CYCLE 6 ACCEPTED ABSTRACTS PROP ID: F003 PROPOSER: Aloisi PROPOSAL TITLE: Unravelling the Nature of the Nearby Primordial Galaxy SBS 0335-052 SBS0335-052 (Z simeq 141 Z_) is a dwarf star-forming galaxy that together with IZw18 holds the record of the lowest metallicity ever observed in the local Universe. A wealth of observational evidence supports the hypothesis that this target is in fact a nearbyprimordial galaxy, contrary to what observationally demonstrated, e.g. for IZw18. However, no conclusive results are available at present. A new (and probably only viable) approach in order to establish the real nature of SBS0335-052 young or old galaxy) is represented by FUSE observations. FUSE gives us access to the richness of interstellar absorption lines arising from the neutral interstellar medium (ISM) of this galaxy in the FUV spectral range. We propose to obtain high SN FUSE spectra of SBS0335-052 in order to estimate column densities of the most common ions and derive the metal content of the neutral ISM with unprecedented accuracy (lesssim .15 dex). In these extremely metal-poor systems, the neutral ISM dominates the baryonic mass, and can hide the bulk of the metals produced by the galaxy during a lifetime. The relative abundances of metals which originate in different types of stars are also like a fossil record of the past star-formation (SF) history, the neutral gas tracing a more ancient past than the ionized gas in the HII regions due to larger timescales of the mixing processes that come into play. Inferring the metal content of the neutral ISM in SBS0335-052 will give us access to its ancient gtrsim 1 Gyr) SF history and will allow us to assess or reject its primordial nature, investigate its connection with the high-redshift Universe (e.g., Lyman Break Galaxies, Damped Lyalpha systems), and put strong constraints on theories of galaxy formation and evolution. Independently of the real nature of SBS0335-052, the proposed FUSE spectra will constitute an invaluable complement to the Spitzer data of this galaxy which shows a very peculiar mid-infrared spectrum. PROP ID: F005 PROPOSER: Savage PROPOSAL TITLE: EUV and FUV Absorption by the Highly Ionized IGM - Physical Conditions and Baryonic Content A recent FUSE snapshot observation reveals that HE,0153--4520 z_ QSO 0.451) is the third brightest moderate redshift (z > 0.4) QSO at FUV wavelengths. The line of sight to HE,0153--4520 provides an outstanding opportunity to obtain information on EUV absorption lines formed in the highly ionized IGM. Our proposed 250 ksec integration will build on our recent successful detection of Ne VIII absorption in a multi-phase system at z 0.20701 toward HE,0226--4110 (z_ QSO 0.497). The observations of HE,0153--4520 will allow access to EUV lines of O II, O III, O IV, N IV, and Ne VIII in addition to FUV lines of H I, C II, C III, N II, N III, O I, and O VI. 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. Studies of the physical conditions and ionization of IGM absorption-line systems are an essential step for observational cosmology to make progress in understanding whether the highly ionized IGM is a major reservoir of baryons in the low redshift universe. There are only a few QSOs with z > 0.4 for which a study as detailed as the one proposed here can be conducted. PROP ID: F011 PROPOSER: Heber PROPOSAL TITLE: The mass of the sdB primary of the binary HS2333+3927 SdB binaries are important to clarify the evolutionary origin of sdB stars because the analysis of light and radial velocity curves can constrain their dimensions and masses. However, only four suitable systems are know up to now. Recently we discovered a fifth one, HS2333+3927, consisting of an sdB star and an M dwarf (period 0.172d) with a very strong reflection effect, but no eclipses. Therefore additional information, such as a spectroscopic gravity measurement are required to derive an unambiguous solution. The reflection is stronger than in any of the other systems which renders a quantitative spectral analysis very difficult because the Balmer line profiles are disturbed by the reflected light. Mass-radius relations were derived from the results of the analysis of light and radial-velocity curves. Comparison with the observed mass-radius relation of the sdB star and with that of lower main sequence stars for the companion reveal a severe discrepancy. The spectroscopically estimated gravity (5.7 dex) of the sdB is too low by 0.1 to 0.15 dex to be consistent with the light and radial velocity curve. An improved spectroscopic measurement of the gravity is urgently needed. The Lyman series is ideally suited for this purpose, because it is not affected by light from the cool companion. The rotation of the sdB star is very likely tidally locked to the orbital motion. Determining the projected rotation velocity would therefore allow an independent estimate of the systems inclination. However, v,sin,i could not be derived from optical spectra. UV metal lines are much better suited. These measurements will allow to constrain mass and radius much better. Short period sdB binaries with dwarf companions, such as HS2333+3927, will evolve into cataclysmic variables, when the sdB has left the EHB. Therefore, these objects are crucial to understand pre-CV evolution. HS2333+3927 is the only sdB+dM system with a period larger than the CV period gap. PROP ID: F016 PROPOSER: Hutchings PROPOSAL TITLE: The Interacting Beneutron-star System X0535-668 We propose to observe the luminous LMC X-ray binary X0535-668 which consists of a highly interacting Beneutron-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 OVI 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. PROP ID: F018 PROPOSER: Lehner PROPOSAL TITLE: Discovery of a Lyman Limit System at z 0.20258 -- The IGMGalaxy Connection In contrast with high redshift studies of the IGM, observations of low z absorption systems provide the opportunity to examine the IGMgalaxy connection in great detail. From STIS E140ME230M observations, we have detected 4 metal systems toward the quasar PKS,0312-77 (z 0.223). One of them is a Lyman limit system (LLS; log N(ionH1) > 17.3) at z 0.20258, which shows one of the strongest ionO6 system ever detected and several elements in different ionization stages, implying a multiphase structure of the gas. This LLS is therefore well suited for a study of the atomic abundances and ionization state. It also provides the rare chance to compare the metallicity in the LLS and in the galaxy that we suspect gives rise to the LLS. The ionH1 column density remains, however, largely unknown from the STIS spectrum. We therefore request a FUSE spectrum of PKS,0312-77 with good signal-to-noise (SN,simeq 14) in order to have access to the whole Lyman series ionH1 from Lygamma down to the Lyman limit. The FUSE spectrum will also provide the ionS6, ionC3, and ionO1 lines for the LLS. Combining FUSE and STIS observations will provide the unique opportunity to derive the overall metallicity of the LSS, the fractions and kinematics of ionized gas, and to compare the abundances of the associated galaxy with the LLS. Our proposed observations will also complete ionO6 surveys at low z to ga 20 mAA. PROP ID: F020 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: F025 PROPOSER: Crenshaw PROPOSAL TITLE: Evolution of the Intrinsic Absorption in the Seyfert 1 Galaxy NGC 3783 We have discovered the first case of a decreasing radial velocity in an outflowing AGN absorber, in the Seyfert 1 galaxy NGC 3783, which we have proposed is the result of an absorbing cloud that is changing its direction of motion as it crosses our line of sight to the broad-line region (BLR). This curved motion is exciting because it is predicted by dynamical models of accretion disk winds. Our recent Cycle 5 FUSE observation supports this geometric model; both the radial velocities and equivalent widths of the absorption lines have decreased, suggesting that the absorber is leaving our line of sight to the BLR. Our model predicts that the absorber will disappear between 2005 July and 2006 September as it exits our line of sight. We request two new FUSE observations of NGC 3783 in Cycle 6, which, together with our observation in 2005 January, will allow us to follow the evolution of the UV absorption on a time scale of sim6 months. The new observations will allow us to 1) definitively test our proposed model, 2) determine an accurate transverse velocity of an absorber for the first time, 3) map the curve of motion of the absorber as it exits the line of sight, and 4) test its uniqueness by following the evolution of the other absorption components. PROP ID: F026 PROPOSER: Wakker PROPOSAL TITLE: Detecting baryons outside galaxies via OVI absorption When comparing the inventory of baryons in galaxies with determinations of Omega_b obtained from deuterium and the 3K background radiation, most of the baryons appear to be missing. It appears that they may be hiding in the warmhot intergalactic matter (WHIM), evidence for which may be provided by the detections of redshifted intervening OVI absorption lines. However, many (maybe all) of these OVI absorbers might be associated with extended halos of galaxies andor with galaxy groups. For FUSE cycle 4 we studied several intergalactic OVI absorptions at v<3500kms, only one of which