUE_CHECKS, UNIQUE_CHECKS=0 */; /*!40014 SET @OLD_FOREIGN_KEY_CHECKS=@@FOREIGN_KEY_CHECKS, FOREIGN_KEY_CHECKS=0 */; /*!40101 SET @OLD_SQL_MODE=@@SQL_MODE, SQL_MODE='NO_AUTO_VALUE_ON_ZERO' */; /*!40111 SET @OLD_SQL_NOTES=@@SQL_NOTES, SQL_NOTES=0 */; -- -- Table structure for table `FUSE_PRG_ID` -- DROP TABLE IF EXISTS `FUSE_PRG_ID`; /*!40101 SET @saved_cs_client = @@character_set_client */; /*!40101 SET character_set_client = utf8 */; CREATE TABLE `FUSE_PRG_ID` ( `prop_id` varchar(4) NOT NULL DEFAULT '', `cycle` int(11) DEFAULT NULL, `title` varchar(200) DEFAULT NULL, `fname` varchar(20) DEFAULT NULL, `lname` varchar(30) DEFAULT NULL, `institution` varchar(100) DEFAULT NULL, `abstract` text, PRIMARY KEY (`prop_id`) ) ENGINE=MyISAM DEFAULT CHARSET=utf8 COMMENT='NULL'; /*!40101 SET character_set_client = @saved_cs_client */; -- -- Dumping data for table `FUSE_PRG_ID` -- LOCK TABLES `FUSE_PRG_ID` WRITE; /*!40000 ALTER TABLE `FUSE_PRG_ID` DISABLE KEYS */; INSERT INTO `FUSE_PRG_ID` VALUES ('A001',1,'Ultra-hot winds from DO white dwarfs','WERNER','KLAUS','Institut fur Astronomie und Astrophysik, Universitat Tubingen, Germany','We propose to study the two prototypes of a new class of hot white dwarfs (WD). The optical spectra reveal absorption lines from ultra-high ionized metals (e.g. O,VIII), a phenomenon never observed before in any astronomical object. The occurrence of such features requires temperatures in the order of 10$^6$,K, far in excess of the stellar T$_{\rm eff}$. The asymmetric profile shapes suggest formation in a rapidly accelerating high-speed wind (10,000~km/s). These stars represent the most convincing proof for on-going mass-loss from WDs. We have demonstrated that a large fraction of hot WDs shows this phenomenon, concluding that perhaps {it all} WD go through this evolutionary stage. We will study the wind properties and possible consequences for WD evolution on hand of detailed NLTE modelling. Recently obtained medium-resolution UV (HST) and FUV (ORFEUS) spectra pose new problems. In particular, the FUV region contains many inter-/circumstellar features which contaminate the photospheric spectrum. Hence we ask for high-resolution high-S/N FUV spectra for a deeper insight into this mysterious phenomenon.'),('A003',1,'Phase-resolved investigation of supersoft X-ray binaries','HUTCHINGS','JOHN','Dominion Astrophysical Observatory, HIA, NRC of Canada, Canada','We propose to obtain phase-resolved $FUSE$ spectra of three supersoft X-ray binaries, achieving S/N of $sim$20 over 0.5--1.0AA in orbital phase bins of $leq$0.1P. The emission line features in the $FUSE$ wavelength range cover a wide range of ionization giving a unique dataset for determination of the binary parameters, component masses, and disk structures which cannot be provided by optical and $HST$ data. We will also use the combined data for each system to detect and measure high-velocity lines from bi-polar jets which are seen in the optical spectra of all three systems. High-ionization lines from these jets are of particular interest since they are formed in the innermost region where the jets are undergoing their collimation and acceleration. An improved understanding of jets has wide astrophysical implications.'),('A004',1,'O VI raman scattering and the geometric structure of symbiotic stars','SCHMID','HANS MARTIN','Landessternwarte Heidelberg, Germany','We propose FUSE observations of the O~VI 1032, 1038 emission line structures in symbiotic systems in order to compare them with spectroscopic and spectropolarimetric observations of the Raman scattered counterparts in the red spectral region. From this we can derive the Doppler shift and polarization induced in the H$^0$ Raman scattering process. This allows to deduce information on the geometric and dynamic structure of the red giant\'s wind region in these interacting binary systems. In particular, our analysis should clarify the geometry of the ionization front between the cool giant and the hot component, which depends in a very sensitive way on hydrodynamical and radiative interaction processes.'),('A010',1,'The magnetic field structure of the 450 MG ultramassive white dwarf EUVE J0317-855','FERRARIO','LILIA','Astrophysical Theory Centre, Australian National University, AUS','We have recently identified the dominant features in the optical spectra of the rapidly rotating (725fs5) magnetic white dwarf EUVE~~J0317--855 with $H{alpha}$ 2s0 - 3p-1, 2s0 - 3p0 and $H{eta}$ 2s0 - 4f-1 in a magnetic field of 100-300 MG, but some features remain unidentified. IUE data show Ly$alpha$ ${sigma^+}$ at 1300AA, and an unidentified feature near 1330 AA. Models using centred and off-centred dipole field structures provide a reasonable fit to the averaged spectra for a dipole strength of $B_d=450$ MG displaced from the centre of the star by 35% $R_*$ and viewed at a mean angle of $30 -60gradi$ to the dipole axis. The nature of the observed spectral variations and of the unidentified lines remains unknown. We propose to carry out phase-dependent FUSE observations of the Lyman line series in order to resolve the field structure responsible for the observed photometric and spectroscopic variations. Based on a single TTAG data set we will reconstruct five seperate high-SN spectra, each at a specific rotational phase.'),('A013',1,'Trace elements and radiative levitation in hot helium-rich white dwarfs','DREIZLER','STEFAN','Institut fur Astronomie und Astrophysik, Universitat Tubingen, Germany','We propose to observe three helium-rich (DO) white dwarfs in order to determine their photospheric abundances of trace elements (e.g. C, N, O, H, Fe, Ni,...). FUSE spectroscopy is ideal for this purpose since the FUV allows to explore a large variety of line transitions of various elements which are not detectable in existing optical or UV spectra of the targets. The data will be analyzed with non-LTE metal line blanketed model atmospheres. The results will be compared to predictions from newly developed, self-consistent diffusion/radiative levitation calculations under non-LTE conditions. The observed metal abundances will serve as bench-marks for such kind of new calculations. As a basis for this work we have obtained high-S/N optical spectra of almost all known DO white dwarfs within the last five years as well as HST GHRS spectra of selected DO white dwarfs. A comprehensive analysis of the atmospheric parameters is now available. For the present proposal we have selected three targets which -- together with calibration and PI targets-- represent the non-DA white dwarf cooling sequence from the hot end down to the DB gap.'),('A019',1,'A FUSE observation of argon on Titan','GLADSTONE','RANDY','Southwest Research Institute, USA','The origin of Titan\'s thick nitrogen and methane atmosphere is a compelling enigma. One key and still missing observable concerns the abundances of noble gases in general, and argon in particular. Detection of argon would indicate that the N$_2$ and CO now found in the atmosphere probably came in with ice during Titan\'s accretion. Alternatively, if there is very little argon, then we have to turn to models starting with frozen ammonia, methane and water ice, indicating a more important role for the Saturn sub-nebula, and requiring subsequent modification by photochemistry. Current estimates on the fraction of argon in Titan\'s atmosphere are crude, and based only on indirect evidence, and range from 0--25%. We have modeled Titan\'s expected photoelectron-generated EUV emissions with argon as an added constituent. The bright resonance line of argon at 1048ang is predicted to be present at a level of 7--12~R, for assumed argon abundances of 5--25% in the lower atmosphere of Titan. At a brightness of 7~R, an 80~ks integration time by FUSE would provide a $>!5sigma$ detection of argon in the atmosphere of Titan (a 30~ks integration would provide a $>!3sigma$ detection). An accurate determination of the abundance of argon on Titan would be useful in preparing for the arrival of the {it Cassini} orbiter and {it Huygens} probe at the Saturn system.'),('A022',1,'Coronal heating during stellar flares and the search for proton beams','FISHER','GEORGE','Space Sciences Laboratory, University of California-Berkeley, USA','We will obtain high resolution FUSE spectra of the dMe star AD Leo during periods of quiescence and during flares to study the physics of atmospheric heating in flare stars. We will also obtain coordinated ground based observations including multicolor photometry and high resolution optical spectroscopy. Light curves obtained during flares will allow us to determine the coronal loop length and flare coverage area on the stellar surface. The FUSE spectra will also allow us to determine the structure and evolution of temperature and density in the corona, transition region, and chromosphere, allowing us to test detailed models of flare evolution. The unprecedented sensitivity and resolution of FUSE will strongly constrain current models. Finally, we will search for significant red-shifted emission in the Lyman series lines of hydrogen during the rise phase of flares, possibly indicating the presence of energetic proton beams. The existence and role of proton beams in both solar and stellar flares is currently a subject of great debate.'),('A023',1,'The FUV spectral energy distribution of star-forming galaxies','BUAT','VERONIQUE','Laboratoire d\'Astronomie Spatiale, CNRS, Marseille, France','We propose to observe several bright star-forming galaxies with FUSE. These galaxies are selected to have been already observed in the near UV, visible and far-infrared. The analysis of the entire spectral energy distribution longward the Lyman break will allow us to study the star formation history, the initial mass function and the effects of dust extinction in these objects. These galaxies will constitute needful templates for the study of high redshift actively star-forming galaxies. Under reasonable assumptions for intrinsically bright galaxies, the UV continuum (912-1200$AA$) is rather insensitive to the star formation history and the initial mass function. Any departure from the expected flat spectrum in our sample of intrinsically bright galaxies may be attributed to the effects of internal dust and will be used to deduce an empirical attenuation curve down to the Lyman break. The analysis of the stellar absorption lines in the far and near UV complemented with the interstellar emission lines in the optical and the overall shape of the spectral energy distribution of the galaxies will give us constraints about the recent star formation history, the initial mass function of the more massive stars and the contribution of an older underlying stellar population.'),('A024',1,'The origin of peculiar UV line ratios in magnetic cataclysmic variables','MOUCHET','MARTINE','Observatoire de Paris-Meudon, France','Magnetic Cataclysmic Variables (MCV) typically show UV emission line intensity ratios broadly compatible with photo-ionization by thermal radiation of ~20-50 eV, arising from accretion onto highly magnetized white dwarfs. However, four systems display peculiar UV line ratios not compatible with any modelling, suggesting a very peculiar ionization/ excitation process or surprising abnormal abundances which might be signs of a recent nova explosion or reflect the non-solar composition of the companion\'s atmosphere. We propose to observe the two Polars, BY Cam (H0538+608) and V1309 Ori (RX J0515.6+0105) which both show a strong deficiency in CIV correlated with a large excess in NV. The unprecedented sensitivity of FUSE in the 905-1195AA{} region will allow the measurement of the expected strong OVI doublet as well as several crucial C and N lines, all of which are essential to discriminate between models for the origin of the C, N emission line anomaly. The program requests a total of {f 16} orbits (including 2 orbits for acquisition) and a total on-source exposure time of {f 28 ksec} for the two sources to obtain spectra with a spectral resolution of 0.3AA{} and a S/N ratio above 5 in the continuum allowing a detailed multi-component line profile study over several orbital phases.'),('A026',1,'Abundances of the pop II sdO stars LS IV-12.1 and ROB 162','HEBER','ULRICH','Astronomisches Institut, Universitat Erlangen-Nurnberg, Germany','LS IV-12.1 and ROB 162 are rare, hot (Teff=50 -- 60,000K) subdwarf O stars of population II, evolving from the asymptotic giant branch to the white dwarf domain. FUSE spectra are proposed to determine the abundances of C,N,Si,P,S and Fe by means of NLTE model atmospheres. In the case of ls, its high radial velocity allows the photospheric resonance lines to be separated from interstellar components. The results of the abundance analysis will shed light on PAGB evolution in population II stars and will allow physical processes such as dredge-up of nuclearly processed matter and/or gas-dust fractionation in the AGB progenitor stars envelope to be investigated. The [S/Fe] ratio is a sensitive tracer of the latter process. The crucial sulphur abundance can most reliably be derived from the ion{S}{4} and ion{S}{6} lines in the FUV.'),('A034',1,'White dwarf evolution: heavy element abundances and the DA temperature scale','BARSTOW','MARTIN','Department of Physics and Astronomy, University of Leicester, UK','We propose FUSE observations of a sample of the hottest known DA white dwarfs to study their evolution and the link between them and their CSPN progenitors. Analysis of the H Lyman lines provides a unique determination of $T_{eff}$ and log g for each star, taking into account the heavy element abundances, which are known to affect the temperature determination, which we will determine from measurements of line strengths in the high resolution FUSE spectra. Importantly, FUSE gives us access to absorption lines of several species which cannot be studied in any other wavelength range. From this work, combined with observations of cooler PI/calibration white dwarf targets, when they appear in the public archive, we will reestablish the hot DA white dwarf temperature scale. In addition, with significantly improved accuracy in the temperature determination we will be able to track the evolution of stellar photospheric abundance with cooling age for the first time.'),('A035',1,'The warm intragroup medium in spiral-rich groups of galaxies','MULCHAEY','JOHN','Carnegie Institution of Washington, USA','Recent ROSAT observations indicate that $sim$ 20% of nearby groups of galaxies contain a low-density, X-ray emitting intragroup medium. If present in all groups of galaxies, the intragroup medium would be the dominant baryonic component in the local universe. However, the ROSAT observations indicate that X-ray emission is almost exclusively restricted to groups that are dominated by elliptical and S0 galaxies. The much more common spiral-dominated groups, such as the Local Group, are not X-ray detected. The most likely explanation for the non-X-ray detection of spiral-rich groups is that the intragroup medium in these systems is too cool to produce detectable X-ray emission. The intragroup medium in spiral-rich groups is expected, however, to produce detectable absorption features in the spectra of background quasars. We propose to observe with FUSE three AGN situated behind low redshift spiral-rich groups to search for the O VI doublet in absorption, as expected from a warm intragroup medium. The detection of O VI absorption from these groups would verify that an intragroup medium exists in all groups and is the dominant baryonic component in the local universe. The S/N of our proposed FUSE observations are such that the failure to detect O VI in absorption would put strict limits on the presence of an intragroup medium in spiral-rich groups. Furthermore, this limit would suggest that our current estimate for the amount of baryonic material in groups is overestimated by at least a factor of ten.'),('A036',1,'Far-ultraviolet studies of metal-deficient blue compact dwarf galaxies','THUAN','TRINH XUAN','Astronomy Department, University of Virginia, USA','How galaxies form is one of the most fundamental questions in astrophysics. Much effort has gone into the search for primeval galaxies at high redshifts. But these galaxies are faint and small, making their study very difficult even with the largest telescopes. We propose here an alternative approach, the study of nearby blue compact dwarf (BCD) galaxies that are chemically young. Our sample consists of 4 BCDs, two of which are among the most metal-deficient galaxies known, and which appear to be truly young, not containing stars older than $sim$100 Myr, SBS 0335--052 ($Z_odot$/41) and UGC 4483 ($Z_odot$/21). The two other BCDs, MKN 59 ($Z_odot$/8) and MKN 71 ($Z_odot$/10), have larger metallicities and ages, and allow us to explore the far-UV properties of BCDs over a wider ange of sub-solar metallicities. The proposed FUSE observations will allow us to investigate: 1) the H$_2$ content of BCDs. This will directly constrain models of galaxy formation as H$_2$ is an important cooling agent in the primordial gas; and 2) the evolutionary history and stellar winds in BCDs by detecting the P Cygni profiles of high ionization lines not observed at longer wavelengths such as S VI and O VI. The proposed observations will give us the opportunity to explore new spectroscopic techniques in the far-UV that can be later applied to the study of the star formation history in high-redshift primeval star-forming galaxies, where the far-UV is shifted to the near-UV or the optical.'),('A041',1,'Finding the onset of convection in main sequence stars','SIMON','THEODORE','Institute for Astronomy, University of Hawaii, USA','Main sequence A stars have both a small convective core as well as a thinconvective layer just below the visible surface. While neither of these two regions is directly observable, convection clearly plays a key role in many aspects of A star behavior. One of the most notable of these is the formation of a high temperature chromosphere or corona. Using FUSE, we propose to observe the far UV spectra of a sample of 8 normal A-type stars, which cover a broad range in $T_{\rm eff}$ and color index. Our goal is to use the diagnostically important lines of O VI, which form at 300,000 K, and the density-sensitive lines of C III, which form at 60,000 K, to find the locus for the onset of convection zones, coronae, and chromospheres along the main sequence, thereby testing the predictions of stellar structure models as well as chromospheric/coronal heating models. Such observations are best made below lya, where A--star photospheres appear much darker and offer less of a hindrance than at near UV and optical wavelengths'),('A044',1,'Wind ionization in high mass X-ray binaries','BOROSON','BRAM','High Energy Astrophysics Division, Smithsonian Astrophysical Observatory, USA','We propose to observe three High Mass X-ray Binaries with FUSE; one LMC source (LMC X-4), one SMC source (SMC X-1) and one galactic source (Vela X-1). We will observe the ion{O}{6}$lambdalambda1031,1037$ P~Cygni line variations over the binary orbit. The orbital variations result from X-ray photoionization of the wind, and allow us to model the wind structure to determine its density and velocity field. We will look for pulsations in the UV lines and continuum. Lyman series absorption lines from the primary star will help us model the wind lines, and can measure the rotation and orbit of the primary. We will also look for ellipsoidal variations in the continuum light curves.'),('A046',1,'The FUV spectra of starbursts','HECKMAN','TIMOTHY','Center for Astrophysical Sciences, Johns Hopkins University, USA','Starbursts are a significant component of the present-day universe, and offer unique laboratories for both studying the processes that have regulated the formation and evolution of galaxies, and for testing models of high-mass stellar evolution. We propose to exploit the unique strengths of FUSE to obtain full-resolution ($sim 10$ km s$^{-1}$) high quality (S/N $geq$ 15) spectra of the six UV-brightest starbursts. These starbursts span ranges of 20 in metallicity (1/8 to 2.5 solar) and $sim$ 10$^2$ in luminosity. The spectra will be used to study: 1) the coronal-phase gas that may dominate the energetics of starburst-driven `superwinds\' 2) the H$_2$ that probably dominates the ISM mass and regulates the star-formation 3) the starburst dust-attenuation law in the unexplored FUV window 4) the stellar content of the starburst (thereby probing the IMF and burst history). These will be the finest UV spectra obtained to-date for starbursts. In particular, the FUSE MDRS aperture allows us to obtain high-resolution spectra of nearly the entire starburst (rather than small pieces, as with HST and STIS).'),('A048',1,'FUV observations of low and high-excitation Herbig-Haro shocks','HARTIGAN','PATRICK','Dept. of Space Physics and Astronomy, Rice University, USA','We propose to test our understanding of radiative cooling behind shocks by comparing the fluxes of far-UV emission lines in stellar jets with predictions from shock models. Our targets include the brightest examples of three distinct types of shock waves in these objects -- high-excitation, low-excitation/molecular, and preionized. Spectra of the high-excitation bow shock HH~1F should have detectable O~VI $lambda$1035 emission if existing models are accurate. The lack of such emission would suggest that magnetic fields play an important role in the dynamics of this object. The unique combination of detectable H$_2$ fluorescent lines and low reddening in the low-excitation object HH~47A will allow us to measure the relative importance of molecular and atomic cooling in low-velocity shocks, and to assess the degree to which pumping by postshock Lyman $alpha$ and Lyman $eta$ photons heats the H$_2$. A FUSE spectrum of the preionized low-excitation bow shock HH~47D will clarify how the ambient UV radiation affects emission line ratios between 900AA and 1200AA . '),('A049',1,'10^5 K gas in the halo of the Large Magellanic Cloud','WAKKER','BART','Department of Astronomy, University of Wisconsin-Madison, USA','One of the stated major scientific goals of the FUSE PI programs is a survey of the amount and distribution of the OVI ion in the Milky Way disk and halo and in the Magellanic Clouds, in order to understand how matter and energy are transferred between the disk and halo. In particular, the halo program allows to understand how plumes generated by OB associations spread out. A study of OVI in the halo must avoid sightlines through active regions. This is the case for about 100 Milky Way sightlines on the reserved-target list, but only for 3 stars selected in the Large Magellanic Cloud (LMC). Since we recently used CIV absorption data to show that the LMC indeed has dex5,K halo gas, we request time with FUSE to study the global distribution of the OVI absorption in the LMC. With these data we will asses the relationship between the dex6,K X-ray emitting gas, the dex4,K Ha maps, and the dex5,K gas.'),('A051',1,'Molecular hydrogen excitation in photodissociation regions','FEDERMAN','STEVEN','Univ. Toledo USA','We propose to study photodissociation regions through observations of absorption from rotational levels in the vibrational ground state of H$_2$. These transitions occur below 1150 AA. Photodissociation regions are found around newly-formed B stars and beyond the H~{small II} regions surrounding newly-formed O stars because their ultraviolet flux is sufficient to convert molecular species into atoms. H$_2$ is destroyed by a two step process: absorption into excited electronic states followed by radiative decay into the continuum of the ground electronic state. This occurs with an efficiency of $sim$ 10%; the remaining decays to excited vibrational states then lead to infrared emission that returns the molecule to the vibrational ground state, but with a non-thermal distribution for the populations of high-lying rotational levels. We will extract the gas temperature from the relative amounts in the lowest rotational levels and the flux of ultraviolet radiation permeating the gas from the amount in excited rotational levels. The estimates for temperature and flux will lead to refined models of photodissociation regions previously based solely on infrared emission.'),('A052',1,'The Lyman continuum radiation from galaxies','DEHARVENG','JEAN-MICHEL','Laboratoire d\'Astronomie Spatiale CNRS, Marseille, France','The amount of ionizing radiation released into the intergalactic medium by star formation is a poorly known but crucial parameter. It would tell how the galaxies can complement the contribution of quasars for ionizing the IGM, especially at the epoch of re-ionization when the number density of quasars is apparently low. Direct measurements are difficult and scarce. Indirect evaluations using stellar population synthesis are plagued by the uncertainties on the Lyman continuum (Lyc) escape fraction. We would like to take advantage of the sensitivity of FUSE down to 900 AA~ to detect (or set significant upper limit on) the Lyc radiation of nearby star-forming galaxies. We have selected two galaxy candidates with a redshift large enough to get rid of the residual galactic opacity resulting from the accumulation of the Lyman series absorption lines.'),('A053',1,'Intergalactic ionized helium absorption toward 15 new bright quasars','REIMERS','DIETER','Hamburger Sternwarte, Universitat Hamburg, Germany','We propose to probe the far-UV continuum fluxes of 15 new bright($V<17$) $2.4 < z < 2.9$ quasars from the Hamburg Bright Quasar Survey by means of single-orbit snapshot exposures, with the aim of identifying one or more suitably bright objects for detailed studies of intergalactic HeII absorption over this redshift range. We also propose to carry out a $4 cdot 10^{4}$~s exposure of the newly discovered quasar HS1549+1919 ($z=2.83$, $Vsimeq 15.6$) -- an object that promises to reach a flux of $F_lambda sim 6 imes 10^{-15}$ erg~s$^{-1}$~cm$^{-2}$ hinspace{AA}$^{-1}$ at redshifted HeII~$lambda304$. If confirmed by its snapshot exposure, this object would be the brightest ``clear\'\' high redshift quasar discovered so far. Since the detailed study of HeII absorption lies at the limit of the capabilities of {it FUSE}, a $simeq5$ and $simeq 2$ times boost in signal over the two other Hamburg quasars and {it FUSE} targets HS1700$+$6416 and HE2347$-$4342 will dramatically increase the amount and quality of information on the physical state of the intergalactic medium that can be extracted from {it FUSE} observations of intervening HeII absorption. '),('A058',1,'H2 as the primary gas component at large galactic radius','MILLER','ERIC','Department of Astronomy, University of Michigan, USA','Molecular absorption line studies and X-ray absorption observations towardextragalactic sight lines indicate that molecular gas is as abundant as neutral atomic gas in the Solar vicinity. At larger Galactic radii, H$_{2}$ exceeds HI in some locations, and if this is generally true, it implies a dramatic revision in the picture of neutral gas in disk galaxies. To determine if H$_{2}$ dominates the ISM at large radii, we propose to measure the H$_{2}$ column toward AGNs projected behind the outer parts of two external disk galaxies with measured HI columns.'),('A060',1,'The FUV spectral energy distribution of quasars','KORATKAR','ANURADHA','Space Telescope Science Institute, USA','A well known feature of Active Galactic Nuclei (AGN) is the Big Blue Bump (BBB) continuum component which extends from 1 micron to soft X-rays, containing more than half the bolometric emission of an unobscured AGN. Its origin is directly related to the main energy production mechanism. Theoretical arguments based on accretion disk models and on photoionization models suggested that the BBB peaks in the EUV. However, recent UV observations by Zheng et al. and soft X-ray observations by Laor et al. suggest the FUV turns over just below 1000~AA and extends as a single power-law to $sim$1~keV. This very surprising spectral shape has important implications for both accretion disk and photoionization models. Since there is no overlap between the high $zsimeq 1$ UV and low $zsimeq 0.2$ soft X-ray samples, it is not clear whether the implied SED in fact holds for any individual quasar. We propose here to obtain complete FUV coverage of a sample of 23 low $z$ PG quasars, for which high quality soft X-ray spectra are available. The combined {em ROSAT PSPC+FUSE} spectra will allow us to set the most accurate constraints on the ionizing SED of quasars from both sides of the Galactic opacity barrier (at 912~AA-0.15~keV). This will allow us to test directly, and in each object, whether the FUV indeed turns over below 1000~AA into a single power-law which matches the 0.15-1~keV power-law. This sample was studied extensively and systematically in nearly all spectral bands, and highly significant correlations were found among the optical, UV and soft X-ray emission properties, providing important hints for the physical processes which shape AGN emission properties. The {em FUSE} data will allow us to explore the expected correlations with FUV emission lines. A few of the objects in this sample show UV and soft X-ray absorption. Higher spectral resolution observations proposed for some of these objects will provide important clues on the nature and possible association between the X-ray and UV absorbers.'),('A061',1,'The hottest stars in M31 and M33','HUTCHINGS','JOHN','Dominion Astrophysical Observatory, HIA, NRC of Canada, Canada','We propose FUSE observations of the brightest OB stars in the local group galaxies M31 and M33. The stars are faint but their UV fluxes are known from HST and UIT data. This will extend the stellar wind and interstellar studies currently under way with HST and ground-based telescopes, with similar resolution (1000) and S/N. The program will expand our comparison of stellar winds, evolution, and the ISM among the major galaxies of the local group.'),('A063',1,'Dust scattering propereties in reflection nebulae','WITT','ADOLF','Department of Physics & Astronomy, The University of Toledo, USA','We propose to observe the three reflection nebulae NGC 2023, NGC 7023, and IC 435 and their illuminating stars with the aim to derive the dust scattering properties in three systems with widely differing far-UV extinction curves. The wavelength dependence of extinction in the 90-120 nm range in these three nebulae will be determined by the pair method, employing the far-UV SEDs of four lightly reddened comparison stars of appropriate spectral types, also to be observed as part of this project. Dust scattering properties in the form of wavelength-dependent values for the albedo and the phase function asymmetry will be derived with the use of Monte-Carlo multiple scattering models and with substantial reference to earlier analyses of these objects carried out at longer UV, visible, and near-IR wavelengths by the PI and his collaborators. The results will aid in the identification of the nature of the grains responsible for the steep far-UV rise in the interstellar extinction curve, and they will provide essential input parameters for models of the far-UV diffuse galactic light and for models treating the radiative transfer in dusty galaxies. '),('A066',1,'Non-radiative shocks in the Cygnus Loop','RAYMOND','JOHN','Smithsonian Astrophysical Observatory, USA','FUSE measurements of the O VI doublet in non-radiative shock waves provide unique diagnostics for the physics of collisionless shock waves (ion-ion and electron-ion equilibration) as well as a means to observe the onset of radiative cooling. It is necessary to understand these processes in order to derive the physical parameters and the evolutionary states of supernova remnants and other astrophysical shocks. We propose to observe two filaments in the Cygnus Loop. One is a 300 km/s pure non-radiative shock. The other is a crisp filament seen in the light of [Ne V] which marks the encounter between the main supernova remnant blast wave and a large, dense cloud.'),('A068',1,'Do elliptical galaxy cooling flows actually cool?','BREGMAN','JOEL','Department of Astronomy, University of Michigan, USA','The fundamental prediction of the cooling flow model for hot gas in elliptical galaxies is that the hot gas loses its thermal energy and becomes cool gas, typically at a rate of 1 $M_{odot}$ yr$^{-1}$ for X-ray bright ellipticals. The most powerful test of this model would be the detection of cooling gas at $sim10^{5.5}$ K, when it has lost more than 90% of it thermal energy. OVI emitting gas is produced in this temperature range and the predicted luminosity is high enough that this gas should be easily observable by FUSE with the LWRS aperture. Measurements of OVI emission for our five galaxies of different $dot M$ permit two important tests of the cooling flow picture, while non-detections will lead to severe limits, $dot M < 0.04 M_{odot}$ yr$^{-1}$, and a dismissal of the model.'),('A070',1,'Probing the very small scale structure (l~10 AU) in the ISM','BOISSE','PATRICK','Laboratoire de Radioastronomie, Ecole Normale Superieure, Paris, France','We propose to investigate the very small scale structure (l $simeq$ 5 - 10 AU) in the molecular, atomic and ionized phases of the interstellar medium by repeatedly observing a bright runaway O star located behind a translucent molecular cloud. The selected star, HD 34078 (AE Aur) moves at a transverse velocity of 103 km/s and the spectra taken during cycle 1 at three distinct epochs separated by 3-4 months will allow to sample adjacent lines of sight distant by $simeq$ 5 AU at the cloud distance. The spectral range covered by FUSE is very well suited to conduct a coordinated search for small amplitude fluctuations of the column density for molecules (H$_2$, $^{12}$CO, $^{13}$CO, ...), atoms (CI, SI, ...) and ions (SiII, CII, FeII, ...). By performing a detailed comparison of the absorption lines detected in the three successive spectra, we expect to significantly improve the characterization of the ubiquitous AU-scale structure in the ISM and better understand its nature and origin. The properties of the proposed source as well as those of the interstellar gas along the line of sight are well characterized by previous observations (IUE, high resolution optical spectroscopy), which makes HD 34078 an ideal target for this project. Depending on the results obtained from cycle 1 observations, we will propose to extend the monitoring of the absorption lines during cycle 2 and/or 3, especially in order to investigate the variability on larger scales (l $simeq$ 30 - 50 AU). If no variations are detected among cycle 1 spectra, the observations proposed will at least permit a detailed study of a well documented line of sight. '),('A075',1,'Abundances in O-rich SNRs: observational tests of nucleosynthesis','MORSE','JON','Center for Astrophysics and Space Astronomy, University of Colorado, USA','We propose to obtain fuse far-UV spectroscopic observations of the oxygen-rich supernova remnants N132D in the LMC and E0102.2--7219 in the SMC. The fuse spectra will be coupled with our existing hst FOS spectra and scheduled axaf GTO spectra of the uncontaminated SN debris to provide complete, unprecedented sensitivity and wavelength coverage of the emission from the X-rays to the near-IR. We will compare the observed line ratios to predictions made by theoretical models in order to determine the excitation mechanisms and to derive reliable elemental abundances. Of primary importance is to measure the O~VI $lambdalambda1032$ emission from these objects with fuse, which is key to determining the relative importance of collisional ionization and photoionization for producing the observed emission. N132D and E0102.2--7219 are the only O-rich SNRs that can be spatially resolved {it and} studied effectively at UV wavelengths. The combined fuse + hst + axaf data will provide important tests for theories of nucleosynthesis in massive stars as well as improve our understanding of the dynamics of supernova explosions and mixing in the ejecta.'),('A083',1,'Solar physics with FUSE: FUV studies of solar analogs and twins','GUINAN','EDWARD','Dept. of Astronomy, Villanova University, USA','We propose to use FUSE for an in-depth