CYCLE 5 ------- ACCEPTED ABSTRACTS ------------------ STANDARD PROGRAMS ----------------- PROP ID: E008 PROPOSER: Sembach PROPOSAL TITLE: Highly Ionized High Velocity Gas in the Distant Galactic Corona and Local Group We propose FUSE observations of two AGNs (NGC 7469 and Mrk 335) to study the properties of highly ionized high-velocity gas associated with the Magellanic Stream and several Local Group clouds. These bright AGNs present a rare opportunity to combine high quality FUSE data with excellent HSTSTIS data, which will allow us to characterize the ionization properties of the high-velocity gas and to discriminate between competing models for the production of highly ionized species such as ionO6. We will determine if the high-velocity ionO6 is produced in interfaces between warm (Tsim10^4,K) clouds and a hot (Tgtrsim10^6,K) Galactic corona or Local Group medium. New FUSE data are necessary to observe important diagnostics below 1000,AA (e.g., ionH1, ionO1, ionC3) and to significantly improve the ionO6 data quality at longer wavelengths for detailed line shape comparisons with ions in the HST band (e.g., ionSi4, ionC4, ionN5). The results of this investigation are relevant to studies of high-velocity clouds, the baryonic content of the local universe, the production of hot gas in the Local Group, the intergalactic medium, and the formation and evolution of galaxies. Secondary science objectives include an investigation of the intergalactic medium absorption toward Mrk335 and a study of the Galactic halo. PROP ID: E010 PROPOSER: Bergeron PROPOSAL TITLE: Tracing the warm-hot intergalactic medium with O, sc v The warm-hot intergalactic medium (WHIM) has been recently detected by O, sc vi absorption features in the spectra of background QSOs at both low (z sim 0.1) and high (z sim 2.2) redshifts. Model simulations suggest that this IGM phase may contain a large fraction of the baryons in the local universe up to sim 50 while still being a substantial component of the intergalactic medium at high z. The baryon fraction inferred from existing observations is still very uncertain, in large part because the nature of the heatingionizing process of the WHIM is still under debate. We propose to observe the O,: sc v lambda630 EUV absorption associated with 11 intervening Ly-alpha systems (FUSE O,sc v redshift range .48-0.88) in PG 1718+481 (z_: em 1.084). The occurrence of O,sc v will be compared to that of O,sc vi from HST data. From the ionic ratios, we will constrain the ionization process as well as the oxygen abundance and determine whether a multi-phase medium is required. Species of different ionization level, O,sc iv and Ne,sc viii or Mg,sc x, might also be detected in some of these absorbers. PROP ID: E018 PROPOSER: Aloisi PROPOSAL TITLE: FUV Spectra of the most Metal-poor Star-forming Dwarf Galaxies in the Local Universe We propose to observe 2 of the most metal-poor (Z lesssim 120 solar) star-forming dwarf galaxies in the local Universe considered to represent the nearby counterpart of primeval galaxies at high redshift, SBS0335-052 and SBS1415+437. In these systems the neutral phase of the interstellar medium (ISM) dominates the baryonic mass, and can hide the bulk of the metals. Determining the metal content of the neutral ISM is thus of fundamental importance to infer the chemical evolutionary state of this class of objects, assess or reject their primordial nature, investigate their connection with the high-redshift Universe (e.g., Lyman Break Galaxies and Damped Lyalpha Systems), and better understand galaxy formation and evolution. The high resolution, sensitivity, and spectral range of FUSE is mandatory. The FUV absorption lines in the very blue spectra of these star-forming galaxies will allow us to derive with an accuracy lesssim 0.1 dex the metal content in the neutral gas by simply adopting the same multi-component fitting technique widely used to study QSO absorption systems. Our pilot study on the FUSE archival data of IZw18, the most metal-poor (Z simeq 150 solar) galaxy known so far in the local Universe, has demonstrated the feasibility of the project, and has brought us to the following exciting discovery. The Hsc i in IZw18 is already enriched in metals, and a certain amount of ancient (gtrsim Gyr) star formation is required prior to the more recent activity responsible for the additional enrichment of the Hsc ii regions. The new FUSE observations of SBS0335-052 and SBS1415+437 will allow us to assess if the behavior of IZw18 is common or an exception for this class of objects. PROP ID: E020 PROPOSER: Evans PROPOSAL TITLE: Massive Star Evolution--Fundamental Parameters Quantitative understanding of the evolution of massive stars is vital in understanding galactic chemical enrichment, as well as the dynamic evolution of the interstellar medium. Masses and radii have now been determined for a number of massive detached eclipsing binaries with an unprecedented accuracy of 2 These results can be used to test stellar evolutionary calculations. Unfortunately, for the hottest stars (O and early B stars) the tests are limited by the large uncertainty in the temperatures. We propose to use FUSE spectra to improve the temperatures using both the energy distribution and line diagnostics. This will provide temperatures of these important stars with an accuracy approaching 2 This will tighten the constraints on parameters such as core convective overshoot and also provide an excellent list of standard stars for comparison with FUSE spectra of, for instance, stars in the Magellanic Clouds. PROP ID: E025 PROPOSER: Raymond PROPOSAL TITLE: Physics of a Fast Collisionless Shock in SN1006 We propose to study the interaction of a fast ejecta knot in SN 1006 with the ISM. Unique XMM and Chandra observations will be combined with the O VI intensity and line profile to study the physics of the ISM shock, which we believe to be faster than 3000 kms. We will obtain the kinetic temperature of oxygen for comparison with proton and electron temperatures. Shocks in the heliosphere show oxygen temperatures above 16 times the proton temperature, while few measurements of supernova remnant shocks are available. We will determine the size and density of the ejecta knot and explore its interaction with the ISM, and we may detect S VI emission from the ejecta. PROP ID: E029 PROPOSER: Henry PROPOSAL TITLE: FUSE Observations of Dust Scattering in the Coalsack The diffuse far ultraviolet background has been difficult to observe and the only observations to cover a significant fraction of the sky have come from voyager UVS observations by Murthy et al. While not optimized for the study of the diffuse background, FUSE is sufficiently sensitive to observe diffuse levels on the order of a few thousand photons. We propose to observe several locations in the Coalsack Nebula where we have already found intense diffuse emission and have placed limits of 0.3 -- 0.5 on the albedo. We cannot, however, determine whether or not the grains scatter isotropically or are strongly forward scattering. Through a suitable choice of locations, we will be able to break this degeneracy and determine, for the first time, the optical constants of the interstellar grains in this wavelength region. PROP ID: E030 PROPOSER: Martin PROPOSAL TITLE: Probing the Evolution of Circumstellar Disks of Pre-Main Sequence Herbig AeBe Stars Herbig AeBe stars (HAeBes) are pre-main sequence stars of intermediate mass. They are the likely precursors of the beta-Pictoris and Vega-type stars, whose circumstellar debris disks are believed to host planetary bodies. At present, we do not know whether planets may form in every disk, or how long the planet formation process takes. We propose to obtain FUSE spectra of a sample of HAeBes of known age whose spectral energy distributions present a low near-IR excess, which shows that most of the dust has been dissipated in the central part of the disk. The analysis of H_2 lines in the FUSE spectra will allow us to quantify the gaseous content in the inner planet-forming regions of the disks around the stars and set limits on the timescale for planet building and dissipation of the circumstellar disks. PROP ID: E031 PROPOSER: Crenshaw PROPOSAL TITLE: Radial-Velocity Variations of an Intrinsic Absorber in the Seyfert 1 galaxy NGC 3783 We have discovered a decreasing radial velocity in an outflowing UV absorber in NGC 3783; this is the first detection of a changing radial velocity in a Seyfert absorber. The velocity decrease could be due to bulk deceleration of the gas or to a change in the direction of motion of the outflow across the line of sight to the broad-line region (BLR). The available evidence favors the latter possibility, which is exciting because