turned out to be not associated with a galaxy. We are now looking at the relation between intergalactic OVI absorption with v<3500kms z<0.012) and nearby galaxies and groups. We find that for impact parameters <350kpc there is strong evidence for associated OVI. We propose to observe four targets in order to a) analyze the physical conditions in the strongest associated OVI absorber, occurring in a pair with an impact parameter of 1kpc, and b) confirm 4 of the 8 tentative detections. This would yield a sample of >25 galaxy-AGN pairs with impact parameter <700kpc and SN>15 spectra, with an almost flat distribution of impact parameters. PROP ID: F027 PROPOSER: Richter PROPOSAL TITLE: Metal abundances in HVC complex A We request an exposure of two extragalactic targets, Mrk,106 and UGC,4305, in order to measure accurate metal abundances in the high-velocity cloud (HVC) complex A. Preliminary results indicate that this object has sub-solar metallicity (<0.3 times solar), making it one of only two clear known examples of infalling intergalactic gas (HVC complex C being the other). At present there are many determinations of ionic abundances for sightlines through complex C summarized by Fox et al. 2004), but unlike what is the case for complexC, we know the distance to complex A (8--10 kpc). Therefore, complex A is the only object for which we can reliably estimate its contribution to the mass flow rate of metal-deficient gas impinging on the Milky Way. As both the infall rate of low-metallicity gas as well as the initial metallicity of this infalling gas are crucial parameters for models of the chemical evolution of the Galaxy, a proper determination of the metal abundances in complex A would represent an substantial advance in understanding such models. The two lines of sight we selected represent the best chance to determine the chemical composition of complex A, through measurements of absorption lines of OI, NI, FeII, and SiII. PROP ID: F028 PROPOSER: Hempel PROPOSAL TITLE: Boundary layers of A stars with disks beta,Pic is the most prominent prototype of stars with circumstellar disks and has generated particular interest in the framework of young planetary systems. Concerning its spectral type A5, stellar activity is unexpected. Nevertheless, resonance lines of C,sc iii and O,sc vi which are typical for a transition region have been unambiguously detected with FUSE. We have developed an accretion disc - boundary layer scenario for beta,Pic which can both explain the presence of C,sc iii and O,sc vi and the absence of X-ray emission in XMM-Newton spectra analysed by us. We propose to observe other A stars possessing conspicuous similarities to beta,Pic concerning IR excess and the presence of circumstellar material in order to investigate whether our boundary layer model is applicable to other young A stars as well. PROP ID: F034 PROPOSER: Massa PROPOSAL TITLE: Wind Variability in the Central Star of the Cats Eye Nebula Required) We propose to carry out the first high spectral resolution study of wind structure in the fast winds of CSPN which can sample the winds on the key characteristic time-scales. We use available fuse spectra to demonstrate that the wind of HD164963, the central star of NGC6543, is variable on a time scale of sim 4hours. We argue that this variability is probably rooted in the photosphere of the star, is indicative of the behavior of the bulk of the wind material and may play a significant role in shaping the nebula. We are requesting 57.6ks of fuse time to observe approximately 4cycles of this activity, in order to fully characterize its temporal behavior and to assess its physical origin. PROP ID: F037 PROPOSER: Massa PROPOSAL TITLE: The Relationship between Gas and Dust in Cep OB3 We intend to utilize the unique characteristics of the cepob association and its molecular cloud to examine the dependence of dust properties upon the physical conditions of the gas in which they reside. New and existing fuse observations will be used to examine the remarkable dependence of UV extinction curve morphology and proximity to the molecular could. The fuse data will enable us to quantify this behavior in terms of hydrogen molecular fraction, gas kinetic temperature and the local UV radiation field. PROP ID: F042 PROPOSER: Long PROPOSAL TITLE: Phase-resolved Spectroscopy of the Intermediate Polars -- TV Col and V1223 Sgr The cataclysmic variables called intermediate polars are characterized by magnetic fields that rip material from an accretion disk and funnel it to a WD that is not phase-locked to the binary period of the system. This is a proposal to use FUSE to conduct a time-resolved spectroscopic study to dissect the emission of two long-period intermediate polars, V1223 Sgr and TV Col, with very different inclination angles. These, along with the short-period high-inclination IP EX Hya (already observed with FUSE), comprise the only IPs with accurate distances derived from HST astrometry. We will isolate emission from the photosphere of the WD, the magnetically dominated accretion curtain, and the accretion stream. Having characterized the emission sources, we will explore the physical conditions in these same regions, and develop an integrated picture of these two intermediate polars. PROP ID: F043 PROPOSER: Long PROPOSAL TITLE: Why do some Dwarf Novae Stand Still Z Cam systems are disk-dominated cataclysmic variables. Unlike normal dwarf novae, which burst and then return to quiescence in a few days to a few weeks, Z Cam systems exhibit extended high states lasting several weeks to several months following some otherwise normal outbursts. In standstill, the disk is in a high mass transfer state, but the flux at visible and UV wavelengths is intermediate between outburst maximum and quiescence. We propose to explore the physics of the standstill phenomenon with FUSE observations of Z Cam, the prototype of this class. We will attempt a fundamental test of the hypothesis that the mass transfer rate from the secondary is higher in the fainter standstill state than in outburst by obtaining FUSE spectra at all orbital phases in standstill and in outburst. Access to the wavelength range below 1200 AA with a high resolution spectroscopic instrument is crucial to the success of such a test. In addition, we will model the FUSE spectra to measure (at least differentially) the structure of the disk and the wind in outburst and standstill, determining the effects of disk luminosity on wind mass-loss rate. PROP ID: F048 PROPOSER: Szkody PROPOSAL TITLE: Unveiling the White Dwarfs in High Accretion Novalikes with TOO During Low States The detection and study of the white dwarfs in close interacting binaries can determine their temperature, rotation and composition, yielding important clues to past evolutionary history and the effects of long term accretion. The novalike systems with the highest mass transfer rates are the most elusive, since their white dwarfs are normally obscured and dominated by their accretion disks. Yet, these systems in the 3-4 hr period regime can provide the best test of evolution models and a link to recent nova events and past or on-going H-burning via CNO reactions. Fortunately, some novalikes sporadically enter low states of vastly diminished accretion. Our past FUSE observation of MV Lyr during a low state demonstrated the capability of FUSE by revealing a 47,000K white dwarf with a rotation vsini of less than 200 kms (with i of 7 deg). We propose Cycle 6 TOO observations from a list of 18 systems known to undergo low states with an expectation to catch 2 systems during low states. These data will provide temperatures for the white dwarfs with the highest accretion rates, a stringent test of rotational spinup due to high accretion, and a test of recent evolution models suggesting that these are all recent unrecorded ex-novae. PROP ID: F049 PROPOSER: Koenigsberger PROPOSAL TITLE: Time-dependent wind-wind collisions of the extragalactic binary HD 5980 HD 5980 is the most luminous binary system in the SMC. The two components of this eclipsing binary are very massive and highly evolved stars whose winds strongly interact. The primary (star A, Msim50 M_) appears to be a Luminous Blue Variable (LBV) while the secondary (star B, Msim28 M_) is a Wolf-Rayet star of the WNE subtype. Star As wind has varied systematically over the past 20 years, reaching a maximum mass-loss rate sim10^-3 M_ yr^-1 in 1994, when the system underwent a Deltam_vsim3 mag brightness increase in what is believed to have been an LBV-like eruptive event of star A. In recent years, the collision between the winds from the two stars has been dominated by the wind of star A, but its declining emission-line strength since 1999 suggests that the geometry of the shock cone, which until recently folded around star B, is in the process of inverting its orientation. This phenomenon has never before been observed. We are requesting a time series of observations of HD 5980 at specific orbital phases during a single orbital cycle in order to a) establish the present geometry of the WWC region; b) obtain constraints on the wind structure of star A and star B through the modeling of wind eclipses; and c) obtain information on the line-emitting characteristics of the WWC region. The broad range of ionization potentials of