study of the evolution of the transition region and low corona of a solar-mass star throughout its main-sequence lifetime. This program is part of a comprehensive study of the ``Sun in Time\'\' across the electromagnetic spectrum. We have defined a homogeneous sample of single G0-5~V stars with well-known rotation periods that are proxies of the Sun at different ages. We intend to study dynamics of the lower layers of the stellar atmospheres by investigating line shifts, line asymmetries, and line broadenings that we presume are related to chromospheric evaporation by high-energy processes identified in the overlying corona. Emission measure and temperature analysis will allow us to obtain a complete 3-D atmospheric model of active regions that we will link to the previously obtained coronal X-ray data. We will infer transition region pressures through the powerful density-sensitive ratio of the C~III 977AA/1176AA lines; this important diagnostic will be adequate to identify and model the relevant magnetic structures based on the solar analogy, and, together with our coronal X-ray (ROSAT, ASCA, SAX), EUV (EUVE), and TR (IUE/HST) data, to infer the importance of coronal energy releases. Our FUSE investigation is central to the understanding of the evolution of magneto-dynamic atmospheric phenomena, and the associated high-energy emissions in the Sun and in solar-type stars. It also bears on the question of the young Sun\'s influence on the developing planetary system. The FUSE observations will further be used to estimate the important D/H ratio along the sightlines to the stars, and to search for the presence of stellar analogs to the solar wind. Coordinated /contemporaneous observations (with XMM, ROSAT, HST, optical photometers, partly from guaranteed time programs) are planned and will be organized.'),('A084',1,'High resolution FUV spectroscopy of EX Hydrae','MAUCHE','CHRISTOPHER','Astrophysics Group, Lawrence Livermore National Laboratory, USA','We propose to obtain high spectral resolution orbit- and spin-phase resolvedFUV spectra of the intermediate polar EX~Hya. These spectra will be used to (1) resolve the FUV emission lines into their various components to constrain the location of, and the physical conditions in, the line-emitting gas, (2) measure the strength and phasing of the narrow absorption features to determine the column density through, and the ionization state of, the bulge on the edge of the accretion disk, and (3) measure the continuum flux distribution in the FUV and its variation on the spin and binary phases to constrain the effective temperature and area of the hot spot on the surface of the white dwarf and the effective temperature of the truncated inner disk.'),('A085',1,'Far-UV absorption-line spectroscopy of the neutral envelopes of planetary nebulae','DINERSTEIN','HARRIET','Astronomy Department, University of Texas at Austin, USA','In the last few years has it become clear that planetary nebulae (PNe) are not quite what they seem to be at first glance: they are {it not} simply fully ionized circumstellar nebulae. Instead, for most PNe the ionized gas is merely the innermost zone of a massive, mostly neutral, circumstellar envelope. These neutral/molecular envelopes have been studied by the PI and her collaborators via fluorescently-pumped near-infrared H$_2$ emission lines, far-infrared emission lines such as [O I] 63 $mu$m, and, most recently, optical Na I absorption lines. We propose to use FUSE to obtain high-resolution spectra of the central stars, using their continua as backdrops for observing UV absorption lines of key neutral and molecular species, in order to determine excitation temperatures, column densities, and other properties of these envelopes. This study will connect tightly to existing and future optical and infrared observations, as well as to previous GRHS and upcoming STIS programs. The FUSE observations are particularly important because {it only} with FUSE will it be possible to directly observe the H$_2$ Lyman and Werner bands, the very lines that pump the cascade that produces the infrared H$_2$ lines. With their high-surface-brightness infrared line emission, PNe provide a remarkable opportunity for tying together the absorption and emission components of the H$_2$ fluorescence process, now known to be widespread in the ISM. FUSE will also enable us to measure the populations of the fine-structure levels of the $^3$P ground state of O I and connect these to far-infrared line observations by the PI of [O I] 63 $mu$m, the primary coolant for the warm atomic gas in PNe, and [O I] 145 $mu$m. In addition, FUSE will sample lines of other species such as C I and Cl I, as well as revealing new spectral features from the central stars. From this study we will learn about both the physics of UV-illuminated nebulae (``PDRs\" or ``photodissociation regions\") and about this enigmatic phase of stellar evolution, during which most of the stellar envelope is removed.'),('A086',1,'Nearby galaxies in the FUV: toward comparison with high-redshift galaxies','KEEL','WILLIAM','Dept. of Physics and Astronomy, Univ. of Alabama-Tuscaloosa, USA','We propose a program of FUSE spectroscopy of star-forming regions in local galaxies to complement planned observations with the STARLITE far-UV shuttle hitch-hiker payload (which offers excelent diffuse-source sensitivity and spatial resolution at the expense of point-source performance and spectral resolution). The two datasets would complement each other uniquely for understanding the overall far-UV spatial and spectral morphology of these galaxies, an important first step toward being able to interpret this passband as seen optically in high-redshift galaxies. We concentrate on M33, whose combination of proximity and star-forming rate makes it especially amenable for this comparison. The S/N requirements are designed to allow separation of the lines in the Lyman $eta$/O VI/C II blend which are diagnostic of the massive-star mix (particularly unevolved versus evolved stars), which has proven very difficult to unravel at longer wavelengths. Comparing the two data sets will tell whether the brightest star-forming regions are representative of the overall FUV-emitting population, and will be used to search for scattering effects. These data will enable us to interpret observations of high-redshift galaxies (higher every month now) in a more realistic context than yet possible.'),('A088',1,'Hot populations in nearby elliptical galaxies','BROWN','THOMAS','Lab. for Astronomy and Solar Physics, NASA/GSFC, USA','Because they are composed of old, passively evolving populations,elliptical galaxies offer great promise for tracing the evolution of the Universe. Their apparent simplicity makes them the first beachhead in the quest to understand galactic evolution, and if they evolve slowly enough, they can be calibrated as standard candles at great distances. The hot stars responsible for the ``UV upturn\'\' phenomenon are key indicators of age and abundance in ellipticals. These stars are well isolated in the {it FUSE} wavelength range from the cooler main sequence stars that complicate interpretation at wavelengths longer than 2000~AA. We propose to observe three ellipticals through the {it FUSE} $30 imes 30^{primeprime}$ aperture: NGC~221, NGC~4649, and NGC~1399. Although NGC~221 is a fundamental testing ground for theories of stellar and galactic evolution, its spectrum has never been measured below Lyman $alpha$. NGC~4649 and NGC~1399 were observed by {it HUT}, but at considerably lower signal-to-noise and resolution than possible with {it FUSE}. With {it FUSE} data, the absorption lines of C, N, and Si prevalent in the far-UV will provide invaluable composition diagnostics for the hot stellar populations in ellipticals. Furthermore, {it FUSE} is uniquely qualified to measure the Lyman series, an important diagnostic of effective temperature and surface gravity. {it FUSE} presents the opportunity to finally and unequivocally characterize the population responsible for the UV upturn.'),('A090',1,'Search for H2 in Mars\' atmosphere','KRASNOPOLSKY','VLADIMIR','Department of Physics, Catholic University of America, USA','We propose to detect H$_2$ on Mars by observing its spectrum with FUSE in the beginning of June 1999 with integration time of 18 ks. This observation will also allow studying the far UV spectrum of Mars with an unprecendented quality. H$_2$ is probably the most abundant species which has not been observed on Mars. Photochemical models predict its mixing ratio from 7 to 50 ppm. The upper limit to the H$_2$ density of $1.1 imes 10^5$ cm$^{-3}$ at the altitude of 560 km was established using the Mariner 9 ultraviolet spectrometer observations. This limit is very close to the value which is required to explain the densities of atomic hydrogen observed with Mariner 6, 7, and 9. A spectrum of Mars observed with the Hopkins Ultraviolet Telescope does not show H$_2$ emissions. This may raise a problem of a H$_2$ deficit on Mars, and a possible detection with FUSE may be of crucial importance. The most sensitive method for spectroscopic detection of H$_2$ is observations of the P1 (6-v\'\') lines of the H$_2$ Lyman band system. These lines are much stronger than other H$_2$ lines due to their excitation by the solar Lyman-beta line, the effect discovered by one of us (PDF) twenty five years ago. However, the expected intensities are low, a few tenths of rayleigh, even for these lines. The unique sensitivity and resolution of FUSE will allow detection of H$_2$ in the upper atmosphere of Mars. Extrapolation of the measured abundance to the lower atmosphere will result in the H$_2$ mixing ratio with an uncertainty of 30%. Thus, H$_2$ can be measured for the first time on Mars, and FUSE can provide a key measurement which was impossible for the numerous spacecraft that visited Mars.'),('A093',1,'FUSE observations of galactic and LMC novae in outburst','SHORE','STEVEN','Dept. of Physics and Astronomy, Indiana University South Bend, USA','We propose target of opportunity observations of classical novae in the Galaxy and the Large Magellanic Cloud in the early stages of outburst. The FUV represents the final frontier in the study of the early history of the expansion of nova ejecta, when the overlying optically thick metallic line absorption spectrum (called the ``iron curtain\'\') lifts and it is possible to see through the ejected shell to the deepest layers of the still optically thick ejecta. During the period following the explosion, the central source illuminates the ejecta. To date, only three novae have been observed in the region from 900 - 1200AA, V1974 Cyg 1992 (Voyager UVS, ORFEUS), Cir 1995 (HUT), and Aql 1995 (HUT). The 1995 novae were observed only at relatively low resolution with HUT during the ASTRO-2 mission and within one month of outburst, while V1974 Cyg was observed nearly 4 years after maximum and only with limited S/N. The ability to correctly model the outburst, determine the abundances in the ejecta, and obtain a comprehensive picture of the energetics of the outburst can only be achieved through multiwavelength observations. The FUV plays a vital part in these studies.'),('A094',1,'Observational constraints for the Galactic fountain','BENJAMIN','ROBERT','Dept. of Physics, University of Wisconsin, USA','We propose to simultaneously search for diffuse OVI~ emission andOVI~ absorption in the same direction for which Martin & Bowyer (MB) detected CIV~ 1549 AA~ emission: $l=155$, $b=58$. This is also the direction of the ``Lockman window\'\'. For OVI~ absorption, we will use the compact UV bright galaxy Mk 153 as a background source. Measurement of Galactic OVI~ absorption and emission along the same line of sight will determine the density and pressure of the hot gas. Our results will be combined with MB\'s CIV~ 1549 AA~ and OIII] 1662 AA~ detections, as well as optical $H alpha$, [S II], and [O III] emission from the Wisconsin $H alpha$ Mapper, and $onequarter {\rm -keV}$ X-ray shadowing studies of this region. Comparison with calculations of nonequilibrium cooling flows will be used to constrain models for the origin of this hot gas and determine whether the gas pressure is high enough to drive a ``galactic fountain\'\' flow.'),('A099',1,'FUV spectroscopy of narrow-line Seyfert 1 galaxy RE 1034+39','LEIGHLY','KAREN','Columbia Astrophysics Laboratory, Columbia University, USA','It has long been thought that the shape of the ionizing continuum of an Active Galactic Nucleus (AGN) should have an effect on its emission-line ratios. This is important since the line ratios then potentially provide a way to infer shape of the continuum in the unobservable EUV wavelength range. It was suspected that the ratio of ion{O}{6} to Ly$alpha$ should be especially sensitive to this shape: ion{O}{6} should be strong when the continuum in the optical--UV--soft X-ray range is hard. Among the recently presented observational evidence lending support for this idea are the {it HUT} spectra showing that some Seyfert 1 galaxies with strong X-ray soft excesses have also strong ion{O}{6} lines. The Seyfert 1 galaxy RE~1034+38 has a remarkable spectral energy distribution. Its optical and UV spectra are very red, but there is no evidence for absorption. Its soft X-rays are very strong, with a steep spectrum. Such a hard ionizing continuum should produce a huge ion{O}{6} line. We propose a 50~ks {it FUSE} observation of RE~1034+39 to test the extreme limits of the trend for strong ion{O}{6} to accompany a hard ionizing continuum. This observation will enhance our understanding of the influence of the continuum shape on the production of the strong broad emission lines in AGN. The signal to noise in the resulting spectrum should be good enough that we can resolve the line, and measure strong deviations of the continuum from a power law. Coordinated {it ASCA} and optical spectroscopic observations are planned as well as accretion disk and photoionization modeling.'),('A100',1,'FUV spectra of evolved late-K and M stars: mass loss revisited','HARPER','GRAHAM','CASA, University of Colorado, USA','The FUV radiation field of evolved late-K and M stars, which is dominated by H Lyman emission lines, controls the ionization balance of key atomic and ionic species, the dissociation equilibrium of molecular H$_2$ and CO, and provides crucial information on the excitation of hydrogen. FUSE observations of the FUV flux below $1044$AA{ } will allow us to constrain the Ca~II/Ca~III balance and remove a key uncertainty in previous studies on stellar mass-loss rates. The FUV photoionization flux was previously {it unknown}, but FUSE spectra can unlock the wealth of information from early optical studies of Ca~II. We propose to construct detailed radiative transfer models from the H Lyman $eta$ and $gamma$ line profiles. These models will provide constraints on the hydrogen ionization, the dominant source of electrons in chromospheres, and the formation of the Lyman continuum which is not directly observable. FUSE will also allow us to observe wind induced line profile asymmetries and to constrain with great sensitivity the volume of $sim 3 imes 10^5$~K plasma which traditional ``non-coronal\'\' stars are now thought to possess. We propose deep exposures of the brightest K bright giant ($alpha$~TrA K3~II), the brightest K supergiant ($lambda$~Vel K4~Ib), and two of the brightest M giants ($gamma$~Cru M3~III, $eta$~Gru M5~III). These stars have been studied extensively in the UV and optical, and we have recently obtained the first radio detections for all these targets. We will incorporate the knowledge gathered from the FUV into our unified chromospheric/wind models for these stars. These spectra will provide a valuable complement to the spectral-types and evolutionary phases of the GTO targets. FUV spectra of the M stars will provide crucial input physics for circumstellar photochemistry.'),('A107',1,'Distribution of Argon in the dayside lunar atmosphere','FLYNN','BRIAN','Center for EUV Astrophysics, University of California-Berkeley, USA','The lunar atmosphere was first detected by Apollo instruments over 25 years ago. Both neutral Ar and He were detected, with peak nighttime number densities of $sim$10$^3$~cm$^{-3}$ (Hodges et al. 1974). However only nighttime surface densities could be measured due to daytime outgassing from spacecraft hardware. Furthermore, due to the nature of the Apollo measurements, the spatial distribution of the most abundant known atmospheric species, Ar and He, could not be measured. In December 1996, the 1048 AA resonance scattering line of Ar was detected at the 3$sigma$ level above the lunar dayside for the first time using the ORFEUS SPAS II satellite (Flynn 1998). Due to the faintness of the Ar signal, and due to the insensitivity (relative to FUSE) of ORFEUS, no spatial information could be extracted from the data. Modeling the atmosphere as an optically thin 400~K barometric distribution indicates an Ar abundance surprisingly $sim500 imes$ greater than the theoretical daytime value (Hodges et al. 1974), which may indicate that the atmosphere is actually optically thick. A measurement of the radial distribution of the 1048 AA emission would not only provide valuable information on the Ar source but also indicate whether or not the atmosphere is optically thick. We propose to use the greater sensitivity of FUSE to confirm the ORFEUS dayside Ar detection, and to measure the spatial brightness distribution for the first time.'),('A108',1,'FUSE spectroscopy of hot post-AGB stars in globular clusters','DIXON','VAN','Space Sciences Laboratory, The University of California, Berkeley, USA','We propose to obtain fuse spectra of four hot post-asymptotic giant branch (PAGB) stars in globular clusters: ROB 162 in NGC 6397, ZNG 1 in NGC 5904 (M5), ROA 5342 in NGC 5139 ($omega$ Cen), and III-60 in NGC 6723. These stars have temperatures greater than 40,000 K and are located in globular clusters with well-known distances, metallicities, and ages. Despite their short ($sim 10^5$ yr) lifetimes, hot PAGB stars may contribute significantly to the enrichment of the interstellar medium, the photoionization of the halo, and the integrated ultraviolet flux of old stellar populations. We will model the fuse spectra with non-LTE line-blanketed stellar atmospheres in order to derive the stars\' effective temperatures and surface gravities and the abundances of important species such as carbon, nitrogen, and silicon. These parameters will be used to set constraints on processes such as mass-loss and dredge-up on the AGB, superwinds at the AGB turnoff, and the white dwarf mass in globular clusters.'),('A109',1,'Werner bands of H2 in CS environments of selected classical T Tau stars','WALTER','FREDERICK','Department of Physics and Astronomy, State University of New York, USA','The circumstellar disks of young stellar objects are likely to be dominated by hydrogen molecules (H$_{2}$). Using the HST/GHRS, we detected strong permitted H$_2$ Lyman band emission from a sample of classical T~Tauri stars. These bands arise either through fluorescent pumping by strong stellar emission lines or by shock heating. We propose FUSE observations of the H$_2$ Werner bands. These could be fluoresced by stellar O~VI emission, by shock heating, or by thermal processes at 1000~K. Measurement of these fluxes will greatly assist our study of the gaseous circumstellar environments of pre-main sequence stars.'),('A111',1,'Interfaces in N51D','CHU','YOU-HUA','Department of Astronomy, University of Illinois, USA','We are studying the interfaces between hot (dex6,K) and warm (dex4,K) gas in the superbubble N,51,D in the Large Magellanic Cloud. N,51,D provides a well defined closed environment with known distance, size, kinetic and thermal energy. We have X-ray, radio and optical data and have been allocated time to obtain HST-STIS spectra for 4 lines of sight. The STIS spectra include lines of NV, CIV, SiIV, and lower ionization species, and the four probe stars sample different projected distances from the center of the superbubble. We propose to use FUSE spectra of these four stars. Two are already on the reserved-target list, we request time for the other two. The integration times will be $sim$10,ks in three cases, so that we can obtain the O,VI emission as well as the OVI absorption. The FUSE spectra will yield information on CI, CIII, NI, NII and NIII, so that we will have spectra for four ionization stages of C and N. Taken together, these data will allow a determination of the density, pressure and ionization of dex2,K, dex4,K, dex5,K and dex6,K gas in N,51,D.'),('A117',1,'Search for UV emission lines from the warm intracluster medium','LIEU','RICHARD','Dept of Physics, University of Alabama-Huntsville, USA','A new component of diffuse soft X-ray and EUV emission has been found in all of the five clusters hitherto observed. In some clusters the soft excess is as luminous as that of the well-known intracluster X-rays. A thermal origin involves large quantities of warm gas, but was predicted by Cen and Ostriker whose cold dark matter model puts 55 % of the present day baryons in this gas. Several authors also suggested a non-thermal (inverse-Compton) interpretation. Both scenarios have their pros and cons, and only further observations by better techniques can lead to a verdict. This proposal concerns a very effective means of gathering independent evidence for the thermal model. If warm gas is indeed present in such vast amounts one will expect prominent O VI emission lines. Previous missions failed to detect them, but their upper limits were not particularly constraining. With the much improved sensitivity of FUSE, one can now make definitive statements about the existence or otherwise of intracluster gas at the temperatures inferred from the soft excess measurements. We suggest observations at various radii of the three brightest soft excess clusters, to measure the spatial distribution of warm gas.'),('A118',1,'FUV extinction: unique insights into the nature and role of small dust grains','WOLFF','MICHAEL','Space Science Institute USA','Understanding interstellar dust and its role in the universe is very important. Virtually all observations of astrophysical objects and their physical processes are affected by the presence of dust either within the system being studied or along its line of sight. We propose a research program that will significantly improve our knowledge of dust properties, specifically those of small grains. Such an advance has not been possible prior to the advent of FUSE and its unique capabilities: the high far ultraviolet (FUV) throughput and the ability to resolve H$_2$ lines, combined with a well-characterized instrumental calibration. We will derive FUV extinction curves for several types of sightlines which possess distinct signatures associated with the small grain population and whose mid-UV extinction curves reveal vastly differing amounts of intermediate-sized particles. In addition to a variety of important Galactic sightlines (ie extreme values of $R_V$, polarized 2175~AA feature), we include objects in each of the Magellanic Clouds where very non-Galactic mid-ultraviolet extinction properties are seen. These data will be used to probe and constrain the properties of the small dust grains, such as abundance and size, and their connection to the very different environments observed.'),('A120',1,'The atomic-to-molecular transition in the halos of dense IS clouds','WANNIER','PETER','Jet Propulsion Laboratory, California Institute of Technology, USA','FUSE observations of interstellar H$_2$ will enable a breakthrough study of the cool atomic and molecular gas (CAMM) associated with dense molecular clouds. We propose to initiate such a systematic study of the extended halos around four nearby clouds, which have been well characterized using radio and infrared techniques. The H$_2$ absorption-line spectra toward hot background stars will yield (1) direct H$_2$ column densities, (2) gas kinetic temperatures and (3) the diffuse UV radiative intensity. From the information in the atomic Lyman series and HD absorption lines, we will estimate (1) the atomic column density, yielding information about the space density, and (2) the cosmic ray ionization rate. In addition to the proposed FUSE observations, we plan an independently-funded observational program which will provide vitally-needed information about the cloud kinematics. For the FUSE sightlines, we will obtain optical spectra of CH and other species, using ultra-high spectral resolution, which will reduce uncertainties in the analysis caused by systematic variations in excitation with radial velocity.'),('A121',1,'High velocity clouds: origin and environment','GIBSON','BRAD','Mount Stromlo & Siding Spring Observatories, Australian National University','High-velocity clouds (HVCs) are an important, but poorly understood componentof the Galactic halo. Our missing knowledge of their metallicities has been a major impediment in unlocking the mystery of their origin. With FUSE a metallicity determination will be possible by observing NI. At the same time, the properties of OVI absorption associated with the HVCs tell us about the relation between hot and neutral halo gas. Since few bright AGNs are projected on a HVC, the FUSE PI program will sample just two HVCs, which are not representative of the general population and thus the results may lead to a biased interpretation. We therefore propose to study metallicities and hot gas in the other HVC populations. Since the FUV flux is not known for any of the possible probes, we will first undertake a limited pilot survey of sightlines through several key HVCs which are not yet sampled. We will follow the identical strategy adopted by the D/H and Milky Way OVI PI programs and acquire 2 ksec exposure snapshots of 11 AGN, to verify our estimated FUV fluxes, from which the 3 highest quality candidates will be identified for subsequent high signal-to-noise (60,ksec) observations.'),('A123',1,'Colliding winds in hot, massive binaries','ST-LOUIS','NICOLE','Departement de physique, Universite de Montreal, Canada','We propose to secure a time sequence of ultraviolet (UV) spectra for aWR+O binary system to study the physical parameters and the structure of the bow shock zone formed when the winds of the two hot stars collide. Of particular importance in the {sl FUSE} UV range is the presence of a broad spread of emission lines with different ionization levels, ranging from O hinspace VI to C hinspace III. These lines are expected to arise in the bow shock zone at progressively larger distances from the X-ray heated bow head, as the compressed plasma flows outward along the shock cone and cools. The study of how these lines vary with orbital phase in the 14.9-day WC4+O5-6 LMC binary Br~22 will allow us to map out the structure and kinematics of the bow shock. This in turn will provide useful constraints on the basic parameters of the winds as well as the collision process itself. Br~22 is a particularly good example of a system in which wind-wind collision effects are known to be strong.'),('A126',1,'The evolution of disks and winds in dwarf nova outbursts','LONG','KNOX','Space Telescope Science Institute, USA','SS Cyg and U Gem are the ``prototypical\'\' dwarf novae. However, EUV and FUV spectra of the two systems in outburst are very different, probably due to the fact that the boundary layer luminosity of SS Cyg is much less than in U Gem. We propose to exploit these differences to isolate the wind and disk signatures in dwarf novae. By using FUSE to obtain multiple high S/N spectra of both systems through outburst, we will (1) probe the ionization and kinematic structure of the wind as a function of system brightness, (2) isolate the contributions of the disk to the FUV spectra, and (3) examine physical conditions and abundances of material just being accreted onto the disk from the secondary. FUSE studies of dwarf novae, coupled with detailed model comparisons, are crucial to a better understanding of disks and winds in non-magnetic cataclysmic variables.'),('A129',1,'Shocks in dense clouds in the Vela supernova remnant','NICHOLS','JOY','IPAC, California Institute of Technology, USA','We propose high resolution FUSE spectra to study a recently identified interaction of the Vela supernova remnant with a dense cloud region along its western edge. The goal is to quantify the temperature, ionization, density, and abundance characteristics associated with this shock/dense cloud interface. Our detection of high-velocity absorption line C~I at +90 to +130 km/s with IUE toward a narrow region interior to the Vela SNR strongly suggests the Vela supernova remnant is interacting with a dense ISM or molecular cloud. The shock/dense cloud interface is suggested by (1) the rarity of detection of high-velocity C~I seen in IUE spectra, (2) its very limited spatial distribution in the remnant, and (3) a marked decrease in X-ray emission in the region immediately west of the position of these stars where one also finds a 100 micron emission ridge in IRAS images. We would like to investigate the shock physics and general properties of this interaction region through a focussed UV absorption line study using FUSE spectra. FUSE is the only instrument that can obtain data that covers the tremendous range in density, temperature, and ionization that are expected. We propose to study the supernova remnant/cloud interaction using O VI coupled with IUE data, as well as several density and temperature line diagnostics in the FUSE range. H$_2$ absorption is also especially important to evaluate the molecular formation and abundances near the interface of the dense cloud.'),('A130',1,'Phase resolved studies of the magnetic A-star 17 Com (HD 108662)','RICE','JOHN','Department of Physics and Astronomy, Brandon University, Canada','We propose to make multiple phase resolved observations of the variable magnetic chemically peculiar star 17~Com~A to improve our understanding its far-UV continuum and line opacity. The fluxes at FUSE wavelengths are expected to be quite sensitive to abundance and temperature variations and to non-LTE effects. These observations will allow us to directly connect flux changes below 1200 AA to the known abundance variations over the stellar surface, and will allow us to test models produced from optical Doppler imaging methods. These will permit us to look for any significant sources of opacity which are absent from our calculations. We expect that this study will result in better determinations of photospheric structure and of the elemental abundances.'),('A133',1,'FUV diagnostics of structure in hot star winds','FULLERTON','ALEX','Dept. of Physics and Astronomy, University of Victoria, Canada','We propose to use the unique capabilities of {it FUSE} to monitor thetime-dependent behavior of the stellar wind profiles of an O4 supergiant in the Large Magellanic Cloud. These observations will enable us to: i) observe how of the state of wind material changes as it traverses structures in the wind; ii) perform a meaningful search for the high excitation, small scale shocks that are thought to generate the X-rays from O stars; and iii) determine how wind activity is affected by metallicity. Previous surveys and monitoring campaigns with {it IUE} and {it HST}have shown that stellar wind variability is both continuous and ubiquitous in the unsaturated P~Cygni profiles of Galactic OB stars. However, because the Si {sc iv} $lambdalambda$1400 doublet is the only unsaturated resonance wind line in early O stars available to these instruments, progress has been hampered in understanding the fundamental behavior of how the wind material evolves as it varies, and in studying the highest excitation wind structures. In contrast, the FUV region accessible to {it FUSE} contains a wealth of resonance line diagnostics which will enable us to study these topics.'),('A134',1,'Emission and absorption line studies of symbiotic binaries','ESPEY','BRIAN','Center for Astrophysical Sciences, Johns Hopkins University, USA','Symbiotic stars are binary systems consisting (generally) of a type K or M giant in orbit with a white dwarf companion. The short wavelength continuum of the white dwarf ionizes the outer atmosphere and wind of the giant, resulting in a rich nebular emission spectrum. The lines from this gas can therefore be used to diagnose conditions both close to the giant, and also in the extended shell of wind material. We propose to obtain emission and absorption line data on a sample of symbiotic binary systems. High resolution far-UV data will enable us to probe the physical conditions in the highest temperature emitting gas, to diagnose conditions in the tenuous white dwarf wind, and the irradiated giant wind. Absorption line data will enable us to probe the coolest gas in the binary systems, including molecular material close to the giant, as well as that in the circumbinary nebula. FUSE data will extend work begun with our analysis of HST, Orfeus and HUT data and will, for the first time, permit comparison of the UV and far-UV line profiles at comparable resolution. Temperature, density and abundance measurements using far-UV lines will provide the basis for improved models of these systems. '),('A139',1,'Tomographic diagnosis of the ionization cone in NGC 1068','ZHENG','WEI','Department of Physics and Astronomy, Johns Hopkins University, USA','Of all the Seyfert Galaxies, NGC~1068, by reason of its proximity, brightness and spatially extended ionization cone provides an ideal case for spectral and spatial diagnostic mapping aimed at determining the nature of excitation mechanisms. In particular, the far-UV lines of C {sc iii} $lambda 977$ and N {sc iii} $lambda 991$ provide a unique diagnostic capability, and can be used not only to separate between photoionization and shocks, but also to determine quantitative values of the parameters of such models. We know from earlier Hopkins Ultraviolet Telescope (HUT) observations that the NGC~1068 ionization cone is characterized by very high electron temperatures. The spatial resolution (close to HST) and the sensitivity of FUSE provide us with the only means of mapping the radial distribution of the electron temperature, and measuring the far-UV line flux data needed to uniquely determine the excitation mechanism. We propose to make maximum use of the FUSE capabilities to: (1) map the radial distribution of electron temperature in the C {sc iii} $lambda 977$ and N {sc iii} $lambda 991$ zones; (2) investigate \'hot spots\' thought to be the locations of ionizing shocks; and (3) study the spatial structure of the sharp boundary between high and low ionization zones. For this purpose, we propose a set of observations with different slit sizes and positions to provide an optimum compromise between spatial resolution and sensitivity in the different parts of the ionization cone. In addition, we will combine the FUSE, HST and optical data to provide a set of points on key diagnostic diagrams that we have developed to distinguish between shock and photoionization models. These data will be analyzed using the combined shock/photoionization code {it MAPPINGS II} to provide a realistic global model for the ionization cones. This study will have application to other AGN, and the data serve as a Seyfert template in studies of the unified model of AGN.'),('A149',1,'Coronal emission and mass loss in the hottest stars of the H-R diagram','BRUHWEILER','FREDERICK','Institute for Astrophysics & Computational Sciences/Physics, The Catholic University of America, USA','We will use FUSE to probe the relationship between mass loss and the ultra-high ionization emission and absorption seen in the pre-white dwarfs, the hottest stars (T$_{eff}$ $sim$ 100-170k K) in the H-R diagram. The presence of these ultra-high ionization species signifies temperatures far in excess of the stellar photospheres. Speculation provides two possible explanations for the ultra-high ionization features. First, uncertain wavelengths for the detected absorption suggest slight blue-shifts and that these features are formed in shocks at the base of the wind. Alternately, the simultaneous appearance of ultra-high ionization and lower ionization photospheric absorption might imply the stars are partially