CYCLE 4 ABSTRACTS ----------------- Prog ID: D003 PI: Welsh Title: Further Probing of the Connection between the Local Interstellar Chimney and the 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. Prog ID: D004 PI: Hutchings Title: The Eclipsing Low-mass X-ray Binary X1822-37 We propose FUSE observations to cover the 5.6-hour orbital period of the prototype eclipsing low-mass X-ray binary X1822$-$37. The system has a complex accretion disk structure which causes nearly continuous variations at all wavelengths. An accretion disk corona envelopes the binary, and X-rays heat the surface of the donor star. Because the compact star is a pulsar, the orbital parameters are well known. FUSE spectra covering the binary orbit, including through eclipse, will probe the hot inner disk by observing its high ionization emission lines, the outer disk via Lyman absorption lines, and the location of hot continuum sources. FUSE data will provide unique new information on the properties of the accretion disk, mass flows within the system, and the surrounding gas envelope. In 7 FUSE orbits we can sample the orbital period fully, accounting for earth occultations. Prog ID: D005 PI: Hutchings Title: X0535-668 An Interacting NeutronBe Star Binary We propose to observe the luminous LMC X-ray binary X0535$-$668 which consists of a highly interacting Be-star/neutron-star pair. During periastron passage in the very eccentric 16.65-day orbit (e$>$0.7), the neutron star plunges into the envelope of the Be star. Optical and IUE studies have shown that significant changes occur in the emission at all wavelengths. FUSE spectra will allow us to sample a wide range of ionization states to see how various species vary with orbital phase and hence infer their origin within the system. Study of O~VI resonance lines around the orbit will give information on mass loss from the system through its variable stellar wind and how it changes through the eccentric orbit. With FUSE data it will also be possible to detect any cool H$_2$ envelope that may surround the system. Prog ID: D006 PI: Crampton Title: Orbital variations of RXJ0513.9-6951 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. Prog ID: D007 PI: Gull Title: FUV Monitoring the 2003 Minimum of Eta Carinae 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. Prog ID: D008 PI: Richter Title: Molecular Hydrogen in the Lower Galactic Halo 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. Prog ID: D010 PI: Shastri Title: Geometry of the hot gaseous outflows in Seyferts We propose to attack the question of whether orientation plays a dominant role in the observed hot gaseous outflows in Seyfert galaxies. We plan to do this by contrasting the properties of the O VI absorbers in a matched sample of Seyfert1s and 2s, which, in the framework of the Unified Scheme, are oriented face-on and end-on respectively w.r.t. us. The OVI emission line is present in all Seyferts, and is a unique characterizer of the kinematics of gas at about 10e6K. The spectral sensitivity and resolution of FUSE in this range makes it possible to discern the different components of the absorbing outflow. The key points of our investigation are (a) the Seyfert1s and 2s have been chosen to be intrinsically similar, and thus provide a very clean statistical comparison of face-on and end-on Seyferts and therefore a rigorous test of orientation effects, and (b) all the Seyfert1s and three of the Seyfert2s are already observed by FUSE, so that only five more targets are required to complete FUSE observations for this unique, well-matched sample of 16 Seyfert galaxies. Prog ID: D012 PI: Harper Title: Fe II Fluorescence in alpha Her (M5Ib-II) 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. Prog ID: D015 PI: Keenan Title: The distance to high-velocity O VI absorption in the Galactic halo Previous FUSE studies have revealed the presence of large amounts of high-velocity ($\mid$V$_{LSR}$$\mid$ $>$ 100\kms) 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 ($\sim$\,0.1\ang 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 9\deg) 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. Prog ID: D021 PI: Meyer Title: AU-Scale Interstellar H_2 Structure Toward HD 37903 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. Prog ID: D023 PI: Vennes Title: Metallicity of X-ray selected DA white dwarfs 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. Prog ID: D024 PI: Sembach Title: High Velocity OVI Emission in the Magellanic Stream and Complex C 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. Prog ID: D025 PI: Rauch Title: The Enigma of AA Dor - is the secondary a planet? 