resonance lines present in the FUSE bandpass as well as the fact that some of these lines are not saturated provide unparalleled diagnostic capabilities for addressing these problems. PROP ID: F055 PROPOSER: Tumlinson PROPOSAL TITLE: Molecules in an Extragalactic Halo Cloud - 3C232 Probes the Starburst Galaxy NGC3067 We propose to obtain a new FUSE observation of the QSO 3C232. This sightline shows a strong N(HI) 10^20 cm^-2 Lyman limit system (LLS) at cz 1420 pm 5 kms arising in the halo of the starburst galaxy NGC3067, 1.8 and 11 kpc above the galaxys plane. This is the best-studied sightline through a galaxy halo other than the Milky Way), including UVoptical spectroscopy of Lyalpha and metal lines (from NaI and MgI to CIV and SiIV) with HST and HI 21 cm emission and absorption with Arecibo, VLA, and VLBA. The existing UVopticalradio data supports the view that this absorber is a low-metallicity (Z simeq 0.25 Z_) HVC-type cloud falling into ngc and illuminated by the extragalactic ionizing spectrum. The existing short FUSE observation P1071402, 11 ksec, SN lesssim 2) shows strong h2 associated with the LLS. Thus this system presents a unique opportunity to test models of h2 in an environment with low metallicity and low radiation, such as might prevail in damped Lyalpha systems (DLAs) at high z. Our new observations will (1) probe h2 formation at low metallicity by breaking the degeneracy in radiation field and metallicity that exists in the Galaxy and the Magellanic Clouds, (2) provide a low-z template for tests of FUV radiation and SFR in high-z DLAs, and (3) provide a critical check on existing models of the cloud, which appears to be analogous to the Galactic HVCs. Optical telescopes (Keck, VLT) are building up samples of high-z DLAs with h2, FUSE is the only way we can study h2 in nearby, resolved DLA prototypes, and 3C232 is the best such test case. This single absorber holds the clues to important problems in both intergalactic and interstellar medium science. If we are to properly interpret the high-redshift QSOALS and DLAs in terms of low-redshift templates, such valuable low-redshift links must be pursued. PROP ID: F060 PROPOSER: Fontaine PROPOSAL TITLE: A Test of Pulsation Theory in Hot B Subdwarfs (bis) There are currently 33 hot B subdwarf (sdB) stars which are known to exhibit low-amplitude (a few to tens of mmag), short-period (100-500 s), multiperiodic luminosity variations caused by acoustic mode instabilities. These pulsations are thought to be driven by an opacity bump linked to the presence of a local enhancement of the iron and other iron-peak elements) abundance in the envelopes of sdB stars. Such an enhancement results quite naturally from the diffusive equilibrium between gravitational settling and radiative support in the stellar envelope. Nevertheless, surveys for pulsating sdB stars show that variable and nonvariable objects with similar effective temperatures and gravities coexist in the log g-Teff diagram. This puzzling result suggests that an additional parameter, perhaps a weak stellar wind, might affect the extent of the iron reservoir and thus the ability of the latter to drive pulsations in sdB stars. Fortunately, it is expected that such a wind might also leave its mark on the photospheric heavy element abundance patterns. The intended FUSE observations will 1) permit a direct comparison of the heavy element abundance patterns in variable and nonvariable stars of similar atmospheric parameters, 2) provide a consistency check with our wind models, and 3) provide a test of the currently-favored explanation for the driving of the observed pulsations. PROP ID: F074 PROPOSER: Sankrit PROPOSAL TITLE: A Far-Ultraviolet Study of Non-radiative Shocks in N49 We propose to observe two locations in N49, one of the brightest supernova remnants in the Large Magellanic Cloud. The first region encompasses a supernova ejecta knot that has overtaken the blast wave. The properties of such knots, and their relationship with the parent supernova remnant are as yet poorly understood. The FUSE spectrum of the eject knot in N49 will reveal its kinematic properties and allow us to estimate the dynamic pressure of the shock. We will search for neon, sulphur and silicon lines in the FUSE spectra of this chemically enriched region and constrain the abundances of these elements with respect to oxygen. The second location is on an intermediate velocity (sim700kms^: -1 ) non-radiative shock. From our proposed observation, we will be able to obtain the oxygen kinetic temperature from the OVI emission line profile. Combined with X-ray data, this will allow us to estimate the electron-ion equilibration in the shock. These regions have been selected on the basis of their X-ray emission seen in textitChandra images; they have little or no optical emission. In addition to addressing important questions about different kinds of shocks found in supernova remnants, our proposed observations will supplement the existing FUSE observations of bright optical regions of N49. The old and new spectra will yield the first complete picture, at high spectral resolution, of the OVI emission from a supernova remnant. PROP ID: F079 PROPOSER: Mathur PROPOSAL TITLE: Understanding the warm-hot intergalactic medium with FUSE and Chandra observations. We propose to extend our highly successful chandra program for study of the warm-hot intergalactic medium (WHIM) to the FUV band, by obtaining observations of two blazars with FUSE. The diagnostic power of combined FUV and X-ray measurements is invaluable for WHIM science, greatly amplifying the scientific return from either wavelength region on its own-- (1) the oviinovi ratio is a sensitive function of the temperature; (2) the oviiinovi ratio provides the diagnostics for the overdensity of the WHIM, and (3) the ovinovi+ovii+oviii ratio allows determination of the ionization state of oxygen, crucial for estimating the baryon content traced by oxygen absorption systems. With the proposed observations we will (1) determine the physical conditions in the Local Group IGM along new lines of sight; (2) detect and study the WHIM at z>0; (3) improve estimates of the baryon content of the WHIM, and (4) compare the observations with predictions from the hydrodynamical simulations and so constrain theoretical models. PROP ID: F085 PROPOSER: Murphy PROPOSAL TITLE: The Galactic Fountain in NGC 4631 We propose to use fuse to determine the extent and kinematics of ovi emission from hot, cooling galactic fountain gas in the halo of the edge-on spiral galaxy NGC4631. In previous fuse Cycles 1 and 3 programs we have detected ovi emission in the halo of NGC4631 at 5 positions. Three of the positions (See Figure 3, NGC4631-A, -B, and I) are coincident with an Halpha emission feature that previously has been interpreted as a chimney of hot gas venting from the plane of the galaxy. The two remaining positions (NGC4631-F and -H) are in the low halo of the galaxy above the disk. The OVI emission appears to be associated with the hot X-ray halo of NGC4631 and suggests that the gas is cooling galactic fountain gas. NGC4631 is the first, and only, galaxy in which a true galactic wide fountain has been detected. We request 5 additional measurements in the high halo of the galaxy to determine the full extent of the ovi emission and to estimate the cooling rate of the halo. With the data from these additional pointings, our fuse observations will cover nearly the full X-ray halo observed with the Chandra X-ray Observatory (Wang 001). A comparison between this observed cooling rate for the halo gas with the mechanical input energy from supernovae will test the effectiveness of ovi emission as a cooling mechanism for fountain gas. These data may also be used to determine the scale height of the ovi gas at various locations in the disk. Subsequently, we will be able to compare the distribution and kinematics of this transition temperature gas with hotter gas Tsim1-3times10^ 6 K) as revealed by ROSAT and Chandra. PROP ID: F088 PROPOSER: Walborn PROPOSAL TITLE: Stellar-Wind Variations in the Ofp Spectrum Alternator HD191612 The Ofp star HD191612 was found in 2001 to display two peculiar, recurrent spectral states at optical wavelengths. In one the spectral type is near O6 and there are strong wind diagnostics, including a PCygni profile at Halpha; while in the other it is O8 with Halpha predominantly in absorption. Other peculiar spectral features alternate correlatively. This year, with the aid of Hipparcos photometry, the spectral variations have been found to be periodic and predictable. The optical behavior suggests that the UV wind features should vary drastically. We propose to investigate with FUSE, the only currently available UV spectrograph. There are favorable windows near three critical phases during 2005, including both extrema and a transition. Although by no means proven, the most promising current model for this bizarre behavior is tidally induced pulsations driving enhanced mass loss near periastron in an eccentric binary. The UV diagnostics should provide a valuable contribution toward a definitive model. PROP ID: F089 PROPOSER: Walborn PROPOSAL TITLE: FUV Spectral Diagnostics of a Nitrogen-Rich O2 Giant in the LMC The new classification O2 was recently introduced to describe the earliest-type optical