covered by \"hot spots\", which produce the ultra-high ionization features. A two component wind might also explain recent far-UV observations showing strong C~III and O~VI P Cygni features in NGC~246. We will observe five targets, RXJ~2117+3412, and the nuclei of NGC~5315, NGC~6905, NGC~6189, and NGC~2371-2. We will use FUSE time-tagged data to search for temporal variability in the O~VI $lambdalambda$1032,1038 and C~III $lambda$977 mass loss features and in the anticipated strong O~VIII $lambda$1165 emission. Since the time span of the FUSE observations should be comparable to the rotational period, any spectral variations due to spots should also be seen. Correlation or variability among the O~VI, C~III, and O~VIII features would represent a fundamental first test of any model. This study will ascertain if spherical geometry and steady-state modeling are even appropriate for modeling mass loss. We will also use non-LTE model atmospheres and spectral synthesis codes including the effects of winds to estimate elemental abundance patterns from lines of C, N, O, and Fe and mass loss rates from O~VI and C~III from the observed FUSE spectra.'),('A151',1,'FUSE spectra of Lyman series emissions from the interplanetary medium','CLARKE','JOHN','Space Physics Research Lab., University of Michigan, USA','Neutral atoms from the local ISM flow into the solar system producing diffuse emissions through resonant scattering of solar emissions. This wind contains the velocity distribution of the local ISM, plus modifications by solar gravity and radiation pressure near the Sun. In addition, the H atom motions are modified by charge exchange collisions with fast protons in the heliospheric interface region, while He atoms are little affected by charge exchange. Recent observations of the He and H flows in the solar system suggest that the He velocity of 26kms is that of the local ISM cloud, while the lower H velocity of 18-21kms and greatly increased velocity dispersion in the flow direction are due to an interface modification of the H flow. Remote observations of the H flow thereby provide a method to remotely study the heliospheric interface. The H flow has been studied from H {lya} line profiles at high spectral resolution observed by Copernicus, IUE, and HST, using the Earth orbital motion to Doppler shift the ISM from the geocoronal emission. One serious ambiguity in the interpretation of these data results from the optically thick {lya} emission, leading to uncertainties in derived values of the H density. Using FUSE to observe the brightness and line profile of the optically thin H lyb line, close in time to SOHO observations of the {lya} emission, we can determine accurately the optical depth and density n(H) along lines of sight upwind, downwind, and cross-flow. Comparing n(H) with the heliospheric helium density, and with the interstellar cloud HI/HeI ratio measured recently by the EUVE, will give the fraction of H atoms removed by charge exchange at the entrance to the heliosphere, and then the Local Cloud (or ambient ISM) electron density which governs the size of the heliosphere. We request FUSE sky aperture spectra in the two narrow science apertures obtained during other pointed observations, through cooperation in scheduling pointed observations in the correct look directions at the proper times of year.'),('A152',1,'FUV observations of a supernova to be named later','KIRSHNER','ROBERT','Harvard College Observatory, Harvard University, USA','We propose observing a newly-discovered supernova with FUSE as a target of opportunity. Our experience with HST and IUE ultraviolet spectra shows how informative they can be. With FUSE, we can explore a previously unobserved part of the spectrum where many important lines will help in building a complete picture, especially of circumstellar interactions. The resolution of FUSE is excellent for this purpose because it neatly separates circumstellar features from interstellar lines and the ability to move promptly to a good target is a very large advantage over HST. A recent example of a type~II, SN 1998S, illustrates what a STIS spectrum can (and cannot) do, and gives us a solid basis for predicting what is required for measurements with FUSE. We hope to continue our HST Target-of-Opportunity program, and we would aim to combine our FUSE observations both with our ground-based data and with STIS data. The probability of having one suitable target per year is high.'),('A153',1,'Investigating the excitation mechanism for cometary X-ray, EUV, FUV emission','WEAVER','HAROLD','Department of Physics and Astronomy, Johns Hopkins University, USA','We propose using FUSE to address two fundamental issues in cometaryscience: the nature of the X-ray, EUV, and FUV emissions from comets and the D/H ratio. We will use FUSE to make a sensitive search for line emission from OVI and other highly ionized species in a suitably bright comet mbox{($m_{0} leq 7$)} observed as a Target of Opportunity. The presence of these emissions at the predicted brightnesses would provide unambiguous evidence that charge exchange of solar wind ions with cometary neutrals is the dominant source of x-rays in comets. FUSE is the only observatory with sufficient spectral resolution and sensitivity to detect these faint line emissions. If the comet has mbox{$m_{0} leq 6 $}, we also propose searching for the Ly-$eta$ lines of D and H, as the deuterium abundance is an important indicator of cometary formation conditions. Accurate determinations of the D/H ratio in many comets are needed to determine whether or not they could have supplied most of the water currently present on the Earth. '),('B001',2,'Central Stars of Planetary Nebulae in the Large Magellanic Cloud','BIANCHI','LUCIANA','The Johns Hopkins University','We propose to observe with FUSE a sample of Planetary Nebulae in theLarge Magellanic Cloud for which we have analysed HST UV and optical spectra. The flux is dominated by nebular continuum in the HST range. Instead, the far-UV spectrum will provide a direct measurement of the stellar continuum, enabling a better measurement of stellar temperature and absolute luminosity, useful to refine post-AGB evolution and nebular ionization modeling. The FUSE spectra will also reveal the hottest layers of the stellar wind, yielding an accurate measurement of the terminal velocity and mass loss rate, which is important to model the nebular dynamics, and to understand the central stars properties and evolution. The H_2 transitions in the FUSE range provide a powerful way to measure the circumstellar molecular gas, which - added to the mass of the central star, and of the ionized shell previously determined, will allow us to test theoretical initial-final mass relations. The far-UV data will be a unique and valuable contribution to constrain the stellar and nebular properties of these objects, which are effectively at a single, unambiguous distance.'),('B003',2,'Probing the Local Bubble-halo connection through the Local Interstellar Chimney','WELSH','BARRY Y.','UC Berkeley','We shall probe the ionization state and kinematics of the lowerhalo-Local Bubble interaction region using hot white dwarf stars of known, increasing distance away from the galactic plane up to z sim 0.3 kpc that of neutral gas. Our main goal is to obtain better constraints on the location of the hot gas of the Local Bubble and the associated conductive interfaces. We shall also search for signs of the infall or outflow of neutral andor ionized gas in this particular region (which could be related to a galactic fountain), and investigate the way the kinetic temperature, electron density, element abundancesdepletions and gross velocity structure of gas in the Local Bubble varies as a function of increasing height above the galactic disk as it merges into the lower galactic halo.'),('B004',2,'The Far-UV Spectra of Powerful Starbursts','HECKMAN','TIMOTHY','Johns Hopkins University','Starbursts are a significant component of the present-day universe,and offer unique laboratories for both studying the processes that have regulated the formation and evolution of galaxies, and for testing models of high-mass stellar evolution. We propose to exploit the unique strengths of FUSE to obtain high-resolution (15 to 20 km s^-1) high quality SN sim 10) spectra of the four most powerful UV-bright starbursts in the local universe. These have bolometric luminosities comparable to the Lyman Break galaxies at z sim3. Together with the lower-power starbursts observed by FUSE in Cycle 1, the sample will span nearly the entire ranges of luminosity and metallicity seen in local starbursts. The spectra will be used to study 1) the coronal-phase gas that may dominate the energetics of starburst-driven superwinds 2) the H_2 that probably dominates the ISM mass and regulates the star-formation ) the starburst dust-attenuation law in the unexplored FUV window 4) the stellar content of the starburst (thereby probing the IMF and burst history). The relatively large FUSE apertures allow us to obtain high-resolution spectra of nearly the entire starburst (rather than small pieces, as with HST and STIS).'),('B006',2,'Far-UV Spectroscopy of Scorpius X-1','BOROSON','BRAM','NASA Goddard Space Flight Center','We propose to investigate the mass transfer in the important Z sourceX-ray binaries by resolving the far-UV emission lines in Scorpius X-1 to reveal Doppler-shifted velocities. The far UV region contains strong emission lines that are sensitive to X-ray illumination and provide valuable diagnostics of physical conditions in the accretion disk. We will use the strengths of ionO6, ionC3, and ionN3 lines as density, temperature, optical depth, and abundance diagnostics. Covering an entire 0.787 day binary orbit will allow us to look for orbital Doppler shifts and to apply the method of Doppler tomography. We will search for variability on time scales of seconds, resulting, for example, from reprocessing of an X-ray flare by the accretion disk.'),('B008',2,'Far-UV Spectroscopy of Hercules X-1','BOROSON','BRAM','NASA Goddard Space Flight Center','HerculesX-1 is the prototypical X-ray binary pulsar, and isfortuitously located behind a very low column density of absorbing gas. We propose to observe the far UV spectrum continuously for a complete binary orbit. From our previous HSTSTIS observations, we expect to be able to separate broad and narrow emission line components, probably due to the accretion disk and X-ray heated atmosphere of the normal star. Concentrating on the O 6 doublet will allow us to probe higher degrees of X-ray ionization than the lines seen with STIS, and with the larger wavelength separation of the doublets, there will be less of the confusing overlap presentin the STIS spectra. From the data, we will form Doppler tomograms, search for evidence of a stellar wind driven from the companion or the accretion disk by X-ray heating, and look for reprocessed pulsations or UV quasiperiodic oscillations. We can measure temperatures using the C,IIIlambda977,1176 lines and densities using the ionN3lambda990 Bowen line.'),('B010',2,'Mapping Hot Gas in a Pristine H, sc ii Region','CHU','YOU-HUA','University of Illinois','The H,sc ii region N11B in the Large Magellanic Cloud (LMC) containsan OB association that is dominated by main-sequence members and contains several O3 stars, the most massive of stars. The velocity dispersion of the 10^4 K ionized gas in N11B is among the smallest in LMC H,sc ii regions. The stellar content and gas kinematics suggest that N11B is a pristine H,sc ii region in which no supernova explosion has occurred. Thus, N11B provides an ideal site to study the interaction between fast stellar winds and the interstellar medium (ISM). medskip We request FUSE observations of nine stars in N11B. These nine stars span a large spatial coverage along the E-W direction and a wide range of spectral types from O3 to B1. Only one of the stars, an O5.5V, is surrounded by a visible ring nebula, indicating the existence of a wind-blown bubble. The FUSE observations of the O,sc vi lines will allow us to map the distribution of hot gas in N11B and to study how fast stellar winds interact with the ambient ISM. We also request an observation of a comparison target in a neighboring superbubble to diagnose possible spillover of its hot gas and large-scale foreground ISM structures at the same velocity.'),('B013',2,'A Systematic Study of Colliding Winds in Wolf-Rayet (WR) Binaries. I. Carbon-Rich WR stars.','ST-LOUIS','NICOLE','Universite de Montreal','We propose to secure a time sequence of ultraviolet (UV) spectra for aseries of WR+O binary systems to study the physical parameters and the structure of the bow shock zone formed when the winds of the two hot stars collide. Of particular importance in the sl FUSE UV range is the presence of a broad spread of emission lines with different ionization levels, ranging from Othinspace VI to Cthinspace III. These lines are expected to arise in the bow shock zone at progressively larger distances from the X-ray heated bow head, as the compressed plasma flows outward along the shock cone and cools. The study of how these lines vary with orbital phase in a selection of WCWO binaries will allow us to map out the structure and kinematics of the bow shock for a broad variety of systems. This in turn will provide useful constraints on the basic parameters of the winds as well as the collision process itself. The 5 systems proposed are known from optical data to show strong wind-wind collision effects.'),('B015',2,'Supersoft X-ray binaries','CRAMPTON','DAVID','HIA, NRC of Canada','This is a continuation of a program assigned time in cycle 1. Wepropose to obtain phase-resolved FUSE spectra of two supersoft X-ray binaries, achieving SN >10 over 1 - 2AA in orbital phase bins of leq0.1P. The emission line features in the FUSE wavelength range cover a wide range of ionization giving a unique dataset for determination of the binary parameters, component masses, and disk structures which cannot be provided by optical and HST data. The O VI lines may provide unique measures that define the stellar masses. We will also use the combined data for each system to detect and measure high-velocity lines from bi-polar jets which are seen in the optical spectra of one system. High-ionization lines from these jets are of particular interest since they are formed in the innermost region where the jets are undergoing their collimation and acceleration. An improved understanding of jets has wide astrophysical implications. '),('B016',2,'Far ultraviolet spectra of classical X-ray binaries','HUTCHINGS','JOHN B.','HIA, NRC of Canada','We propose to obtain binary-phase-resolved FUSE spectra of threeclassical X-ray binaries (Sco X-1, X1822-37, and LMC X-3) through their orbital cycles. Each of these systems is the prototype of its type of system, and each has unsolved problems associated with it. The optical and ultraviolet spectra of the first two are dominated by an accretion disk. The third, LMC X-3, contains a luminous B supergiant, whose light is dominant in the visible, but opticalUV data also reveal the presence of a large accretion disk. FUSE data will allow study of these disks over a wide range of temperature and density, hence revealing physical properties of these accretion disks and kinematics of the gas.'),('B018',2,'Molecular and atomic hydrogen, abundances and stellar content in giant extragalactic HII regions','LEQUEUX','JAMES','Observatoire de Paris','FUSE offers the unique possibility for obtaining far-UV spectra in thedirection of giant HII regions in nearby galaxies. The ionizing star cluster is a far-UV source, and the interstellar matter in front will produce absorption lines of H, H_2 and various atoms and ions. We will obtain the H_2H ratio, the HDH_2 ratio, the COH_2 ratio, the dustgas ratio as well as the abundances of various ions, and an integrated spectrum of the ionizing cluster which will be compared to our evolutionary models. We have already tested this technique by observing with FUSE the ionizing cluster of the blue compact galaxy I Zw 18. We wish to observe 8 targets having radial velocities differing by more than 130 km s^-1 from those of the Galactic interstellar gas. For these targets, the lines will be well separated from the galactic absorption lines.'),('B022',2,'The Interstellar Medium of Blue compact dwarf galaxies','THUAN','TRINH XUAN','University of Virginia','Blue compact dwarf (BCD) galaxies are metal-deficient and thusconstitute excellent nearby laboratories for studying how the properties of the interstellar medium (ISM) in galaxies change with metallicity. Our sample consists of 4 BCDs chosen to span the metallicity range from 15 to 12 of the solar metallicity. This sample will extend the metallicity range covered by our Cycle 1 observations (141 to 110 solar). The proposed FUSE observations will allow us to investigate the 1) H_2 content of BCDs as a function of metallicity. No H_2 line has been detected in the 2 very metal-deficient BCDs which have been observed by FUSE so far. Will diffuse H_2 be present in more metal-rich BCDs and with less UV radiation density? 2) the structure of the ISM in BCDs. Analysis of 2 BCDs observed by FUSE in Cycle 1 (IZw18 and Mrk 59) show that in the first, the ISM appears to be relatively homogeneous while in the second, it is very clumpy. What are the factors which determine the gas clumpiness in BCDs 3) the abundances in the ISM. Analysis of the FUSE spectrum of Mrk 59 showed C, N, O, Si, Fe and S absorption lines which allow to derive abundances in the ISM using photoinization models. How do these abundances compare with the abundances derived from the emission-line optical spectra? 4) the evolutionary history and stellar winds in BCDs by detecting the P Cygni profiles of high ionization S VI and O VI lines.'),('B023',2,'FUSE Observations of WC-PG1159 Central Stars of Planetary Nebulae','PERINOTTO','MARIO','Universita di Firenze','We propose to observe three central stars of planetary nebulae tostudy their winds, and perform a detailed atmospheric comparison. Groundbased and IUE observations show these stars, A30, A78, and Lo-4, to be nearly identical in temperature, radius, and masss, although IUE spectra show very different wind characteristics. The limitations of the previous UV observations, the lack of O IV and/or lack of O V 1371AA P Cyg, will be addressed with the FUSE observations. We will perform detailed analysis of the photospheres and winds of these stars using the latest version of PHOENIX. Finally, we will also include analyses of four similar stars for which IUE spectra are available but that are already FUSE targets PI targets NGC 1535, NGC 7094, and IC 3568, and the Cycle 1 GO target NGC 6210.'),('B025',2,'Fine structure in interstellar H_2 clouds seen against an open star cluster','MARGGRAF','OLE','Universitat Bonn','The physical conditions in extended molecular clouds are still notwell known. Most of our knowledge is based on CO emission, widely used to map the structure of molecular gas. Since there is no H_2 emission available from the cold cores of molecular clouds, the H_2 abundance is usually calculated by linking it to that of CO. Direct observation of H_2, the most abundant molecule in the universe, could provide information on the physical state in the core of a molecular cloud and on the spatial variation of this physical state over small scales. We plan to observe a sample of seven sightlines towards the Galactic open cluster NGC6231. The small angular separation of the target stars of overall 5.8arcmin will be used to examine the structure of the molecular interstellar medium down to scales of less than 0.3pc. Physical parameters like abundances of H_2 and various metals, depletions, temperatures, electron densities, and the level of radiation will be determined and their spatial variation will be examined.'),('B029',2,'Small-Scale Interstellar Structure Toward the Open Cluster chi Persei','MEYER','DAVID M.','Northwestern University','We propose to obtain FUSE observations of the interstellar H_2 and CIabsorption toward six early-type stars in the core of the open star cluster chi Persei. High-resolution optical observations of the interstellar Na I absorption toward these stars and others in the core of chi Per have revealed a rich variety of small-scale diffuse ISM structure in both the distant Perseus and more local Orion spiral arms. At the approx. 1arcmin scales typically probed by these stars, this structure corresponds to respective physical length scales of 0.6 and 0.15 pc in the Perseus and Orion arm gas. By comparing the abundances and excitation of H_2 and CI in these six closely-spaced chiPer sightlines, we plan to (1)investigate the possibility that the high-velocity NaI structure is associated with a density-wave shock interaction with gas on the inner edge of the Perseus arm, and (2)study the physical character of the small-scale Orion arm structure that seems to be evident not only in the NaI lines but also the lambda5797 diffuse interstellar band.'),('B030',2,'Effects of Star Formation and Stellar Death on Interstellar Gas Associated with Cep OB2','FEDERMAN','STEVEN R.','Univ. of Toledo','Interstellar clouds that give birth to stars are subsequently affectedby those stars. In particular, massive stars, through their stellar winds, intense ultraviolet radiation, and their terminal supernovae explosions, contribute to the dispersal of the clouds and seed the clouds with newly synthesized elements. In order to understand the details of cloud dispersal, on the one hand, and chemical evolution, on the other, in a site of star formation, the interstellar material toward stars in Cep OB2 will be probed through a study of absorption lines. After three episodes of star formation, the material in front of Cep OB2 is all that remains of the original molecular cloud. Analysis of H_2 absorption will yield information on the physical conditions for the material; gas temperature and incident ultraviolet flux will be extracted from the measurements. These derived quantities will help constrain models of the evolution of interstellar clouds on Galactic scales. A search for the F small I resonance line at 954 AA will establish the interstellar F abundance, which may be used to resolve the origin of this element is F synthesized primarily in Type II supernovae, whose effects should be revealed in a region of ongoing massive star formation, or in asymptotic giant branch stars'),('B032',2,'Hot Gas in Planetary Nebulae','GRUENDL','ROBERT','University of Illinois','Planetary nebulae (PNe) are formed by the interaction between the faststellar wind and a previous slow wind. In this interacting stellar wind model, the fast stellar wind which fills the PN interior is shocked and heated to X-ray-emitting temperatures. On the other hand, ROSAT observations of 80 PNe show indications of emission from a 10^6K plasma in only 6 PNe. Chandra has observed 3 of these PNe and 2 of them, BD+30^circ3639 and NGC,6543, have finally been resolved and show that hot gas fills their central cavities. Thus, to date the presence of 10^6K hot gas has only been unambiguously detected in two PNe. smallskip The deficit of detections of X-ray emission from PNe suggests that the PN interiors may have a lower temperature. Heat conduction processes, and the mixing and evaporation of the cold dense nebular material into the hot interior will enhance the cooling rate and might account for the temperature drop of the PN interiors. The determination of the physical structure and state of the hot gas in the PN interiors is necessary to address the details of the interaction of the winds (including the interface physics) in order to understand the physical structure and evolution of PNe. smallskip We propose to observe the nebular absorption of OVI against the spectrum of the PN central star to probe the physical conditions of PN interiors. Whereas the nebular absorption lines of CIV and NV can be produced by photoionization from the hot central star of PNe, the OVI lines offer a reliable diagnostic of the presence of sim3times10^5K gas for central stars as hot as 125,000K. These lines can only be observed by FUSE.'),('B033',2,'A test of Pulsation Theory in Hot B Subdwarfs','FONTAINE','GILLES','Universite de Montreal','There are currently of the order of 15 hot B subdwarf (sdB) starswhich are known to exhibit low-amplitude (a few to tens of millimag), short-period (100-500 s), multiperiodic luminosity variations. These pulsations are thought to be driven by an opacity bump linked to the presence of a local enhancement of the iron abundance in the envelopes of sdB stars. Such an enhancement results quite naturally from the diffusive equilibrium between gravitational settling and radiative support in the stellar envelope. Nevertheless, surveys for pulsating sdB stars show that, in several instances, variable and non-variable objects with similar effective temperatures and gravities may coexist in the HR diagram. This result suggests that an additional parameter, perhaps a weak stellar wind, might affect the extent of the iron reservoir and thus the ability of the latter to drive pulsations in sdB stars. Fortunately, it is expected that such a wind might also leave its mark on the photospheric heavy element abundance patterns. The intended FUSE observations will i) permit a direct comparison of the heavy element abundance patterns in variable and nonvariable stars of similar atmospheric parameters; ii) provide a consistency check with our wind models; and iii) provide a test of the currently-favored explanation for the driving of the observed pulsations.'),('B034',2,'The origin of peculiar UV line ratios in the Magnetic Cataclysmic Variable AE Aqr','MOUCHET','MARTINE','Observatoire de Paris, Section de Meudon','We propose to observe the atypical Magnetic Cataclysmic Variable (MCV)AE,Aqr which is one of the few systems showing anomalous UV emission line ratios. The far-UV spectra will provide a crucial test on whether this system is characterized by peculiar ionization conditions or by anomalous non-solar abundances. The measurements of the resonance OVI emission line, combined with those of the NIII and CIII lines, will provide strong clues to discriminate between these different possibilities. Other hallmarks of AE,Aqr are its extreme strong flaring activity, and a unique spectrum extending from TeV to radio wavelengths likely due to the propeller mechanism related to the fast magnetized white dwarf spin (33 sec). A total on-source exposure time of 40 ksec, will allow us to study the phase-resolved far-UV spectrum along the rotational and orbital (9.98 hr) periods in order to constrain the temperature and structure of the accretion-heated polar regions of the white dwarf. We will also observe for the first time far-UV flares which will provide further parametrization of the active regions thought to be produced by blob impacts at the magnetosphere.'),('B038',2,'High temperatures and disks around PMS stars FUSE Spectra of Three Herbig AeBe Stars','CATALA','CLAUDE','Observatoire Midi-Pyrenees','Previous optical and UV (IUE & HST) observations have shown that theintermediate mass PMS Herbig AeBe stars possess strong stellar winds and dense chromospheres. These winds and chromospheres are the seat of active variable phenomena, most likely linked to surface magnetic fields. Detailed models of the outer atmospheres of these stars have been constructed, and predict that the Lybeta line at 1025 AA and the C III resonance line at 977 AA must appear with an intense emission component. We intend to check this prediction with FUSE observations, and take advantage of the observed fluxes and profiles to further constrain the models of these stars. In addition, we will also search for the presence of H_2 absorption bands between 950 and 1150 AA, which are expected if these stars are surrounded by massive accretion disks.'),('B039',2,'Carbon, Nitrogen, and Helium Abundances in Planetary Nebulae','KWOK','SUN','University of Calgary','We propose to use FUSE to obtain high resolution spectra of 5planetary nebulae. The FUSE spectral range contains lines from 3 different ionization stages of carbon, allowing for a much better determination of the ionization correction factors necessary for accurate abundance determination. The carbon abundance in planetary nebulae is crucial in the testing of nucleosynthesis models and dredge-up theories on the AGB. FUSE provides a unique opportunity to test these models. We have chosen both type I and type II planetary nebulae for this study, as the latter group in particular are expected to have unusual abundances of the CNO elements. The FUSE observations will also provide some data on the N and He abundances for these higher excitation nebulae.'),('B043',2,'Probing Shocks and Winds in the Peculiar Binary Star VSagittae','WOOD','JANET','San Diego State University','VSge is an extremely unusual close binary. Once thought to be relatedto CVs or LMXBs, it is now suggested to be a colliding wind system. If so, with its 12.3 hr period, it is the shortest orbital period colliding wind system known. It appears to be undergoing a short-lived phase of evolution, and may be in the very final stages of common envelope evolution. VSge shows high and low photometric states, possibly related to its evolutionary state, in which the spectroscopic behaviour changes dramatically. High resolution, phase-resolved UV spectra have been studied previously in the low state but no such observations exist for the high state and there are no published observations in the FUSE FUV wavelength range. Still-unexplained phenomena occur in VSge which need to be investigated before the colliding wind model can be firmly established, including the mechanism causing the high and low states. We speculate that this mechanism is related to a change in wind behaviour but this idea needs to be tested by observing and modeling the wind line profiles around the binary orbit in both states. We therefore propose to obtain orbital phase-resolved FUSE spectra of VSge in two epochs. With its rich spectrum of wind emission lines at a variety of abundances and ionization states, FUSE will allow us to model the structure and kinematics of the stellar winds and the shock front in the binary and probe a new regime of stellar wind collisions in evolved close binary systems.'),('B045',2,'Far-Ultraviolet Spectra of a Supernova to be Named Later','KIRSHNER','ROBERT P.','Harvard University','We propose using FUSE to observe a newly-discovered supernova duringCycle2 as a target of opportunity. Our experience with HST and IUE ultraviolet spectra shows how informative they can be. With FUSE, we can explore a previously unobserved part of the spectrum where many important lines will help in building a complete picture, especially of circumstellar interactions. The resolution of FUSE is excellent for this purpose because it neatly separates circumstellar features from interstellar lines and the ability to move promptly to a good target is a very large advantage over HST. A recent example of a typeII, SN 1998S, illustrates what a STIS spectrum can (and cannot) do, and gives us a solid basis for predicting what is required for measurements with FUSE. We hope to continue our HST Target-of-Opportunity program, and we would aim to combine our FUSE observations both with our ground-based data and with STIS data. The probability of having one suitable target per year is high, but not unity. In Cycle 1, we exercised restraint because there was not a suitable target for FUSE. We hope for better luck in Cycle 2.'),('B046',2,'The Physical Character of Small-Scale Interstellar Structures','LAUROESCH','JAMES','Northwestern University','Recent optical and radio studies have found convincing evidence forpervasive small-scale structure in the diffuse ISM on 10-10^4 AU scales. The seemingly ubiquitous existence of such small, dense pockets of gas in the diffuse ISM is an important puzzle since the inferred over-pressures of these clumps imply lifetimes of only a few thousand years before they should diffuse away. Measurements and comparisons of the interstellar absorption line profiles towards members of resolvable binary star systems with FUSE can greatly expand our knowledge of the physical conditions and abundances in these clumps. Therefore, we propose to obtain FUSE observations of the interstellar H_2 absorption lines towards six members of three multiple star systems of varying separations with the goal of deriving accurate densities, temperatures, and radiation fields for the clouds associated with the observed small-scale structures in these sightlines. By using the many lines of H_2, we can determine if these clumps are indeed as dense as they appear and discriminate between competing models for the origin of these features.'),('B047',2,'Accretion Onto Magnetic White Dwarfs','SZKODY','PAULA','University of Washington','We will observe the far UV emission of the highest field (230 MG)magnetic cataclysmic variable AR UMa and of the typical field (30 MG) polar VV Pup in order to confront theories of buried shocks and accretion heating. A measurement of the far-UV flux in AR UMa will help to resolve ambiguities in our HST data about the field strength and the heating of the white dwarf under extreme field conditions. In VV Pup, the ability to directly view the white dwarf, combined with a simple geometry where the primary pole rotates behind the white dwarf for part of its short orbital period, allows a clear separation of the contributions of the unheatedheated white dwarf and the accretion funnel. The high resolution and large excitation range of lines covered by FUSE allows the delineation of the composition, temperature, density and velocity of the line-forming regions in the accretion funnel and at the photosphere of the white dwarf. The analysis of FUSE data on the 2 very different systems AR UMa and VV Pup will provide a clearer understanding of the conditions of magnetic accretion and their ultimate effect on the underlying white dwarf.'),('B048',2,'Understanding the Enigmatic SW Sex Stars','SZKODY','PAULA','University of Washington','The SW Sex stars are a subgroup of cataclysmic variables that areknown for several peculiar features, including high excitation single-peaked lines in their spectra, absorption features in the low excitation lines, phase offsets between the radial velocity curves and photometric eclipse times, unusual high velocity components, and orbital periods between 3-4 hrs. The cause of these peculiarities is controversial, with possibilities ranging from mass transfer stream impact and overflow at high mass transfer rates to magnetic propellers, winds and jets. As many of these suggestions depend on the inclination of the system, we propose to confront such theories by contrasting FUSE observations of the low inclination SW Sex star LS Peg and a more typical high inclination system DW UMa. The high quality, high resolution FUSE spectra we will obtain will allow us to construct detailed models of the inner accretion disk and velocity flows of both systems. This will resolve which of the properties are geometry dependent, and thereby lead to a basic advance in our understanding of this class of objects and ultimately, of the general effects of high mass transfer in close binaries.'),('B050',2,'Investigating the Excitation Mechanism for Cometary X-Ray, EUV, and FUV Emissions and the D/H Ratio','Weaver','Dr. Harold','Johns Hopkins University','We propose using FUSE to address two fundamental issues in cometary science - the nature of the X-ray, EUV, and FUV emissions from comets and the D/H ratio. We will use FUSE to make a sensitive search for line emission from O VI and other highly ionized species in a suitably bright comet (V <= 7) observed as a Target of Opportunity. The presence of these emissions at the predicted brightnesses would provide unambiguous evidence that charge exchange of solar wind ions with cometary neutrals is the dominant source of x-rays in comets. FUSE is the only observatory with sufficient spectral resolution and sensitivity to detect these faint line emissions. If the comet has V <= 5, we also propose searching for the Ly-beta lines of D and H, as the deuterium abundance is an important indicator of