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. Prog ID: D026 PI: Andersson Title: Characterizing the generation of OVI ions in a hot-cold interface 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. Prog ID: D027 PI: Savage Title: Physical Conditions and Baryonic Content of the Highly Ionized IGM 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 \AA will permit the study of $\sim$13 \OVI\ IGM systems with rest equivalent widths $>$50 m\AA. The redshifts of the QSOs and the presence of only weak interfering absorption from Galactic H$_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. Prog ID: D028 PI: Wakker Title: Intergalactic O VI absorption at redshift <0.004 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\ $\lambda\lambda$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 m\AA. 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 m\AA. 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. Prog ID: D030 PI: Martins Title: Stellar and wind properties of very young massive stars We propose to obtain FUSE spectra of a sample of young massive stars, which are part of the poorly understood class of Vz stars supposed to lie close to the ZAMS. In particular, as our preliminary work shows, such objects seem to have extremely weak stellar winds compared to other O stars, challenging thereby our current understanding of the radiation driven wind theory. Our main goal is to determine the stellar and wind properties of these objects to understand this apparent peculiarity, and in general to understand their evolutionary status and their link with regions of massive star formation. The requested observations, together with optical ESO/EMMI/NTT and UV STIS/HST observations, will provide a large set of spectral lines leading to stellar and wind parameters through line fitting with non-LTE spherically extended models including line blanketing. The opportunity offered by FUSE to observe stars in the Magellanic Clouds will also allow to investigate a possible link between the Vz class and metallicity. The results of this multi-wavelength study will improve our knowledge of the earliest optically visible phases of the evolution of massive stars. Prog ID: D032 PI: Roberge Title: Circumstellar Gas in Young Planetary Debris Disks 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. Prog ID: D033 PI: Walter Title: Line Profiles and Variability in Ultra Rapid Rotators 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. Prog ID: D034 PI: Bianchi Title: Central Stars of Planetary Nebulae in the Large Magellanic Cloud 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. Prog ID: D037 PI: Smith Title: FUV Spectroscopy through the Pulsation Cycle of BW Vul 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. Prog ID: D039 PI: Hoopes Title: FUSE Observations of Coronal Gas in the Nuclear Outflow of NGC3079 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. Prog ID: D040 PI: Skillman Title: Multiphase Observations of the Dwarf Starburst Galaxy NGC625 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. Prog ID: D041 PI: Mathur Title: Metallicity Determination in a Narrow Line Seyfert 1 Galaxy using Chandra, HST a 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. Prog ID: D042 PI: Szkody Title: Hot White Dwarfs in New CVs Among the approximately 100 new Cataclysmic Variables (CVs) currently found in the 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. Prog ID: D044 PI: Moffat Title: Towards the Origin of the Ubiquitous Small-Scale Structures in Hot-Star Winds 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. Prog ID: D047 PI: Brown Title: STELLAR ACTIVITY AND MASS LOSS FROM A AND F SUPERGIANTS 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. Prog ID: D049 PI: Blair Title: Detailed FUSE Study of a Star Behind the Cygnus Loop 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. Prog ID: D053 PI: Cheng Title: FUSE Observation of the Standard Star Vega 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. Prog ID: D054 PI: Tripp Title: The Sight Line to Mrk205 -- A Unique Opportunity to Investigate the Metal Enrich 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. Prog ID: D055 PI: Bowen Title: A Search for Hot Baryons in the Intragroup Medium 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. Prog ID: D058 PI: Vidal-Madjar Title: Deuterium abundance measurements beyond the Local Bubble 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. Prog ID: D059 PI: Barstow Title: A FUV search for white dwarfs in unresolved binary systems 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. Prog ID: D063 PI: Friedman Title: DH and OH Within 500 pc of the Sun-Connecting Results From fuse, copernicus, and 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. Prog ID: D064 PI: Sonnentrucker Title: Chlorine in the Interstellar Medium 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. Prog ID: D065 PI: Grady Title: Probing the Evolution of Stellar Activity in Young A Stars with FUSE Required) 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. Prog ID: D066 PI: Hebrard Title: Surveying the sight lines of subdwarfs and white dwarfs beyond the Local Bubble 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. Prog ID: D071 PI: Gansicke Title: The evolution of cataclysmic variables Clues