it is predicted by dynamical models of accretion disk winds. A simple geometric model of a changing velocity vector predicts that the absorption lines will decrease in depth, and possibly even disappear, by early 2005. We propose two new FUSE spectra of NGC3783, separated by 7 -- 12 months, to 1) follow the evolution of the absorbers radial velocity, 2) tightly constrain the tangential velocity of the absorber, and 3) provide a definitive test of the changing velocity-vector hypothesis, thereby constraining dynamical models of the outflowing gas. PROP ID: E037 PROPOSER: Heber PROPOSAL TITLE: The nature of the compact companion of the sdB star HD188112 We discovered that HD188112, a nearby (80pc) B-type star, is a unique subluminous B (sdB) star. SdB stars are usually identified with models of core helium burning Extreme Horizontal-Branch (EHB) stars of half a solar mass. A spectral analysis of the hydrogen and helium lines place the star below the EHB. HD188112 was found to be radial velocity (RV) variable and the RV curve has been measured to be perfectly sinusoidal with a period of 0.606585 days and a semi-amplitude of 188.3 kms, indicating that it is a close binary system. From the atmospheric parameters and the Hipparcos parallax we conclude that the mass of the sdB star is too low (0.24,Msolar) to sustain core helium burning and it is now evolving into a helium core white dwarf. A lower limit to the mass of its unseen companion of 0.73,Msolar is derived from the mass function. Because the companion does not contribute to the spectral energy distribution from the UV to the infrared it cannot be a main sequence star but must be a white dwarf (WD), a neutron star (NS) or a black hole. Because of the large companion mass, HD188112 is a crucial system to test the double degenerate scenario for progenitors of SN Ia (sdB+WD). Due to gravitational wave emission it will merge and explode if its total mass is above the Chandrasekhar limit (1.4,Msolar). It may also be a post-supernova (sdB+NS) if the companion mass is above that limit. An estimate of the inclination angle is crucial to better constrain the companion mass. We propose FUV spectroscopy to measure the vs of the sdB star whose rotation is tidally locked to the orbital motion. In addition we will determine the metal content of the star. If a SN had occurred the ISM in the vicinity should show enhancements of alpha elements (esp. O). An abundance analysis of ISM metal lines might provide further evidence. PROP ID: E045 PROPOSER: Hebrard PROPOSAL TITLE: Is the present-epoch DH below 1x10e-5 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 one of the main objectives of FUSE. According to the first FUSE results, the DH ratio likely has a single value in the local interstellar medium (within sim100pc). However, with increasing distance and column density the DH values show significant dispersion and the three values measured at large distances are low; they may imply an averaged DH ratio significantly below the local value. These preliminary results suggest a present-epoch deuterium abundance below 1 x 10^-5, ie significantly lower than the value usually assumed. If these results are confirmed, they would challenge present models of deuterium evolution. The small sample size of the distant targets available has not allowed definitive conclusions to be drawn. Moreover, the availability of hydrogen column density measurements is limited. Using oxygen and, to lower extent, nitrogen as hydrogen proxies, we propose to measure deuterium abundance toward four extra distant targets. Selected from previously completed FUSE snapshots observations, they are in the column density range of the three distant sight lines where low deuterium abundances were measured. PROP ID: E046 PROPOSER: Hebrard PROPOSAL TITLE: DO and DN ratio in the far distant interstellar medium 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 one of the main objectives of FUSE. According to the first FUSE results, the DH ratio likely has a single value in the local interstellar medium (within 100 pc). However, with increasing distance and column density the DH values show significant dispersion and the three values measured at large distances are low; they may imply an averaged DH ratio significantly below the local value. If these results are confirmed, they would challenge present models of deuterium evolution. There is no information on the abundance of di at column densities greater than 1times10^16cmmd. Using DO and DN as proxies for DH, we propose to measure the interstellar abundance of deuterium for di column densities beyond that limit. The two targets that we propose to observe have been selected from FUSE snapshot observations. Our studies indicate that they are likely to be in that column density range. These observations will thus allow an unexplored area to be probed. PROP ID: E054 PROPOSER: Andre PROPOSAL TITLE: DH ratio in the Small Magelanic Cloud It has long been recognized that the primordial abundance of Deuterium can be used as a baryometer and is directly linked to the Omega_b cosmological parameter. Measurments of the primordial DH ratio have been performed in different astrophysical sites, in particular within Damped Lyman Alpha (DLAs) systems and Lyman Limit Systems (LLS) observed towards high redshifted quasars. The DLAs show generally a few percent solar metallicity and are the best candidates to investigate the primordial abundance of Deuterium. To date, the large measurement scatter prevent definitive conclusions to be drawn although a trend towards DH_primordial approx 2.5--3. 10^-5 has emerged. DLAs and LLS are not the only low metallicity targets available for the investigation of the history of the Deuterium both the High Velocity Clouds (HVCs) and the Magellanic Clouds ISM are well known to have tenth solar metallicity. HVCs targets have already been observed with FUSE using distant QSOs as background sources. However, SN ratios greater than approx 7 have never been achieved making the analysis quite uncertain. In the SMC, despite higher SN, the situation is worst since the D small I lines are blended with the Galactic H small I lines to the point where the D small I absorption lines has never been reported. However, the detection of the HD molecule in the diffuse SMC ISM with FUSE makes it possible to have an indirect measurement of the DH ratio through HDHmol. In a recent mini--survey of the HD molecules in the Magellanic Clouds we have noticed an unexpectedly large HD column density towards AV95. Higher SN FUSE dara are mandatory to confirm our preliminary assesment and reduce the error bars on the HD column density (HDHmol 2 times DH). PROP ID: E055 PROPOSER: Ehrenreich PROPOSAL TITLE: Search for mol H 2 in the Sagittarius dwarf spheroidal galaxy The Sagittarius dwarf spheroidal galaxy (SgrdSph) is located about kpc below the Galactic plane and is three times closer to the Galaxy than is the Large Magellanic Cloud (LMC). Numerous studies and surveys were done to characterize the stellar population and the dynamics of this galaxy. In particular, explorations of the orbital history of SgrdSph are all consistent with a total mass above 10^9Msun, which is one order of magnitude higher than the mass expected from the integrated luminosity. It is clear that the interstellar medium (ISM) component of SgrdSph might play an important role in the final mass budget. However, the ISM in dwarf galaxies remains observationally challenging and has not been thoroughly investigated yet. Comparison of CO emissivity with infrared emission in a sample of dwarf galaxies suggests that the CO-to-molH2 conversion factor is more than thirty times the assumed Galactic value. These observations suggest that a fraction of the dark matter associated with these galaxies is in the form of a large amount of hidden molH2. In fact, up to this date, spheroidal dwarf galaxies have never been observed in the far ultraviolet (FUV) domain and no one has been able to put strong constraints on their H 2 content. However, finding bright FUV sources able to enlight the SgrdSph ISM is extremely difficult. Here, we propose to observe the globular cluster M54 (NGC6715), which has been proven to be physically associated with the center of SgrdSph. Luckily enough, the line-of-sight (l-o-s) towards M54 does not only give the unique opportunity to investigate the ISM of our closest neighbour, but it is also one of the very few fuse l-o-s that probe the close neighborhood of the Galactic center. In particular, we argue that the expected flux of M54 in the FUV along with a relatively reduced reddening should allow for the detection of a large amount of diffuse ionOvi near the Galactic center. PROP ID: E061 PROPOSER: Knauth PROPOSAL