cometary formation conditions. Accurate determinations of the D/H ratio in many comets are needed to determine whether or not they could have supplied most of the water currently present on the Earth.'),('B051',2,'Surface Abundance Pattern of Accreting White Dwarfs in Non-Interacting Close Binaries','VENNES','STEPHANE','Australian National University','Our HST GHRS investigation of white dwarfs in the EUV-selected closebinaries EUVE J0720--317 (WD0718-316), EUVE J1016--053 (WD1013-050), and EUVE J2013+400 (WD2013+400) revealed photospheric abundances of helium and carbon much larger than measured in isolated white dwarfs with similar parameters. This peculiar abundance pattern bears the signature of diffusive equilibrium supplied by accretion from a close red dwarf companion. Additional evidence for the accretion scenario emerged with the discovery of V471 Tau-like EUV variability in EUVE J0720--317 and J1016--053, which suggests abundance inhomogeneities across the stellar surface. We propose to obtain high quality FUSE spectra of these three binaries and secure abundance measurements of He, C, Si, P, and S. The data will enable a study of the distinctive roles played by accretion and selective radiation pressure. Because selective radiation pressure on He and Si is inefficient, their abundance is determined by steady-state equilibrium between the accretion flow and downward diffusion and holds a ratio of log(SiHe)-3.7, while the abundance of C, P, and S should be determined by radiation pressure correlated with effective temperature. We also propose to study the surface abundance pattern of the white dwarf in EUVE J0720--317 with a series of spectra resolving the rotation phase. The data will also improve orbital parameters initially established in GHRS measurements.'),('B052',2,'THE EVOLUTIONARY LINK BETWEEN CSPN AND DA WHITE DWARFS','BARSTOW','MARTIN','University of Leicester','We propose FUSE observations of a sample of central stars of oldplanetary nebulae to study the evolutionary link between them and the H-rich DADAO white dwarfs. Analysis of the H Lyman and OVI resonance lines provides a unique determination of T_eff and log g for each star, taking into account the heavy element abundances, which are known to affect the temperature determination. We will measure detailed element abundances from the metal line strengths in the high resolution FUSE spectra. Importantly, FUSE gives us access to absorption lines of several species which cannot be studied in any other wavelength range. From this work, combined with observations of a smaller number of related PI targets, when they appear in the public archive, we will re-establish the temperature scale for these stars and compare their compositions with their supposed white dwarf descendants. A search for ongoing mass-loss will be carried out, looking for P-Cygni signatures in the CIII and OVI resonance lines. Evidence of current activity might explain the discrepancies often observed between the PN kinematic ages and the stellar evolutionary timescale.'),('B053',2,'TEMPERATURE, GRAVITY AND COMPOSITION OF DAO WHITE DWARFS','BARSTOW','MARTIN','University of Leicester','We propose FUSE observations of a sample of DAO white dwarfs to studytheir relationship with the DAO central stars of planetary nebulae and the DA white dwarfs, where helium is not, or no longer, present. We will analyse the H Lyman lines, providing a unique determination of T_eff and log g for each star, taking into account the heavy element abundances, which are expected to significantly affect the temperature determination. These abundances will be determined from the heavy element lines detected in the high resolution FUSE spectra. This is particularly important for species which cannot be detected in any other wavelength range. With the improved accuracy of self-consistent determinations of elemental abundances and T_eff we will be able to compare the compositions with the CSPN and DA white dwarfs. With multiple exposures spread across several orbits, we will be able to use the strongest of the narrow metal lines detected to check for evidence of binarity.'),('B055',2,'The fundamental parameters of white dwarfs in Sirius-type binary systems','BURLEIGH','MATTHEW','University of Leicester','We will use FUSE to accurately determine the fundamental parameters(T_eff , log g, radius and mass) of a sample of white dwarfs in Sirius-type binary systems. Far-ultraviolet spectroscopy of the H Lyman series is the only means available to achieve this goal. We will then use the mass determinations to investigate the initial-to-final mass relation for white dwarf stars. In addition, Hipparcos provides us with well constrained parallaxes for many of the primaries in this sample. We will use this data, together with the parameters determined with FUSE, to retrieve the stellar masses and hence test the white dwarf mass-radius relation, in particular the high mass end. Finally, we will search for evidence of elements heavier than He in these stars photospheres and in the circumstellar environment, and determine their abundances. This proposal is complimentary to our Cycle 1 program (A054, PI Burleigh), in which we are observing 11 targets with T_eff >= 35,000K. We now seek time to observe those systems with cooler white dwarf secondaries, T_eff <= 35,000K. We note that some of these systems have been resolved in our complimentary HSTWFPC2 UV-imaging program, and within a few years we will be able to derive astrometric masses for the white dwarfs in several cases.'),('B056',2,'The Truth About Cooling Flows in Elliptical Galaxies','BREGMAN','JOEL','University of Michigan','The most fundamental quantity needed to understand cooling flows inelliptical galaxies is the rate that gas cools from the hot million degree state to the warm ionized or neutral state. In AO1, we measured this rate to be about an order of magnitude lower than the cooling flow prediction in two elliptical galaxies. If generally true, this will lead to a major revision of the model, and here we propose observations to determine the cooling rates in a complete sample of nearby ellipticals. Together with X-ray and optical observations, the FUSE data will determine which alternative models are at work, such as those where much of the gas is flowing outward rather than inward.'),('B058',2,'Far UV Spectroscopy of the VV Cep System KQ Pup','GONZALEZ-RIESTR','ROSARIO','INTA','KQ Pup is one of the most representative examples of the VV Cep binarysystems. It is an spectroscopic, non--eclipsing, binary with a period of 26.7 years. The UV spectrum is dominated by the continuum of the hot star (presumably B0V), with two types of lines superimposed on it narrow absorptions --with or without red emissions-- of singly ionized elements, and broad absorptions of resonance lines with a wide ionization range and of excited lines of doubly ionized metals. The orbit of the system is very eccentric, and therefore a strong enhancement of the interaction effects is expected associated to the periastron passage, which took place in May 1999. Conjunction (M supergiant in front of the B star) will occur during the period covered by the FUSE Cycle 2. In this geometrical configuration we will able to see the side of the B star facing the M supergiant, as well as a signature of a possible eclipse (not observed so far) by the extended M--star atmosphere or by its inner wind. The FUSE data will provide a deeper insight into the nature of the hot star and a better determination of the complex geometry of the line forming regions.'),('B060',2,'A Study of the Atmospheres of the Main Sequence B Stars','FITZPATRICK','EDWARD L.','Villanova University','We request observing time with FUSE to obtain far-UV spectra of 5mid- to late B-type main sequence stars (BVs) in the Orion OB1 association. These data will be part of a comprehensive investigation of the ability of current model atmosphere calculations to reproduce the observed properties of the BVs, including the overall energy distributions and the detailed absorption line spectra. This study will provide a benchmark and a reality check for studies of more exotic early-type objects, since the BVs are the hottest and most luminous stars whose atmospheres can be modeled with simple assumptions, such as LTE, plane-parallel geometry, and hydrostatic equilibrium. The targets span a T_eff range of 11000--17000 K, a vsini range of nearly 400 km s^-1, are lightly reddened to minimize the impact of the ISM, and are located in a relatively small volume of space to minimize differential extinction effects. The sample is large enough to allow general conclusions to be drawn and to distinguish individual peculiarities from general trends. This program will produce a valuable archive of uniformly high quality far-UV spectra uncompromised by interstellar absorption and spanning a stellar temperature range within which the 900-1200 AA flux constitutes a significant fraction of the total emitted stellar energy and is extraordinarily sensitive to stellar atmosphere conditions. These data will be ideal for evaluating the success of current stellar atmosphere calculations and examining the effect of rapid rotation on the far-UV energy distributions of the BV stars.'),('B062',2,'FUV Spectroscopy of Narrow Line Seyfert 1 Galaxies','MATHUR','SMITA','The Ohio State University','We propose FUSE observations of two bright well-studied narrow-lineSeyfert 1 galaxies (NLS1s), Akn 564 and NGC 4051, to determine the properties of the emission lines, absorption lines, and the continuum in the FUV region of this important class of AGNs. The FUV bridges an important gap between the UV and soft X-ray regions, both in terms of wavelength and in terms of ionization states of key elements in the emission and absorption-line regions. The proposed observations will enable us to determine the physical conditions from a few to a few hundred Schwarzschild radii in two NLS1s and to compare these with the properties of other types of Seyfert 1s.'),('B063',2,'Probing the very small scale structure (l simeq 30 AU) in the interstellar medium (continued)','BOISSE','PATRICK','Ecole Normale SuperieureDEMIRM','We propose to extend our study of the very small scale structure inthe molecular, atomic and ionized phases of the interstellar medium initiated during cyle 1 to larger scales (l simeq 30 AU) by taking two additional spectra of the runaway O star HD 34078. HD 34078 (AE Aur) moves at a transverse velocity of 103 kms (or 20 AU/yr); thus the 3 spectra which will be obtained during cycle 1 will allow us to sample adjacent lines of sight distant by simeq 10 and 15 AU at the cloud distance. The two spectra we propose to acquire during cycle 2 will allow to probe separations up to 30 AU and better characterize the column density fluctuations for a broad range of species, including H_2, HD, CO, CI, SI, SiII, CII, FeII ... Presently, only the first cycle 1 spectrum has been taken. It is excellent (SN simeq 20 at 1100 AA); HD lines are clearly detected as well as many lines from highly excited levels of H_2 (v=1, J=0, 1, 2, 3, 4 and v=0, J=9). From the analysis of this superb spectrum, we find that prospects are extremely encouraging for i) detecting variations deltaNN as low as a few H_2 (J=0, 1, 2) or weaker, nearly optically thin lines and ii) performing a very detailed modelling of this line of sight and of the physical conditions in the foreground gas.'),('B065',2,'Far-UV Spectroscopy of X-Ray Novae','SHRADER','CHRIS','NASA Goddard Space Flight Center','We propose to obtain Far-UV spectroscopic observations of X--Ray Novaevents selected on the basis of their optical--UV brightness and absorption characteristics. A recent case, XTE J1118+480, represents an excellent candidate to achieve our goals if it remains (or becomes) active during FUSE Cycle-2. This program, if approved, will be executed in coordination with related ToO programs utilizing the Rossi X-Ray Timing Explorer and the Hubble Space Telescope. Specific goals for FUSE include simultaneous measurement of the ionizing X-ray flux and the strengths of O 6 , ion C 3 , and ion N 3 lines. These measurements can then be applied as density, temperature, optical depth, and abundance diagnostics within the context of photoionization model calculations. In addition, we will search for variability on time scales of seconds, resulting, for example, from reprocessing of an X-ray flare in an accretion disk.'),('B066',2,'The Hot Stellar Population and Cooling Flow of M87','BROWN','THOMAS M.','NASA/GSFC','We propose FUSE observations of M87, the central giant ellipticalgalaxy of the Virgo Cluster. These data will investigate two important questions in extragalactic astrophysics bullet What is the origin of the excess UV light in M87 bullet Can we detect the warm gas that should be present in galaxy cluster cooling flows The UV upturn phenomenon is a key indicator of age and abundance in elliptical galaxies. It originates in a population of hot evolved stars that are only well-isolated in the far-UV. In quiescent elliptical galaxies, the UV optical flux ratio correlates strongly with the optically-determined metallicity of the cool stars. However, the UV upturn in active galaxies is systematically bluer than one would expect from their optically-determined metallicities. In the case of M87, its UV emission is four times greater than expected, although non-thermal emission from its active nucleus comprises only sim10 to this puzzle lies in the far-UV, where the diagnostics characterize the appropriate hot population. In Cycle 1, we will obtain FUSE spectra of three quiescent ellipticals. Cycle 2 observations of M87 would explore the origins of the excess UV light in active ellipticals. The Virgo Cluster contains the nearest X-ray bright cooling flow, which is centered on M87. As the hot intracluster gas cools from sim 10^7K to sim 10^5K, it should emit strongly in the O 6 lambdalambda1032,1038 doublet. Although X-ray observations provide strong evidence for the hot gas, the emission from the warm gas has not yet been detected in an intracluster cooling flow. Our observations will provide an important test of the cooling flow interpretation, as they will be much more sensitive to the O 6 emission than was possible with earlier far-UV missions.'),('B067',2,'The early evolution of the circumstellar environment of solar-like stars','WALTER','FREDERICK M.','SUNY, Stony Brook','The UV spectra of the youngest cool stars, the classical T Tauristars, are dominated by emission lines of molecular hydrogen (H_2), yet within a few million years the H_2 lines fade and the spectra take on the characteristics of the solar chromosphere and transition region. We propose to obtain the FUV spectra of four low mass pre-main sequence stars to study the early evolution of the circumstellar material. This sample fills in the observational gap between the T Tauri stars in the FUSE cycle 1 program and the ZAMS stars like AB Dor. We propose 4 targets 2 very young naked (diskless) T Tauri stars, one transition object with an inner hole in its circumstellar disk, and a classical T Tauri star. We have (or will soon get) UV spectra of these stars with the HST, and one star is our XMM spectroscopic target.'),('B069',2,'Nebular UV Absorption Lines in Planetary Nebulae','DINERSTEIN','HARRIET','University of Texas at Austin','We propose to continue our Cycle 1 program of studying the Lyman andWerner bands of H_2, seen in absorption against the UV continua of planetary nebula central stars, which arise within neutral-molecular envelopes surrounding the ionized gas. These are the pump lines for a fluorescent cascade of near-infrared emission lines which are observed in many planetary nebulae. By observing the UV lines we can probe the chemical and thermal structure of the envelopes, as well as measure molecular column densities and clarify the excitation processes for the infrared lines. In Cycle 1 we were granted time for three targets, one of which was successfully observed shortly before submission of this proposal. Although the data were not yet available for examination, similar target observed by the project team revealed a rich set of H_2 circumstellar absorption features, demonstrating the feasibility of our program. FUSE spectra also include absorption features from atomic species such as O I and C II, which give rise to important far-infrared fine-structure cooling lines that likewise have been observed from planetary nebulae. In Cycle 2, we add as a secondary goal a search for nebular components of the O VI 032, 1038 AA absorption lines, which trace the presence of hot shocked gas, in nebulae with anomalously strong optical recombination lines of ions of oxygen and nitrogen. This will test a plausible hypothesis for the origin of this anomaly. '),('B070',2,'Physics of Boundary Layers/White Dwarf Accretion in Dwarf Novae','SION','EDWARD','Villanova University','The central accreting object in compact binaries and other accretingsystems is usually hidden from direct observation, enshrouded by optically thick accretion disks which are opaque to the radiation emitted by the central object as it accretes matter. In the dwarf novae RX And, WZ Sagittae and VW Hydri the underlying white dwarf accreter is clearly exposed with HST in the far UV, during quiescence. However, there is an unidentified second hot component in these systems. Since the hot white dwarf photospheric continuum is turning down, the contribution from a hotter inner disk region/boundary layer, accretion belt, or corona will show up in the FUSE wavelength regime. FUSE spectroscopy will deliver the following fundamental information: (1) delineation by profile shape and velocity, of lower temperature line formation regions associated with the rotating photosphere of the white dwarf from line formation region(s) of higher temperature ion species associated with a boundary layer/accretion belt (or putative hot corona?) still present surrounding the white dwarf; (2) white dwarf rotation rates, yielding critical information on the boundary layer temperature/structure and spinup of the white dwarfs by accretion; (3) detection of metal line profiles of the most abundant element, C, and also N in WZ Sagittae to test accretion versus dredgeup for the origin of carbon, and test physical mechanisms that control the flow of accreted elements and hence abundance changes (diffusion, mixing, dilution, dredeup and ongoing accretion during quiescence).'),('B071',2,'Anomalous Oxygen and Krypton Abundances in Interstellar Gas','CARTLEDGE','STEFAN I.B.','Northwestern University','We propose to obtain FUSE observations of interstellar ionH1 and H_2absorption toward 10 stars observed by STIS as part of the ISM SNAP Survey, a Cycle 8 HST observing program. The ISM SNAP Survey was designed to produce a database of high quality, high resolution spectra from which gas-phase abundances for large portions of the Galaxy could be derived. Krypton and oxygen have been chosen during initial analysis as tracers of the amount of absorbing material along the various sightlines. The gas-phase oxygen and krypton abundances relative to total hydrogen column density have previously been shown with GHRS to be essentially constant in the local Milky Way. Further, krypton is a noble gas not expected to be depleted much into dust in the ISM. The ISM SNAP Survey has extended precision measurements of these elements to significantly higher column densities than GHRS. Intriguingly, several Survey sightlines have yielded anomalously high Kr 1/ O 1 and O 1/H 1 ratios. By measuring the total hydrogen column density along these 10 sightlines, it will be possible to better determine the nucleosynthetic and/or dust depletion implications of these anomalies.'),('B072',2,'Magnetospheres and Winds in the Rapid Braking Zone','AYRES','THOMAS','University of Colorado','FUSE exposures of five late-Fearly-G giants will probe fundamentalplasma dynamics in their hot magnetized outer atmospheres; as encoded in spectral line widths, Doppler shifts, broad components, asymmetries, and wind-induced circumstellar absorptions. The giants lie in or near the Rapid Braking Zone where moderate mass stars undergo a radical transformation of their coronal outer atmospheres. We also will explore the even more extreme extension of the RBZ to higher masses two G0 supergiants in the so-called hybrid region where hot coronae mix freely with cool stellar winds. FUSE / spectra of the key O~VI $lambda$1032 and CIII lambda977 features will allow us to separate the influences of temperature and opacity on the super-rotational broadening of the RBZ subcoronal emissions; and will strongly complement an ongoing HST STIS (1150--3100 A) survey of late-type stars. Our ultimate objective is to understand stellar magnetic activity; crucial to solar-terrestrial relations, the early evolution of solar system, and one face of a myriad of hydromagnetic phenomena that occur in many cosmic environments protostellar envelopes, neutron star magnetospheres, the accretion disks of cataclysmics, and those of AGN. The dramatic, rapid magnetic evolution of the RBZ stars allows us to view many fundamental aspects of stellar activity---coronal structuring, heating, and angular momentum loss---from an entirely different perspective than afforded by the highly accessible---but singular---case of our Sun. It is through these different perspectives that we can hope to gain new insights into the underlying physical processes.'),('B074',2,'Molecular Hydrogen in the Quiescent Disk of SW UMa','RAYMOND','JOHN','CfA','Disk-instability models, which are usually invoked to explain theoutbursts of transient close binaries, predict that the gas in the quiescent disks of Dwarf Novae and X-ray Transients should be neutral. In fact, if the reduced viscosity of the low state results from the disappearance of MHD turbulence as predicted by the Balbus-Hawley instability, the required ionization state is so low that the gas should be molecular. There is currently no direct observational evidence for this. We propose a spectroscopic observation of the Dwarf Nova SW UMa, in an attempt to detect the molecular hydrogen bands at 1060 and 1105 AA in the quiescent disk of this system. H_2 band diagnostics could provide valuable information on the ionization fraction of the gas which is essential for determining the nature of viscosity in the disk.'),('B075',2,'Particle Acceleration in SN1006 Shock Waves','RAYMOND','JOHN','CfA','We will attempt to measure the fraction of a shock waves energy thatgoes into cosmic rays. The NE sector of the young SNR SN1006 shows strong non-thermal X-ray and gamma ray emission. The Hopkins Ultraviolet Telescope observed the pure Balmer line filament in the NW section of the young supernova remnant SN1006. The observation demonstrated that the electrons and ions do not reach temperature equilibrium in this 2300 kms collisionless shock. However, the NW section of SN1006 shows very little non-thermal emission at radio or X-ray wavelengths. We propose to obtain the line widths, intensities and spatial brightness profiles of the O VI lines in sections of the NW and NE shock waves to compare the electron-ion and ion-ion temperature equilibration efficiencies in shocks with very strong and very weak non-thermal X-ray and radio emission. If a substantial fraction of the energy dissipated in the shock goes into cosmic ray acceleration, the line profile in the NE shock will be narrower.'),('B077',2,'The Cosmic Distance Scale An Accurate Distance to the LMC Using Eclipsing Binaries','GUINAN','EDWARD F.','Villanova University','The distance to the LMC is crucial to calibrating the cosmic distancescale but remains controversial and uncertain despite the efforts of many investigators. We have demonstrated that the analysis of eclipsing binaries (EBs) has the potential to resolve this controversy. Guinan et al. (1998, ApJ, 509, L21) and Fitzpatrick et al. (2000, BAAS, 196, 2806) analyzed ground- and space-based observations of HV2274 and HV982 and determined LMC distance moduli of V-M v circ 18.30 0.07mag and V-M v circ 8.32 0.10mag, respectively. Such an excellent agreement demonstrates the potential of this method, and the suitability of EBs as accurate standard candles. However, these are only results for two stars and the method must be verified with additional observations and extended wavelength coverage into the Far-UV where the stars strongly radiate. The primary goals of the FUSE observations are to secure accurate, definitive temperatures and interstellar extinctions to the target stars (Sp. Typ. O7-B2), whose energy maxima occurs in the FUSE spectral range. All of the targets have FOSSTIS spectrophotometry covering 1150--4820AA. The FUSE observations will be combined with UVoptical spectrophotometry and with light and radial velocity data that will yield the radii, T_ eff, E(B-V), log g, and FeH of the stars. The distances to the stars (and the LMC) are directly determined from their radii, temperatures and apparent brightnesses (flux received at Earth corrected for ISM extinction). The FUSE observations, when combined with our other datasets, will reduce the uncertainty of the LMC distance to better than 2-3%.'),('B078',2,'The FUV Sun in Time A Study of Solar Analogs of Different Ages','GUINAN','EDWARD F.','Villanova University','We propose to use FUSE to complete an in-depth study of the evolutionof the transition region and low corona of a solar-mass star throughout its main-sequence lifetime. This program is part of a comprehensive study of the Sun in Time across the electromagnetic spectrum. We have defined a homogeneous sample of single G0-5V stars with well-known rotation periods that are proxies of the Sun at different ages. We are studying the dynamics of the lower layers of the stellar atmospheres by investigating line shifts, line asymmetries, and line broadenings that we presume are related to chromospheric evaporation by high-energy processes identified in the overlying corona. Emission measure and temperature analysis will allow us to obtain a complete -D atmospheric model of active regions that we will link to the previously obtained coronal X-ray data. We will infer transition region pressures through the powerful density-sensitive ratio of the Csc iii 977AA1176AA lines; this important diagnostic will be adequate to identify and model the relevant magnetic structures based on the solar analogy, and, together with our coronal X-ray (XMM, ROSAT, ASCA, SAX), EUV (EUVE), and TR (IUEHST) data, to infer the importance of coronal energy releases. Our FUSE investigation is central to the understanding of the evolution of magneto-dynamic atmospheric phenomena, and the associated high-energy emissions in the Sun and in solar-type stars. It also bears on the crucial question of the influence of the young Suns expected strong FUV emissions on the developing planetary system -- particularly on the erosion of Mars primitive atmosphere. Coordinated contemporaneous observations (with XMM, Chandra, HST, optical photometers, partly from guaranteed time programs) are planned and will be organized.'),('B079',2,'Fossil Fuel in the Local Group','GIBSON','BRAD','Swinburne University','We propose a direct observational test of the Local Group Infallhypothesis that the majority of High-Velocity Clouds (HVCs) are the extragalactic building blocks of the Local Group. The line of sight to the Seyfert PG1011-040 fortuitously passes through HVC,246+39+125 in the Wannier Clouds, a collection of HVCs in the direction of the Local Group anti-barycenter. The proposed FUSE Cycle2 observations will be used to constrain the metallicity and ionization properties of HVC,246+39+125, which in turn will reveal its local (higher metallicity) or extragalactic origin. Unlike the HVCs currently under study by the FUSE PI Team (eg, Magellanic Stream, Complexes A, C, and M), HVC,246+39+125 is expected to lie at a distance >~ 400,kpc, be of low intrinsic metallicity, and reside in the M31--Milky Way filament predicted by the BlitzSpergel Local Group Infall model. None of the Galactic HVCs being studied by the FUSE PI Team have these same a priori predictions, and thus our program provides a natural complement to the more general PI programs.'),('B081',2,'A Study of Hot Gas in Shock Wave--Interstellar Cloud Interactions','BLAIR','WILLIAM P.','Johns Hopkins University','We will use FUSE to obtain detailed information about the kinematics,resonance line scattering properties, and physical conditions of gas involved in the collision of the Cygnus Loop supernova blast wave with an interstellar cloud. The region, known as XA, is located on the eastern side of the supernova remnant and a wealth of supporting information at optical, UV, and X--ray wavelengths is available. High resolution line profiles for CIII lambda 977, NIII lambda 989.8, and OVI lambdalambda1032,1038 (and possibly many other lines) will be used to sort out the competing effects of turbulence, thermal instabilities, projection effects, and resonance line scattering at several key locations on and ahead of the core of the shocked cloud. Investigating such interactions is of primary importance for understanding SNR evolution in a cloudy medium and for assessing the effectiveness of SNR shock waves in heating and mixing the ISM.'),('B084',2,'The Outer Atmosphere of Mira Variables','LUTTERMOSER','DONALD G.','East Tennessee State University','We propose to use FUSE to probe the temperature-density structure ofthe shocked atmospheres of long-period variable (Mira-type) stars. For the first time, FUSE gives us the capabilities to study the outer shocked region of the atmosphere using the hydrogen Lyman lines. At 5 separate phases, we wish to obtain MDRS spectra of the Lyman series from Lybeta to the Lyman limit (1030AA --- 912AA) for the warm Mira star, SCar. With these spectra, we will make comparisons (1) between Lyman flux (and possibly H_2 emission) variability and the variability in the UV emission lines and hydrogen Balmer lines using previously obtained HST HRS, IUE, and ground-based optical spectra at coincident phases to the FUSE observations to study the effect that the radiation field from the lower, hotter shocks (where Mg 2 and the Balmer lines form) have on the upper shocked region (where the Lyman lines form), and (2) to synthetic spectra from representative dynamic models we have generated. These NLTE radiative transfer calculations have shown that the radiation field of the inner shocks dominate the ionization throughout the entire atmosphere. The calculations also have shown that the Lyman emission lines form in the outer reaches of the atmosphere where the shocks are much weaker as they propagate outward. This is the first time such a diagnostic has been measured for the outer atmosphere of these stars. It also gives us a pioneering attempt to record the suspected strong FUV H_2 in emission. Such an observation will have strong constraints on the atmospheric structure of the outer layers of these stars. Finally, it is imperative to obtain fairly high dispersion (R approx 10,000) spectra of the Lyman lines in Miras, since these lines are fundamental in the understanding of the energy flow in their outer atmosphere, and of mass loss in this critical stage of a stars evolution.'),('B085',2,'beta Pic-like Circumstellar Gas Disk Around 2 And','CHENG','K.