spectra. Subsequent work on giants of that type in the Magellanic Clouds has revealed a range of relative CNO and HeH line strengths, and three of them have been reclassified as ON2III. Available HST data show corresponding anomalies in the stellar winds. Modeling of these spectra shows that the phenomena correspond to abundance differences most likely caused by mixing of CNO-cycled material to the surfaces of evolving, very massive stars. We shall investigate the spectrum of one of the LMC nitrogen-rich objects, which is also helium-rich, at FUSE wavelengths, to search for and model additional relevant wind and photospheric diagnostics in the rich FUV spectral range. Two normal LMC O2 giants and an ON2 in the SMC have already been observed with FUSE and will serve as comparison objects; optical and HST data are also available for all four stars to support unified (windatmosphere) analysis. Another LMC ON2 has higher reddening, so that our target is the best case for FUSE investigation. These very hot N-rich objects may be evolving homogeneously and in any event will provide vital information about the evolution of the most massive stars, likely including the mixing effects of rotation according to current models. PROP ID: F107 PROPOSER: Steeghs PROPOSAL TITLE: The accretion flow in the ultra-compact binary ES Cet Recently, three variable stars have been identified as likely accreting binary systems with ultra-short orbital periods. Optical and X-ray observations have revealed periodicities of 5-10 minutes, making them the closest binaries known as well as strong sources of gravitational wave emission. Such short-period accreting binaries form the cornerstone to our understanding of binary formation and evolution, in particular of the large double white dwarf population in our galaxy, a candidate progenitor population for Type Ia supernovae. We propose to obtain the first phase-resolved UV observations of the brightest of these three, ES Cet. With the FUSE observations, we will (i) determine the temperature of the primary and the composition of their donor stars, (ii) correlate the UV variability with other wavebands and determine if the periods are indeed orbital, (iii) look for dynamical signatures of direct-impact accretion that is expected to govern the survival rate of double white dwarfs. These UV observations are essential in order to unequivocally determine whether these are indeed the most compact binaries known. PROP ID: F111 PROPOSER: Herczeg PROPOSAL TITLE: The Effect of FUV Emission on Remnant Gas in Optically Thin Disks The residual gas content in intermediate-aged optically thin disks (3--100 Myr) is important to the formation and early evolution of terrestrial and giant planet formation, but it is currently poorly constrained. FUV radiation is expected to significantly impact the photochemistry of the disk by photodissociating H_2 and CO and ionizing S, and will determine our ability to detect the gaseous component of the disk. Spitzer offers several emission lines to probe the gas at planet-forming radii of the disks. However, inferring a gas mass from these lines requires accurate measurements of the FUV field, which we can use to model the abundance structure and excitation of the gas. Therefore, we propose to use FUSE to measure the emission from 912--1185 AA for a sample of intermediate-aged solar analogues that have optically thin disks and span the range of timescales when residual gas may still be present. We will use this data, combined with disk models, to measure the gas content in disks from Spitzer spectra, ultimately leading to estimates of the evolution of gas mass with time in the planet forming regions of disks. PROP ID: F132 PROPOSER: Gull PROPOSAL TITLE: Exploring the FUV Nebula Around Eta Carinae FUSE observations of the star,ecar, and its surrounding stellar ejecta present a unique opportunity to study the FUV properties of recently ejected material from a very massive stellar system and to identify the hot secondary companion. We propose to 1) use the MDRS to obtainecars polar stellar spectrum scattered from the SE lobe, which should provide spectral signature of the mysterious companion star, 2) use the HIRS and MDRS to disentangle the stellar spectrum from the dust-scattered, nebular emission, and 3) obtain the nebular spectrum of the S-condensation, where recent, fast moving ejecta are colliding with previously-ejected, nitrogen-enriched material. This proposal builds on multiple observing programs using FUSE, HSTSTIS, RXTE, CHANDRA, VLTUVES and other ground-based instruments that have followedecar over the recent 5.54-year cycle. These proposed observations, along with improved modeling of this very complex system, will provide new insight on ! the nature of massive (binary) stars in their last stages of stellar evolution and on how they interact with, and enrich, the ISM. Since very massive, Population III stars are thought to be the source of heavy elements and dust in the early Universe, we need a complete description of how stars of extreme mass, such asecar, deposit nucleosynthesis products into the ISM, and how they form dust. PROP ID: F139 PROPOSER: Blair PROPOSAL TITLE: FUV Kinematics of the Galactic SNR G65.3+5.7 We will observe twelve positions across the face of the large (sim70 pc), old (sim26,000 years) galactic supernova remnant G65.3+5.7 to study the global OVI and CIII kinematics. This object is the newest and nearest member of the thermal composite sub-class of supernova remnants, and the only one accessible for observation in the FUV. An archival Voyager UVS data set for this remnant shows CIII and OVI lines at levels readily detectable with the excellent diffuse source sensitivity of FUSE, but the Voyager spatial and spectral resolutions are far too low to provide the kinematical information we request here. Since the optical and X-ray emissions from the remnant are relatively faint, this supernova remnant appears to be dominated by FUV emission, making FUSE the ideal instrument to understand the global kinematic properties. The FUSE positions will sample a combination of edge-on filaments and face-on regions covering several major lobes seen in deep optical OIII images, thus providing and overview of the global structures. These observations will make G65.3+5.7 only the fourth galactic remnant detected with FUSE, and will provide a very different case study from the better studied objects (the Cygnus Loop and Vela supernova remnants). PROP ID: F141 PROPOSER: Hoopes PROPOSAL TITLE: Probing the Galactic Fountain in NGC891 We propose to obtain sensitive FUSE observations of ionO6 emission from the halo of the edge-on spiral galaxy NGC891. Emission from ionO6 traces the Tsim3times10^5K coronal gas which is an integral part of the disk-halo cycle in spiral galaxies. The O 6 1032AA emission line has been detected in FUSE spectra of the edge-on galaxy NGC4631, but not in the starburst galaxy M82 or in less-sensitive FUSE spectra of NGC891. Deeper spectra will answer the question of whether the NGC4631 halo is unique, or whether coronal gas is common in spiral galaxy halos. With these data we will ) measure the mass circulation rate in the NGC891 halo, 2) compare the ionO6 cooling rate with that in the X-rays, and 3) begin to measure the distribution of coronal gas. Comparison of NGC891 with the previous NGC4631 detection will allow us to probe how these halo properties depend on star formation rate and galaxy mass, important steps toward quantifying models of the disk-halo interaction. This project will take advantage of the unique capabilities of FUSE to answer important questions about the disk-halo cycle in spiral galaxies. PROP ID: F142 PROPOSER: Neff PROPOSAL TITLE: Emission Line Filaments in CenA - How Are They Ionized Jets are markers of AGN, which live quietly in most galaxies today but were much more commonly active at earlier epochs. Large-scale star formation, aligned with the jet, also occurred much more frequently at high redshifts, and probably played a major role in shaping the galaxies we see today. Centaurus A is the nearest active galaxy, and is close enough to permit detailed study of an AGN jet interacting with its host galaxy. Recent GALEX observations have detected Mid-UV (MUV, 200-1800AA) emission associated with the radio jet at distances up to 20 kpc from nucleus, particularly associated with the (optical) emission line filaments. Recent Chandra observations detect soft X-ray emission associated with one of the filaments. Taken together, these strongly suggest significant amounts of shock heating in at least one filament. However, the X-ray and optical data are not consistent with pure shock heating, and the X-ray detected filament is not directly impacted by the radio jet. Optical spectra are also not consistent with pure photoionization, e.g. beamed radiation from an obscured (to us) AGN. A FUSE detection, and measurement, of the O,VI flux associated with the optical, MUV, and X-ray observations, will allow us to determine the importance of shocks in ionizing this filament. Comparisons of FUSE observations with models will allow us to constrain the properties of whatever shocks are present. This in turn will improve greatly our understanding of how jets transfer mass and energy from AGN back into their host galaxies. PROP