TITLE: Where has the N_2 gone Molecular nitrogen has never been observed in the interstellar medium. Its abundance in translucent clouds is of considerable interest as the molecule is predicted to be the main sink of atomic nitrogen in these regions and an important precursor to dense cloud nitrogen chemistry. Recent FUSE observations of atomic nitrogen (ionN1) have shown a deficiency at total column densities above N(H_tot) 1 times 10^: 21 cm^ -2 . However, our preliminary search for the N_2 band at 958 AA has not yielded any reliable detection, even at levels well below those implied by the deficiency in NI. Existing observations below 000 AA have achieved only marginal signal-to-noise (SN < 15), due to the steep rise of interstellar extinction. Here we propose to obtain observations with high enough signal-to-noise (SN sim 50) to allow for a very sensitive search for N_2 toward a carefully selected sample of high column density targets. PROP ID: E062 PROPOSER: Wang PROPOSAL TITLE: O,VI Emission from the Halo of the Edge-on Galaxy NGC,3556 We propose three sl FUSE observations to sample the O,VI line emission from the halo of the nearby edge-on galaxy NGC 3556. The O,VI line emission traces the gas at temperatures near the peak of the cooling curve and can be compared with the X-ray radiation from the hotter component (Tgtrsim1times10^6,K), which has already been characterized by our sl Chandra study, and with the mechanical energy input from supernovae in the galaxy. The intensity and spatial distribution of the line emission will be used to infer or tightly constrain the temperature distribution of the extraplanar corona gas. The line centroids and widths of the emission will further enable us to measure the line-of-sight size and the dynamics of the gas. The results will have strong implications for our understanding of the disk-halo interaction of the galaxy. PROP ID: E063 PROPOSER: Tripp PROPOSAL TITLE: Warm-Hot Gas in the Milky Way Halo -- A FUSE+Chandra Study of OVI, OVII, and OVIII Absorption toward Recent observations of ionO6 and ionO7 absorption lines in the spectra of low-redshift QSOsAGNs offer tantalizing evidence that the missing baryons have been found, and that they are located in shock-heated warm-hot intergalactic gas at T 10^5 - 10^7K. However, important uncertainties remain in the nature of the O 6 - and ion O 7 -bearing gases. Are these large, low-density, low-metallicity absorption systems that contain the large majority of the baryons, or are they smaller objects with higher densities and metallicities We have been awarded 100 ksec of Chandra time to observe the bright X-ray binary LMC X-3 to study ionO7 and ionO8 absorption in the Milky Way halo with unprecedented sensitivity. This observation will provide crucial constraints on the size and distance of the absorbing gas since the target is in the Large Magellanic Cloud, i.e., these are both lesssim 50 kpc for any absorption detected in front of LMC X-3. To investigate key questions about the ionO7ionO8 absorption, we must have high-resolution ionO6 observations in the same direction. Here we propose to observe LMC X-3 with FUSE to obtain complementary constraints on ionO6 in the Galactic halo. With the combined FUSE+Chandra data, we will address the following questions -- (1) Are these absorbers located in the Galactic halo, or are they at greater distances in the Local Group (2) Do the ionO6 and ionO7 absorption lines arise in the same (single-phase) gas, or are these lines more likely from different phases in a multiphase medium (3) Do the line properties indicate that the gas is collisionally ionized, photoionized, or both Could the absorption arise in non-equilibrium cooling gas The combined X-ray and UV data will also be invaluable for studying the accretion physics of this X-ray binaryblack hole candidate. Velocity variations of the ionO6 emission from LMC X-3 will place tight constraints on the accreting black hole mass. PROP ID: E065 PROPOSER: Jenkins PROPOSAL TITLE: Using Spectroscopic Binaries to Detect Broad Interstellar O VI and Diffuse Bands In conventional observations of hot stars, shallow, broad interstellar absorption features can escape detection because they are confused with stellar absorption features, even those that are rotationally broadened. We propose to observe wide noninteracting) spectroscopic binary systems at different phases so that we can remove the stellar features by detecting their translations. Our objective is to sense the presence of (1) gaseous material at Tsim 300,000,K with a velocity dispersion of order or more than 100, kms^-1 and (2) diffuse interstellar bands in the FUSE wavelength region. To accomplish these goals, we plan to observe 3 binary systems at 7 different phases and then apply, in each case, a special analysis program that produces three separate spectra -- (1) the primary stars spectrum, (2) the secondary stars spectrum and (3) the stationary absorption features arising from the ISM. The ISM features should be free of any perturbations arising from the stars. PROP ID: E066 PROPOSER: Crampton PROPOSAL TITLE: FUV Spectroscopy of the Short-period Nova-like Variable TT Arietis TT Ari is a bright nova-like cataclysmic variable (CV) which is a member of the VY Scl subclass, since it occasionally drops 5 or more magnitudes when its luminous accretion disk dissipates. TT Aris short orbital period (3.3 hr) differs by a few percent from its variable photometric period, which is modulated by precession effects in the disk. The brightness of the system also varies on several other timescales. The stellar components, a hot white dwarf and a faint M dwarf, are only seen when the system drops into one of its rare faint states. With FUSE spectra it will be possible to obtain high signal-to-noise and high time-resolution spectra through the orbit, providing new information about the physics and kinematics of the disk. The far-ultraviolet continuum will give information about the temperature of the innermost accretion disk and the white dwarf. Continuum variations in the FUV will be compared with concurrent optical photometry. The FUSE spectra will provide unique velocity measurements of the inner disk, particularly using the OVI resonance lines, which should better define the white dwarfs motion (and hence the stellar masses). If the FUSE observations are obtained during a faint state, the data may provide constraints on the white dwarfs rotation rate. Mass lost from the system, via its phase-dependent stellar wind, will be detected through P Cygni profiles and in H_2 absorption from cool material expected to surround the system. PROP ID: E068 PROPOSER: Lobel PROPOSAL TITLE: Wind Acceleration Mechanism of Cool Supergiants We propose to observe with the FUSE the far-UV spectrum of the peculiar variable yellow hypergiant rho Cassiopeiae, which offers an exceptional laboratory to investigate the poorly understood acceleration and wind driving mechanisms of evolved pulsating stars. This cool enigmatic star became recently very active with a tremendous outburst event in the fall of 2000. During the event we directly observed the largest mass-loss rate (sim0.05 M_, yr^-1) in any stellar object so far (Lobel et al. 2003, ApJ, 583, 923). Over the past two years since the eruption we observed a very prominent inverse P Cygni profile in Halpha, signaling a strong collapse of the upper atmosphere, also observed before the 2000 outburst. Our continuous spectroscopic monitoring reveals that the Halpha line profile has transformed into a P Cygni profile over the past five months, presently signaling supersonic expansion velocities up to sim120 km,s^-1 in the upper atmosphere, similar as in the 2000 event. The fast atmospheric expansion is expected to continue over the coming year based on our recent monitoring. We propose to observe the pumped Fesc ii emission lines at lambda1119 and lambda1124 to investigate their detailed line shapes using the high spectral resolution of FUSE. These line profiles will provide important clues about the wind acceleration mechanism in rho Cas during the exceptionally fast atmospheric expansion in Cycle 5. As the hypergiant changes spectral type from late F to G-K (or even early M), the Fesc ii emission lines are expected to reveal peculiar asymmetric shapes. These profiles are observed in the smaller G-type supergiant alpha Aqr, but cannot provide direct evidence that its wind velocity structure is in fact accelerating outwards. FUSE observations of asymmetric FUV Fesc ii emission profiles in rho Cas will directly reveal if the wind velocity structure globally accelerates outwards in this cool star, or whether it is determined by the local gas dynamics that drives the fast expansion. PROP ID: E075 