-P.','California State University, Fullerton','Ultraviolet observations of 2Andromedae with the Goddard HighResolution Spectrograph onboard the Hubble Space Telescope (HSTGHRS) clearly reveal the existence of circumstellar gas as well as the interstellar gas along the line-of-sight toward this nearby star. We also detected varying red-shifted CaII absorptions in our ground-based optical spectra, which we interpret as gaseous infall. These variable CaII absorption features and the presence of circumstellar absorption from AlIII lambdalambda1854.716,1862.790 and excited fine-structure levels of FeII near 2600 AA in our HSTGHRS data of And are similar to those observed in the proto-planetary system candidate betaPictoris. However, unlike betaPic, 2And has no detectable IR excess based on our previous IRAS survey of dust disks around nearby A stars. The detection of gaseous infall with characteristics similar to betaPic in an apparently dust-free stellar system suggests that we should re-examine existing models that attempt to explain the gaseous infalls in betaPic with grazing comets or erosion from the surrounding extensive dust disk. FUSE observations of 2 And will allow us to study the characteristics and origin of the circumstellar gas. Our results will provide insight into the link between the circumstellar gas and dust.'),('B086',2,'Far-Ultraviolet Interstellar Extinction in the Large Magellanic Cloud','CLAYTON','GEOFFREY','Louisiana State University','Understanding interstellar dust and its role in the universe is veryimportant. Virtually all observations of astrophysical objects and their physical processes are affected by the presence of dust either within the system being studied or along its line of sight. We propose a research program that will significantly improve our knowledge of dust properties, specifically those of small grains. Such an advance has not been possible prior to the advent of FUSE and its unique capabilities the high far ultraviolet (FUV) throughput and the ability to resolve H_2 lines, combined with a well-characterized instrumental calibration. We will derive FUV extinction curves for several types of sightlines which possess distinct signatures associated with the small grain population and whose mid-UV extinction curves reveal vastly differing amounts of intermediate-sized particles. We will study sightlines in the Large Magellanic Cloud where very non-Galactic mid-ultraviolet extinction properties are seen. A new analysis of the mid-ultraviolet extinction found a region near the supergiant shell LMC2 where the 2175 A bump is very weak. LMC sightlines inside and outside this region will be sampled with FUSE. These data will be used to probe and constrain the properties of the small dust grains, such as abundance and size, and their connection to the very different environments observed.'),('B087',2,'Physical Properties of a z ll 1 Lyman Limit System','PROCHASKA','JASON X.','Carnegie Observatories','One of the most exciting aspects of quasar absorption line studies isto test and constrain theories of galaxy formation and evolution. A principal challenge to this quest is to obtain coincident knowledge of the physical properties of the absorbing gas and the host galaxies or large-scale structure. We propose to analyze the physical properties e.g. metallicity, ionization state) of the z0.167 partial Lyman limit system towards PKS0405-12. By synthesizing our investigation of the physical properties of this QAL system with the galaxy data we have obtained we will compose an unprecedented study of a low redshift QAL system. FUSE observations are essential for an accurate HI column density of this system as well as measurements of its metallicity, ionization state, and relative abundances of C, S, Si, and Fe. This detailed examination of a z sim 0 QAL system when combined with our knowledge of the absorbing galaxies will provide a benchmark for comparisons against high redshift systems, pose questions on the nature of halointragroup gas, and advance our understanding of OVI absorbers. '),('B089',2,'Abundances and Physical Conditions in the SMC ISM','WELTY','DANIEL E.','University of Chicago','We propose to obtain far-UV spectra of two stars in the SMC, as partof a detailed study of the interstellar medium in the Magellanic Clouds. Together with optical andor near-UV spectra obtained at higher resolution and SN, these far-UV spectra will be used to determine accurate abundances, pressures, temperatures, densities, and radiation fields for both neutral and ionized clouds in the SMC and in the Galactic disk and halo. Because of the low metallicity, low dust-to-gas ratios, and strong radiation fields in the SMC, the derived properties of the SMC clouds will provide valuable tests for theoretical models of interstellar clouds. Determining detailed abundancesdepletions and physical conditions for diverse environments in our Galaxy and in the Magellanic Clouds will also aid in understanding the absorption-line systems seen toward distant QSOs.'),('B090',2,'Molecule Formation at High Extinction and Low Metallicity in the Magellanic Clouds','SHULL','MICHAEL','University of Colorado','The fundamental physical and chemical processes at work in molecularclouds are key objects of FUSE science. Preliminary results on h2 in the LMC, based on available PI Team data, suggest a reduced molecular fraction in the low-metallicity LMC gas. Although this result provides the first direct evidence of a metallicity dependence in the formation rate of interstellar h2, the available FUSE targets do not sample the high-extinction regime where the correlation between E(B--V) and molecular fraction is strong. Therefore, we cannot test whether the apparent reduction in molecular fraction is due to reduced formation rates, high radiative destruction rates, or selection effects. We propose observations of 7 LMC stars and 2 SMC stars with E(B--V) 0.20 -- 0.42, which will allow us to test cloud models that incorporate different assumptions about the formation rate of h2 as a function of metallicity. We will also obtain CO emission maps in these selected regions to assess the COh2 ratio in this gas. As a key goal of FUSE h2 science, this test can be applied only to sight lines for which the variation of molecular fraction with extinction can be tightly controlled.'),('B091',2,'Search for Molecular Hydrogen Around Vega-type Stars','JURA','MICHAEL','University of California, Los Angeles','Giant planets are believed to form in the disks of gas and dustsurrounding young stars. However, CO surveys of dusty Vega-type stars have found little gas. In an effort to understand the dissipation of molecular gas in young debris disk systems, we propose to conduct a spectroscopic search for absorption in the Lyman and Werner series of H_2 surrounding the Vega-type stars sigma Her, HR 7188, HR 3314, alpha CrB and HR 4796. Observations of these absorption features with FUSE will provide an extremely sensitive test for the existence of circumstellar molecular gas. We have selected sources for study with the FUSE prime spectrograph which have not been reserved by the FUSE PI teams and 1) contain dusty debris disks indicative of youth. (2) lie within 100 pc of the sun. (At such close distances, the amount of interstellar gas should be minimal.) (3) emit enough ultraviolet photons to be useful to detect H_ 2 in absorption.'),('B094',2,'Excitation and Abundances in N132D','MORSE','JON A.','University of Colorado','We propose to obtain fuse far-UV spectroscopic observations of theshocked outer rim of the young, oxygen-rich supernova remnant N132D in the LMC. These data will be used to calibrate the relative contribution of OVI emission from the blastwave expanding into the ambient ISM in our previous fuse spectrum of the ejecta in N132D. In addition, the fuse spectra will be combined with existing and proposed hst and chandra imaging and spectroscopic data to completely characterize the excitation of the outer blastwave.'),('B095',2,'A FUSE Search for H2 on Mars','Gladstone','Dr. Randy','Southwest Research Institute','We request 40ks of FUSE time to observe Mars twice during 2001 to search for H2 emissions that would provide an important constraint on photochemical models and the escape rate of hydrogen. The best times for observation are 30 degrees before and after opposition (on or about May 17 and July 8, 2001), when Mars is close to Earth (subtending 17\'\' and 20\'\', respectively). The best existing FUV spectrum of Mars has a poor SNR in the 90-100nm range where H2 Lyman and Werner band emissions are most easily detected. Other dayglow emissions, notably those due to H, O, Ar, and CO, are also expected in the FUSE 90-120nm range, and we will search for N2 bands as well. We will use state-of-the-art model martian atmospheres and photoelectron production and transport codes to simulate these airglow emissions and derive useful atomic and molecular abundances from the data.'),('B097',2,'Diffuse Molecular Hydrogen in the Galactic Plane','DEWDNEY','PETER E.','National Research Council of Canada','As part of a high-resolution multiwavelength survey of interstellarmatter in the Galactic plane, we are investigating the physical state of cold diffuse interstellar matter traced by dust, HI self-absorption, and various molecular species. An increasing body of evidence from our survey and others suggests that far-IR emission and H 1 self-absorption may trace a significant amount of molecular hydrogen which lacks traditional proxy tracers like ^12CO. Far-UV spectroscopy of these clouds will provide the first direct measure of their molecular hydrogen content. We have selected a set of stars with foreground dust but no detected CO emission to observe with FUSE. All of these probe the molecular content of dusty diffuse environments, with some also sampling ionH1 self-absorption features. Obtaining H_2 column densities for these clouds is essential for understanding their physical properties, structure, and evolution, as well as the larger role of the cold diffuse medium in star formation and the Galactic ecosystem.'),('B101',2,'Time-resolved spectroscopy of high field polars','BARRETT','PAUL','Space Telescope Science Institut','A long sought-after group of polars are those with high magnetic field>60 MG), because they may provide valuable clues to the structure and dynamics of accretion in strong magnetic fields and the evolution of CVs in general. The discovery of several soft X-ray polars by ROSAT and their subsequent identification as high field polars supports the conclusion that the bremsstrahlung is suppressed at higher fields and cyclotron cooling predominates. We propose time-resolved FUV spectroscopy of high field polars to study their accretion kinematics, their high excitation lines (e.g. OVI, OIV, and SiIV), and the distribution of gas in the binary. '),('B104',2,'Density, Velocity and Ionization Structure in Accretion-disc Winds','LONG','KNOX','Space Telescope Science Institute','We propose to exploit the unique capabilities of it FUSE to monitorvariations in the wind-formed spectral lines of 3 luminous, low-inclination, cataclysmic variables (CVs). Our principal goal is to improve our understanding of the dynamics of accretion-disc winds. We have previously used HST to investigate substantial and rapid (sim hours to minutes) variability in our target stars, BZ Cam, RW Sex and V603 Aql, and have demonstrated that their disc-outflows are highly structured. We aim here to follow up our discoveries by securing FUSE time-series data. These observations will allow us to determine the relative roles of density and ionization state changes in the outflow and to search for spectroscopic signatures of stochastic small-scale structure and shocked gas. By monitoring the temporal behavior of blue-ward extended absorption lines with a wide range of ionization potentials and excitation energies, we will track the changing physical conditions in the outflow. A new sophisticated Monte Carlo code will be used to calculate the ionization structure of and radiative transfer through CV winds. This will allow us to establish the wind geometry, kinematics and ionization state, both in a time-averaged sense and as a function of time. Our FUSE observations will provide a legacy that will be fundamental to the development of dynamical models of accretion-disc-driven winds, permitting critical tests of recent hydrodynamic simulations of unstable, line-driven disc winds.'),('B105',2,'Wind Emission in Narrow-line Seyfert 1 Galaxies','LEIGHLY','KAREN','The University of Oklahoma','Narrow-line Seyfert 1 galaxies (NLS1s) are known to havecharacteristically different X-ray properties than Active Galactic Nuclei (AGN) with broad optical lines. The most promising explanation for this behavior is that NLS1s have a higher accretion rate with respect to Eddington. This result is fundamental, since accretion is thought to be the ultimate power source for all AGN. Our recent HST spectra from two NLS1s reveal unusual UV emission line properties. The high-ionization lines are broad and strongly blueshifted, in contrast with the low-ionization lines which are narrow, centered at zero velocity, and symmetric. The most plausible explanation is that the high-ionization lines are emitted by a wind and the low-ionization lines are emitted by a disk. Such models have been discussed previously, but our spectra provide perhaps the strongest evidence to support these models to date. We now seek to understand the geometry and physical conditions in the wind. The proposed FUSE observations of two NLS1s, 1H0707-495 and IRAS13224-3809, will allow us to examine the profile of the high ionization resonance line ionO6lambda1034. This line is typically emitted in material with higher ionization parameter than the lines observed in our HST spectra and thus comparison of the O 6 and ion C 4 line profiles will allow us to distinguish between classes of models that do and do not predict ionization stratification. These targets are particularly suited for this investigation since only a few objects are known that have high-ionization lines dominated by wind emission. '),('B106',2,'The Supernova Heating Rate in Spiral Galaxies','BREGMAN','JOEL','University of Michigan','In spiral galaxies, supernovae dominate the energy input into the ISM,controlling the volumes of hot and cold gas, the pressure, and star formation itself. Previously, the heating rate was estimated from the supernova rate and the energy per supernova, the product of which is uncertain to half an order of magnitude. FUSE provides a direct, accurate, and independent measure of the heating rate because the shocked gas emits O 6 as it cools through the 3times10^5 K regime. With the large aperture, we propose to measure the ionO6 emission from spiral arm and interarm locations for 4 nearby normal galaxies. Ultimately, measurements of ionO6 may prove as important as studying ionH1 or molecular gas in spiral galaxies.'),('B107',2,'Monitoring the Variable Absorption in the Seyfert 1 Galaxy NGC 3783 with FUSE, HST, and Chandra','CRENSHAW','D. MICHAEL','Catholic University of America','More than half of all Seyfert 1 galaxies show intrinsic UV absorptionlines and X-ray warm absorbers. The frequent occurrence of this phenomenon suggests that photoionized, warm absorbing gas is an important component of the nuclear structure of AGN. To understand the nature and origin of this gas, we must know its location, physical conditions, and kinematics. By simultaneously monitoring the variability of the absorption at UV and X-ray wavelengths, we can determine the radial location, density, and ionization state of the absorbing gas and measure its evolution in ionization, column density, velocity, and coverage of the active nucleus. NGC 3783 is an ideal target for such a study due to its brightness, and its extremely variable absorption and rapid continuum variability in both the UV and the X-rays. FUSE is a crucial tool for our work since the high-order Lyman lines provide an accurate measure of the neutral hydrogen column, and the high-ionization sc Ovi lines provide a key link between the UV and X-ray absorbing gas.'),('B108',2,'Investigation of Supernova Remnant Shocks in the Vela-Puppis Region','SANKRIT','RAVI','Johns Hopkins University','We propose to use FUSE to observe ultraviolet emission spectra ofsupernova remnants (SNRs) in the Vela-Puppis region. With its sensitivity to emission from extended sources, its spatial resolution and its particular wavelength coverage, FUSE is an excellent instrument for such a study. The FUSE bandpass includes CIIIlambda977 and OVIlambdalambda1032,1038, which are strong lines in SNR shocks and trace low ionization and high ionization gas respectively. The spectral resolution of FUSE will allow us to compare line profiles and study the kinematics of the post-shock flow. Since the OVI doublet is well separated, we will be able to use the flux ratio between the lines to estimate the amount of resonance scattering present. We will also be able to detect the presence of multiple components if they are sufficiently well separated in velocity space. In addition to these strong lines, we expect that several lines such as SVIlambdalambda933,944 and NIIIlambda991 will provide additional constraint on models.'),('B109',2,'The Lyman break in the luminous BCG Haro 11','BERGVALL','NILS','Uppsala astronomical observatory','Deep galaxy surveys have indicated that luminous starburst dwarfs mayplay an important role in explaining the increasing star formation activity towards higher redshifts. The relatively low masses and high star formation efficiency of these galaxies allows for a significant leakage of Lyman continuum photons into intergalactic space. They may therefore play an major role in the reionization of the universe at early epochs. To assess the importance of these objects in this respect we want to use FUSE to study, as a first step, one local luminous blue compact galaxy with extreme starburst properties, Haro 11. When compared with similar galaxies, Haro 11 is remarkably devoid of HI. This may be understood if a major part of the ISM is ionized by the starburst or is in molecular form. We propose to use FUSE to measure the strength of the Lyman continuum break to estimate the amount of Ly-continuum photon leakage and seach for molecular absorption lines of diffusely distributed H_2 to determine or set upper limits of the column density.'),('B110',2,'Iron abundance in the WC-PG1159 central star of Abell 78','WERNER','KLAUS','Universitat Tubingen','The very first attempt to measure the iron abundance of a hotH-deficient post-AGB star arrived at a surprising result. Based on the absence of Fe lines in a FUSE spectrum of the PG,1159-type central star of the planetary nebula K1-16 we could show that this object is Fe-deficient by a factor of at least 10--100. The same might be true for two other PG1159 central stars with similar stellar parameters based on IUE spectra, but firm results have to be waited for until FUSE spectra are acquired (PI team targets). Here we propose to look for iron lines in the central star of Abell78, which is of spectral type WC-PG,1159, hence, it is an immediate progenitor of the PG,1159 stars. We intend to see if the Fe-deficiency can be traced back in evolution closer towards the AGB phase. If this is the case then the Fe-deficiency might be caused by dust fractionation on the AGB, hence, it is caused by the same phenomenon which is responsible of the extreme Fe-deficiency found in some (H-rich) early post-AGB stars.'),('B112',2,'Molecular Hydrogen Fluorescence in IC 63','ANDERSSON','B-G','Johns Hopkins University','FUV radiation shortward of 1108 AA causes electronic excitations ofthe hydrogen molecule through the Lyman (B-X) and Werner (C-X) transitions. The relaxation back to the electronic ground state gives rise to a rich fluorescent spectrum. Under favorable conditions this spectrum can be observed. We propose to observe this fluorescence at unprecedented resolution and sensitivity in the reflection nebula IC 63. Earlier observations suffered from restricted wavelength coverage or lack of spectral and spatial resolution. Although the results are in general agreement with theory, distinct discrepancies persist, most notably a shortfall in the absolute intensity of the fluorescent flux by a factor of 10, compared to theoretical models, in the FUSE wavelength range. In order to provide a detailed test of existing models, we propose to acquire high quality data in three locations within the reflection nebula at different distances from the ionization front. By observing several locations and comparing the strength of the fluorescence, we will also be able to address the transfer of the continuum radiation through the nebula.'),('B114',2,'Observations of O VI Emission in the Hot Halo of NGC 891','MURPHY','EDWARD','University of Virginia','We propose to use fuse to search for ovi emission from hot, coolinggas in the halo of the well studied, edge-on spiral galaxy NGC891. Our proposed search for ovi emission in the halo of NGC891 will allow us to determine the total mass of transition temperature cooling gas (Tsim3times10^5 K), the scale height of the ovi gas, and to compare the distribution of this transition temperature gas with hotter gas (Tsim3times10^6 K) as revealed by ROSAT. We have selected 3 positions in the halo of NGC891 for exposures of 30 ksec each (90 ksec total). One position is sim 2.25 kpc above the nucleus of the galaxy to search for hot material escaping from the bulge. The remaining two positions are placed sim 1.5 and 2.5 kpc above an active star-forming region in the NE section of the disk. A similar fuse Cycle 1 observation of the strongly-interacting edge-on spiral NGC 631 produced a detection of ovi emission in 20 ksec. Since NGC 891 is not interacting with other large galaxies, it provides a better comparison with the halo properties of the Milky Way.'),('B119',2,'A FUSE Search for Nitrogen and Carbon in Hot White Dwarfs','HOLBERG','JAY B.','University of Arizona','We propose a FUSE investigation of presence of spectral lines due tothe first and second ionization stages of carbon and nitrogen in the photospheres of hot DA white dwarfs. In general, knowledge concerning the presence of N and C is available only for the hottest stars (T_eff > 35000 K), from the C IV 1550 AA) and N V (1240 AA) resonance lines. In cooler DA stars, these lines are weakened and are difficult to observe, leaving few spectral lines longward of 1200 AA to indicate the presence of these important elements in the atmospheres of DA stars. With FUSE, we will measure the presence of N and C using the strong N II, N III, C II, and C III lines in the FUSE band pass. We will also use these lines to investigate and test models of the stratification of these heavy elements in the atmospheres of DA stars.'),('B120',2,'Observations of the LISM with Hot White Dwarfs','HOLBERG','JAY B.','University of Arizona','We propose FUSE observations of the interstellar lines of sight for aset of white dwarf stars. For each of these stars, the full ionization state of interstellar hydrogen and helium has now been measured. Using EUVE, we have determined the ionization fractions of H and He, and from STIS observations with HST, we have detailed knowledge of the velocity structure and composition for each of these lines of sight. We will use FUSE observations of these stars to complete our models of these unique lines of sight through the Local Interstellar Medium (LISM) by measuring ground state and fine structure transitions of Ar I, C II, C III, N II and N III ions which occur in the FUSE band pass.'),('B122',2,'A Search for Trace Elements in Ultramassive White Dwarf Photospheres','DUPUIS','JEAN','University of California, Berkeley','Ultramassive white dwarfs form a relatively large proportion of whitedwarfs discovered during recent extreme-ultraviolet surveys of the sky. Their exact origin is unknown but it is believed that some of them might be white dwarfs with an oxygen-neon core resulting from the evolution of single star with an initial mass between 8 ltappeq M ltappeq 11 msun. Another possibility is that these may be the result of the merger of two normal mass white dwarfs (Msim 0.6msun). The surface composition of ultramassive white dwarfs is likely to be sensitive to their formation scenario. We propose to observe 2 of the brightest known ultramassive white dwarfs with fuse to search for presence trace elements (mainly C, N, O, Si, S, P, and Fe). We plan on using non-LTE synthetic spectra of white dwarfs to model the profiles of Lyman lines and measure or set upper limits on abundances of trace elements with resonance lines in the fuse range. These sources are also excellent background sources to investigate the local interstellar medium and we plan on measuring column densities of detected interstellar absorption lines.'),('B127',2,'Just What is Eta Carinae?','GULL','THEODORE','NASA/GSFC/LASP','Eta Carinae, when observed by FUSE during the Early ReleaseObservations (ERO), was found to have surprisingly bright far ultraviolet fluxes clear down to 920AA. Eta Carinae is a very massive star nearing the end of its lifetime and has undergone episodic outbursts. Over the past few decades, Eta Carinae has brightened continuously with a 5.5-year modulation in the visible and X-rays. What is the cause of the variability? Is Eta Carinae a single star or a binary system? Based upon the periodic variability, the hardness of the X-ray spectrum, and now the large UV flux measured by FUSE, we strongly suspect that Eta Carinae has a hot companion with a fast, massive wind. A 40 Modot star could easily be the secondary companion of the >100 Modot primary. Neither current radial velocity measurements nor visible spectroscopy would detect it. The FUSE spectral region offers the best opportunity of direct detection. In Cycle 2, we propose to observe Eta Carinae once early and once late in the cycle to look for variations in the stellar continuum, in the stellar line profiles and in circumstellar line absorptions.'),('B128',2,'CNO Abundances in LMC BN and BC Supergiants','MASSA','DERCK','Raytheon ITSS','We propose to observe 10 BN, BC and normal B1 Ia supergiants in theLMC. By matching normal and CNO peculiar stars, the stellar wind line data will enable us to determine the relative C, N and O abundances between the different groups. Finally, by employing a simple model for the origin of the CNO enhancements, it will be possible to derive absolute abundances for all of the paired stars. This information will enable us to address long standing questions concerning the origins of the BNBC phenomenon, and elucidate the latter stages of massive star evolution. Because our analysis requires unsaturated wind lines, only FUSE can provide access to C, N and O wind lines. Furthermore, all of these lines will be unsaturated only in stars near spectral type B1 Ia.'),('B129',2,'O VI Emission from the Interstellar Medium','SHELTON','ROBIN','Johns Hopkins University','Currently there is no significant observation of the O VI flux fromthe Local Bubble. Such an observation will be very important for understanding the conditions and history of the Local Bubble and similar bubbles in the local interstellar medium. In this proposal, we describe a strategy for observing the Local Bubble, screening out other sources of flux, and minimizing the necessary spacecraft time spent on the guest observer investigation. The observed O VI flux will be combined with the soft X-ray spectrum for this direction in order to create the high energy spectral signature of the Local Bubble. The results will be compared with the average Local Bubble O VI column density in order to estimate the physical parameters of the hot gas. They will also be used to test and highly constrain theories for the formation and evolution of the Local Bubble and to determine the gas phase abundance of oxygen in hot gas. In addition, this observation will make it possible to determine the O VI flux from the halo. The combined Local Bubble and halo flux has been measured for a direction several degrees from the proposed Local Bubble observation. By subtracting the Local Bubble flux, the halo flux will be determined.'),('B130',2,'Solar Ultraviolet Radiation and the Origin of Life on Earth','HEAP','SARA R.','NASA\'s Goddard Space Flight Center','We are currently using STIS and EUVE to obtain high-quality, far-UV(1160--1700AA ) and extreme-UV (60--760AA ) observations of three analogs of the early Sun. We now propose to obtain FUSE spectra of these three stars in order to obtain spectral coverage over the wavelength range, 60 -- 1700 AA. We will perform a detailed non-LTE analysis of each star, which involves constructing a model photosphere and an empirical model chromosphere that can be used to extrapolate the emission to the Lyman continuum region. Given a realistic flux distribution of the early Sun by proxy, we will then develop photochemical models of weakly reducing primitive atmospheres to determine the lifetime and photochemistry of methane (CH_4). In particular, we will estimate the concentration of CH_4 in the prebiotic atmosphere (sim 3.5 b.y. ago) and during the Late Archean 2.5-3.0 b.y. ago). We will use these results to determine whether methane would have been sufficiently abundant to help offset the reduced solar luminosity at that time. We will also use our photochemical models to solve for the concentrations of greenhouse gases and important pre-biotic molecules.'),('B131',2,'Outbursts in Symbiotic Binaries','KEYES','CHARLES D.','Space Telescope Science Institute','To study the accretion and outbursts in symbiotic systems, we haveorganized a multi-wavelength, target-of-opportunity (TOO) observing program including Chandra, XMM, HST, and the VLA. XMM observations have been approved and proposed Chandra data will provide supporting high-resolution spectral coverage that will probe the hottest regions during an outburst. XMM TOO observations have been approved for any of the targets on our list that go into outburst between July 2000 and at least December 2001 the XMM A01). The XMM observations will provide UV and soft X-ray coverage at several times during an outburst. The evolution of the X-ray and UV spectrum throughout the outburst will play a vital role in distinguishing between the outburst models currently in contention for describing the behavior of these outbursts. Emission line strengths of the FUSE-band species, especially when combined with lines of the same species from the other spectral regions, will provide diagnostics of the colliding windshock region. The high-resolution of FUSE-band absorption features will provide a unique opportunity to probe several aspects of the outburst material. Note especially that FUSE provides important information for the analysis of the x-ray data as FUSE observations of HI absorption are at sufficiently high resolution to allow the separation of the interstellar component from the systemic component of the absorption. '),('B134',2,'Towards Understanding Starburst Galaxies at Low and High Redshift','HEAP','SARA R.','NASAs Goddard Space Flight Center','We propose FUSE observations of a small set of OB stars in the SMC tosupplement the extensive sample being taken by the FUSE PI team. The combined dataset will complete the coverage of representative OB stars at low metallicity. We will then combine the resulting FUSE spectral atlas with our existing HST spectral atlas of the same stars to form a comprehensive UV spectral library (900 - 1700 AA) of massive stars in the SMC. We will use this library itemto determine the stellar content (e.g. metallicity, star-formation rate) of star-forming galaxies at high redshift; itemto determine the properties, particularly mass-loss rates and abundances, of massive stars at low metallicities.'),('B137',2,'Intrinsic Absorption in the Seyfert 1 Galaxy NGC4593 Contemporaneous FUSE, XMM, and HST Observations','KAISER','MARY ELIZABETH','The Johns Hopkins University','High resolution HST spectra indicate that more than 50 Seyfert,1galaxies possess an intrinsic UV absorber (Crenshaw et,al.,1999). Furthermore, there appears to exist a one-to-one correspondence between the presence of the warm X-ray absorber and intrinsic absorption in the UV. However, the UV absorption often arises in multiple components some of which may be lower column density and lower ionization. The far-UV bandpass of FUSE provides a critical tool for understanding the nature and origin of this gas. The high spectral resolution of FUSE permits the isolation of multiple kinematic components in the absorption spectrum of O,VI facilitating the association of an UV absorber with its X-ray counterpart. Furthermore, O,VI is critical for establishing the connection between the lower ionization lines of C,IV and N,V seen in the UV with the high ionization absorption edges of O,VII and O,VIII seen in the X-ray. We propose to examine the near-nuclear gaseous environment of NGC,4593 by obtaining near-simultaneous observations of this target in the UV (HSTSTIS), far-UV (FUSE) and X-ray (XMM). We have been granted time with both HSTSTIS and XMM for contemporaneous observation of this target. The addition of contemporaneous FUSE observations of O,VI will greatly enhance our understanding of the ionization and kinematic state of the gas in the near-nuclear environment of this Seyfert,1 galaxy and provide a rare opportunity to probe the ionization state of the gas over a wide range of ionization levels.'),('C001',2,'A far UV study of high velocity atomic and molecular gas associated with the evolved Shajn 147 SNR','WELSH','BARRY','University of California, Berkeley',''),('C002',2,'FUSE Observations of LMC and SMC O3-4 Stars - the Physical Parameters of the Hottest Stars','MASSEY','PHILIP','Lowell Observatory',''),('C007',2,'Radiative Cascade Emission from Molecular and Ionized Gas in Planetary Nebulae','DINERSTEIN','HARRIET','University of Texas, Austin',''),('C008',2,'Mass Transfer in the Interacting Binary White Dwarf AM Canum Venaticorum','HOARD','DONALD W.','Cerro Tololo Inter-American Observatory',''),('C010',2,'Flares, Magnetic Reconnections and Accretion Disk Viscosity','WOOD','JANET H.','San Diego State University',''),('C011',2,'The Mass of the Classical Cepheid S Mus','EVANS','NANCY REMAGE','Smithsonian Astrophysical Observatory',''),('C017',2,'The early evolution of the circumstellar environment of solar-like stars','WALTER','FREDERICK M.','SUNY Stony Brook',''),('C018',2,'The Peculiar B Star HD 28867E','WALTER','FREDERICK M.','SUNY Stony Brook',''),('C020',2,'Time resolved spectroscopy of the sdB variable PG1605+072','DREIZLER','STEFAN','Universitat Tubingen',''),('C022',2,'Chromospheric Activity in Population II Giants','HARPER','GRAHAM M.','University of Colorado at Boulder',''),('C023',2,'Evolved Late-Type Star FUV Spectra Mass Loss & Fluorescence','HARPER','GRAHAM M.','University of Colorado',''),('C026',2,'FUSE Observations of Key DBA and DAB White Dwarfs','LANZ','THIERRY','University of Maryland',''),('C027',2,'Orions Veil, Magnetic Bomb or Gossamer Sheet','FERLAND','GARY','University of Kentucky',''),('C029',2,'A Face-On Collisionless Shock in the Cygnus Loop','RAYMOND','JOHN','CfA',''),('C030',2,'The Physics of AAL Quasars','SABRA','BASSEM M.','University of Florida',''),('C034',2,'Probing The Most Oxygen-Poor Halo Planetary Nebula','TOVMASSIAN','GAGHIK','San Diego State University',''),('C036',2,'Molecular Gas In The Disk-Halo Interface','BENJAMIN','ROBERT A.','University of Wisconsin-Madison',''),('C037',2,'A search for OVI emission from high-velocity clouds','BENJAMIN','ROBERT A.','University of Wisconsin',''),('C038',2,'Seeing Double - Do the X-Ray Luminous Early A Stars Have Active Binary Companions','SIMON','THEODORE','University of Hawaii',''),('C041',2,'A Study of the Inner Disk and Hot White Dwarf in Novalikes Above the Period Gap','SZKODY','PAULA','University of Washington',''),('C043',2,'The Stellar Wind of Deneb (Alpha Cygni, A2 Ia)','MORRISON','NANCY D.','The University of Toledo',''),('C046',2,'The Temperature Scale and Chemical Composition of DB White Dwarfs','PROVENCAL','JUDITH','University of Delaware',''),('C048',2,'A UV Spectroscopic Survey of Starburst Galaxies','HECKMAN','TIMOTHY','Johns Hopkins University',''),('C049',2,'Young Stellar Populations in Nuclear Starbursts and AGNs','PELLERIN','ANNE','Universite Laval',''),('C050',2,'The white dwarf companions of late-type B stars','BURLEIGH','MATT','University of Leicester',''),('C051',2,'Kinematics and Composition of O-rich Material in Puppis A','BLAIR','WILLIAM P.','Johns Hopkins University',''),('C052',2,'Absorption-Emission Line Study of the Northeast Cygnus Loop','BLAIR','WILLIAM P.','Johns Hopkins University',''),('C053',2,'The mass distribution of white dwarfs in cataclysmic variables','BARSTOW','MARTIN A.','University of Leicester',''),('C055',2,'The Distribution of Shock Velocities in N49 - a Bright Supernova Remnant in the LMC','SANKRIT','RAVI','The Johns Hopkins University',''),('C056',2,'Central Stars of Planetary Nebulae in the Small Magellanic Cloud','BIANCHI','LUCIANA','The Johns Hopkins University',''),('C057',2,'Observations of O VI Emission in the Halo of NGC 4631','MURPHY','EDWARD M.','University of Virginia',''),('C058',2,'O stars in M33','HUTCHINGS','JOHN B.','NRC of Canada',''),('C060',2,'AM CVn Stars - Structure and Evolution of Ultra-Short Period Interacting Binaries','FRONING','CYNTHIA','Space Telescope Science Institute',''),('C063',2,'Is Gas Really Cooling in Cluster Cooling Flows','BREGMAN','JOEL','University of Michigan',''),('C064',2,'The Flow Velocities in Elliptical Galaxy Cooling Flows','BREGMAN','JOEL','University of Michigan',''),('C067',2,'Fluorescence and Excitation of Molecular Hydrogen in the Circumstellar Environment of PMS Stars','LINSKY','JEFFREY L.','University of Colorado',''),('C068',2,'Why do some Dwarf Novae Stand Still','LONG','KNOX S.','Space Telescope Science Institute',''),('C070',2,'The Disk-Halo Connection in the Spiral Galaxy M101','OCONNELL','ROBERT','University of Virginia',''),('C073',2,'Probing the very small scale structure (l approx. 