ID: F144 PROPOSER: Ake PROPOSAL TITLE: Outer Wind Mapping of the Zeta Aurigae System 22Vulpeculae Required) 2 Vul (G3 Ib + B9 V; period249^d) has become a pivotal laboratory for studying solar-type supergiants and the zetaAur phenomenon in general. The primary star lies near the dividing line in the HR diagram that separates stars with hot, solar-like coronae from those with extended atmospheres and cool winds, and its binary nature allows the spatial mapping of the chromosphere and envelope at the critical onset of winds in these stars. We obtained excellent phase coverage of the May--June 2004 eclipse. It is clear from the variation of high excitation lines such as O VI that observations at other phases are needed to disentangle the relative contributions from various components of this system. For Cycle 6 we are proposing five observations of 22 Vul at critical positions in the orbit, particularly to sample the outer wind beyond the interorbit region. Besides the wind absorption lines, of particular importance are O VI and CIII lambda977 at these phases, which are needed to assess shock front emission and wind accretion and which, unlike Si IV and C IV in the IUE and HST region, are always seen above the local photospheric level of the B9 star in the FUSE range. PROP ID: F148 PROPOSER: Keyes PROPOSAL TITLE: Cycle 6 Multi-wavelength Observations of Symbiotic Stars in Outburst Required) To investigate the cause and nature of classical symbiotic outbursts, we initiated a program of multi-wavelength observations of these events. The first target for our campaign -- the 2000-2002 outburst of Z Andromedae -- confirmed the utility and need for coordinated multi-wavelength observations to make progress in understanding the nature of the outburst mechanisms in symbiotic stars. The FUSE data were the cornerstone of this project (which included data from the VLA, MERLIN, ground-based optical spectroscopy and photometry, Chandra, and XMM). Our Z And observations have motivated us to propose a new scenario which we term the disk-instability trigger. To test this new model, we received FUSE cycle 5 time to continue the multi-wavelength campaign with FUSE observations at 6-8 epochs during the outburst of a second target-of-opportunity (TOO). As our cycle 5 program has not yet been triggered, we propose here to continue this TOO observing opportunity into cycle 6. Coordinated XMM, and VLA observations for a second target have already been approved. The evolution of the UV spectrum throughout the outburst plays a vital role in distinguishing between the outburst models currently in contention for describing outburst behavior. Emission line strengths of the FUSE-band species, especially when combined with lines of the same species from the other spectral regions, provide diagnostics of the colliding windshock region. Note especially that FUSE provides important information for the analysis of the x-ray data as FUSE observations of HI absorption are at sufficiently high resolution to allow the separation of the interstellar component from the systemic component of the absorption. PROP ID: F149 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 (V < 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. New core-collapse supernovae, primarily SN type II, have strong, nearly featureless UV continua that provide outstanding opportunities to obtain high-quality absorption line spectra of the gas on the line of sight to the SN, but only if the observations are executed within sim1 week of outburst. Our team has the experience and extensive ground-based support to promptly assess the suitability of each newly-discovered supernova for this program and to quickly provide all the necessary parameters to rapidly execute the observations. PROP ID: F150 PROPOSER: Charpinet PROPOSAL TITLE: Testing Nonradial Oscillation Theory and Mode Identification in hot B Subdwarfs We propose to monitor the rapid pulsations of the hot subdwarf B (sdB) star PG 1219+534 in the Far UV using the Time Tag (TTAG) mode of FUSE. The apparent amplitude of a nonradial oscillation mode depends on both the geometry of the mode (through the degree ell) and the wavelength at which it is observed. For hot sdB stars, calculations clearly indicate that the relative mode amplitudes as seen in the optical and in the Far UV strongly discriminates between values of the degree ell, allowing these to be easily determined. Such constraints on the mode identification are otherwise very difficult to obtain from optical multicolor photometry alone, as the discrimination between different ell values is weak when confined in this bandpass. The comparison of the FUV amplitudes of the modes detected by FUSE with their optical counterparts (from existing CFHT data and from planned contemporary observations at the Mt Bigelow 61 Telescope) will lead to an independent determination of the degree ell of the pulsation modes of PG 1219+534. Our goal is to provide, for the first time, a direct test of the predicted mode identification derived from a recent asteroseismic analysis of this star based on optical white light photometry only. PROP ID: F158 PROPOSER: Araujo-Betancor PROPOSAL TITLE: Fuse Observations of Post Common Envelope Binaries Probing Stellar Evolution in Close Binaries Post common envelope binaries (PCEBs) represent a common evolutionary track in the early lives of the most exotic objects in the Galaxy. All close binaries evolve from the common envelope phase (CE) to shorter orbital periods due to orbital angular momentum loss. Despite its enormous importance for our understanding of close binary evolution, our current knowledge of the agent(s) responsible for extracting angular momentum from the system is very limited. One of the main reason for this discomforting situation is the scarcity of accurate systems parameters, which are necessary to calibrate and test theories of the CE phase and the subsequent loss of orbital angular momentum. The absence of mass transfer in PCEBs allows the determination of their binary parameters at a level unachievable in interacting close binary systems. Among the PCEBs, the detached white dwarfmain sequence binaries (WDMSs) offer the best environment in which to test any theory of close binary evolution, as they are numerous, bright, and their stellar components well-understood. Here, we propose to observe with FUSE seven WDMSs (HS1857+5144, KDP2154+4048, DE,CVn, RXJ,0144+3233, GD,543, PG1114+187, HS1316+6747) and in order to accurately measure the effective temperatures, masses, photospheric abundances, and rotation rates of their white dwarf primaries. These seven systems, together with three additional WDMSs from our previous FUSE programs, provide a sufficiently large sample for a detailed assessment of the evolutionary state of these stars. PROP ID: F160 PROPOSER: Kruk PROPOSAL TITLE: D, O, and other abundances beyond the Local Bubble The DH and DO abundance ratios have been found to be uniform within the Local Bubble, for lines of sight typically shorter than 100 parsecs. At distances of 100 pc to 1000pc measurements of DH show considerable scatter, and at greater distances the values are well below that of the Local Bubble. FUSE measurements of DO exhibit a trend of decreasing values with increasing distance beyond 100 pc. A consistent framework encompassing the behavior of DH and DO has proven elusive. Measurements of DH, DO, and other elemental abundances in different environments are essential for improving our understanding of chemical evolution within the Galaxy. It has been suggested that some of the seemingly contradictory abundance patterns may be the result of differential depletion of D and H onto dust grains. Unfortunately, relatively few lines of sight beyond the Local Bubble have a velocity structure that is simple enough for reliable measurements to be made, so the present sampling of different Galactic environments is insufficient to disentagle the possible contributing processes. Existing FUSE spectra for the three stars in this program (distances ranging from 400 to 1000 pc) reveal isolated DI lines. Preliminary analyses indicate that log N(DI) > 15, hence N(HI) should be high enough to be determined from the Ly,beta damping profile. This proposal requests additional observing time to obtain signal-to-noise ratios adequate for measuring column densities of HI, DI, OI, NI, and FeII. N(HI) will also be determined from archival IUE, GHRS, or STIS data for of the 3 stars, and compared to that derived from the FUSE Lyman beta profiles. PROP ID: F166 PROPOSER: Espey PROPOSAL TITLE: FUV Observations of an Eclipsing Symbiotic Nova PU-Vul is the only known eclipsing symbiotic nova. These objects are a rare subclass of symbiotic binary that undergo a single nova-like outburst lasting decades. The basic mechanism involved is the same as in classical novae, although occurring over much longer timescales, which permits a detailed monitoring of the outburst. FUSE observations present a prime opportunity to examine the processed material ejected from the outburst star, where we can take advantage of the finite size of the hot component to probe different layers of the circumstellar material in absorption. It is possible to identify FeII absorption features in some IUE spectra and our models show that we can successfully study