PROPOSER: Cheng PROPOSAL TITLE: Circumstellar Gas of Nearby A-type Stars Since the discovery of Vegas (A0V) large thermal infrared excess over the expected photospheric flux, dust disks have been found around a large fraction of main-sequence A-type stars. Visual and ultraviolet observations have revealed dynamic circumstellar gas disks around several Vega-type stars. Recent models of the dynamics of gas-dust coupling in Vega-type circumstellar disks suggest that the structure of dust disks strongly depends on the properties of gas disks. With high-resolution and high signal-to-noise visible and UV data, we have identified a least a dozen nearby A-type stars with circumstellar gas through a volume-limited survey. We have observed one of them (2And) with FUSE, and we propose to obtain FUSE spectra of four other early A-type stars with circumstellar gas identified by our survey. The FUV spectral range contains many absorption lines that are good diagnostics of circumstellar gas. Our proposed FUSE observations will help answer the following questions related to the evolution of circumstellar disks. Are A-type stars with circumstellar gas and those with dust disks in the same evolutionary stage Do dust disks develop only after most of the first generation gas has disappeared Is the observed circumstellar gas second generation, formed from destruction of falling bodies (comets or planetesimals) through collisions and evaporation PROP ID: E076 PROPOSER: Boisse PROPOSAL TITLE: Probing the very small scale structure (l simeq 100 AU) in the interstellar medium (continued) HD34078 has a transverse velocity of 22 AUyr; the five FUSE spectra already obtained during cycle 1, 2, 3 allow us to probe the internal structure in the foreground translucent cloud by comparing lines of sight distant by simeq 10 to 0 AU at the cloud distance. The intercomparison of these high quality spectra SN simeq 20 at 1100 AA) led us to set an upper limit as low as 5 percent on N(H_2) variations. This result points towards very little ubiquitous density structure. In order to improve the sampling and increase the range of scales probed, we propose to extend our follow-up to five years by taking two spectra during cycle 5. A long-term increase in both N(CH) and N(HI) has been detected and FUSE cycle 5 observations could reveal similar variations for N(H_2). The FUSE data set accumulated on HD34078 is unique and, given the low cost in observing time involved, we think is important to increase its scientific potential by extending the follow-up as long as possible. PROP ID: E079 PROPOSER: Smith PROPOSAL TITLE: FUV Diagnostics for Co-Rotating Disks of the He-Peculiar B Stars HD 184927 and 36 Lyn The phenomenalogy of several variable subclasses of B stars arises from the interactions of magnetic fields, winds, diffusion, and rotational effects. We request FUSE observations at occultation and quadrature phases (2 for target 1, 3 for target 2) of a prototype of each of the magnetic He-strong and He-weak Bp classes. The C,IV and N,V resonance lines of these stars IUE spectra are at some phases strongly in absorption, and at other phases show redshifted emissions. These features form in shocks where the wind impacts the magnetospheric torus-disks co-rotating over these stars. But what is the process responsible for the implied heating UV spectroscopy can answer this by exploring the disk geometry inferred from the Fe-curtain and resonance lines from a large range of ions. These diagnostics will be aided by turbulent broadening in resonance lines observed at disk-occultation. The behavior of both types of features will be contrasted with high-excitation photospheric lines, which show little change over the cycle. We will also explore the chemical fractionation of the metals in the disks by comparing UV analyses with ground-based observations of Balmer lines. PROP ID: E082 PROPOSER: Massa PROPOSAL TITLE: P V and the mass loss discrepancy in O stars Psc v has emerged as an important wind diagnostic in fuse spectra of O stars. Recent studies have demonstrated that mass loss rates determined from Psc v lines in LMC O stars are factors of 3 - 5 times lower than predicted by currently accepted models or mass loss rates determined from Halpha and radio measurements. Furthermore, initial estimates for Galactic stars suggest a similar discrepancy. This problem underscores the importance of deriving mass loss rates from independent observational material. To examine the origin of the disagreement more closely, we propose to obtain Psc v data for a set of stars that have been modeled at Halpha and many of which have been observed in the radio. These stars are the fundamental set which have been repeatedly compared to models and were a cornerstone in deriving the Wind Momentum-Luminosity relationship for O star winds. PROP ID: E084 PROPOSER: Collins PROPOSAL TITLE: The Mixing of Infalling and Galactic Gas in High-Velocity Cloud Complex C We propose substantial FUSE observations of the sight-line towards Mrk 290, which intercepts the high-velocity cloud (HVC) Complex C. These data will be used, along with new data for Mrk 290 and PG 1626+554 in the FUSE archive, as well as data from planned observations of Mrk 501, to address Galactic interstellar gas mixing, infalloutflow, and chemical history. The origin of Galactic HVCs seen in ionH1 emission and metal absorption lines has recently become better understood. Our recent study (Collins, Shull, & Giroux 2003a) includes FUSE and HST data for eight sight-lines through Complex C, an HVC in the northern Galactic hemisphere. The large angular size of Complex C, as well as the existence of several extragalactic targets whose sight-lines pass through the cloud, allow us to investigate the interaction of an HVC with the Galactic halo as it plunges toward the disk, as well as the opportunity to probe the fossil record of earlier star formation. With accurate metallicities based on O 1 ion H 1 , plus measurements of Si 2 , ion Fe 2 , ion S 2 , ion Ar 1 , and ion N 1 , our study suggests that Complex C is a mixture of infalling low-metallicity gas and enriched gas from the Galactic disk. In addition, for the three sight-lines for which ionO1ionH1 could be measured, we found significant metallicity variations, ranging from ZZsubsun0.1-0.25. The data quality for half of the sight-lines needs to be enhanced to permit sensitive abundance studies and to improve the statistics on any possible metallicity variations. FUSE observations of Mrk 290 will provide the sensitivity necessary to measure the abundances of the important ions ionO1, ionAr1, ionSi2, and Fe 2 . In addition, the measurement of (ArO) in a second Complex C sight-line could test for a top-heavy IMF in earlier generations of stars. PROP ID: E087 PROPOSER: Tumlinson PROPOSAL TITLE: IGM Phases and HVCs in 37 SDSS Galaxy Groups We propose new observations of two AGN previously observed by FUSE, to explore the relationships between galaxy groups and the intergalactic medium (IGM). These observations will search for absorption lines of H I, C III, and OVI associated with 37 SDSS galaxy groups at known velocity along the sightlines. Such absorption could arise from the predicted hot phase of the IGM (the missing baryons) or from distant analogs of the high-velocity clouds (HVCs) seen near the Galaxy and Local Group. Theory predicts that 30 - 40 percent of low-z baryons reside in the warm-hot intergalactic medium (WHIM; 10^5 - 10^7K), but only sim 10 percent have been found. Because galaxy groups are common, occupy a small fraction of space, and have been predicted to hold intragroup gas at temperatures just right for the WHIM, they are excellent places to look for the missing baryons. We will also address the origins of OVI-bearing HVCs seen with FUSE, by complementing the FUSE survey of HVC OVI with multiple probes of galaxy groups along chordal sightlines. Our approach maximizes scientific return by searching for absorption in groups identified in the SDSS. Prior knowledge of galaxy group coincidences improves search efficiency because the number of such pairings varies widely between sightlines. Our targets are chosen to maximize the number of groups that can be observed within a lesssim 200 ksec program. Ultimately, our discovery program for OVI in galaxy groups will enable detailed probes of galaxyIGM associations, measure metallicity and excitation, improve statistics on the IGM OVI absorbers, and help generalize FUSE results on Local Group HVCs. PROP ID: E088 PROPOSER: Andersson PROPOSAL TITLE: Cold Clouds in the Upper Centaurus-Lupus Superbubble Using a combination of FUSE and ROSAT data, we have shown that the Southern Coalsack is surrounded by a hot, OVI bearing, envelope. Based on these