50 AU) in the interstellar medium (continued)','BOISSE','PATRICK','Ecole Normale SuperieureDEMIRM',''),('C076',2,'Constraining the Scale of Variations in the Hot Interstellar Medium','HOWK','J. CHRISTOPHER','The Johns Hopkins University',''),('C078',2,'Observing the Accretion Disk Around Miras Companion in the FUV','WOOD','BRIAN','University of Colorado',''),('C079',2,'The O I and N I Abundance in the Local Interstellar Cloud','WOOD','BRIAN','University of Colorado',''),('C080',2,'Far-Ultraviolet Spectra of a Supernova to be Named Later','KIRSHNER','ROBERT P.','Harvard University',''),('C081',2,'Weighing the Low-Redshift Lyman alpha Forest','SHULL','MICHAEL','University of Colorado, Boulder',''),('C083',2,'Probing the Reverse Shock in an Oxygen-Rich Supernova Remnant','GAETZ','TERRANCEJ.','Harvard-Smithsonian Center for Astrophysics',''),('C084',2,'O VI Absorbers in Spiral Dominated Groups of Galaxies','STOCKE','JOHN T.','University of Colorado, Boulder',''),('C086',2,'FUSE Observations of the Dwarf Seyfert Nucleus of NGC 4395','KRAEMER','STEVEN B.','Catholic University of America',''),('C088',2,'A search for the 10^5--10^6 K gas in clusters of galaxies with massive cooling flow','LECAVELIER','ALAIN','Institut dAstrophysique de Paris, CNRS',''),('C090',2,'Simultaneous FUSE, HST, and Chandra Observations of Intrinsic Absorbers in NGC 7469 and Mrk 279','KRISS','GERARD A.','Space Telescope Science Institute',''),('C092',2,'Simultaneous FUSE, HST, and Chandra Observations of the Seyfert Galaxies NGC 4151 and NGC 5548','CRENSHAW','D. MICHAEL','Catholic University of America',''),('C094',2,'A FUSE Study of the Planetary Nebula NGC 246','SZENTGYORGYI','ANDREW','CfA',''),('C095',2,'Monitoring the Intrinsic Absorption Complex Toward RX J1230.8+0115','GANGULY','RAJIB','The Pennsylvania State University',''),('C096',2,'The Influence of Weak Winds on DAO Abundances','FINLEY','DAVID S.','Eureka Scientific, Inc.',''),('C097',2,'The Wolf-Rayet Star HD 192163 And Its Surroundings','DUFOUR','REGINALD J.','Rice University',''),('C101',2,'O,VI Emission from the Cats Eye Nebula','GUERRERO','MARTIN','University of Illinois',''),('C102',2,'FUSE Observations of the Sun in Time - Transition Region Physics and Evolution of FUV Irradiances','GUINAN','EDWARD F.','Villanova University',''),('C103',2,'Eclipsing Binaries in the Large Magellanic Cloud Accurate Distances and Physical Properties','GUINAN','EDWARD F.','Villanova University',''),('C105',2,'FUSE observations of warm gas in clusters of galaxies and of Galactic OVI emission','BONAMENTE','MASSIMILIANO','University of Alabama in Huntsville',''),('C106',2,'Glimmers of Life in the Coronal Graveyard','AYRES','THOMAS R.','University of Colorado',''),('C107',2,'Coronal Iron Survey The Yellow Giants','AYRES','THOMAS R.','University of Colorado',''),('C109',2,'A search for OVI absorption in the halo of the Large Magellanic Cloud','BOWEN','DAVID V.','Princeton University',''),('C110',2,'Probing White Dwarf Accretors and Inner Disk Structure of High Accretion Rate Dwarf Novae','SION','EDWARD','Villanova University',''),('C111',2,'An Evolving Trio of Hybrid Stars','DUPREE','ANDREA K.','Smithsonian Astrophysical Observatory',''),('C114',2,'Coronal Dynamics and Complete Flare Energy Budget for the M Dwarf AD Leo','BROWN','ALEXANDER','University of Colorado',''),('C116',2,'A FUSE Determination of the Gravitational Redshift and Spectroscopic Mass of Sirius B','HOLBERG','JAY B.','University of Arizona',''),('C118',2,'The Atmospheres of High-Latitude Early B Stars','FITZPATRICK','EDWARD L.','Villanova University',''),('C123',2,'Intergalactic Ionized Helium Absorption toward the UV-brightest high-z Quasar HS 1140+2711','REIMERS','DIETER','Universitat Hamburg',''),('C125',2,'Scattering From Interstellar Dust Near Stars','HENRY','RICHARD C.','The Johns Hopkins University',''),('C126',2,'Tracing the Molecular Environments of Herbig Ae Stars with FUSE','GRADY','CAROL','Eureka Scientific',''),('C127',2,'Searching for Far-UV Fluorescence of Molecular Hydrogen in NGC 2023','MCCANDLISS','STEPHAN R.','The Johns Hopkins University',''),('C128',2,'How Does Abundance Affect the Strength of UV Emission in Elliptical Galaxies','BROWN','THOMAS M.','STScI',''),('C129',2,'The Formation Mechanism of Helium-Rich Subdwarf B Stars','BROWN','THOMAS M.','STScI',''),('C131',2,'Probing the Coronal Gas in Starburst Superwinds Through O VI Emission','HOOPES','CHARLES','Johns Hopkins University',''),('C132',2,'Probing Hot and Cold gas in Beta Pictoris Circumstellar Environment','BOURET','JEAN-CLAUDE','LAS de Marseille',''),('C133',2,'Investigating Argon, D/H, O VI, and other FUV emissions in Comets','WEAVER','HAROLD','Johns Hopkins University','We propose using FUSE to address several fundamental issues in cometaryscience: the abundance of the noble gas argon, the D/H ratio, and the nature of the X-ray, EUV, and FUV emissions from comets. We will use FUSE to make a sensitive search for line emission from argon, O VI, and several other species in a suitably bright comet ($V leq 7$) observed as a Target of Opportunity. The abundance of Ar is a sensitive probe of the formation temperature and evolutionary history of cometary nuclei, and FUSE observations can detect this noble gas even if its abundance relative to water is 10 times smaller than the value recently observed in C/Hale-Bopp (i.e., $sim$5 times less than solar). The presence of O VI at the predicted brightness would further clarify the role of charge exchange of solar wind ions with cometary neutrals as the dominant mechanism for producing x-rays in comets. If the comet has $V leq 5$, we also propose searching for the Ly-beta lines of D and H, as the deuterium abundance is an important indicator of cometary formation conditions. Accurate determinations of the D/H ratio in many comets are needed to determine whether or not they could have supplied most of Earth\'s water.'),('C134',2,'The Nova-Dwarf Nova Connection','DE MARCO','ORSOLA','American Museum of Natural History',''),('C135',2,'Jupiter\'s Heavy Ion Aurora: Coordinated FUSE, Chandra, and HST Observations','GLADSTONE','RANDALL','Southwest Research Institute','Recent Chandra observations have overturned our understandingof Jupiter\'s heavy ion auroras by showing that they 1) originate from a fixed location well inside the main FUV auroral oval and 2) pulsate with a 40-m period (they were expected to be associated with the Io Plasma Torus and appear equatorward of the main oval). The same high-latitude x-ray emitting region is also the site of intense FUV ``flares\'\' and a thermal IR hotspot. These unusual emissions may result from reconnection of solar wind plasma onto jovian magnetic field lines of the cusp region, or possibly from energetic S and O ions inside Jupiter\'s magnetosphere, but precipitating at great distances from the planet. Simultaneous Chandra x-ray and FUSE Lyman region spectra of the high-latitude aurora can distinguish between these two possible sources by allowing the correlation of x-ray heavy-ion events and the H$_2$ aurora on commensurate time scales, and by possibly detecting heavy-ion (e.g., OVI 103.2nm) emissions in the FUSE data. We note that during the recent Cassini flyby, none of the FUSE data overlapped with either the Chandra or HST observations. We are proposing 180ks of Jupiter auroral observations in coordination with those already proposed with Chandra and HST.'),('C138',2,'Atmospheric Eclipsing Binaries HR6902 and 22Vul','AKE','THOMAS B.','Johns Hopkins University',''),('C140',2,'FUSE Observations of Massive Evolved Stars in the LMC','KING','NICHOLE','Space Telescope Science Institute',''),('C141',2,'RR Tel getting under the flux limit -- an observation with FUSE','YOUNG','PETER R','Harvard-Smithsonian Center for Astrophysics',''),('C149',2,'Identifying the Physical Nature of Low z O,VI Absorbers','PROCHASKA','JASON X.','Carnegie Observatories',''),('C150',2,'Far UV Spectroscopy of X-Ray Novae','SHRADER','CHRIS','NASA Goddard Space Flight Center',''),('C151',2,'A Systematic Study of Colliding Winds in WR Stars. I. The Very-Short Period WC+O Binary HD36521','ST-LOUIS','NICOLE','Universite de Montreal',''),('C152',2,'Outbursts in Symbiotic Binaries Z And Continued Observation','KEYES','CHARLES D.','Space Telescope Science Institute',''),('C153',2,'Using FUSE to Measure the Galactic Halos O VI Intensity','SHELTON','ROBIN L.','Johns Hopkins University',''),('C154',2,'Eta Carinae Probing for the Physics','GULL','THEODORE','NASAs GSFC',''),('C155',2,'The Physical Conditions in Grand Design Stellar Wind Variability','OWOCKI','STAN','Univ. of Delaware',''),('C157',2,'A Study of the High Temperature Polar Plasma in B-Type Interacting Binaries','PETERS','GERALDINE J.','University of Southern California',''),('C158',2,'Heavy Element Abundances in Two B0-B0.5 Main Sequence Stars in the Small Magellanic Cloud','PETERS','GERALDINE J.','University of Southern California',''),('C160',2,'The Metallicity Dependence of the Bistability Jump in Hot-Star Winds','MASSA','DERCK','Goddard Space Flight Center',''),('C161',2,'Time-resolved spectroscopy of high field polars','BARRETT','PAUL','Space Telescope Science Institute',''),('C162',2,'Time-resolved spectroscopy of eclipsing polars','BARRETT','PAUL','Space Telescope Science Institute',''),('C163',2,'Geometry of hot outflows in Seyfert galaxies','SHASTRI','PRAJVAL','Indian Institute of Astrophysics',''),('C164',2,'Investigating OVI emission in the Eridanus Superbubble.','KORPELA','ERIC J.','University of California, Berkeley',''),('C165',2,'Observations of comet bombardment, planetary aurorae, and chromospheric activity in the young stars Epsilon Eri and Chi^1 Ori','HARRIS','WALT','University of Wisconsin','We propose to study nearby young stars for evidence of comets andauroral emissions from Jovian-class planets, and to monitor FUV diagnostics of chromospheric activity to increase our understanding of temperature, structure, and flares in cool star atmospheres. SOHO/SWAN observations of comet C/1995O1 (Hale-Bopp) and models of its (r $>$ 100000 km) optically thick H coma suggest that comets crossing our line of sight to their stars will attenuate stellar Ly-$eta$ emission over a narrow band corresponding to their astrocentric velocity. During the bombardment phase of planetary formation, the frequency of comets is much greater than the modern rate, increasing the likelihood of a transit occurring. Discovery of a transit would be significant for our understanding of planet formation and provide another technique for finding planet systems. FUV auroral emission on Jovian class planets that are near their parent star provides a potential means of directly observing these objects. Extrapolation from the Jovian aurora suggests that detection of a large planet inside of 1 AU is possible around a nearby active star. Our targets are the EMS active stars $chi^{1}$ Ori (G0, 9 pc, 100 Myr) and E Eri (K2, 3.3 pc, 1 Gyr). $epsilon$ Eri has a known planet of 1.2 Mj with a 0.7 AU perihelion distance.'),('C169',2,'FUSE Cycle 3 observations of the EG-AND eclipse ingress phases','ESPEY','BRIAN','Space Telescope Science Institute',''),('C171',2,'Study of the Elongated Superbubble Around Cyg OB1','NICHOLS','JOY','Smithsonian Astrophysical Observatory',''),('C172',2,'The Hot ISM of the Antennae - The Nearest Galaxy Merger','IPING','ROSINA','Catholic University of America',''),('C176',2,'Ionization Structure of the High-Excitation Planetary Nebula NGC 7009','IPING','ROSINA','Catholic University of America',''),('C177',2,'Temperature scale and metal abundances of hot hydrogen-rich central stars of planetary nebulae','WERNER','KLAUS','Universitat Tubingen',''),('C178',2,'Exploring the evolutionary status of the O(He) stars','RAUCH','THOMAS','Universitat Tubingen',''),('D003',4,'Further probing of the connection between the Local Interstellar Chimney and the Inner Halo','Welsh','','University of California at Berkeley','We shall observe the absorption characteristics of interstellar gas residing in the Local Chimney, which is an extension of the hot Local Bubble cavity that reaches into the inner-halo region. By combining these data with previous FUSE observations of this interstellar cavity we shall be able to accurately determine the kinetic temperature, electron density, element abundance/ depletions and gross velocity structure of gas in the Local Bubble as a function of increasing height above the galactic disk as it merges into the inner galactic halo. A key feature of these observations will be to detect infall of interstellar matter from the halo onto the galactic plane.'),('D004',4,'The eclipsing low-mass X-ray binary system X1822-37','Hutchings','','Herzberg Institute of Astrophysics','We propose FUSE observations to cover the 5.6-hour orbital period of the prototype eclipsing low-mass X-ray binary X1822$-$37. The system has a complex accretion disk structure which causes nearly continuous variations at all wavelengths. An accretion disk corona envelopes the binary, and X-rays heat the surface of the donor star. Because the compact star is a pulsar, the orbital parameters are well known. FUSE spectra covering the binary orbit, including through eclipse, will probe the hot inner disk by observing its high ionization emission lines, the outer disk via Lyman absorption lines, and the location of hot continuum sources. FUSE data will provide unique new information on the properties of the accretion disk, mass flows within the system, and the surrounding gas envelope. In 7 FUSE orbits we can sample the orbital period fully, accounting for earth occultations.'),('D005',4,'X0535-668 - An interacting neutron star - Be star binary','Hutchings','','Herzberg Institute of Astrophysics','We propose to observe the luminous LMC X-ray binary X0535$-$668 which consists of a highly interacting Be-star/neutron-star pair. During periastron passage in the very eccentric 16.65-day orbit (e$>$0.7), the neutron star plunges into the envelope of the Be star. Optical and IUE studies have shown that significant changes occur in the emission at all wavelengths. FUSE spectra will allow us to sample a wide range of ionization states to see how various species vary with orbital phase and hence infer their origin within the system. Study of O~VI resonance lines around the orbit will give information on mass loss from the system through its variable stellar wind and how it changes through the eccentric orbit. With FUSE data it will also be possible to detect any cool H$_2$ envelope that may surround the system.'),('D006',4,'Orbital variations of RX J0513.9-6951','Crampton','','NRC of Canada','In a successful Cycle 2 FUSE program we observed RX~J0513.9$-$6951 through its 16-hour binary orbit. The spectra revealed extraordinarily broad ($pm$ 3000 km/sec) O~VI emission with a velocity variation which appears to define the orbital motion of the accreting white dwarf, assuming the lines arise in the inner accretion disk. The FUV O~VI profile is unique, and it provides the only direct measurement of the component masses in a supersoft binary. However, the system is known to show non-orbital spectral changes as well as long-term changes in the disk structure. Since only slightly over one orbital cycle was observed by FUSE, we do not know if the measured velocities truly represent the WD\'s motion or if some non-orbital changes influenced the spectral lines. Therefore, we propose a second observational sequence in order to make a more definitive determination of the periodic O~VI velocity variations and hence the important stellar masses. We will also investigate the origin of the strong FUV continuum variations and the peculiar moving Lyman absorptions which were observed during our first series of observations.'),('D007',4,'FUV Monitoring the 2003 Minimum of Eta Carinae','Gull','','NASA/Goddard Space Flight Center','An unique opportunity will occur in early summer 2003 - Eta Carinae will go through its periodic minimum, which occurs every 5.52 years (2020+/-10 days). This very massive stellar system may harbor clues to the final evolutionary stages of massive stars before the supernova event, possibly even a Gamma Ray Burster event. Some have suggested that we may gain insight to the proposed very massive stars that likely formed of hydrogen and helium in the early Universe, perhaps before the first galaxies. We have considerable motivation to understand the physics of Eta Carinae and its ejecta. Systematic studies with HST/STIS since 1998.0, the time of the last minimum, have demonstrated that excitation and ionization of ejecta close to the central star(s) drop during the minimum, but return over the next year. Emission lines of doubly-ionized Fe, N, Ne, Si, and Ar disappear; Lyman alpha-pumped Fe II lines weaken, but Mid-UV and NUV continuum-pumped Fe II lines actually brighten! FUV radiation from the central source(s) is thought to drive this system. Attempts to model the central source as a single massive P-Cygni star have failed. Models of the X-Ray emission suggest wind-wind collisions of a binary star system with the companion being an early O-star! Recently we have determined that the apparent FUSE P-Cygni profiles are actually multiple absorption components from ejecta, not the stellar wind. During Cycle 4 we propose to observe the FUV spectrum directly, and monitor its changes across the minimum that influence the NUV, visible and near-red spectrum. These observations would be coordinated with Hubble Treasury and CHANDRA proposals already accepted for the upcoming minimum. FUSE will provide very important insight on the changes in excitation and ionization of the very clumpy ejecta that cannot be provided any other way. This may be the ONLY opportunity to obtain this information in the near future.'),('D008',4,'Molecular Hydrogen in the Lower Galactic Halo','Richter','','Osservatorio Astrofisico di Arcetri','FUSE is the first instrument allowing a systematic investigation of the abundance and properties of diffuse molecular hydrogen (H_2) beyond the local Galactic ISM. In a large survey, we have studied the H_2 content of intermediate-velocity clouds (IVCs) in the Milky Way halo with FUSE data available from the FUSE data archive. The quality of the archival data, however, is not sufficient to study in detail the physical processes in the IVCs that govern the formation and dissociation of H_2 in this gas. We therefore propose to observe three Galactic halo stars with FUSE to sample the molecular gas phase at good S/N in the Low Latitude Intermediate Velocity Arch (LLIV Arch), where H_2 has been detected before. This will allow us to investigate the properties of the cold neutral medium in these halo clouds, and will be important to better understand the abundance of diffuse H_2 in other galaxies and in the intergalactic medium.'),('D009',4,'The AG Dra nebula - a test for photoionization codes','Young','','Rutherford Appleton Laboratory',''),('D012',4,'Fe II Fluorescence in alpha 1 Her (M5Ib-II)','Harper','','University of Colorado, Boulder','We propose to study the fluorescent emission spectrum of Fe II and CrII from the M supergiant alpha_1 Her (M5 Ib-II). The strongest FUV features in the non-coronal evolved stars have been identified as fluorescent emission pumped from excited states by coincident stellar H Ly alpha radiation (Harper et al. 2001 ApJ 551, 486). A study of the fluorescent patterns reveals the shape of the intrinsic H Ly alpha radiation field which is otherwise not directly observable because of attenuation by the ISM, and also provides clues to the inhomogeneous structure of stellar chromospheres. Simulations of fluorescence patterns with trends in spectral-type, as suggested by the Wilson-Bappu effect, in the existing sample of cool stars observed by FUSE, are not in accord with the observation of Betelgeuse (M2 Iab). However, Betelgeuse is the only M supergiant that has been observed and alpha_1 Her fills an important gap in stellar parameter space of Teff, surface gravity and mass-loss rate. The proposed observation will help determine whether the fluorescence observed in Betelgeuse is a result of additional scattering in the overlying massive wind, or that the nature of the inhomogeneities in the stellar chromospheres does not follow simple trends in stellar parameters, but is instead related to the specific nature of chromospheric heating.'),('D013',4,'Volatile Abundances, D/H Ratio, and X-ray Emission in Bright Comets','Weaver','','The Johns Hopkins University',''),('D014',4,'Interstellar Fluorine Via the Nu Process','Federman','','University of Toledo',''),('D015',4,'The distance to high-velocity O VI absorption in the Galactic halo','Keenan','','Queen\'s University of Belfast','Previous FUSE studies have revealed the presence of large amounts of high-velocity ($mid$V$_{LSR}$$mid$ $>$ 100kms) hot gas towards Galactic halo sightlines, detected via ion{O}{6} absorption lines in high-velocity clouds (HVCs). However, these sightlines are all extragalactic, and hence the observations do not provide any insight into a crucial HVC parameter --- the distance. As part of a continuing program to investigate the distribution and origin of hot stars in the Galactic halo, we have obtained high resolution ($sim$,0.1ang FWHM) optical echelle spectra of many faint B-type Post-AGB stars at high Galactic latitudes. Detailed model atmosphere analyses of these spectra have allowed us to derive reliable atmospheric parameters, and hence determine stellar distances accurate to $sim$,20%. We have identified a sample of our stars at distances from the Galactic plane ({em z}) of up to 13,kpc, and which lie close in the sky (within 9deg) to AGNs with HVC ion{O}{6} absorption in their sightlines. The detection of HVC ion{O}{6} absorption in our stellar sample will show that this hot gas lies close to the Galaxy, and hence either originates from the Galaxy (e.g. a Galactic fountain or wind), or arises via some interaction with the Galaxy (e.g. cloud interactions with a Galactic corona). However null detections will also provide useful constraints, indicating that the HVCs are extragalactic in origin, such as intergalactic gas in the Local Group.'),('D021',4,'AU-Scale Interstellar H2 Structure Toward HD 37903?','Meyer','','Northwestern University','Based on high-resolution HST STIS observations over the 1165-1360 A wavelength region, Meyer et al. (2001) have discovered that HD 37903 (the illuminating star of the bright reflection nebula NGC 2023 in Orion) exhibits a rich spectrum of vibrationally-excited interstellar H2 absorption. A FUSE spectrum of HD 37903 obtained 20 months after the STIS observations and recently made publicly available in the FUSE data archive reveals excited H2 lines that are appreciably weaker than one would expect from the STIS data. If these variations are real, they would imply structure on scales of 1-2 AU in the foreground vibrationally-excited H2 gas of the NGC 2023 photodissociation region (PDR). We propose to obtain a higher S/N FUSE spectrum of HD 37903 and through a comparison with the initial FUSE data determine if and to what extent there are real temporal variations in the excited H2 absorption toward this object. These observations will provide a unique view of small-scale PDR structure that is well beyond the capability of near-IR H2 emission observations.'),('D023',4,'Abundances in the atmosphere of X-ray selected DA white dwarfs of intermediate temperatures','Vennes','','Australian National University','We have completed our optical survey of X-ray DA selected white dwarfs and built a new sample of 178 objects with well defined stellar parameters. Some 104 objects from this sample are joint detections in the ROSAT/PSPC and EUVE/lexan surveys; they range between temperatures of 24,000 and 84,000 K. We calibrated the PSPC/lexan count rate ratios and discovered a class of X-ray deficient DA white dwarfs with intermediate temperatures (26,000 < T < 40,000) which are most likely contaminated with heavy elements such as iron. We propose a direct spectroscopic identification of iron---and lighter elements--- in a sub-sample of four objects which would constitute the first evidence that trace heavy elements persist in the atmosphere of these objects at all temperatures. We interpret the phenomenon as evidence of on-going accretion from the immediate environment of the white dwarfs.'),('D024',4,'High Velocity OVI Emission in the Magellanic Stream and Complex C','Sembach','','Space Telescope Science Institute','We will observe a position near one AGN behind the Magellanic Stream (Fairall 9) to measure the O VI emission associated with the hot gas detected in O VI absorption along this sight line. Our goals are to [1] Quantify the amount of O VI emission associated with the O VI absorption in this direction toward the Magellanic Stream. [2] Estimate the physical conditions ($n_e$, $p/k$, etc.) in the gas and the likely cloud geometry by comparing the O VI emission and absorption-line strengths, and determining which hot gas models are capable of producing the observed emission/absorption ratios. [3] Lay the groundwork for future O VI emission-line maps with the SPIDR mission by observationally quantifying the amount of O VI emission expected in directions with O VI absorption estimates. The proposed observations will also provide HIRS aperture absorption-line spectra of the the extragalactic continuum source near the LWRS position.'),('D025',4,'The Enigma of AA Dor - is the secondary a planet?','Rauch','','Universitaet Erlangen-Nuernberg','AA Dor is a close binary consisting of an sdOB primary star and possibly a planet (M = 0.066 Msun). The planet may have survived a common envelope phase and has even gained mass. A recent spectral analysis of the primary based on high-resolution CASPEC and IUE spectra was hampered by the relatively long exposure times (1h and 2 -- 3h, respectively) and hence, a relatively large orbital velocity coverage. We propose high-resolution and high-SN spectroscopy with FUSE in order to determine precisely the photospheric metal abundances of the primary. The relatively short exposure time (10 * 200 sec) and the much better S/N ratio in the co-added spectrum at a higher resolution will reduce the error range in the abundance ratios by a factor of ten. Moreover, the high resolution allows to identify individual iron an nickel lines in the spectrum and thus, the iron/nickel abundance ratio can be analyzed. Since there still exists a discrepancy between the resulting stellar parameters from spectral analysis and those derived from the radial-velocity and the eclipse curves, the evaluation of the higher members of the Lyman series will additionally improve the determination of the surface gravity which should solve this problem. Moreover, from the comparison to evolutionary models we can derive the mass of the primary and derive the mass of the secondary, which is a candidate for the first planet found as a by-product of spectral analysis by means of NLTE model atmospheres.'),('D026',4,'Characterizing the generation of O VI ions in a hot-cold interface','Andersson','','The Johns Hopkins University','Five times ionized oxygen, OVI, is an important diagnostic of the interstellar medium (ISM) in both the Galaxy and in extragalactic environments, where it traces gas transitioning between hot and cool states. However, direct observations of such transition zones are few as the location and geometry of the individual regions are usually not known. We have, in a pilot study, identified one such OVI formation region in the outskirts of the Southern Coalsack molecular cloud, where X-ray emitting plasma interacts with a cool dense cloud. We will here further probe this hot-cold interface in order to elucidate the details of the gas mixing and OVI generating processes.'),('D027',4,'Physical Conditions and Baryonic Content of the Highly Ionized IGM','Savage','','University of Wisconsin','We propose to obtain 100 and 250 ksec integrations of the bright QSOs HE,0226$-$4110 (z = 0.495) and Ton,236 (z = 0.450) in order to study the physical conditions and baryonic content of the highly ionized IGM. The FUSE observations when combined with HST measurements from 1150 to 1800 AAwill permit the study of $sim$13 OVI IGM systems with rest equivalent widths $>$50 mAA. The redshifts of the QSOs and the presence of only weak interfering absorption from Galactic H$_2$ will allow us to probe multiple ion states of oxygen (OVI, OIV, and OIII) and possibly NeVIII. Having access to a range of ion states is crucial for determining the origin(s) of the ionization and the baryonic content of the highly ionized IGM.This is an important problem in observational cosmology since the first estimates (Tripp et al. 2000; Savage et al. 2002) imply that the highly ionized IGM is a major reservoir of the baryons in the universe at low redshift.'),('D028',4,'Intergalactic OVI absorption at redshift <0.004','Wakker','','University of Wisconsin Madison','Simulations of the formation of large-scale structure in the universe predict that at the present time a large fraction of the baryons is in a warm/hot phase, T=dex5--dex7 K. This gas probably has been detected in absorption through the OVI $lambdalambda$1031.926, 1037.671 doublet at redshifts of $sim$0.1--0.3. A value of dN/dz(OVI)=14$^{+9}_{-6}$ is derived for absorption with equivalent width $>$50 mAA. In our sample of 100 extra-galactic objects observed with FUSE, we find 5 such detections of OVI at redshifts $<$0.004, where 2 are expected for the redshift path of 0.099. We also find 7 more probable or possible OVI absorbers with EW$<$50 mAA. We propose to obtain improved data for the four most intriguing of these detections (toward Ton,S180, Mrk,876, PG,0844+349 and Mrk,478) in order to be able to accurately measure their properties, something that is not feasible with the current data. Three of these sightlines pass within 250 kpc of large, nearby spirals and may sample their halos. We should be able to determine the relation between the nearby galaxies and the OVI absorption and also whether these absorbers are similar to or different from the detections at higher redshifts.'),('D032',4,'Circumstellar Gas in Young Planetary Debris Disks','Roberge','','Carnegie Institution of Washington','Circumstellar (CS) disks orbiting young stars fall into two categories: primordial disks, composed of unprocessed interstellar dust and gas, and debris disks, produced by the destruction of solid planetary bodies. In the first class, the most abundant gas is H_2; in the second, it appears that the H_2 gas has disappeared, possibly through incorporation into gas giant planets. The lifetime of H_2 gas in a CS disk is therefore of great importance, as it dictates the timescale for the formation of giant planets.FUSE observations of H_2 in CS disk systems have shown that FUV absorption spectroscopy may sensitively probe for small amounts of gas along the line of sight to the star. Most importantly, the FUSE non-detection of H_2 gas in the Beta Pictoris disk suggests that the primordial gas lifetime is less than about 12 Myr, and that gas giant planets must form very quickly. However, this suggestion is based on one system, and needs to be tested in additional systems with a range of ages, especially since there are indications that age is not the only factor in the evolution of a CS disk. We propose for FUSE observations of 3 additional debris disk systems, Fomalhaut, HD3003, and HD2884. Fomalhaut is an intermediate age debris disk, one of the Fabulous Four CS disks first discovered in 1984. The other two disks are younger, with ages similar to that of Beta Pic. All three stars are brighter in the FUV than Beta Pic, permitting us to sensitively probe for traces of H_2 gas. We will also measure the amount of secondary atomic gas produced from planetary bodies in these disks, in an effort to understand the entire evolution of CS gas in young planetary systems.'),('D033',4,'Line Profiles and Variability in Ultra Rapid Rotators','Walter','','SUNY Stony Brook','We propose to obtain high S/N O VI line profiles for the ultra-rapid rotator PZ Tel. The goals are twofold - to detect and characterize the broad line wings that may arise in an extended region near the Keplerian corotation radius, and to study the transient absorption (prominence) events in high temperature gas. A 60 ksec observation of PZ Tel will sample about 1.7 rotation periods, after accounting for Earth occultations. The line profiles and the variability of the broad pedestal emission provide a test of the hypothesis that much of the chromospheric and coronal emission arises in an extended volume near the Keplerian co-rotation radius. We will organize simultaneous or contemporaneous observations at other wavelengths.'),('D034',4,'Central Stars of Planetary Nebulae in the Large Magellanic Cloud','Bianchi','','The Johns Hopkins University','We propose to complete our FUSE observations of Planetary Nebulae in the Magellanic Clouds, with the hottest LMC objects selected from the entire sample studied with HST. The flux in the HST UV and optical range is dominated by nebular continuum emission. Instead, the far-UV range reveals the spectrum of the central star (CSPN), uniquely enabling a direct estimate of the ionizing source parameters. The FUSE spectra provide a measurement of Teff, log g, L_bol, abundances, wind velocity and mass loss rate for these post-AGB stars. These parameters are needed to model the nebular dynamics and evolution, and constrain post-AGB evolution at low metallicity. Theoretically, metallicity affects several aspects of the post-AGB evolution, including mass loss and the yield of processed material, important factors in the chemical evolution of galaxies. Therefore, it is very important to observe PNe in different environments. Results for Milky Way, LMC and SMC CSPNe (combining our observations from previous cycles) will be compared with detailed post-AGB calculations. The brightest (but cooler) LMC CSPNe were observed in Cycle 2. The successful observations and results so far support our request to complete the sample of such objects accessible to the FUSE sensitivity, observing the LMC CSPNe with highest temperatures. The FUSE data are a unique contribution to constrain the properties of these objects, which are effectively at a single, unambiguous distance. FUSE spectra 1) disclose the central star spectrum, thus provide the only direct measurement of the ionizing source, and 2) provide a measurement of the circumstellar H_2 and HI, which - added to the mass of the central star and of the ionized shell- allows us to test theoretical initial-final mass relations, and to put together a complete picture of the star\'s evolution.'),('D037',4,'FUV Spectroscopy through the Pulsation Cycle of BW Vul','Smith, M.','','The Catholic University of America','BW Vul is a beta Cep star with an extraordinarily strong radial pulsation. It shows attributes of two shocks during its cycle: the first during the emergence of a pulsation wave and the second as a result of its nearly free-fall return. Each of these causes local heating. IUE studies have demonstrated that the primary shock can be observed in resonance lines moving outward through the wind for half a period. We propose FUSE observations of the star to follow the response of both photospheric and wind lines of many ions through a pulsation cycle. These time-serial spectra will constitute the first to be analyzed for the response of both photospheric and wind lines to a shock in any beta Cep star. The data will be analyzed using a progressively more sophisticated series of atmospheric models.'),('D039',4,'FUSE Observations of Coronal Gas in the Nuclear Outflow of NGC 3079','Hoopes','','The Johns Hopkins University','Galactic scale superwinds have an important impact on the evolution of galaxies and the intergalactic medium. However, the full extent of their influence is still in question, due to the lack of information on the ``coronal\'\' phase in the wind. Emission from this 10^5 - 10^6 K gas may dominate the cooling in the superwind, and thereby determine the evolution of the wind and its ability to deposit mass and energy into the intergalactic medium. We propose to observe O VI 1032, 1038 Angstrom emission from the coronal gas in the energetic outflow from NGC 3079. With these observations we will determine the cooling rate of the coronal gas. This will allow us to determine whether cooling strongly affects the dynamical evolution of the winds. We will also investigate the kinematics of the gas in the wind. Comparison of O VI emission with optical emission lines from warm gas and X-ray emission from hot gas will illuminate the physical processes that create the coronal gas, which will constrain the dynamical evolution of the wind. Together with our Cycle 3 observations of O VI emission in the M82 outflow and previous O VI absorption measurements in other starbursts, this project will provide much new information about the physics of superwinds.'),('D040',4,'Multiphase Observations of the Dwarf Starburst Galaxy NGC 625','Skillman','','University of Minnesota','Nearby dwarf galaxies offer an unique opportunity to study the multiphase ISM at high resolution. Of special interest are those galaxies which exhibit starburst activity, as they may represent nearby analogs to the star-forming galaxies seen in large numbers at higher redshifts. These objects display a complicated interplay of ISM phases, with molecular, neutral, ionized and coronal gases each tracing a different component or consequence of the star formation process. The high spectral resolution of FUSE in the vacuum UV provides the unique opportunity to study each of these phases simultaneously in relatively nearby galaxies. We therefore propose a deep FUSE integration of the Sculptor Group dwarf starburst galaxy NGC625. In particular we will study the coronal gas content and kinematics using the OVI 1032, 1038 Angstrom doublet in absorption, and the diffuse molecular component using the absorption lines of H_2 in the Lyman-Werner bands. These data will be compared with ground-based and HST optical imaging, XMM-NEWTON x-ray imaging and spectroscopy, high-resolution radio data, and forthcoming SIRTF mid-IR spectroscopy in a detailed multiwavelength study of this paradigm starburst galaxy.'),('D041',4,'Metallicity Determination in a Narrow Line Seyfert 1 Galaxy using Chandra, HST and FUSE observations.','Mathur','','The Ohio State University','By virtue of their extreme properties, narrow line Seyfert 1 galaxies (NLS1s) have given us crucial leverage on the key physical parameters underlying the AGN phenomenon (.m and $M_{BH}$). There is also suggestive evidence of super-solar abundance in some NLS1s, possibly as a result of rapid nuclear star formation in the early/rejuvenated phase of galaxy evolution. Our goal is to measure accurately the metallicity in a carefully selected NLS1 with high resolution X-ray, UV and FUV spectroscopy. We propose to observe with FUSE Mrk~1044 for which we have been awarded Chandra and HST time. FUSE will provide the crucial FUV range with observations of OVI, NIII and CIII. With these observations, we not only have a longer baseline in ionization stage, we also observe the crucial metallicity-sensitive nitrogen and oxygen lines. The combined X-ray, UV and FUV analysis will break the degeneracy between metallicity and ionization correction. This is not only important for understanding the NLS1 phenomenon, but also for investigating evolutionary aspects of