absorption from excited levels of low-ionisation species throughout the FUSE bandpass. We have experience modelling circumstellar absorption in FUSE data for a number of symbiotics and our experience and techniques can be applied to this system. The absorption from the ejected material will be compared to absorption due to the giant wind by taking a observation when the dwarf is eclipsed by the outer regions of the cool wind. The high-excitation transitions available will also allow a diagnosis of the nebular and hot wind conditions. PROP ID: F169 PROPOSER: McCandliss PROPOSAL TITLE: Lyman Continuum Search It has been asserted that the contribution of stars to the metagalactic background radiation, which ionizes most of the baryons in the universe, remains almost completely unknown at all epochs. Here we propose to discover Lyman continuum photons escaping from nearby galaxies. Direct detection of Lyman continuum photons escaping from galaxies at low redshift can provide critical constraint to models of reionization at high redshift, where the first star forming galaxies are thought dominate the process. We have developed a pool of 6 candidate objects with the criteria that the redshift is z > 0.025, the logF_1516 ge -14.1 and the objects are extended in the Sloan survey. We show that with these six objects we will be able to either limit or detect the escape fraction of lyman continuum photons from star forming galaxies at the 5 threshold. This program will significantly reduce the uncertainty in Lyman continuum escape fraction at low redshift. PROP ID: F173 PROPOSER: Guinan PROPOSAL TITLE: FUSE Observations of the Sun in Time FUV Studies of Solar Analogs and Twins We propose to complete an in-depth study of the evolution of the transition region (TR) and low corona of a solar-mass star throughout its main-sequence lifetime. These FUSE observations are part of a comprehensive study of the Sun in Time across the electromagnetic spectrum. We have defined a homogeneous sample of single G0-5V stars with well-known rotation periods that are proxies of the Sun at different ages. We are studying the dynamics and energetics of the lower layers of the atmospheres of these solar-like stars, and investigating the variations of the properties with age and rotation period. Emission measure and temperature analysis will allow us to obtain a complete 3-D atmospheric model of active regions that we will link to previously obtained coronal X-ray data. TR electron densities are inferred through the well-established density-sensitive ratio of the Csc iii 1176AA977AA lines. This important diagnostic will be used to identify and model the relevant magnetic structures based on the solar analogy and, together with our coronal X-ray (ROSAT, ASCA, XMM, Chandra), EUV (EUVE), and TR (IUEHST) data, to infer the importance of coronal energy releases. Our FUSE investigation is central to the understanding of the evolution of magneto-dynamic atmospheric phenomena, and the associated high-energy emissions in the Sun and in solar-type stars. It also bears on the crucial question of the influence of the young Suns strong FUV emissions on the developing planetary system - in particular, the photochemical and photoionization evolution (and possibly erosion) of early planetary atmospheresionospheres. To this end, we are constructing spectral irradiance tables for the Sun at different ages for which the proposed FUSE observations fill a vital spectral and energy gap. With the newly expanded FUSE visibilities, our previously approved (Cycle 3) stars 18 Sco - the solar twin, the ultra-fast rotator ER Vul, and 59 Vir) can PROP ID: F320 PROPOSER: Brown PROPOSAL TITLE: The 12 Myr Old Beta Pic Moving Group We propose a comprehensive FUSE survey of stellar activity levels, as seen in the O VI and C III transition region emission lines, for all known members of the beta Pic Moving Group, which is a 12 million year old subgrouping within the Local Association. This will significantly expand the sample of young active, zero-age-main-sequence (ZAMS), A-M dwarfs with measured transition region emission line fluxes. Thus, allowing detailed studies of the influence of stellar activity on the immediate circumstellar environment of very young stars during a crucial phase of protoplanetary system formation, when formation of gas giant planets is thought to be well underway and formation of terrestrial planets just starting. The sample chosen for this study have identical ages and formed together during the same small star formation episode. By studying a sample of low and intermediate mass stars with identical ages and formation history, a clearer determination of the factors controlling stellar magnetic activity can be obtained, thus enabling better characterization of the evolution in stellar activity during the crucial early phases of stellar, circumstellar disk, and protoplanetary system evolution. PROP ID: F321 PROPOSER: Iping PROPOSAL TITLE: Massive O + O Binaries in the Magellanic Clouds We propose FUSE observations for a complete binary orbit of three early-type, double-lined spectroscopic binaries in Magellanic Clouds. The spectra obtained will enable quantitative and systematic studies of phase-dependent stellar wind properties, wind collision effects in O+O binaries at lower metallicities, improved radial velocity curves, and FUV spectrophotometric changes as a function of orbital phase. These data will lead to improved mass and radius estimates for some of the most massive stars known. Most massive stars, if not all, are or were members of binary or multiple systems. The proposed systems have very short periods (1.4 - 2.25 days), represent rare, young evolutionary stages of massive stars and binaries, and provide a unique glimpse at some of the most massive systems that form in dense clusters of massive stars. These Magellanic Cloud systems have little reddening and foreground gas, unlike the few known comparable Galactic counterparts. PROP ID: F323 PROPOSER: Walter PROPOSAL TITLE: Phase Variations in the O VI Emission in CF Tuc Observations of the temporal variability of stellar activity provide important insights into the spatial distribution of stellar active regions, and of the configuration of the stellar magnetic field. We propose to observe the bright partially eclipsing RSCVn system CFTuc for two complete and uninterrupted stellar orbits while it is in the CVZ. Uninterrupted observations are crucial for studying the short term flaring and flux variations of the stellar atmosphere, and to separate secular trends from true periodic phenomena. We will use the radial velocities of the OVI lines to separate the emission of the two stars. Spectral imaging techniques will constrain the location of the emission, and will permit us to determine whether or not the emission comes from close to the stellar surface or from within an extended magnetosphere. The partial eclipses may further constrain the spatial location of the emitting regions. This is the brightest active RSCVn binary within the FUSE CVZ, and as such can serve as a template for interpretation of perhaps better-known systems in less favorable parts of the sky. PROP ID: F325 PROPOSER: Arav PROPOSAL TITLE: AGN Outflows Putting Real Numbers Into Quasar Feedback Scenarios AGN outflows impact the evolution of supermassive black holes, host galaxies, surrounding IGM, and cluster cooling flows. However, while the theoretical interest in these outflows increased dramatically, we have only weak constraints on the most important properties of real AGN winds kinetic luminosity, chemical abundances and physical conditions. The best approach to advance our understanding of these issues is to execute simultaneous X-ray and FUSE observations of the brightest AGN outflows, which are found in local Seyfert 1 galaxies. Our group has made significant strides in overcoming the major obstacle in analyzing outflow absorption troughs, the velocity-dependent non-black saturation. Thus, we have the ability to extract the essential physical properties from the data of carefully chosen objects. Our FUSE proposal targets the four most promising objects, for which we either have approved Chandra grating time, or a parallel submitted XMM and Astro-E2 proposals. This effort is designed to create a combined UVX-ray data set, which will leave a long lasting FUSE legacy in the field of cosmological structure formation. PROP ID: F327 PROPOSER: Hoopes PROPOSAL TITLE: The FUSE Starburst Legacy Probing Galaxy Evolution at Low and High Redshift Starbursts are a significant component of the present-day universe, and offer unique laboratories for studying the processes that have regulated the formation and evolution of galaxies and the IGM. An All-sky Imaging Survey being conducted by the Galaxy Evolution Explorer (GALEX) has discovered many star-forming galaxies with UV fluxes bright enough for detailed study with FUSE. We propose a Legacy project to obtain high quality (SN > 20) spectra of the 14 most favorable of these bright starbursts with em FUSE in order to form a representative sample of local star forming galaxies which can be compared to galaxies at high redshift. The em FUSE data will be especially valuable to study 1) the coronal-phase gas that may dominate the energetics of starburst-driven superwinds, 2) the properties