observations we have identified the hot interior of the Upper Centaurus-Lupus UCL) super-bubble as the source of the heating of the cloud envelope. This hypothesis is supported by a detection of OVI in the Lupus cloud, which is also embedded in the UCL bubble. Here we propose to search for OVI absorption in four additional dense clouds located inside the UCL bubble. The clouds span distances from the center of the bubble from 0.5 to 1.0 of the bubble radius and hence trace a time series of immersions of the clouds into the hot bubble interior. Combined with observations of other highly ionization species, such a time series, in particular when analyzed together with the high spatial resolution data of the Coalsack, will allow quantitative tests of models of hot-cool interaction regions. PROP ID: E090 PROPOSER: Korpela PROPOSAL TITLE: Investigating OVI emission in the Eridanus Superbubble The Eridanus superbubble has been called the Rosetta Stone of superbubbles because virtually all of the processes which shape the interstellar medium are taking place somewhere within its boundaries. One of the features of this region is the Eridanus Soft X-ray enhancement. It is understood that this enhancement is a region of hot gtrsim 3times10^6 K) gas that fills the Eridanus cavity. We propose to investigate two lines of sight for ionO6 lambdalambda 032,1038 emission, one which intersects an optically thick neutral cloud located within the X-ray emitting region and one which does not intersect the cloud. The observation of the line of sight not intersecting the cloud, combined with a high signal-to-noise Cycle 2 archival absorption measurement of a QSO on a very nearby line of sight, will allow us to accurately determine the physical properties of 10^5.5 K gas within the superbubble. The line of sight intersecting the cloud will provide additional information about the physical location of the emitting regions and the interface between the cloud and the hot gas in which it is embedded. These data will allow us to distinguish between contrary theories of the structure of the ISM and energy transport mechanisms that occur within it. PROP ID: E091 PROPOSER: Stocke PROPOSAL TITLE: Probing Outflowing Winds from the Galactic Center In order to complete the suite of HST and FUSE observations necessary to detect and characterize the outflowing wind from our own Galaxys nuclear region, we request 25 ksecs on FUSE to observe 3 B-type comparison stars near one of our primary AGN sight lines. While there is indirect evidence for either a starburst or AGN-type wind from the Galactic Center (GC), this project seeks to detect this hot wind directly in absorption. Our two HSTFUSE AGN targets (PKS,2005-489 and Mrk,1383) lie within 10dd of directly over the GC, and so absorption lines of highly-ionized species like CIII, CIV, SiIV, NV, and OVI are expected. However, other potential sources of outflowing gas lie in the foreground of the GC (Sco-Cen OB Associations, 2-4 kpc away). In order to make sure that the absorptions we see in the AGN spectra are due to the GC, we require spectra of bright B stars, which are behind the Sco-Cen Associations but foreground to the GC. HSTSTIS observations are scheduled for HST! cycle 12, and the necessary FUSE observations are all in-hand excepting spectra of 3 B stars near PKS,2005-489, which we are requesting here. PROP ID: E093 PROPOSER: Lecavelier PROPOSAL TITLE: Search for the 10^5--10^6K gas in the cluster of galaxies Abell2199 Our knowledge of the hot gas (>10^6K) in the intra-cluster medium of clusters of galaxies has recently considerably increased with the new Chandra and XMM X-ray observations. It is now clear that the amount of hot gas which is cooling below sim1keV is more modest than previously thought. Still, the real level of the cooling flows (if any) is yet to be clarified. FUSE has already been successfully used to detect the Osc vi doublet at 032, 1038AA in the cluster of galaxies Abell2597 (Oegerle et al. 001). This provided the first direct evidence for the presence of sim 3 10^5K gas in a cluster of galaxies. The detection of the emission lines (with a flux lower than initially anticipated), together with the non-detection of O,sc vi lines in the clusters Abell1795 (Oegerle et al. 2001), Abell2029 & Abell3112 (Krishna, Lecavelier & Durret) appears in agreement with the new emerging picture that the cooling flow rate is lower than concluded from earlier X-ray observations. To search for the much needed similar evidence for warm gas associated with rich clusters of galaxies, we propose FUSE observations of Abell2199 in which the presence of a moderate cooling flow up to sim12 M_yr^-1 is allowed by the recent Chandra observations Johnstone et al. 2002). Abell 2199 is the last known candidate for which, using new estimates of the flowing rate, the detection of the O,sc vi lines is within sl FUSE capabilities. The detection of O,sc vi and C,sc iii lines (or not) will allow us to conclude on the presence (or the absence) of this moderate cooling flow at an unprecedented sensitivity. This observation, even in case of a non-detection, will allow us to constrain the heating rate needed to maintain the high temperature of the gas observed in the X-rays. Even a single addition to the very small number of cooling flow clusters observed with FUSE, will help in identifying the trends and constraints on the warm ICM in such clusters. PROP ID: E095 PROPOSER: Bregman PROPOSAL TITLE: OVI in the Bulges of Normal Spiral Galaxies The tremendous amount of star formation in starburst galaxies gives rise to supernovae, hot gas, and superwinds. So it is no surprise that absorption by the OVI is seen in these systems, but we are stunned by the detection of even stronger OVI absorption in the bulge of M31, an extremely quiescent environment with little star formation. Not only is this line strong, but is nearly black, which occurs only if the hot gas is pervasive in the bulge, and optically thick. To determine if this is a common phenomenon, we propose to observe three other bulges of normal spirals, as hardly any have been observed with FUSE. Also, we can determine whether this hot gas is flowing outward or inward by measuring the radial properties of the gas in M31. PROP ID: E096 PROPOSER: Bregman PROPOSAL TITLE: The Molecular Gas Content in M 51 In the standard picture for grand design spirals, HI is converted to H_2 near spiral arms, triggering star formation. This may not be occurring in the inner part of M51 as the amount of HI present is completely inadequate. Either the molecular gas content, determined from CO, is badly wrong in the arm andor interarm regions, or the model paradigm must be discarded. These issues will be resolved by an independent and accurate measurement of H_2 in the arm and interarm regions, which we can obtain with the proposed FUSE observations. We have shown that H_2 absorption can be measured against the UV stellar light of the disk and we apply that technique for carefully chosen arminterarm pairs in M51. PROP ID: E098 PROPOSER: Herczeg PROPOSAL TITLE: Dissipation of gas in disks around nearby young stars We propose to use FUSE to search for gas in dissipating circumstellar disks around young stars in two nearby associations, the TW Hya association and the eta Cha association. FUSE is uniquely capable of detecting H_2 gas in absorption, and can also detect fluoresced H_2 in emission. This combination allows us to detect the gas and diagnose its origin in a disk or surrounding circumstellar material. This proposal will yield valuable results on the ability of gas to survive in disks as the dust in the disk is dissipating. The detection or non-detection of this gas will provide important constraints on timescales of planet formation. PROP ID: E101 PROPOSER: Wood PROPOSAL TITLE: Accretion Disk Renewal in Mira AB MiraAB is one of the few wind accretion systems in which the components of the binary are resolvable. It is therefore a unique laboratory for studying wind accretion processes, a common but not yet understood phenomenon in many astronomical sources. Previous HST and FUSE spectra of MiraB, taken in 1999 and 2001 respectively, show a dramatic drop in UV emission from what IUE observed from 1979 to 1995. Another baffling development is the appearance of a forest of Lyalpha-fluoresced H_2 emission lines, which dominate the HST and FUSE spectra despite not being seen at all by IUE. One possible interpretation for the UV variability is that it is caused by periodic disk renewal, possibly associated with a 4-year periodicity previously seen in the optical. Our proposed observation will test this interpretation, which predicts that MiraB should return to a high state during FUSE Cycle5, making a new FUSE