from FUSE observations of Post Comm 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. Prog ID: D073 PI: Lauroesch Title: The Abundance of Interstellar Fluorine 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. Prog ID: D075 PI: Ayres Title: A New Spin on FK Comae 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. Prog ID: D076 PI: Lee Title: Probing absorber kinematics with simultaneous FUSE & Chandra HETGS observations 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. Prog ID: D078 PI: Sankrit Title: Vela Knot D - Kinematics of a Bow Shock 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. Prog ID: D079 PI: Massa Title: Temperature Variations in Slowly Pulsating B Stars 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. Prog ID: D080 PI: Howell Title: FUSE Observations of Two Schizophrenic Magnetic CVs PQ Gem and V405 Aur 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. Prog ID: D081 PI: Bergin Title: The FUV Flux Irradiating the Surfaces of Protostellar Disks We propose to use FUSE to determine the Far-Ultraviolet (FUV) radiation field between 912-1100A in the GM Auriga proto-planetary disk system. These data will be combined with already allocated HST observations that will characterize the FUV field for lambda > 1100A. GM Aur is among a handful of sources that can be subjected to detailed chemical studies with the current generation of millimeter-wave instruments. Such studies have found that the disks have a rich molecular chemistry, which appears to be controlled by the FUV radiation field (Qi 2001; Dutrey et al 1997; Kastner et al 1997). These observations will allow a firm characterization of the full FUV radiation field impinging on the surfaces of circumstellar disks. Knowledge of the FUV field allows for more realistic theoretical chemical models to be constructed and compared to observations. Since a handful of objects will remain, for some time, the main templates for chemical studies of extra-solar disks, this project will provide the real UV data required to push theory forward. Given that molecules are excellent probes of their environment, the new information will place better constraints on the virtually unknown vertical structure of proto-planetary disks. This project is unique in scope and will increase our limited understanding of disk chemical evolution, in addition to improving our knowledge of uncertain physical processes, such as the possible dissipation of outer disks by photo-evaporation and the timescales of dust grain growth. Prog ID: D084 PI: Bianchi Title: The Youngest, Most Massive Star Clusters in M33 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. Prog ID: D088 PI: St-Louis Title: Spectacular Wind-Collision Effects in the LMC WR+O Binary Brey22 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. Prog ID: D089 PI: Dinerstein Title: FUSE Observations of Neutron-Capture Elements in W-R Planetary Nebulae 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, such as 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. Prog ID: D092 PI: Holberg Title: FUSE Observations of Orbital and Rotational Variations in the Unique System HS11 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. Prog ID: D098 PI: Blair Title: New FUSE Stellar Observations in the Large Magellanic Cloud 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. Prog ID: D099 PI: Redfield Title: Doppler Imaging a Late-A Star in the FUV 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. Prog ID: D101 PI: Allard Title: Quasi-molecular satellites of Lyman lines in ZZ Cetis 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. Prog ID: D103 PI: Howk Title: Probing the Physical Nature of the Cosmic Web with Extreme Ultraviolet Spectrosc 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. Prog ID: D107 PI: Lobel Title: Modeling Transition Region Wind Dynamics of F-type Supergiants 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. Prog ID: D108 PI: Redfield Title: The Fe XVIII lambda974 Line, A New Tool for Measuring the Size and Dynamics of S 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. Prog ID: D109 PI: Barrett Title: Phase-resolved spectroscopy of eclipsing polars 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. Prog ID: D113 PI: Dufour Title: The O6.5IIIef Star BD+60D2522 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. Prog ID: D114 PI: Long Title: V592 Cas A study of a bipolar outflow and precessing accretion disk 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. Prog ID: D115 PI: Ayres Title: The Holely Coronal Graveyard 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. Prog ID: D117 PI: Benjamin Title: OVI and CIV Emission in the Local Interstellar Chimney 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. Prog ID: D118 PI: Stocke Title: O VI Absorbers in Spiral-Rich Groups of Galaxies 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). Prog ID: D120 PI: Guerrero Title: An OVI Emission Line Survey of Hot Gas in