of the stellar populations in starbursts (including the IMF and burst history), 3) the abundances and chemical evolution history of starbursts, 4) the escape of ionizing radiation from starbursts, 5) the effects of the strong UV radiation field on the formation and destruction of H_2, and 6) the starburst dust-attenuation law in the FUV window. This sample represents a large increase in the inventory of em FUSE spectroscopy of comparable quality for starbursts. This project will capitalize on the synergy between em FUSE and GALEX to build a lasting legacy for research on starbursts at both low- and high-redshift. em FUSE is the only facility that can obtain high resolution UV spectra that measure the global properties of local starbursts. PROP ID: F329 PROPOSER: Welsh PROPOSAL TITLE: The Local ISM Legacy Project We propose to provide a legacy database of far ultraviolet absorption spectra (912 - 1100AA) of 44 bright early-type B stars residing within sim 50pc of the Sun. These spectra will primarily be used to map the physical and chemical characteristics of the neutral and ionized interstellar gas that lies both within and just beyond the contours of the Local Bubble region. Of particular importance will be the detection of the OVI ion, which is known to trace highly ionized, hot (sim 300,000K) interstellar gas. We shall produce plots of the spatial distribution of the OVI ion with respect to the cold and dense neutral boundary to the rarefied Local Bubble cavity. This information will provide new insights into the possible production mechanisms for this ion that is widely believed to be formed at the conductive interfaces of evaporating gas clouds. Our database will also allow study of the spatial distribution of the ions of ArI, OI, FeII, CII, CIII, NI and NII, such that both diffuse neutral and ionized local gas can be probed in order to determine if photo-ionization conditions dominate within the local cavity. These data will also allow an investigation of the gas phase element abundances in the local gas, such that we will be able to compare their relative depletion patterns with both the galactic disk and halo gas. In addition to these prime science objectives these data will also provide a large database of observations of local H_2 molecular absorption, as well as a large, high SN set of early-type star spectra that can be modelled with appropriate stellar atmospheres. PROP ID: F331 PROPOSER: Wannier PROPOSAL TITLE: Gas in the Disk and Halo of M31 - a Legacy Program M31 (Andromeda) is an ideal system in which to study the behavior of gas in a galaxy comparable to our own Milky Way. It is close enough to enable FUSE observations toward its brightest hot stars, and its systemic velocity allows the gas of M31 to be clearly distinguished from that of our own Galaxy. It has been well studied at radio, infrared and optical wavelengths, providing an excellent knowledge of the distribution and velocities of features in its central disk. As part of its long-term legacy, FUSE should turn its attention to our nearby companion. We propose to observe six sightlines with exposure times adequate to measure velocities and column densities of important neutral and ionized species. The spectra will provide a rich data set for study of high velocity features in the M31 halo and of the dynamics of gas in the thick disk. The brighter M31 O stars have FUV fluxes similar to those QSOs used to survey O VI in the Milky Way halo. Existing, short FUSE exposures of some of these stars demonstrate feasibility. The proposed program will leave as a legacy the first quantitative, systematic study of the gaseous content of an external galaxy using FUV resonance lines. PROP ID: F907 PROPOSER: Smith PROPOSAL TITLE: A far-UV search for gamma,Cas analogs in the Small Magellanic Cloud gamma,Cas, the classical Be prototype, is a highly unusual X-ray object for which there is no known counterpart in the Galaxy. The next best places to search for analog objects are the Magellanic Clouds. The Clouds have uniform distances, little intervening reddening, and an average age similar to gamma,Cas (10-15 Myr). We have identified 5 stars in the SMC whose light curves exhibit peculiar cycles similar to gamma,Cas and, in some cases, whose peculiar spectroscopic properties may be conducive to X-ray production. This is an extension of an approved HSTSTIS program to obtain mid-UV spectra of these objects. We plan soon to extend our study to GALEX and to the X-ray region ( Chandra). Here we outline a plan to obtain FUSE snapshots of these objects in order to better place these objects in the HR Diagram by defining their SEDs over a wide wavelength range, to look for evidence of high-energy activity, such as anchored, corotating clouds, and for the presence of evolved subluminous companions. PROP ID: F909 PROPOSER: Chayer PROPOSAL TITLE: Studying Abundance Anomalies in Subdwarf B Stars Using FUSE Required) We propose FUSE observations of a sample of hot subdwarf B stars (sdB) in order to carry out an abundance analysis of heavy elements and see how their abundance patterns emerge from the observations. It is a well known fact that the atmospheres of these extreme horizontal branch stars exhibit abundance anomalies. Diffusion processes such as gravitational settling, radiative levitation, weak stellar winds, and accretion have been proposed to explain the abundance anomalies. Our goal is to identify which mechanisms operate in the atmospheres of these stars, study their interactions, understand the abundance patterns, and ultimately, constrain the structure of the atmospheres of sdB stars. With this proposal we want to pursue the goal of our FUSE proposal E152 by doubling the number of stars in our sample. To study and interpret the abundance patterns in sdB stars, we need a large sample of stars with atmospheric parameters that cover the whole effective temperature and gravity domains for this type of stars 20,000 K leq T_: eff leq 40,000 K ; 5.0 leq log g leq 6.5). To achieve a thorough abundance analysis we need FUSE observations, because many resonance lines of elements such as phosphorus, sulfur, chlorine, and many iron peak elements are only visible in the FUV range for the effective temperatures of interest. This study will not only provide new insights into the stellar atmosphere structure of sdB stars, but also to the evolution of galaxies since these stars are the most important candidates for the source of the UV excess in elliptical galaxies and early-type spiral bulges. PROP ID: F912 PROPOSER: Redfield PROPOSAL TITLE: A Far-Ultraviolet Spectroscopic Survey of RS CVn Binary Systems RS CVn systems are detached late-type binaries that are very active as a result of their tidally-enforced rapid rotation. They are actively studied and bright at X-ray and UV wavelengths, but very few have been observed by FUSE. Located in the FUSE spectral range are emission lines formed in plasma at 0,000--300,000K e.g., CIII and OVI) and the coronal emission line FeXVIII 974AA formed at 6,000,000K. The spectral resolution and wavelength scale (relative to nearby interstellar lines) of FUSE permit us to measure the width and velocity shift of the OVI and CIII lines and perhaps also the FeXVIII line, providing a new window on stellar atmospheric dynamics and structure. We propose to use this new tool to answer the following important questions, (1) Which star in selected active close binary systems is the dominant emitter in lines formed at different temperatures Studies of Capella show that the 10^5K lines are predominately from the G1III star, whereas the coronal line is mostly from the G8III star. (2) Are the broad profiles seen in these rapidly rotating stars due to geometrically extended structures rigidly rotating with the star, or are they due to some other mechanism Observations of our selected high declination systems observed at different orbital phases will allow us to answer these questions. (3) Search for outflows and downflows in lines formed at different temperatures. This proposal is an extension of a productive Cycle 4 program of the same name, but since the pointing constraints for Survey targets have been relaxed, many of the most important RS CVn systems are now accessible and merit FUSE observations. PROP ID: F913 PROPOSER: Dupuis PROPOSAL TITLE: Metals and Quasi-Molecular Satellites in Cooler DA White Dwarfs Required) We propose to expand a survey of DA white dwarfs cooler than about 0,000K initiated in FUSE Cycle 4. These stars have not been studied as extensively than hotter white dwarfs by FUSE as they tend to be fainter and are not as good background sources for deuterium studies. We will search for the presence of trace elements such as C, N, Si, and Fe in the atmosphere of these cooler white dwarfs. Previous observations of white dwarfs in this temperature range have revealed surprisingly high metallicity in a subset of stars. This is in spite of the dwindling of support by selective radiative acceleration at these temperatures. The current wisdom about this phenomenon is that these stars are accreting matter, either interstellar or circumstellar, which then pollutes their atmospheres. These observations will allow us to potentially discover new cool metal-enriched DAs and further our understanding of this peculiar phenomenon. These