spectrum radically different from the 2001 observation. A new observation will also provide a UV spectrum contemporaneous with a planned Cycle5 Chandra observation of Mira, which is crucial for a proper interpretation of the X-ray data, and valuable for an accurate estimate of the total accretion luminosity of the system at that time. PROP ID: E105 PROPOSER: Bowen PROPOSAL TITLE: The Metallicity of Gas in the Local Universe---the sightline to PG1543+489 We wish to obtain a FUSE spectrum of the z0.40 QSO, PG1543+489. The sightline to this quasar intercepts a high HI column density log N(HI)19.1 absorption system at z0.07489, which likely arises in the outskirts of an edge-on spiral galaxy 45h from the line of sight. Our principal objectives are five-fold. First, we wish to measure the oxygen abundance in the absorber, from which we can calculate a nitrogenoxygen ratio when combined with existing HST data. This will enable us to infer the chemical history of the absorbing material. Second, we seek to detect ArI and NII lines in order to validate that the bulk of the absorbing material is neutral. Third, we will search for OVI absorption from the absorber, giving us the first clear detection of these lines from a galaxy beyond the Magellanic Clouds. Fourth, we will measure molecular hydrogen lines from the absorber, in order to study the seeds of star-forming regions in a galaxy beyond the Local Group. Finally, it is quite possible that this system is ideal for the measurement of Deuterium. Determining the DH ratio in a nearby, low metallicity galaxy is a crucial step in relating the degree of astration of D to the progress of galactic chemical evolution. PROP ID: E108 PROPOSER: Iping PROPOSAL TITLE: Ionization Structure of the Stellar Wind in the High Mass X-ray Binary Vela X-1 The high-mass X-ray binary Vela X-1HD,77581, consisting of a 283 s pulsarB0.5 Iab supergiant, will be observed at five critical phases of the binary orbit (8.96 days) to probe the effects of X-ray photoionization. The pulsar ionizes its surroundings as it moves through the binary orbit, producing X-rays while accreting some of the ambient stellar wind from BO.5 Iab supergiant. The FUSE spectra will be used to 1) characterize the phase-dependent X-ray ionization of the stellar wind and its density distribution, including the photoionization wake at phi0.6-0.9, 2) study enhanced abundances in the atmosphere of the primary, and 3) search for the 283-s pulsar periodicity in the stellar wind lines. o6 1032-38, s4 1063-73, and p5 1118-28 are the primary diagnostics to achieve these objectives. These line profiles are unsaturated across the full velocity range of the stellar wind, resulting in a complete picture of the run of optical depth (or .: M q) with velocity. Strong saturation in the stellar wind lines at longer wavelengths (n5, c4, si4) have precluded such studies. p5 is the only unsaturated transition of a dominant ionization stage in the wind, hence it provides a direct measure of the bulk wind properties. Chandra HETGS spectra show the temperature of the X-ray ionized region of the wind is sim120,000 K, making o6 an excellent diagnostic of this plasma. Our recent Cycle 4 observations of another HMXB system (4U1700-37) demonstrate the power of the FUSE region for studying the effects of the X-ray source on the stellar wind that feeds the accretion. PROP ID: E109 PROPOSER: Iping PROPOSAL 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 (Vle 14). 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 HSTSTIS TOO observations E140M, 116050mAA. The redshifts of the QSOs will allow us to probe multiple ion states of oxygen (OVI, OIV, and OIII), CIII, SiIII, 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 with FUSE and HST imply that the highly ionized IGM is a major reservoir of the missing baryons in the universe at low redshift. The observations will nearly double the number of QSOs for which medium quality (SN >10) FUSE spectra will exist. The measurements will also be valuable for numerous Legacy studies by the general astronomical community including -- the physical conditions in the Milky Way halo and disk H_2), OVI and other ions in HVCs, the properties of the low redshift HI forest, photoionized QSO metal line systems, and the properties of QSOs and their associated absorption line systems. We recommend that the 6 brightest QSOs be observed in Cycle5 and the 5 faintest in Cycle6 of this two year program. PROP ID: E542 PROPOSER: Ayres PROPOSAL TITLE: Seven Days in the Life of AR Lac A week-long FUSE stare at short-period eclipsing RS CVn binary AR Lac K0IV+G4IV; P2d), coordinated with groundbased radio imaging and optical Doppler mapping, will provide an unprecedented view of structure, energetics, and dynamics of hot-gas activity, through time-resolved measurements of FUV diagnostics like C III 977, O VI 1031, and (coronal forbidden line) Fe XVIII 974. As a class, RS CVns are notorious for extreme high-energy emissions even during quiescent periods, but are most spectacular during flare outbursts. Our project is the cool star equivalent of a Hubble Deep Field, in the time domain; a new window on magnetic activity in extreme environments ubiquitous in the Cosmos, but only now beginning to be characterized and understood. (Although the FUSE program is stand-alone, we plan to broaden and enhance the campaign by requesting Chandra HETGS and HST STIS time to be coordinated with the FUV spectroscopy.) PROP ID: E548 PROPOSER: Howk PROPOSAL TITLE: A Legacy Survey to Probe the Cosmic Web with Extreme Ultraviolet Spectroscopy The baryons associated with galaxies, galaxy clusters, and the lyalpha forest in the present epoch fall well short of the total baryon density of the universe. Cosmological hydrodynamical simulations predict that much of the low-redshift baryons (sim30 phase of the intergalactic medium (IGM) associated with large-scale (unvirialized) filaments. We propose a comprehensive FUSE Legacy program to study the physics of the WHIM and other metal absorbers and their relationships to large-scale galaxy structures. We will observe six moderate-redshift AGNs (0.3 la z la 1.0) to determine the physical state of WHIM absorbers by using extreme ultraviolet (EUV) transitions redshifted into the FUSE bandpass. The EUV spectrum offers unique physical diagnostics, including strong lines from the adjacent ions ion: N 2 ion N 3 ion N 4 and ion: O 2 ion O 3 ion O 4 ion O 5 (which complement HST coverage of ion: N 5 and ion O 6 ). The species ion Ne 8 and ion: Mg 10 , which have strong EUV transitions, are particularly important since they are more abundant than ovi at the temperatures thought to contain the bulk of the WHIM baryons. Our proposed survey of the low-redshift IGM will increase the observed redshift path for detection of these ions by factors of 2--6. The observations of the ions available in the EUV bandpass will allow us to (i) test the current models of the WHIM by studying the ionization mechanisms responsible for producing highly-ionized metals in the IGM and determining the frequency of genuine high-temperature metal absorbers in the low-redshift IGM; (ii) derive high-quality elemental abundances for the low-z lyalpha forest; and (iii) investigate the relationship between WHIM and other metal-line absorbers and large-scale galaxy structures by combining the proposed FUSE observations with galaxy redshift measurements obtained using DEIMOS on Keck and IMACS at Las Campanas Observatory. We will make high-level science products derived from these data freely available to the general astronomical community. PROP ID: E568 PROPOSER: Holberg PROPOSAL TITLE: A Legacy Program of FUSE White Dwarf Spectroscopy Although FUSE has devoted a considerable fraction of its observing program to the study of white dwarf stars, significant unfilled gaps remain in the scope and depth of these observations. The majority of FUSE white dwarf observations have been motivated by a variety of objectives, including instrumental calibration, studies of the ISM, as well as programs focused on particular details of the photospheres of these white dwarfs. We propose a Legacy program of white dwarf observations designed to fill these gaps. This program is tightly focused on H-rich DA white dwarfs, which constitute the overwhelming majority of all white dwarfs, and is specifically designed to address the resolution of the recently discovered discrepancy between Lyman line and Balmer line temperature and gravity determinations. The observations resulting from this program will ensure that the final FUSE archive contains the widest possible sampling of the population of DA white dwarfs. SURVEY PROGRAMS --------------- PROP ID: E805 PROPOSER: Bianchi PROPOSAL TITLE: The fundamental