Planetary Nebulae 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. Prog ID: D121 PI: Chu Title: Resolving the Conduction Front in the Bubble S308 Fast stellar winds sweep up ambient media to form bubbles. The interior of the dense swept-up shell of a bubble is filled with shocked fast wind at high temperatures. At the interface between the hot (10^7--10^8 K) interior gas and the cool (10^4 K) swept-up shell, conduction lowers the temperature and mass evaporation raises the density of the hot interior gas. This conduction front plays an important role in determining the physical structure and evolution of a bubble. Conduction fronts have been previously studied via C IV, N V, O VI absorption lines with very limited success. No spatial information of the conduction front is available in these absorption observations. We request FUSE observations of the bubble S308 to search for O VI emission lines from the conduction layer in this bubble. Our XMM observations of S308 show limb-brightened diffuse X-ray emission; furthermore, comparison between X-ray and optical images reveal a 90--140 arcsecond gap between the outer edge of the X-ray emisison region and the optical shell rim. This gap provides vivid evidence of the existence of conduction fronts. We request FUSE LWRS observations of three positions in S308 to resolve the structure of its conduction front. The FUSE observations of the O VI emission lines, together with the HST STIS observations of the C IV and N V absorption line observations, will provide the most comprehensive views of a conduction front and allow us to evaluate the efficiency of conduction. Prog ID: D122 PI: Christian Title: Transition region properties at the bottom of the main sequence 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. Prog ID: D123 PI: Bennett Title: Stellar Parameters and Winds of Red Supergiants in Binaries 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). Prog ID: D126 PI: Dupree Title: AB Dor Beyond the Photosphere 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. Prog ID: D127 PI: McCandliss Title: Fluorescent Molecular Hydrogen in IC405 and NGC7023 - TheRoleofEnvironment 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. Prog ID: D131 PI: Wannier Title: High-Velocity Gas on the QSO 0045+3926 Sightline 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. Prog ID: D136 PI: Bouret Title: Origin of the Far-UV Emission from Binary Pre-Main Sequence Herbig AeBe Stars 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. Prog ID: D137 PI: Dobbie Title: Studying the CMa ISM tunnel by FUSE spectroscopy of the hot DA WD RE J0723-277 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. Prog ID: D138 PI: Peters Title: The Abundances of the Iron Group Elements in Early B Stars in the Magellanic Clo 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. Prog ID: D144 PI: Godon Title: The Inner Disk and Hot White Dwarf in the Novalike V794 Aql 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. Prog ID: D145 PI: Sion Title: Probing the Inner Accretion Disk, Boundary layer and White Dwarf in Long Period 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. Prog ID: D146 PI: Sion Title: Probing the Nature of the Hot Components of Symbiotic Variables with FUSE 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 Prog ID: D152 PI: Iping Title: Accretion flow in the High-Mass X-ray binary 4U1700-37 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. Prog ID: D153 PI: Gizis Title: Colliding Winds in the LMC Massive Binary SK-67D105 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. Prog ID: D154 PI: Arav Title: Connecting the X-ray and UV ionized absorbers in Mrk279 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. Prog ID: D155 PI: Gabel Title: Probing the Intrinsic Absorption in NGC 5548 with Coordinated FUSE and HST Obser 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. Prog ID: D156 PI: Hartley Title: Examining a unique binary star, QU Car a softer than supersoft source with a car 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. Prog ID: D157 PI: Dixon Title: FUSE Spectroscopy of Hot Post-AGB Stars in Globular Clusters 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. Prog ID: D158 PI: Napiwotzki Title: Verification of a double degenerate progenitor of supernova type Ia 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. Prog ID: D160 PI: Chayer Title: FUSE Observations of Two Very Peculiar Central Stars of Planetary Nebulae 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. Prog ID: D161 PI: Fontaine Title: Probing the Interior of the hot subdwarf KPD1930+2752 by measuring its vsini 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. Prog ID: D162 PI: Heap Title: Role of Rotation in Massive-Star Evolution 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. Prog ID: D163 PI: Iping Title: Probing the Halo and ISM of Low-Redshift Galaxies with Young Supernovae 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