observations will also allow us to improve our understanding of quasi-molecular satellites which become prominent in the wings of Lyman beta and Lyman gamma profiles at these temperatures. PROP ID: F914 PROPOSER: Chu PROPOSAL TITLE: Hot Gas in the Giant HII Region 30 Doradus 0 Doradus is an archetypical example of a starburst region. At a distance of 50 kpc, its stellar content and interstellar structure can be resolved and studied in detail. The mechanical energies injected by massive stars have yielded a large amount of hot, X-ray-emitting gas in 30 Dor. Optical and X-ray observations of 30 Dor reveal a good correlation between shell structures and bright X-ray emission. We request FUSE observations of 30 Dor to use emission lines to study both the physical conditions and kinematic properties of the hot gas in X-ray-bright shells. In particular, we will use the OVI emission lines, in conjunction with complementary X-ray and optical data, to study SNR shocks and interfaces between hot (>10^6 K) gas and the surrounding cooler (10^4 K) shell gas. The results will aid in our understanding of the generation and conditions of hot gas in distant, unresolved starburst regions. PROP ID: F915 PROPOSER: Bennett PROPOSAL TITLE: Masses and Mass Loss Rates of Red Supergiants in Binaries II We propose to observe all remaining cool, non-interacting supergiant binaries with hot companions from the Parsons & Ake (1998) catalog, satisfying certain feasibility requirements, that were not targets in FUSE program E937, as a Survey and Supplemental Program. The objective is to determine stellar masses of a diverse sample of massive, evolved, late-type stars and their B-type main sequence companions, accurate to 1--2 accurate stellar masses are known for any cool supergiants. An important secondary goal is to determine mass-loss rates of the stellar winds of these evolved stars by observation of wind absorption features superimposed on the hot companions FUV continua. These supergiant binary systems are important, fundamental stellar laboratories useful in verifying and constraining models of stellar structure and evolution. We will proceed by measuring the hot stars radial velocity, preferably at more than one epoch (we will propose continuing observations for FUSE Cycles 7--8). The orbits of the cool supergiant primaries of the target binaries are being accurately determined from the PIs decade-long radial velocity program on the DAO 1.2m McKellar coude telescope. Then the companions velocity amplitude, K_2, can be found from a single radial velocity observation, although multiple observations are preferable. Nevertheless, a single observation will suffice to determine the mass ratio of the stars to 2--4 separated in orbital phase, the accuracy will be 1--2 Some target stars eclipse, and for these accurate stellar masses can be directly obtained. Masses of the remaining stars will be obtained from optical interferometry; these binaries are on the NPOI target list. With the loss of HSTSTIS, bf FUSE is the only available UV spectrograph and therefore, the proposed program is essential to determining fundamental, accurate masses of cool supergiants. PROP ID: F916 PROPOSER: Dixon PROPOSAL TITLE: FUSE Observations of the Hot Post-AGB Star ROA 5342 in Omega Centaurus We propose fuse observations of the hot post-asymptotic giant branch (PAGB) star ROA 5342 in the globular cluster omega Cen NGC 5139). With an effective temperature near 70,000 K, ROA 5342 is the hottest known PAGB star in a Galactic globular cluster. As such, it provides an important test of the possible relationship between the photospheric iron abundance and temperature of cluster PAGB stars. Once its temperature and metallicity are known, the star will provide a sensitive probe of the dust extinction toward omega Cen, which is known to be spatially variable. The star is also an interesting osix target -- a low-SN Cycle1 fuse spectrum shows that its photospheric osix lines are stronger than are predicted by non-LTE stellar atmosphere models, suggesting either an oxygen enhancement or some interesting stellar physics. Zargo et al. 2003) find evidence for high-velocity interstellar osix absorption in the Cycle 1 spectrum of this star. If confirmed, it would be the first high-velocity osix absorption seen towards a star in our Galaxy. PROP ID: F918 PROPOSER: Thilker PROPOSAL TITLE: Extranuclear Star-Forming Regions from SINGS NASAs Spitzer Space Telescope and Galaxy Evolution Explorer (GALEX) now provide high-resolution MIR--FIR and FUV--NUV probes for the internal structure of nearby galaxies, effectively constraining the spatial distribution of dust and stars of varied age. Both observatories have committed to a common Legacy project to ascertain the star formation activity and its effect on dust properties in a large representative sample of local targets. This effort is called SINGS -- the Spitzer Infrared Nearby Galaxy Survey. Highlighted within SINGS are a collection of 75 optically- or IR-bright star-forming regions, for which dedicated high-resolution IR 5-37mum) spectroscopy will be obtained. In order to best capitalize on this opportunity to gauge the entire (stellar and dust) FUV--FIR SED for such intermediate luminosity starbursts, we propose FUSE survey observations for 19 optically-selected, extranuclear star-forming regions in six SINGS galaxies. The entire proposed sample benefits from completed GALEX FUV and NUV imaging, which we have used to assess feasibility. The extranuclear SINGS star-forming regions span a representative range of key physical parameters. The FUSE spectra of these star-forming regions, when combined with GALEX and Spitzer observations, will constrain the massive stellar content in each object and permit determination of the UV attenuation law. We will also explore the possibility of using the equivalent width of ionN4, ionC3, and ionP5 winds lines as metallicity indicators, with application at high redshift. This project complements a related Cycle 6 proposal to observe the central regions in a larger fraction of the SINGS galaxies. The proposed dataset will have exceptional archival value, given the GALEXSINGS Legacy program. PROP ID: F919 PROPOSER: Thilker PROPOSAL TITLE: Probing the Central Regions of Nearby Galaxies NASAs Galaxy Evolution Explorer (GALEX) is conducting wide-field imaging and spectroscopic surveys in FUV (1350-1750AA) and NUV 1750-3000AA) bands. A dedicated campaign to image 300+ nearby galaxies (Nearby Galaxy Survey, NGS) is nearly complete. We propose FUSE survey observations for the central region of 25 galaxies with completed GALEX imaging, which are also being observed at .6-160mum as part of either the Spitzer Infrared Nearby Galaxy Survey (SINGS) or Mid-IR Hubble Atlas (MIR-atlas) projects. Our sample galaxies span a wide range of star formation activity in the local universe. The FUSE spectra, when combined with GALEX and Spitzer observations, will constrain the star formation history (SFH) in the central region of each target, placing the sample into an evolutionary context. The SFH will be estimated via direct comparison with reddened Starburst99 population synthesis predictions, improved by the FUSE spectral library of hot stars. Our analysis will be based on the FUV to UV continuum slope, spectral line diagnostics, and the overall FUV--FIR SED. We will concurrently determine the FUV attenuation law with unprecedented accuracy for ordinary star-forming galaxies, and test for correlation of the extinction law with SFH and galaxy type, given that copious star formation may modify dust grain properties. The combination of FUSE, GALEX, and Spitzer data provides a rare opportunity to decisively test and calibrate the IRX-beta attenuation-reddening relation, which may be used to gauge UV extinction for >10^7 galaxies detected in the GALEX imaging surveys. Our GALEX FUV, NUV imagery was used to select targets and will aid interpretation of spatially integrated FUSE spectra. Radial profiles and spatially-resolved SEDs in UV--IR bands will allow us to extend our results beyond the circumnuclear region. The proposed dataset will have additional archival value, given the GALEXSINGS Legacy program. PROP ID: F927 PROPOSER: Iping PROPOSAL TITLE: A Far-UV Survey of O Star Binaries in the Galaxy and Magellanic Clouds We propose a survey of close, massive binary stars not previously observed by FUSE. The target sample includes detached and semi-detached systems that are at pre and post Roche lobe overflow evolutionary stages. The binaries are generally double-line spectroscopic binaries, many are eclipsing systems, with well-determined orbits and periods in the range 1.6 - 12 days. The far-UV spectra will be used to determine stellar wind mass loss rates and terminal velocities from species tracing a range of wind ionization states. The spectral features will be modelled to study photospheric abundances, evidence for CNO enhancements as the result of mass transfer, and measure projected rotational velocities. We will look for spectroscopic evidence of mass transfer and wind-wind collision effects. The proposed observing plan provides the possibility for each system to be observed more than once to sample different orbital phases and spectral variability. The ISM properties of the ! sight lines will also be analyzed.