parameters of massive stars We analysed archival FUSE and HSTIUE spectra of O-type stars in the Milky Way and found T_eff and luminosities significantly lower (approx 10 to 20 than previous determinations for our sample stars, and than values assigned to their spectral types from previous compilations. This result has great implications for our understanding of massive stars evolution, and of the energy balance of HII regions. An effort to analyse homogeneously a representative number of stars covering the early spectral types, would ultimately provide a refined calibration of the temperature scale versus spectral type and luminosity class, as well as other important parameters such as mass loss rates. However, crucial gaps remain in the coverage of the early spectral types in the list of FUSE observed or approved Galactic stars. We propose to observe a small number of stars to remedy the most conspicuous gaps. By contrast, a very good coverage of spectral types for Magellanic Cloud stars is already available in the FUSE archive. A similar sampling of the early spectral types in the Milky Way will provide a unique opportunity to compare massive stars parameters among the three galaxies with very different metallicities (MW, LMC, SMC). Additionally, the data will be of great value for population synthesis work. PROP ID: E813 PROPOSER: Werner PROPOSAL TITLE: Iron abundance in PG1159 stars The very first attempt to measure the iron abundance of a hot hydrogen-deficient post-AGB star arrived at a surprising result. Based on the absence of Fe lines in a FUSE spectrum of the PG,1159-type central star of the planetary nebula K1-16 we could show that this object is Fe-deficient by a factor of at least 10--100. We showed by subsequent FUSE spectroscopy that the same phenomenon is exhibited by two related objects, a WC-PG1159 transition-type star and a so-called PG1159-hybrid star. Here we propose a systematic investigation of PG1159 stars to show if Fe-deficiency is a common phenomenon among these objects. We speculated that the iron underabundance is caused by the destruction of iron through s-process neutron capture as a consequence of a late helium-shell flash. If this is true, then all PG1159 stars should be Fe-deficient, because they all are the outcome of a late helium-shell flash. PROP ID: E821 PROPOSER: Brown PROPOSAL TITLE: The Formation Mechanism of Hot Helium-Rich Subdwarfs In FUSE Cycle 3, we obtained the first far-UV observations of He-sdB stars, which complemented the ongoing FUSE observations of normal sdB stars. Based on our theoretical models, we demonstrated that some He-sdB stars likely form from a delayed He-core flash on the white dwarf cooling curve (Lanz et al. 2003). The convection zone produced by such a flash penetrates the hydrogen envelope, mixing hydrogen into the hot He-burning interior, and triple-alpha carbon outward into the envelope. The resulting flash-mixed star shows greatly enhanced helium and carbon at its surface. This phenomenon is analogous to the born again scenario for producing H-deficient R CrB stars following a very late He-shell flash. The spectra of two of the three He-sdB stars in our previous FUSE program show a striking enhancement of carbon, just as expected for flash mixing. In view of this success, we propose to follow our He-sdB work with observations of three high-gravity (logg> 6) He-rich sdO stars. The location of these stars in the logg - log T_ eff diagram is not populated by canonical evolutionary tracks for stars leaving the horizontal branch or asymptotic giant branch (AGB). We hypothesize that the high-gravity stars may be the progeny of the flash-mixed He-sdB stars. Although FUSE is observing many He-rich and He-poor sdO stars, most of these are post-AGB stars; in contrast, the high-gravity region of parameter space is largely unexplored in the UV. Our proposed observations would therefore extend the library of subdwarf spectra and further explore this newly discovered evolutionary channel for producing hot stars. PROP ID: E848 PROPOSER: Sembach PROPOSAL TITLE: An Updated Snapshot Survey of AGNsQSOs for Intergalactic Medium Studies We propose a no-cost continuation of our FUSE Cycle 4 snapshot program to find QSOs and AGNs having ultraviolet fluxes bright enough for detailed follow-up observations with FUSE and the Hubble Space Telescope Cosmic Origins Spectrograph. Our intent is to find sources for absorption-line studies of the distribution and baryonic content of the low-redshift (z0.1-0.5) intergalactic medium. The start of this program in Cycle4 was particularly promising, with 3 of 10 objects observed being considered for follow-up studies. We will perform detailed spectroscopic follow-up of the best objects with guaranteed COS time, and we will propose for extended FUSE observations of the brightest objects in the next proposal cycle. In particular, we want to conduct a better ionO6 baryon census, study the physical conditions of individual absorption systems, determine the ionization mechanisms in the warm-hot intergalactic medium traced by ionO6 and other highly ionized species, and explore the structuredistribution of the ionized IGM. Increasing the limited number of UV-bright sources currently available for such studies will allow for improved tests of the predictions of hydrodynamical simulations of galaxy formation and evolution in the present-day universe. PROP ID: E853 PROPOSER: Young PROPOSAL TITLE: Activity and fluorescence among nearby 1.2--2.5M_ clump giants The causes of stellar activity among giants of masses1.0--3.0msun in and around the K-giant clump are poorly understood. In this region most stars have low rotational velocities yet activity, as measured through X-ray emission, varies by over 3 orders of magnitude. Only recently through the higher sensitivity of modern instruments onboard emphHST and ROSAT have giants previously considered inactive been found to weakly emit ionCiv, ionSiiv ayres97) and X-rays (schroder) indicating that coronae are ubiquitous in this part of the HR diagram. This proposal seeks to use the high sensitivity of fuse to understand the activity levels of inactive giants in and around the K giant clump, through a sample of five stars of different masses and evolutionary states. Coupled with data obtained through the FUSE PI Teams Cool Star Survey the important parameters governing activity amongst clump stars will be isolated. PROP ID: E897 PROPOSER: Dupke PROPOSAL TITLE: The Local Missing Baryons in the Cosmic Web Most of the baryons in the local universe are missing in that they are not in galaxies or in the previously detected gaseous phases. These missing baryons are predicted to be in a moderately hot phase, 1E5 to 1E7 K, largely in the form of giant cosmic filaments that connect the denser virialized clusters and groups of galaxies. These filaments can be detected through absorption lines they produce in the spectra of background AGNs. Models show that the highest covering fraction of such filaments occurs in superclusters and the archive has two AGNs projected behind superclusters, both of which show absorption systems (in LyalphaLybetaOVI) at the supercluster redshift. These results are impressive considering that these AGNs were not even optimally located. Following upon this success, we selected the best targets that lie close to the expected central axis of supercluster filaments to search for OVI and Lyman series absorption lines with FUSE. This study will expand our archival sample by a factor of 4 and will be complemented by an approved HST program to search for Lyalpha absorbers. PROP ID: E900 PROPOSER: Blair PROPOSAL TITLE: A FUSE Survey of Magellanic Cloud Supernova Remnants, continued We propose to continue an unbiased ultraviolet survey of supernova remnants in the Magellanic Clouds that was begun in Cycle 4. Work with FUSE indicates that optical andor X-ray characteristics of supernova remnants are not always good predictors of the objects that will be bright and detectable in the UV. This survey proposal will continue to test this conclusion by obtaining spectra of additional Magellanic Cloud remnants with a broad range of radio, optical, and X-ray properties. Previously observed objects and remnants with known high extinction (or high column densities) are the only objects eliminated from consideration. A standard request of 0 ks per object using the LWRS aperture is used for the survey, reaching a limiting flux in OVI lambda1032 about a factor of 100 below the flux observed for the LMC remnant N49. To date in our Cycle 4 survey program D904 we have obtained significant detections of OVI in 5 out of 11 objects observed. In this proposal, we request time to observe any of the candidate objects in D904 not