active galactic nuclei.'),('D042',4,'Hot White Dwarfs in New Cataclysmic Variables','Szkody','','University of Washington','Among the approximately 100 new Cataclysmic Variables (CVs) currently found inthe Sloan Digital Sky Survey (SDSS) are 2 systems that are optically bright (about 15.5 mag in V) and show evidence of a hot continuum and high excitation emission lines of HeII. We will use FUSE to obtain the first UV spectra in order to characterize the white dwarf temperatures and compositions as well as the source of the remaining UV light (accretion column or boundary layer). Both objects show large variability on timescales of hours and stand out among the usual low mass transfer rate CVs being found by SDSS. Analysis of the FUSE spectra of these bright objects, in combination with the line and continuum variations throughout their binary orbits, will enable us to parameterize the accretions areas in these likely magnetic systems.'),('D044',4,'Towards the Origin of the Ubiquitous Small-Scale Structures in Hot-Star Winds','Moffat','','Universite de Montreal','All hot, luminous stars emit copious X-rays. However, the origin of the X-rays remains uncertain. The most likely scenario is that they essentially arise in regions of very hot shocked gas associated with radiatively driven instabilities throughout the winds. At the same time, variable subpeaks are observed on optical emission lines, that suggest the winds consist of a large number of stochastic clumps, probably following a size distribution dictated by compressible turbulence. Are the X-ray shocks and the clumps related? We propose to unveil the possible link between the hot shocked gas seen in X-rays and the wind clumping seen in optical emission lines by searching for variable structures in the O VI 1032, 1038 Angstrom emission feature, which must arise in superionization conditions related to the X-ray regions. We plan to monitor one carefully pre-selected target, a luminous hot star known to show a highly variable, structured wind - the single Wolf-Rayet star WR135 = HD 192103. This should lead to far greater understanding of the fundamental processes operating in hot-star winds. Failure to reveal the link will provide a challenge to current ideas on the variable substructures seen in virtually all hot-star winds.'),('D047',4,'Stellar Activity and Mass Loss from A and F Supergiants','Brown, A.','','University of Colorado, Boulder','We will obtain 30 ksec FUSE spectra of five A and F supergiants (spectral types A8 Ib to F8 Ib) that sample a section of the H-R diagram that is poorly explored in the FUV and UV, but which is crucial for understanding the causes of stellar activity and the role of mass loss on the evolution of massive stars. Previous FUSE spectra of the F0 Ib star Canopus provided excellent line profiles for transition region emission lines such as O VI and C III; profiles for similar lines in the UV are difficult to obtain due to the bright continuum. The proposed FUSE spectra will allow study of stellar activity indicators and the search for wind diagnostics; thus establishing whether the unusal properties of Canopus are typical of A/F supergiants.'),('D049',4,'Detailed FUSE Study of a Star Behind the Cygnus Loop','Blair','','The Johns Hopkins University','We will observe an sdOB star behind the Cygnus Loop supernova remnant to study the line-of-sight interstellar medium structures toward and through this prototypical remnant. The star was identified from Ultraviolet Imaging Telescope UV imaging and lies behind the bright NE Cygnus Loop filaments. New ground-based data and a preliminary FUSE Cycle 3 spectrum (program C052) demonstrate conclusively that the star is behind the supernova remnant. This is the first FUV background source known for the Cygnus Loop. We will re-observe this star to obtain improved signal-to-noise ratio data, and will also observe optically-emitting filaments directly adjacent, making a combined emission-absorption line study of the region possible. These two nearly complementary ways of studying the same region will provide the most detailed look to date at the workings of the Cygnus Loop blast wave as it encounters an interstellar cloud.'),('D053',4,'FUSE Observation of the \"Standard Star\" Vega','Cheng','','California State University, Fullerton','Vega (A0 V) has always been the primary spectrophotometric standard star. It was observed in 1984 with IRAS for calibration purposes, resulting in the startling discovery that Vega is surrounded by cool dust. Vega became the prototype for a class of young stars with infrared excesses implying circumstellar dust. Since then, Vega has been studied extensively at all wavelengths, and Vega-like stars have been the focus of many proto-planetary system studies. Vega\'s low Vsini implies that it is viewed nearly pole-on , so our line of sight does not pass through an equatorial disk, and we would not expect to see strong circumstellar absorption lines. We were surprised to find strong suggestions of circumstellar absorption lines in Vega\'s ORFEUS/BEFS spectrum. With the relaxed bright limit constraint, it is now possible to observe Vega with FUSE. This new observation could be used for FUSE\'s absolute flux calibration and for relative flux comparisons with other FUV instruments that have used Vega as a calibration target. Atmospheric models for early A stars that fit the ultraviolet continuum often do not fit the observed FUV continuum. A better absolute FUV flux calibration will permit us to improve atmospheric models for stars in this temperature regime.'),('D054',4,'The Sight Line to Mrk205: A Unique Opportunity to Investigate the Metal Enrichment of the Nearby Universe','Tripp','','Princeton University Observatory','The sight line to the AGN Mrk205 ($z_em = 0.071$) penetrates the foreground spiral galaxy NGC4319 ($z = 0.0043$) at a projected distance of 4 kpc from the galaxy center. The sight line also pierces a compact high-velocity cloud (CHVC) in the Milky Way halo or Local Group. Using absorption lines in the Mrk205 spectrum, we propose to study the metal enrichment, physical conditions, and gas kinematics in these contrasting objects. FUSE is crucial for this purpose because the unsaturated H~I, O~I, and N~I lines are all in the FUSE bandpass, as well as the best tracers of low-density, ionized gas, e.g., O~VI and C~III. With this observation, we will (1) Measure absolute abundances. The spiral galaxy and the CHVC have vastly different overdensities, and their metallicities provide a useful discriminant of enrichment theories. (2) Measure relative abundances to constrain the stellar populations that contribute to the enrichment. (3) Compare refractory species (e.g., Fe and Al) to non-refractory elements (e.g., O) to constrain the absorber\'s dust content. (4) Compare the high ions to the neutral gas tracers to search for highly-ionized outflows and/or evidence of interactions with an ambient medium.'),('D055',4,'A Search for Hot Baryons in the Intragroup Medium','Bowen','','Princeton University Observatory','It is possible that galaxy groups contain a substantial fraction of the expected baryons in the local universe, some of which should be detectable as intragroup gas. Gas within the group should have been shock-heated to temperatures of 10^{5-7}K as the group collapsed, cooler than the X-ray emitting material found in giant clusters, and possibly in a multiphase form. We propose observing several QSOs and AGN whose sightlines pass within 1.7~h-1 Mpc of nearby groups of galaxies, in order to search for OVI (and corresponding Lyman-beta CIII and/or NII) absorption lines from the intragroup medium surrounding the constituent galaxies. Two of the selected groups are known to have extended X-ray emission from ROSAT observations, the rest have only upper limits to the X-ray flux. Searching for absorption from _nearby_ groups is particularly useful since the environment, properties, and composition of the group can be more easily determined than at higher redshift.'),('D058',4,'Deuterium abundance measurements beyond the Local Bubble','Vidal-Madjar','','IAP - CNRS','Deuterium abundance measurements can be used to constrain the Big Bang Nucleosynthesis, the baryonic content of the Universe, and the chemical evolution of galaxies. Such measurements in a variety of astrophysical environments are one of the main objectives of FUSE. Since HI, OI, and DI have nearly the same ionization potential, the D/O ratio is an important clue to the D/H ratio and its putative variations. D/O is indeed very sensitive to astration, both because of DI destruction and OI production. The first FUSE results on the interstellar abundance of deuterium have showed that it is likely that the D/H and D/O ratios have both a single value in the local interstellar medium, but that they may present spatial variations beyond the Local Bubble. However, the reduced size of the sample of lines of sight analyzed so far does not allow definitive conclusions to be drawn. We selected 2 targets which were already observed with the FUSE large apperture. Long MDRS observations of them will allow us to perform accurate DI, NI, and OI mesurements. That will increase the number of abundance measurements beyond the Local Bubble, in the context of understanding the relationship between D, N, O, and H.'),('D059',4,'A FUV search of white dwarfs in unresolved binary systems','Barstow','','University of Leicester','Far UV images covering about 5% of the sky, obtained with the FAUST telescope, have detected several thousand UV sources. Many of these are associated with readily identifiable stellar sources. However, in more than 30 examples, there is a strong excess of UV flux compared what would be expected from the apparent identification. The most likely explanation of this excess is that these otherwise normal stars have a hidden hot subluminous companion, probably a white dwarf. We propose to obtain FUSE spectra of a sample of the UV excess objects detected by FAUST to confirm (or not) the present of a white dwarf companion. We will also include in our sample 3 stars identified to be binaries astrometrically, by Hipparcos, which have suspected white dwarf components. From comparison of the Lyman series lines with synthetic spectra, we will be able to measure the temperature and surface gravity in each case and ultimately determine the white dwarf mass. This will dramatically extend the sample of systems for which we have accurate white dwarf masses.'),('D063',4,'D/H and O/H within 500 pc of the Sun - Connecting Results From FUSE, Copernicus, and IMAPS','Friedman','','Space Telescope Science Institute','Recent FUSE measurements of the D/H and D/O abundance ratios in the local interstellar medium indicate that D/H is uniform within the local bubble, at distances <~ 100 pc. At greater distances, results from IMAPS and, to a lesser extent, Copernicus, show variability. Due to astration of D and enrichment of the interstellar medium by supernovae explosions, O/H is expected to be anti-correlated with D/H. Recently perhaps the first indications of this anti-correlation have been seen toward a very distant Galactic D/H target, but the situation is far from clear. We will measure D/H and O/H toward two very bright stars previously observed with Copernicus or IMAPS, in order to test for previously undetected systematic errors or instrumental signatures in these unexpected results. The targets are gamma 2 vel and lambda sco. The sight lines span a wide range of D/H values, 2.18e-5 and 0.76e-5, which make them particularly interesting values to confirm. They are at distances 260 and 215 pc.'),('D064',4,'Chlorine in the Interstellar Medium','Sonnentrucker','','The Johns Hopkins University','Cl I and Cl II exhibit absorption transitions exclusively in the far ultraviolet and were, hence, first detected with the Copernicus and IUE satellites. A few surveys were carried out to better constrain empirically the oscillator strengths of those newly detected lines, study the abundance of this species in the ISM and search for depletion but large uncertainties remain. We propose to determine empirically the f-value of the Cl I lines using 8 low-to-highly reddened stars. We will derive the column density of Cl I, Cl II and H2 and estimate the chlorine abundance for our star sample. We will test whether the correlation found between Cl I, Cl II, H I and H2 for low-to-moderately reddened stars extends to the higher reddening accessible to FUSE. We recently showed that chlorine plays an important role in the search for translucent components along often complicated lines of sight. We will, therefore, use our measurements to search for these components, constrain their local molecular fractions and search for depletions, expected in those components.'),('D065',4,'Probing the Evolution of Stellar Activity in Young A Stars with FUSE','Grady','','Eureka Scientific','Spatially resolved spectroscopy of several Herbig Ae stars at Lyman alpha has demonstrated that these stars drive collimated, bipolar outflows through much of their pre-main sequence evolution, and therefore closely resemble young solar-mass T Tauri stars. For those objects, the stellar magnetic field is important in channelling material accreting onto the star and in collimating the outflow. Older A stars, in general, do not exhibit X-ray emission or FUV emission lines indicating the presence of stellar activity associated with a magnetic field, but recent FUSE observations of beta Pic indicate that such activity persists into at least the early phases of an A star\'s main sequence lifetime. At present we do not know the frequency, duration of such activity, nor do we know whether activity signatures are enhanced in systems with protoplanetary or debris disks compared to coeval stars lacking disks. These are the questions we will address by supplementing the current FUSE archival holdings of actively accreting Herbig Ae stars and the brightest debris disk systems with observations of older Herbig Ae stars, and a suite of comparison A stars which are members of nearby stellar associations with secure age measurements.'),('D066',4,'Surveying the sight lines of subdwarfs and white dwarfs beyond the Local Bubble','Hebrard','','IAP - CNRS','Deuterium abundance measurements allow constraints to be put on Big Bang Nucleosynthesis, the baryonic content of the Universe, and the chemical evolution of galaxies. Such measurements in a variety of astrophysical environments are among the main objectives of FUSE. Since HI, OI, and DI have nearly the same ionization potential, the D/O ratio is an important clue to the D/H ratio and its putative variations. D/O is indeed very sensitive to astration, both because of DI destruction and OI production. The first FUSE results on deuterium interstellar abundance shown that it is likely that the D/H and D/O ratios have both a single value in the local interstellar medium, but that they may present spatial variations beyond the Local Bubble. On the other hand, D/N appears to be a less accurate D/H proxy because of ionization effects. However, the reduced size of the sample of lines of sight analyzed so far does not allow definitive conclusions to be drawn. We propose here a survey of targets located outside the Local Bubble, in order to select good candidates for deuterium measurements. The final goal is to perform long exposures of the selected targets during Cycle 5.'),('D071',4,'The evolution of CVs: Clues from FUSE observations of Post Common Envelope Binaries','Gansicke','','University of Southampton','Cataclysmic variables (CVs) represent an important class of close interacting white dwarf + K/M dwarf binaries which routinely serve as astrophysical laboratories for the study of accretion discs and of plasma phyiscs at extreme temperatures and B-fields. However, it is precisely the accretion-related emission in CVs which makes accurate measurements of their binary parameters extremely difficult - and without the detailed knowledge of fundamental properties, such as their stellar masses, our understanding of the evolution of CVs is severely limited. Post Common Envelope Binaries (PCEBs), close but detached white dwarf/late type star binaries, will eventually evolve into CVs through the loss of angular momentum. The absence of mass transfer in these systems permits to determine their binary parameters at a level of precision unachievable in CVs, and measuring these parameters for an ensemble of PCEBs holds great potential for improving the theory of close binary evolution. Here, we propose to observe with FUSE four PCEBs (HR Cam, LM Com, RX J2130.3+4709, and KPD 2154+4048) in order to derive the effective temperatures, masses, photospheric abundances, and rotation rates of their white dwarf primaries.'),('D073',4,'The Abundance of Interstellar Fluorine','Lauroesch','','Northwestern University','We will obtain high signal-to-noise ratio FUSE observations of the interstellar neutral fluorine absorption lines at 951 and 954 Angstroms toward the star HD103779 in order to determine an accurate gas-phase abundance of fluorine. The nucleosynthetic source(s) of fluorine are still a matter of debate -- the present day abundance of fluorine can potentially constrain models for pulsationally driven dredge-up in asymptotic giant branch stars. An accurate measure for the depletion behavior of fluorine will determine whether it may be detectable in quasar absorption line systems -- an unambiguous detection of fluorine at suitably high redshifts would provide the best evidence to date for the neutrino process in massive stars. Furthermore, due to its extreme reactivity, measurement of the gas-phase interstellar fluorine abundance is important for models of gas and grain chemistry. Despite the importance of measuring the interstellar fluorine abundance, only one previous detection has been made due to the low relative abundance of fluorine, the lack of lines outside the far-ultraviolet, and blending of the available transitions with lines of molecular hydrogen. The detection (or stringent upper limits) on the strength of the weaker 951 Angstrom line is essential in determining an accurate fluorine abundance.'),('D075',4,'A New Spin on FK Comae','Ayres','','University of Colorado, Boulder','FUSE observations of the ultra-fast rotating Hertzsprung gap giant FK Comae (G5 III; v-sin-i= 160 km/s) will exploit the phenomenon of super-rotational broadening to test whether such stars have extended co-rotating regions of 100,000 K subcoronal gas. Extended emission zones are expected in a magnetospheric scenario that describes a possible fundamental dramatic change in magnetic activity as rapidly evolving moderate-mass giants first enter the convective part of the H-R diagram. A 15 ks exposure will obtain moderate S/N profiles of O VI 1032 and C III 977, suitable to test the super-rotation hypothesis.'),('D076',4,'Probing absorber kinematics with simultaneous FUSE and Chandra HETGS observations of Mrk 290','Lee','','MIT Center for Space Research','We propose a 50~ks FUSE observation of the Seyfert~1 galaxy Markarian~290 to overlap with some portion of the planned 250~ks Chandra HETGS observation in spring/early summer 2003. Such an observation will allow us to resolve the kinematics and ionization states of both the X-ray and UV absorbers in this source, and search for any kinematic (in)consistencies.The proposed simultaneous look will provide the necessary information for assessing the relationship and location of these absorbers. We will additionally search for possible O VI absorption which may be attributable to the ``missing\'\' baryons found in the warm-hot component of the intergalactic medium.'),('D078',4,'Vela Knot D - Kinematics of a Bow Shock','Sankrit','','The Johns Hopkins University','Knot D, one of six X-ray features outside the boundary of the Vela supernova remnant, is believed to be a bow shock driven by a fragment of supernova ejecta (though a Chandra spectrum showing normal abundances casts doubt on the nature of the driver). The emission at the edge of Knot D is broadly stratified - there are optical filaments along the edge, but separated from the brightest X-ray emission by a gap of about one arcminute. Such a gap has not been seen in any other supernova remnant shock, and is most likely the consequence of the physics of bow shock dynamics. The region, in between optical and X-ray emitting gas and therefore likely to have intermediate properties is best explored in the far-ultraviolet. We propose a set of four observations to study the temperature structure, the kinematics and the shock velocity variation in Knot D. We will observe three regions (optical, the gap, and X-ray) near the edge and one position farther behind the apex. We will use the C III (low ionization) and O VI (high ionization) emission detected by FUSE to obtain the progression of properties of the emitting gas. The observations will allow us to study the dynamics of an evolving bow shock. Bow shocks are frequently invoked in the interpretation of emission from a range of objects such as jets from young stars and active galaxies, and Knot D presents an example of a simpler case when the shock is non-radiative over most of its surface.'),('D079',4,'Temperature Variations in Slowly Pulsating B Stars','Massa','','SGT, Inc','We intend to use FUSE observations to determine temperature variations of a Slowly Pulsating B star throughout its pulsation cycle. Precise measurements of the temperature changes are essential for interpreting the optical observations of this important class of objects which are potential candidates for astro-seismology studies. We demonstrate that for late B stars, the FUSE wavelength band provides a sensitive and robust temperature diagnostic that is unavailable at any other wavelength.To determine the best star to monitor, we require single observations of four potential targets.'),('D080',4,'FUSE Observations of Two Schizophrenic Magnetic CVs: PQ Gem and V405 Aur','Howell','','Planetary Science Institute','V405 Aur is one of a small class of Intermediate Polars (IPs) which show strong, soft X-ray emission, have properties of both IPs and Polars, and are likely to evolve into AM Herculis stars (Polars), within a short astronomical time. Decomposition of PQ Gem (the brightest member) has identified three or more spectral components and the modulations of these components (both the lines and continuum) phase with the white dwarf spin period, the binary orbital period, and the beat period between these two. ORFEUS observations of PQ Gem provided the first look into the FUV spectral range but were too brief (0.4 of the orbit) to allow detailed analysis. However, strong FUV line emission (C, He, and O) was observed as well as complex line behavior probably related to the WD spin interaction with the partial accretion disk. We propose here to obtain the first detailed time-resolved FUV observations of the second brightest member of this small sub-class of objects, V405 Aur.'),('D084',4,'The Youngest, Most Massive Star Clusters in M33','Bianchi','','The Johns Hopkins University','Young massive clusters, which appear to be abundantly forming in merging galaxies, but are not found in the Milky Way, provide the opportunity to study the conditions necessary for the formation of massive, compact stellar systems. This insight into conditions present during the earliest epochs of galaxy formation, when ancient globular clusters (GC) are believed to have formed, helps constrain scenarios of galaxy formation and evolution. We propose to observe two extremely young, UV-luminous star clusters in the Local Group spiral galaxy M33. These young, massive, and compact objects provide a key link to the young cluster systems in mergers, where our insight is currently limited, and these may be the only such counterparts accessible to the FUSE sensitivity. The objects are selected from our previous extensive survey of M33 with HST WFPC2 imaging in 4 bands (U, B, V and 1700A) and optical spectroscopy. From multiband integrated photometry we determined age upper limits of a few million years for our target objects, by comparison with synthetic single-age population evolutionary models. Spectra in the FUSE range will provide precise ages for these objects, and unambiguously reveal their properties, by comparison with synthetic model spectra of extremely young single-stellar populations, and by the analysis of the strong spectral signatures that will reveal the massive star content. The wind momentum and UV radiation flux from the massive stars will be compared with gravitational properties of each cluster (from mass estimates and light profiles), to assess whether such systems can survive internal dynamical evolution.'),('D088',4,'Spectacular Wind-Collision Effects in the LMC Binary Brey22','St-Louis','','Universite de Montreal','We propose to secure a time sequence of ultraviolet (UV) spectra for the 14.9-day WC4+O5-6 LMC binary Brey 22 to study the structure of the bow shock zone formed when the winds of the two hot stars collide. This will lead to constraints on orbital parameters and on characteristics of the WR star itself. Of particular importance in the FUSE wavelength range is the presence of a broad spread of emission lines with different ionization potentials, ranging from OVI to CIII.These lines are expected to arise in the bow-shock zone at progressively larger distances from the X-ray heated bow-shock head as the compressed plasma flows outward along the shock-cone and cools. The study of how these lines vary with orbital phase will allow us to map out the structure and kinematics of the bow shock. This in turn will provide useful constraints on the basic parameters of the winds as well as the collision process itself. Brey 22 is a particularly good example of a system in which wind-wind collision effects are known to be strong. Among the 5 WC/WO+O binaries observable with FUSE in the Galaxy and the Magelanic Clouds, this is the last one to be examined. We will compare its behavior with our data already obtained for the other four systems. By examining a limited number of binaries with different WC types and different orbital separations, we will be able to test how the wind-wind collision process depends on wind density, speed and ionization state.'),('D089',4,'FUSE Observations of Neutron-Capture Elements in Wolf-Rayet Planetary Nebulae','Dinerstein','','University of Texas at Austin','We propose to obtain FUSE observations of planetary nebula central stars of the WC Wolf-Rayet ([WC]) class, in order to search for the products of neutron-capture processes in these stars and provide constraints on their evolutionary status. Although the origin of the [WC]\'s is controversial, their H-deficient, C-rich surface compositions indicate that they have experienced a high degree of mixing and/or mass loss. Thus one might expect the nebulae they produce to show enhanced concentrations of He-burning and other nuclear products, suchas nuclei produced by slow neutron capture during the AGB phase. We have already detected an absorption line from one such element, Germanium (Sterling, Dinerstein, & Bowers 2002), while conducting a search for H2 absorption from nebular molecular material FUSE GI programs A085 and B069). Since the strongest Ge enhancements were found in PNe with [WC] central stars, we propose to enlarge the sample of such objects observed by FUSE. THIS TEMPORARY AND PARTIAL SCRIPT COVERS ONE TARGET, HE 2-99, AND REQUESTS AN EXPOSURE TIME OF 15 KSEC. PHASE 2 INFORMATION FOR THE REMAINDER OF THE PROGRAM\'S TOTAL TIME ALLOCATION OF 60 KSEC WILL BE SUBMITTED AT A LATER TIME.'),('D092',4,'FUSE Observations of Orbital and Rotational Variations in the Unique System HS1136+6646','Holberg','','Lunar and Planetary Laboratory','HS1136+6646 is a recently discovered close binary system consisting of a hot Teff ~120,000 K DAO white and a K6V main sequence primary. It is unique in being a relatively bright nearby example of both a very young post-common envelope system and a pre-cataclysmic variable system. Although the system has been well observed from the ground, the white dwarf can only be effectively studied, from space, at UV wavelengths. We propose extended FUSE observations of the HS1136+6646 which focus on the nature of the white dwarf, its mass, temperature, photospheric composition and possible magnetic field. Observations covering the entire 0.83607 day period orbital of the system will provide the first accurate determination of the velocity curve for the hot DAO white dwarf and hence the system mass ratio. A photometric time series from these same observations will help establish the hypothesis that the low amplitude modulations seen in the optical light curve are associated with the rotation of the white dwarf.'),('D098',4,'New FUSE Stellar Observations in the Large Magellanic Cloud','Blair','','The Johns Hopkins University','We propose FUSE observations of a select set of stars in the Large Magellanic Cloud to build on and improve earlier work in significant ways. A set of 22 stars has been pared to 12 in Phase 2 to fit into the TAC allocation. We propose 6 new sight lines in close proximity to previously observed stars to provide more detailed sampling of coherent sub-structures in the LMC such as bubbles or shells. A set of 4 sight lines to stars in the previously unobserved superbubble N70 will provide a detailed study of this region. Also, building on our earlier detailed analyses of LMC sightlines, we will re-observe 2 objects whose current LWRS aperture data sets are contaminated by nearby stars and are useless for ISM work. Using MDRS will isolate the stars of interest and will provide ``new\'\' sight lines in the important 30 Doradus region. Observing these new sight lines will leverage the much larger LMC data set by providing better studies of ISM sub-structures.'),('D099',4,'Doppler Imaging a Late-A Star in the FUV','Redfield','','University of Colorado at Boulder','FUSE, STIS, and Chandra observations show that plasma heated to temperatures of 10^4 K to > 10^6 K is present in the outer atmospheres of late-type dwarf stars including the late-A type stars. Aside from the detection of coronae in late-A stars and the emission rates from these hot plasmas, we know very little about their structure and heating mechanisms. FUSE has the unique capability to provide new information on both of these two questions. FUSE can Doppler image rapidly rotating late-A stars in lines of C III and O VI. If the hot plasma is located primarily in bright active regions, then the shapes of these emission lines will change with time as the active regions rotate on to one limb and off of the other limb. The existence of active regions will tell us unambiguously that the hot plasma is magnetically confined and magnetically heated, rather than heated by acoustic waves. Our target is Altair, for which existing FUSE spectra of the O VI and C III emission lines have a horned appearance, indicating that emission near the limbs can be resolved due to the rapid rotation of the star. We propose to observe Altair through multiple rotational periods.'),('D101',4,'Quasi-molecular satellites of Lyman lines in ZZ Cetis','Allard','','IAP - CNRS','Quasi-molecular satellites are due to transitions which take place during collisions of the radiating hydrogen atom and a perturbing atom or ion. These spectral features provide an important source of opacity in the DA white dwarf atmospheres in the red wings of Lyman series lines. From theoretical profiles it can be predicted that both H2 and H2+ satellites of the Lyman-alpha and Lyman-beta lines should be detectable in a small range of temperature (between 14000K to 11000K). We will observe two variable DA in the ZZ Ceti range. The spectra of these stars should allow us to detect the H2+ quasi-molecular features at 1060A and 1080A, and, for the first time, a broad H2 quasi-molecular feature at 1150A, a spectral region being studied in concurrent laboratory experiments. In combination with existing optical and ultraviolet data, they will allow us to determine accurate stellar parameters for these stars which are among the few white dwarfs defining the blue edge of the ZZ Ceti instability strip. These stars will be the coolest white dwarfs observed by FUSE so far, will extend our understanding of Lyman line profiles, and will provide insights crucial in the modeling of cool white dwarf atmospheres.'),('D103',4,'Probing the Physical Nature of the Cosmic Web with Extreme Ultraviolet Spectroscopy','Howk','','University of California San Diego','We will observe two moderate-redshift (z=0.574, 0.631) quasars o study the physical state of warm-hot intergalactic medium (WHIM) absorbers using EUV transitions redshifted into the FUSE bandpass. We will measure the column densities of multiple ionization states of oxygen (O II, O III, O IV, and O V) complementing HST observations of O VI), as well as of the very highly-ionized species Ne VIII and Mg X in intervening IGM absorbers along these three sight lines. We will model the ionization balance of these systems to determine the extent to which they are affected by photoionization and, therefore, whether they represent the shock-heated WHIM predicted by the simulations or simply trace the metal-enriched Lyman-alpha forest. We will also investigate the connection between WHIM absorbers and large-scale galaxy structures by combining our FUSE observations with galaxy redshift measurements obtained using DEIMOS on Keck and the WFCCD at Las Campanas Observatory.'),('D107',4,'Modeling Transition Region Wind Dynamics of F-type Supergiants','Lobel','','Smithsonian Astrophysical Observatory','We propose to observe the bright F-type Iab supergiant Beta Dor,to investigate and model the wind acceleration physics and thermal structure of transition region plasma in the extended outer atmosphere of this unique star. This investigation will provide important clues about the acceleration mechanisms that drive the high-temperature supersonic winds of cool supergiant stars. Previous FUSE observations of the early G-type hybrid supergiant Alpha Aqr (G2 Ib), and HST-STIS observations of Beta Aqr (G0 Ib) show evidence for the formation of P Cygni-type profiles in high-temperature transition region plasma emission lines of C III 977 A, C IV 1551 A, and Si III 1206 A. Our semi-empirical non-LTE radiative transfer modeling reveals that in Alpha Aqr the C III 977 A line forms in a supersonic transition region wind, which quickly accelerates above the upper chromosphere, with a steep increase of the kinetic gas temperature into the lower transition region. The model indicates outflow velocities above ~140 km/s at temperatures of 65,000 K and higher. Asymmetric O VI resonance emission lines in Alpha Aqr and Beta Dra (G2 Ib-II) reveal substantial scattering opacity in the upper transition region. FUSE observations of Beta Dor (F6) will reveal if the wind acceleration mechanism at high atmospheric temperatures is correlated with the larger effective temperatures of F-type supergiants, and if so, demonstrate the importance of the radiative wind driving mechanism with detailed radiative transfer fits in spherical geometry to the C III 977 A (and O VI) line(s). The proposed FUSE observations offer a unique opportunity to constrain the outflow dynamics and thermal structure of transition region plasma above the chromospheres of F supergiants. These observations are important for studies of heatings mechanisms at very high atmospheric temperatures and the related mass-loss mechanisms, which play a crucial role for the evolution of late-type stars.'),('D108',4,'The Fe XVIII 974A Line; A New Tool for Measuring the Size and Dynamics of Stellar Coronae','Redfield','','University of Colorado at Boulder','FUSE spectra of active late-type stars contain the Fe XVIII 974 A coronal emission line. The spectral resolution and wavelength scale (relative to nearby interstellar absorption lines) of FUSE permit us to measure the line width and velocity shift of this coronal emission line, providing a new window on stellar coronal dynamics and structure. We propose to use this new tool to measure the widths and Doppler shifts of the Fe XVIII line in rapidly rotating stars. In a survey of coronal emission lines observed in late-type stars by FUSE, Redfield et al. (2002) found that