observed in Cycle 4. The time and number of targets listed is thus an upper limit to the actual request. PROP ID: E903 PROPOSER: Dupuis PROPOSAL TITLE: Mapping the Abundances of Heavy Elements in Hot DA White Dwarfs Atmospheres We propose to conduct a survey of high latitude hydrogen-rich atmosphere white dwarfs. The selected stars sample a wide range of effective temperatures and surface gravities and will allow us to better characterize the metal abundance patterns during the early phases of the cooling of a white dwarf. Metals in radiative white dwarf atmospheres are tracers of diffusion processes, but abundance patterns in white dwarfs observed to date are generally not in strict accordance with theoretical predictions. Only an increased sample of white dwarfs with accurate abundance measurements will help us put some order in the somewhat confusing current situation. For instance, this would help us to assess the role of residual mass loss in hot white dwarfs for which a convincing direct evidence is still lacking. PROP ID: E937 PROPOSER: Bennett PROPOSAL TITLE: Masses and Mass Loss Rates of Red Supergiants in Binaries We propose to observe a reasonably complete sample of northern, late-type, mostly supergiant, binaries with FUV-bright B-type companions, as a Survey and Supplemental Program. The objective is to determine stellar masses of a diverse sample of massive, evolved, late-type stars accurate to 1 a category of stars for which few, accurate stellar masses are known. A secondary goal is to determine mass loss rates of the stellar winds of these evolved stars. These supergiant binary systems are important, fundamental stellar laboratories, useful in verifying and constraining models of stellar structure and evolution. We will proceed by determining accurate radial velocity orbits of the early-type companions. The program stars are all selected from the PIs DAO radial velocity program (the Precise Mass Project) target list, and have been extensively observed in the optical for nearly a decade. All the DAO binaries have primary radial velocity orbits determined, or have sufficient optical observations available such that these orbits can be well-determined. Therefore, the single observation of the companions FUV spectrum proposed here will suffice to determine the companions orbit and thus the stellar mass ratio. Some of the target stars eclipse, and for these binaries, accurate individual stellar masses will be directly obtained. Masses of the remaining systems will be obtained from optical interferometry; all these binaries are planned to be observed by NPOI for this purpose. The proposed FUSE observations are an essential link in the process of determining accurate masses of these evolved stars. PROP ID: E949 PROPOSER: Peters PROPOSAL TITLE: A FUSE Survey of Algol-Type Interacting Binary Systems We propose a survey of Algol-type interacting binaries with FUSE. The observing list contains 15 systems with deltage40^o for which systemic parameters are known. The program stars span the range from early-type contact systems that will eventually become conventional Algols to wide binaries in an advanced evolutionary state with prominent accretion disks. Some physical parameters that can be obtained include the ionization temperature and density in the accretion disk, domain of infall (gas stream), high temperature plasma on the trailing side of the system, and in certain systems the splash zone. We will look for the presence of ionO6 absorption and assess the phase interval over which it is observed. Emission from this ion has already been found in FUSE observations of three Algols (V356Sgr, TTHya, and RYPer) during total eclipse and confirms the presence of a sim300,000K plasma abovebelow the orbital plane. In accordance with the policy on the FUSE Survey and Supplementary Program, the observations will be obtained at random phases, but we request 5 visits of each target in order to secure good phase coverage and maximize the probability of obtaining data at interesting phases, such as the interval containing the mass outflow in the splash region where a tangentially-impacting gas stream is deflected off of the mass gainers photosphere. The physical parameters that are obtained in this project will constrain future 3-D hydrodynamical simulations of mass flow in Algols. This project will build upon the successful one (Z902) carried through in FUSE Cycle3. PROP ID: E950 PROPOSER: Espey PROPOSAL TITLE: A FUV Survey of Extragalactic Symbiotic Binary Stars We propose a survey of all 14 known symbiotic systems in the Magellanic clouds. Extragalactic symbiotic systems are objects which have relatively few observations in all wavelength regions, especially the UV, and have never been observed in the wavelength region of FUSE. Due to their well determined distances, the systems in the Magellanic clouds are ideal objects to derive the absolute luminosities of the stellar components - which are not well known for galactic symbiotics. Continuum FUV fluxes, free from nebular and cool flux contributions, will be compared with HeII 1640AA IUE fluxes to find luminosities. This is extremely important when trying to situate symbiotics in an evolutionary scenario. These systems are also a reliable source of abundances for late-type giants and FUV observations will contribute to abundance studies of the Magellanic clouds. The FUSE region also contains many diagnostically important transitions for symbiotics, which are rich in emission and ! absorption lines from many different ionisation levels. This, combined with the FUV being the best region to study the hot components and the lack of observations of extragalactic symbiotics, makes them ideal candidates for a FUSE survey. PROP ID: E957 PROPOSER: Jones PROPOSAL TITLE: UV Spectroscopy of Be Stars in the Magellanic Clouds Be and Be stars rotate rapidly and are associated with gaseous circumstellar matter. Often the circumstellar material has a disk-like distribution, but the physical processes that form and maintain these structures are not well understood. Be and Be stars also share some other common characteristics, and some Be stars occupy a region of the HR diagram similar to the Be stars suggesting a possible connection to the traditional Be stars. We wish to pursue this potential connection by acquiring FUV spectra of a number of Be stars in the Magellanic Clouds. These observations will form the first data set of FUV spectra for the Be stars. To analyze the data, we will employ a new, sophisticated, non-LTE, axisymmetric radiative transfer code to model the spectral lines arising from the extended circumstellar material surrounding such stars. By predicting spectral line profiles and comparing these predictions with observed line profiles, we can decipher the physical parameters of this circumstellar material. Using our FUV data, combined with other existing optical and IR data, we will be better able to constrain our models and greatly improve our understanding of the Be stars. PROP ID: E989 PROPOSER: Froning PROPOSAL TITLE: A Continuing FUSE Survey of Disk-Accreting Cataclysmic Variables Cataclysmic variables (CVs) are a nearby, non-obscured population of systems in which the physics of accretion, particularly disk accretion, can be studied. FUV observations of CVs target the disk, disk winds and the white dwarf (WD); with FUSE, we can address questions concerning the structure of the disk, the driving mechanism of the winds, and the physical interaction between the disk and WD that cannot be addressed through ground-based observations. Over its lifetime, FUSE has been used to observe numerous CVs. These studies of individual objects have produced important results, but a broad examination of the FUV properties of CVs is necessary to distinguish class-dependent characteristics from those particular to the history and structure of individual systems. In Cycle 4, we were awarded FUSE observing time to survey disk-accreting CVs. Of our list of 20 objects, 5 have been observed to date, suggesting that about half of our targets may be observed by the end of Cycle 4, at which point that program will terminate. We propose here to continue the FUV survey by submitting a list of CVs that will round out samples of the various CV sub-classes. Our ongoing analysis --- using the survey targets plus observations from publicly-available individual programs --- employs existing stellar, disk, and wind models to characterize the FUV properties of the white dwarfs, accretion disks, and outflows in CVs as a function of viewing inclination, binary geometry, mass accretion rate, and evolutionary history. Initial results will be presented in Fall 2003 and we anticipate submission of the final results by early 2005.