the Fe XVIII line width is thermal for slowly rotating stars, but for rapidly rotating stars the line is much broader than predicted given thermal and rotational broadening at the photospheric value of v sin i. They proposed that the extra width of the Fe XVIII lines in the rapidly rotating stars is due to geometrically extended coronae rigidly rotating with the star. However, the available line profiles are very noisy, and this important new tentative result must be confirmed by deeper observations of the previously observed stars.'),('D109',4,'Phase-Resolved Spectroscopy of Eclipsing Polars','Barrett','','Space Telescope Science Institute','Eclipsing polars have long provided important information about the structure and dynamics of magnetic cataclysmic variables (mCVs) by providing precise information about the location of the emitting gas within the binary system. Previous such studies have shown that the X-ray and FUV (S III, S IV, Si IV, O VI) emission lines are located on or very near the white dwarf surface, while the optical and near-UV emission lines are predominantly from the surface of the secondary star. However, EUV and FUV observations of some eclipsing CVs show these emission lines to be present throughout the eclipse, indicating a third location for the EUV and FUV emission lines that is displace from the two stars. We propose phase-resolved observations of several eclipsing polars to better understand the far UV emission in these binaries. The combination of eclipse mapping and doppler tomography will enable us to make detailed maps of the accretion stream and to better understand the location of the EUV and FUV line emission regions.'),('D113',4,'The O6.5IIIef Star BD +60 2522','Dufour','','Rice University','Of-type emission line stars are thought to represent a short-lived phase in the evolution of massive stars, intermediate between the main sequence and Wolf-Rayet stages. The increase in wind luminosity affects not only the mechanical input into the star\'s surroundings, but presumably the shape of the stellar ionizing continuum. Observations of these relatively rare stars provide valuable insight into the post-main sequence evolution of massive stars and the impact on their environments. One peculiar subclass of Of stars exhibits, in the morphology of its emission lines, the hallmarks of both rapid rotation and a strong stellar wind. Designated as Oef, one member of this stellar type is BD+60 2522, whose UV flux ionizes the HII region NGC 7635 (S 162). The ram pressure of the wind has swept nearby material from the HII region interior into a spherical bubble. In addition, there are complexes of knots in proximity to the star; images of the region imply an area of strong interaction between the stellar wind and the photoevaporative flow from the closest of the knots. We propose to observe BD+60 2522 with FUSE to better determine the stellar and wind parameters of the star and the corresponding impact on its local environment, using a unified model atmosphere code already developed.'),('D114',4,'V592 Cas: A study of a bipolar outflow and precessing accretion disk','Long','','Space Telescope Science Institute','We propose to use the unique capabilities of FUSE to explore the time-dependent behavior of the bipolar outflow of the low-inclination, nova-like cataclysmic variable V592 Cas. Our previous FUSE monitoring of the nova-like system RW Sex revealed extensive variability in the UV resonance lines, entirely confined to blue-shifted velocities, and modulated on a time-scale close to the system orbital period. This surprising result implies that the outflow in RW Sex is not axisymmetric with respect to the disk plane! V592 Cas has optical emission lines that suggest wind line variability similar to RW Sex. However, unlike RW~Sex, V592 Cas has been studied carefully using time-resolved optical photometry, resulting in the discovery of permanent negative superhumps. This is a sure sign of a warped, precessing accretion disk in this system. By observing V592 Cas on three occasions, we propose to establish that the wind in V592 Cas varies on near orbital time-scales and then to determine whether the asymmetry in the wind is associated with the superhump asymmetry or phenomena, e.g. a disk-stream interaction, that would be expected to produce wind variations at precisely vary the orbital period.'),('D115',4,'The Holely Coronal Graveyard','Ayres','','University of Colorado, Boulder','A 100 ks FUSE pointing will probe the O VI and C III emissions of an archetype denizen of the coronal graveyard--Aldebaran (Alpha Tauri; K5 III). HST spectra suggest the possible--surprising--presence of solar-like magnetic activity on the old, spun-down red giant. But, many of the characteristic 1150-1500 A UV emissions apparently are extinguished by a cool absorber overlying the hot (100,000 K) structures. Detection of O VI by FUSE suggests that the cool absorber opacity thins out just above the LyC edge, so O VI 1032 (and C III 977) could be a sensitive probe of the submerged activity through the far-UV opacity hole. The deep pointing will achieve high S/N, to search for discrete absorption structure in the hot lines, impressed on them by the cool absorber; and will allow an assessment of temporal variability due to the heating process, which might be convective-acoustic but probably is magnetic. If the latter, the buried magnetic activity on red giants possibly plays a key role in driving their winds--a long-standing astrophysical mystery, and a crucial component of galactic chemical evolution. The existing FUSE spectrum is too low in S/N to unambiguously measure discrete absorption components, and its singular nature precludes any variability analysis.'),('D117',4,'O VI and C IV Emision in the \"Local Interstellar Chimney\"','Benjamin','','University of Wisconsin-Madison','We propose to characterize the diffuse OVI emission and absorption in two directions where diffuse ultraviolet CIV emission has already been detected, near Mrk 153 ($l=155^{circ}$, $b=58^{circ}$) and 3C249.1 ($l=130^{circ}$, $b=39^{circ}$). The comparison of the OVI emission to absorption will constrain the density and pressure of the emitting gas. The OVI emission will also be compared with the detected CIV 1549 AA line, as well as diffuse optical line emission (H$alpha$, [SII],[NII], [OIII]) and broadband ROSAT X-ray emission. The combination of these measurements will be used to diagnose whether the emission arises in shocks, cooling zones, mixing layers, or conduction fronts. For Mrk 153, this observation will also allow us to confirm if there is high velocity OVI emission corresponding to the high velocity OVI absorption known to exist along this line of sight. For 3C 249.1, the data will be combined with archival CIV absorption data from a 50 ksec HST STIS observation. This will allow us to determine the density/pressure in underline{both} the CIV and OVI emitting gas. We will also use the absorption spectrum of 3C249.1 to search for intergalactic OVI absorption in this $z=0.311$ quasar.'),('D118',4,'O VI Absorbers in Spiral-Rich Groups of galaxies','Stocke','','U of Colorado','We propose to investigate whether nearby spiral rich galaxy groups are a significant reservoir of gas in the so-called warm-hot phase; i.e., collisionally-ionized gas at temperatures between 1.0e5 and 1.0e7 degrees. Numerical simulations of intergalactic gas predict that this warm-hot phase gas could account for 40-60 percent of all baryons locally, and yet HST/FUSE spectra have found a baryon fraction of only about 10 percent in O VI absorbers, which is the most viable detection method for such gas. Where might these warm-hot baryons be hiding? One possibility is spiral rich groups of galaxies which are very numerous, marginally bound, and which have been predicted to have intragroup gas at the right temperature to be O VI absorbers. In addition, spiral rich groups occupy a fractional volume small enough that they have not been probed extensively by current FUSE/HST observations. While this project was approved in FUSE Cycle 3, our two highest priority targets were not observed due to their low declinations. Here we target two high declination AGN (declination greater than +40) whose sightlines penetrate the very nearby M101 galaxy Group (cz = 250-500 km/s).'),('D119',4,'Superionization in the wind of X-ray anomalous B stars. Is tau Sco a prototype of such stars?','Zsargo','','The Johns Hopkins University',''),('D120',4,'An OVI Emission Line Survey of Hot Gas in Planetary Nebulae','Guerrero','','Univ of Illinois at Urbana-Champaign','A planetary nebula (PN) is formed by the current fast stellar wind sweeping up the previous slow wind. The shocked fast wind is over-pressurized and drives the nebular expansion. X-ray observations of PNe have revealed the shocked fast stellar wind in their interiors, but the low temperatures of the X-ray-emitting plasma in PNe and the low frequency of X-ray detections among PNe are puzzling. It is possible that some PN interiors are dominated by gas at temperatures below 10^6 K. To understand the physical conditions of PN interiors, we need to investigate the 10^5 K gas in order to study the interface between the hot interior and the cool nebular shell and to determine whether 10^5 K gas is the dominant temperature component in the PN interior. The 3x10^5 K gas is best probed with the O VI 1032,1037 A lines. FUSE observations of the PN NGC 7009 have demonstrated that it is easier to detect O VI in emission than in absorption. We propose an O VI emission line survey for a sample of 9 carefully selected PNe. These observations will reveal the content of 3x10^5 K gas in their interiors and allow us to study the conduction fronts and to select candidates for future X-ray observations.'),('D122',4,'Transition Region Properties at the bottom of the Main Sequence','Christian','','The Johns Hopkins University','The theory of stellar dynamos predicts that the distributed dynamo is at work in fully convective stars. The small scale fields generated in these objects affect the properties of their outer atmospheres. The present proposal will use FUSE spectra to derive the atmospheric parameters of the dM6e star Prox Cen, an object which is expected to be fully convective. The method of escape probabilities will be applied to line ratios of C III and O VI to derive optical depths and path lengths in the transition region. The path lengths and emission measure, will be combined with estimates of the electron density to determine the filling factors of the emission.'),('D123',4,'Stellar Parameters and Winds of Red Supergiants in Binaries','Bennett','','University of Colorado at Boulder','The proposed target stars (zeta Aur, 31 Cyg) are eclipsing binary systems with K supergiant primaries and B-type main sequence companions. From these binaries, we will determine key information about fundamental stellar parameters and outer atmospheric structure that can not be obtained from observations of single red supergiants. The proposed observations are directed towards understanding the mass loss process driving the massive winds of red supergiants. In particular, the proposed FUSE observations will support the following analyses: -- detailed model atmosphere analyses of the B-stars\' continua -- determining accurate radial velocities of the B-type secondaries -- analyses of the wind absorption features of the red supergiant primaries. From these FUSE observations, we will determine improved fundamental stellar parameters of red supergiants (effective temperatures, radii, masses and luminosities) and wind properties (velocity laws and mass loss rates).'),('D126',4,'AB Dor: Beyond the Photosphere','Dupree','','Smithsonian Astrophysical Observatory','FUSE spectra can provide the connecting link between the photosphere and corona of a rapidly rotating (12.4 hour) pre-main sequence star, AB Dor, to test quantitatively the magnetic models constructed with contemporaneous optical observations. Changes in far ultraviolet flux and line profiles of O VI and C III with rotational phase in this extreme atmosphere can signal the presence of closed and open magnetic fields, leading to enhanced emission or mass outflow. We expect sufficient signal in Fe XVIII to pinpoint the source of coronal emissions. AB Dor is in the FUSE CVZ at the end of December 2003 when our contemporaneous optical observations are scheduled. A continuous pointing totalling 90 ks will give 2 complete rotations of the star.'),('D127',4,'Fluorescent Molecular Hydrogen in IC 405 and NGC 7023 -- The Role of Environment','McCandliss','','The Johns Hopkins University','IC 405 and NGC 7023 are gas and dust rich interstellar regions known to exhibit the double-peaked emission feature near 1600Angstroms characteristic of fluorescent molecular hydrogen. The exciting stars reside in very different environments. AE Aur (Teff~34 kK) is a runaway star, while HD 200775 (Teff~20 kK) is just emerging from its proto-stellar nebula. We propose to exploit the high resolution capability of FUSE to observe the fluorescence process in the far UV where 70% of the fluorescence energy is emitted. From these observations we will determine the relative degree to which the population of the electronic ground state is influenced by the processes of fluorescence, shocks, formation pumping and multiple pumping. These data will compliment our ongoing FUSE studies of fluorescent molecular hydrogen emission in diverse environments.'),('D131',4,'High-Velocity Gas on the QSO 0045+3926 Sightline','Wannier','','Jet Propulsion Laboratory-Caltech','The QSO 0045+3926 (IO And) sightline is intriguing from the perspective of studying high-velocity gas in our Local Group. It passes close to the Local Group galaxy M31, and is about 15 degrees from material thought to be part of the Magellanic Stream. Exploratory FUSE observations (8 ksec, Cycle 2) have revealed four kinematic components, a local one, two highly redshifted ones associated with the background quasar, and one high velocity component (blue- shifted) originating somewhere within our Local Group. The high-velocity Local Group component shows H I, O VI and C III at a velocity consistent with that of an extended M31 disk, or with that of gas tidally stripped from our own Galaxy. The existing FUSE observations have insufficient S/N to clearly establish the origin or the composition of the high-velocity material. We request longer observations, which will greatly improve our knowledge of the gas composition and kinematics. Such observations will also improve our knowledge of the foreground (Galactic) and background (QSO) material evident in the exploratory observations.'),('D136',4,'Origin of the Far-UV Emission from Binary Pre-Main Sequence Herbig Ae/Be Stars','Bouret','','LAM - CNRS','Herbig Ae/Be stars are pre-main sequence (PMS) stars of intermediate mass. They present signs of intense activity, the origin of which is not understood. Various speculations concerning the origin of the FUV emission of these stars have been proposed. They include processes involving stellar coronae and winds, massive accretion of circumstellar material onto the stellar surface, or, in the case of binary Ae/Be stars, coronal emission from low-mass, possibly T Tauri star companions. We wish to obtain FUV spectra of a sample of binary systems, which have not been studied previously, in order to assess the affects of binarity on Ae/Be star activity. These new spectra will be supplemented by archival FUSE data which we will use to build two other samples of Herbig stars; one sample of stars showing signs of massive accretion disks, the other with stars exhibiting signatures of stellar winds. By comparing the three samples, we will study the occurrence and the origin of high temperature regions in these stars. More precisely, differences in detection rates, FUV luminosity distribution and FUV line profiles between these three samples will enable us to test the various interpretations outlined above.'),('D137',4,'Studying the CMa ISM tunnel by FUSE spectroscopy of the hot DA WD RE J0723-277','Dobbie','','University of Leicester','We propose to obtain FUV spectroscopy of the DA white dwarf RE J0723-277. This will permit us to determine the column densities of ions such as ArI, CII, CIII, NI, NII, NIII and OI along the first ~ 100pc of the line of sight towards the DAO white dwarf RE J0720-318 (d ~ 188$pc), which has been observed previously by FUSE. The measurements of column densities towards both white dwarfs will be used, in conjunction with the limits placed on N(HI), N(HeI) and N(HeII) from EUVE data, to investigate further the origins of the large ionisation fractions found for the local interstellar medium in the direction of the CMa tunnel. In addition, as RE J0723-277 lies very close in the T_eff v log g plane to the DA GD394, which has a most peculiar pattern of photospheric heavy element abundances, we will use this observation to undertake a detailed analysis of the photospheric composition of the former in a bid to shed further light on the processes at play in the atmosphere of the latter.'),('D138',4,'The Abundances of the Iron Group Elements in Early B Stars in the Magellanic Clouds','Peters','','University of Southern California','FUSE observations of four sharp-lined early B main-sequence band stars in the Magellanic Clouds will be carried through to determine the abundances of the heavy elements, especially those of the Fe group. The FUSE spectral region contains numerous Fe III lines, including the resonance multiplet (UV1) near 1130 A that is excellent for abundance determinations and two strong multiplets of V III, an ion that does not produce measurable lines longward of 1200 A in metal-deficient stars. In addition there are several measurable lines from Cr III and Mn III. Although abundances of the Fe-peak elements are of interest because they are important for assessing opacities for stellar evolution calculations and the validity of theoretical calculations of explosive nucleosynthesis, ground-based studies do not yield this information because measurable lines from these species, except for a few Fe III lines, are found only in the UV spectral region. The abundances of heavy elements provide information on the production of such elements in previous generations of stars. From FUSE data obtained in Cycle 3 we are determining the abundances of the Fe group elements in two sharp-lined early B stars in the SMC (AV 304, a field star, and NGC346-637, a star in a mini-starburst cluster). This project will allow one to compare the abundances in AV 304 and NGC346-637 with those in the LMC and other regions in the SMC and look for asymmetry in heavy element production in the Magellanic Clouds.'),('D144',4,'The Inner Disk and Hot White Dwarf in the Novalike V794 Aql','Godon','','Villanova University','While IUE and HST provide ideal information on low temperature (10,000-20,000K), White Dwarfs (WDs) and disks in Cataclysmic Variables (CVs), the importance of FUSE lies in its ability to study the hottest WDs and the inner disk. This high temperature regime involves the higher accretion rate systems that are located above the gap at periods longer than 3 hours. Unfortunately, only a few such Novalike objects (in permanent high state of accretion) have been observed, and only one spectrum was obatined in the far UV with FUSE (MV Lyr). We have chosen the Novalike system V794 Aql for which preliminary IUE studies show a hot white dwarf and inner disk. A comparison of the disk/WD in this systems with the low accretion rate Dwarf Nova (DN) systems will provide important constraints on the accretion limits for disk instability outbursts. We will use the SYNSPEC/TLUSTY/TLUSDISK model code to characterize the basic properties (such as Teff, log g, Vsini, chemical abundances, accretion belts and evidence of past thermonuclear runaway) of the WD accretors in Novalike systems.'),('D145',4,'Probing the Inner Accretion Disk, Boundary Layer and White Dwarf in Long Period Dwarf Novae with FUSE','Sion','','Villanova University','A major source of serious problems with the disk instability theory of dwarf nova outbursts is its inability to reproduce the behavior of dwarf novae during quiescence (Lasota 2002, Hameury 2002, Menou 2002). Most DN systems during quiescence behave contrary to theoretical predictions. Above the CV period gap, the state of the accretion disk (optically thick?) and properties of the central white dwarf (Teff, Vsini, log g, chemical abundances, signs of past TNRs?) remain largely unknown. Our FUSE and archival IUE studies show that the disk and white dwarf properties appear to vary greatly from system to system. In order to gain deeper insight into the cause of these differences from system to system and to increase the number of white dwarfs above the period gap with known properties beyond the mere four that we now have (U Gem, RX And, SS Aur, RU Peg), we propose FUSE investigations of four additional systems, EY Cyg, BV Cen, CH UMa and WW Ceti, all of which are excellent candidates for understanding the disk structure and white dwarfs/boundary layers during quiescence.'),('D146',4,'Probing the Nature of the Hot Components of Symbiotic Variables with FUSE','Sion','','Villanova University','We propose FUSE observations of 8 symbiotic binaries (red^M giant + white dwarf/accretion disk?) around superior spectroscopic^M conjunction when the accreting, hot component is in front of the red^M giant. The 8 systems were selected because they show no clear evidence of^M an accretion disk or nebular continuum shortward of 1800A and thus offer^M the opportunity to carry out the first NLTE synthetic spectral analyses of^M the hot components with high gravity photosphere models and accretion disk^M models with vertical structure. Our objectives are: (1) determine whether^M a disk is really absent and, if not, derive the accretion rate; (2)^M determine the first temperatures for the hot components, independent of^M past Zanstra techniques or black body fits; (3) determine the first^M rotation rates for the white dwarfs in these systems; (4) search for^M evidence of thermonuclear processing from the chemical abundance ratios of^M the mix of ionic absorption features identified with their photospheres;^M compare the properties (temperatures, rotation rates, abundances,^M accretion heating) of this class of white dwarf wind or disk accreters^M with the properties of the accreting white dwarfs in cataclysmic^M variables. ^M'),('D149',4,'Multi-wavelength Studies of Symbiotic Stars in Outburst','Keyes','','Space Telescope Science Institute',''),('D152',4,'Accretion flow in the High-Mass X-ray binary 4U 1700-37','Iping','','The Catholic University of America','We propose to obtain phase resolved FUSE observations of the high mass X-ray binary, HD153919 /(4U1700-37). The luminous O6.5 Iaf star eclipses the compact object with a 3.411581 day period. This system is unique and has unsolved problems that only FUSE can address. The compact object, a neutron star or a blackhole, ionizes the surrounding area and acts as a probe of the stellar wind as it moves through the binary orbit. We propose to obtain 4 time constrained observations, at orbital phases 0.00, 0.25, 0.50 and 0.75. We will search for orbital modulations of the many stellar wind lines in the FUSE band, due to the X-ray photoionization of the wind. The so-called Hatchett & McCray effect, observed in several other HMXR binaries, has not been observed yet in HD153919 due to the fact that the wind is very dense, which saturates the NV, Si IV and C IV lines in the UV longward of 1200 A. We need observations with FUSE ( 905-1187 A) where many of the lines are higher excitation lines and/or are not saturated. Studying the line profile changes with orbital phase will provide detailed information on the geometry and physical conditions of the X-ray ionized region and the accretion flow near the compact X-ray source.'),('D153',4,'Colliding Winds in the LMC Massive Binary SK-67 105','Gizis','','University of Delaware','We propose to make FUSE spectra of the massive binary SK-67D105 at six orbital phases. This LMC binary (O4f + O6V) represents one of the most massive known binaries comprised of O-type stars, and the close proximity of the stars and the probable strengths of their stellar winds makes SK-67D105 an ideal target for a study of colliding winds in massive binaries. The spectra would record the orbital phase variations in the strong wind lines found in the FUSE wavelength range, and would allow us to study the geometry of the colliding winds bow shock. The ratios of lines of different ionization states will be especially useful for estimating temperature effects in the colliding winds. We would also use the photospheric FUV lines to refine the orbital parameters, reconstruct the spectra of the individual components (using Doppler tomography), assign spectral types, and measure projected rotational velocities. The investigation will yield important first results on colliding winds and stellar evolution in a massive binary system comprised of low metallicity O-stars.'),('D154',4,'Connecting the X-ray and UV ionized absorbers in Mrk 279','Arav','','University of Colorado at Boulder','Our proposed FUSE observations are the last component of a deep X-ray/UV spectroscopy campaign on the bright Seyfert 1 galaxy Mrk 279. In the current Chandra cycle, 360 ksec Chandra LETGS and 16 HST/STIS orbits have been approved for this project. Our main scientific goal is to study the AGN outflow seen as an ionized absorber in this galaxy, focusing on the crucial connection between the X-ray and UV manifestations of the outflows. We will map the ionization and velocity structure, measure the elemental abundances and then determine the mass and kinetic luminosity flux of the outflow, all stepping stones for studying the importance of the outflows in the evolution of AGN and their host galaxies. The combination of unblended outflow troughs, very low Galactic column (avoiding the plague of H_2 contamination) and very high UV flux, makes Mrk 279 the most promising of all AGN outflow targets in the FUSE band. In addition, the proposed FUSE observa tions will allow for a unique high-quality variability study of an AGN outflow, since we will have three epochs of excellent FUSE AGN outflow data (35-100 ks each) with simultaneous HST echelle data for two of these epochs.'),('D155',4,'Probing the Intrinsic Absorption in NGC 5548 with Coordinated FUSE and HST Observations','Gabel','','Catholic University of America','NGC 5548 is an ideal target for a detailed study of mass outflow in active galaxies. This bright Seyfert 1 galaxy exhibits a rich absorption spectrum in the UV, far-UV, and X-ray, and has been one of the most intensely studied AGNs for its absorption properties. However, recent studies have produced conflicting results concerning the level of saturation in its UV absorption; hence the fundamental quantities that are measured in the absorbers, their column densities, remain uncertain. We have been awarded 20 orbits of observing time with HST/STIS to address this issue so that further progress can be made in understanding the mass outflow in NGC 5548. We propose a coordinated, deep exposure with FUSE that will provide crucial results needed to obtain a definitive answer. The FUSE spectrum samples the full set of higher order Lyman lines, providing the tools needed to separate the individual line-of-sight covering factors of the continuum and emission line sources. Since the individual kinematic components of absorption are easily resolved with FUSE, the covering factors can be solved at each velocity. These results are critical for measuring accurate column densities for many of the lines in the far-UV -- UV bandpass and will provide unique constraints on the absorption and emission geometry in the AGN. Additionally, the far-UV spectral coverage of FUSE samples numerous key lines that are needed to fully constrain the ionization state, effective column density, and abundances in the absorbers. The results obtained from this study will provide a crucial step towards testing dynamical models of mass outflow in AGNs.'),('D156',4,'QU Car: a softer than supersoft source with a carbon enriched companion','Hartley','','Space Telescope Science Institute','We propose to study the interacting binary star, QU Car, which may be the most luminous CV known and is certainly the first to show carbon overabundance in the secondary. We require the high time-resolution and spectral coverage of the FUSE satellite to probe the structure of this poorly understood system. We will measure the FUV spectral energy distribution and, from this, improve our calculation of the luminosity, which has already been shown to be close to the supersoft X-ray domain. From the unique combination of spectral lines available with FUSE we will calculate atomic abundances of C, N and O in the accretion disk. At time-resolutions of down to 100s we will measure the spectral line variability on timescales on the order of both the orbital period and the 2000s variability apparent in HST STIS-range spectral lines. We aim to examine the role of an outflow versus a high temperature disk in shaping the spectral characteristics of QU Car. In developing a better physical model of this apparently atypical system and establishing its relationship to other luminous binaries we seek to better understand the evolution of close binary systems.'),('D157',4,'FUSE Spectroscopy of Hot Post-AGB Stars in Globular Clusters','Dixon','','The Johns Hopkins University','We propose FUSE observations of three hot (T_eff > 40,000 K) post-AGB stars in globular clusters with exposure times sufficient to achieve a single-channel signal-to-noise ratio of 25--30 per resolution element. The resulting data set will allow detailed studies of both the stars themselves and the intervening interstellar medium. By comparing their FUSE spectra with synthetic spectra derived from non-LTE stellar atmosphere models, we will determine the stars\' temperatures, surface gravities, and abundances, place them accurately on the HR diagram, and advance our understanding of the late stages of stellar evolution. By modeling the absorption features of interstellar S III (1013 A), O VI (1032, 1038 A), and Fe III (1123 A), we will derive the mass and velocity distribution of both the warm and hot components of the Galactic halo along these lines of sight. Besides answering our questions, these data will provide an important contribution to the FUSE archive.'),('D158',4,'Verification of a double degenerate progenitor of supernovae type Ia','Napiwotzki','','University Erlangen-Nuernberg','We have identified a binary white dwarf system (double-degenerate - DD) with an orbital period of 7h 12min and an estimated total mass of 1.45Msun (i.e. above the Chandrasekhar limit of 1.4Msun). This system will merge within 4 Gyrs. The confirmation of a DD which is massive enough and will merge within a Hubble time will have severe impact on the progenitor models of supernovae type Ia (SN Ia). This object was found in the ESO Supernovae Ia Progenitor surveY (SPY) which is carried out as Large Programme at the ESO Very Large Telescope. The remaining uncertainty concerns the mass of the secondary in this binary, which could be further constrained with our proposed FUSE observations. The proposed observations are critical to verify the total mass, which is close to the limit for a SN Ia in about 4 Gyrs. The needed accuracy can only be reached with the unique FUV capabilities provided by FUSE. If the mass is confirmed, this would be the first known DD progenitor of a SN Ia.'),('D160',4,'FUSE Observations of Two Very Peculiar Central Stars of Planetary Nebulae','Chayer','','The Johns Hopkins University','Most central stars of planetary nebulae are stars that evolve along post-asymptotic giant branch (post-AGB) evolutionary tracks en route to become CO white dwarfs with average masses of M ~ 0.6 solar masses. We know of at least two stars that are an exception to the rule: PHL~932 (Teff = 35,000 K, log g = 5.9) and EGB~5 (Teff = 42,000 K, log g = 5.8). The high surface gravities and low effective temperatures of these two central stars imply that they are not post-AGB stars. Both show a sdOB spectral type surrounded by planetary nebulae with low surface brightness and large angular size. As of now, no one has resolved the evolutionary status of these two stars. We propose to obtain FUSE observations of both stars to analyze their photospheric abundances. We predict there is a close link between the episode of mass loss recently experienced by these stars and their photopheric abundances. And this analysis will provide useful data to resolve the puzzle of the evolutionary status of both stars.'),('D161',4,'The pulsating/ellipsoidal variable hot B subdwarf KPD 1930+2752','Fontaine','','Universite de Montreal','We propose to measure the projected rotational velocity of KPD 1930+2752, a unique binary system consisting of a sdB primary undergoing acoustic mode pulsations and ellipsoidally distorted by the presence of an unseen white dwarf companion. The orbital period of the system is 2.383 hrs. The measurement of v sin i is the one datum currently missing that prevents us from modeling the ellipsoidal light curve in terms of the basic parameters of the two stellar components. Once this measurement is secured, we should be able to derive the values of the masses and radii of these two stars. We should be able to verify if indeed KPD 1930+2752 is a genuine progenitor of a Type Ia supernova as was recently suggested by a British group. More importantly, by combining the values of the mass and the radius of the sdB pulsator with the period data, we should be able to model, for the first time, the interior structure of a sdB star through asteroseismological techniques. FUSE time tag observations are unique for this type of measurement. They allow us to remove the star\'s orbital velocity (348 km/s) that inevitably smears out the photospheric lines. We have already successfully implemented such a procedure in the CalFUSE pipeline. The projected equatorial velocity, v sin i, is then determined by comparing the star\'s line profiles to computed rotation profiles.'),('D162',4,'Role of Rotation in the Evolution of Massive Stars','Heap','','NASA/Goddard Space Flight Center','By confronting the effects of rotation, astronomers have come to the threshold of a major advance in understanding massive stars. Theoreticians have recently developed a new generation of evolutionary models that account for rotation, and observers are starting to test these models. The SMC, a low-metallicity galaxy, is an excellent environment for discerning the role of rotation because of the high initial rotational velocities and weak winds of its massive stars. In our earlier FUSE+STIS+optical spectral analysis of O-type stars in the SMC (Heap et al.2002), we found signatures of rapid rotation in the form of (1) a lower effective gravity due to centrifugal force and (2) enrichment of atmospheric nitrogen. We now propose to extend our study to B-type stars in the SMC in order to include stars at later evolutionary phases. We expect that the proposed FUSE observations will result in a robust calibration of the spectral properties of B-type stars at low metallicity and that they will have important implications for understanding the precursors to core-collapse supernovae and to the sources of nitrogen in the early universe.'),('D163',4,'Probing the Halo and ISM of Low-Redshift Galaxies with Young Supernova','Iping','','The Catholic University of America','We propose a Target of Opportunity program to study the halo and ISM of a low-redshift galaxy hosting a bright new supernova (about 14 m.). The primary objectives are to characterize the ionization state, gas-phase abundances, metallicity, and gas kinematics in the ISM and halo of the host galaxy, and, if the properties of the sightline are favorable, in the intervening intergalactic medium. Core-collapse supernovae occuring in galaxies out to the Virgo cluster are the potential targets for this program. The FUSE spectral range provides a comprehensive set of lines to study the hot, warm, and cool phases of the ISM. The FUSE spectra will be augmented by HST/STIS TOO observations E140M, (1160A