FUSE CYCLE 8 ------------ Accepted Program Abstracts -------------------------- PROP ID: H001 PROPOSER: Welsh PROPOSAL TITLE: Probing the IVC gas associated with blow-out from the W4 superbubble We propose to examine intermediate velocity (IV) ionized and neutral interstellar absorption components associated with gas blown into the halo by the underlying W4 nebula. Massive early-type stars of the Cas OB6 association appear to be powering a huge ejection of gas into the lower halo through a galactic chimney that has produced a giant arch of IV gas above the Perseus spiral arm. Through the use of absorption-line analysis our FUSE investigation will focus on the physical, chemical and dynamic conditions of the disturbed atomic and molecular gas for subsequent comparison with other IV gas associated with halo IV clouds and IV gas surrounding galactic SNRs. Our study will therefore shed light on the differences between both IV gas clouds in the disk and halo and between high velocity clouds in the halo and how their presence is linked to the formation and evolution of galaxies. The topic of galaxy evolution and formation is presently of prime scientific interest to NASA. PROP ID: H002 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 K1-16 we found an Fe-deficiency by a factor of at least 10. By subsequent FUSE spectroscopy we showed that the same phenomenon is exhibited by the prototype of the PG1159 spectral class as well as two related objects. Our proposal has two immediate aims : We will perform a systematic investigation of PG1159 stars to show if Fe-deficiency is a common phenomenon among these objects. We think that iron was destroyed by s-process neutron captures in combination with a late He-shell flash. If this is true, then all PG1159 stars should be Fe-deficient, because they all are the outcome of a late He-shell flash. The pulsating PG1159 stars define the GWVir instability strip in the HRD. Our target sample comprises the two coolest known PG1159 stars, a pulsatornon-pulsator pair. FUSE spectroscopy allows to precisely determine their effective temperatures and, hence, the position of the red edge of the instability strip. PROP ID: H003 PROPOSER: Crenshaw PROPOSAL TITLE: Evolution of the Intrinsic Absorption in AGN proposal site. We propose to follow the long-term evolution of mass outflows from AGN FUSE observations of Seyfert galaxies that have previously-detected blueshifted absorption lines. The new observations, combined with our archive program on intrinsic absorption in AGN, will allow us to track the absorption variability over a range of time scales up to sim9 years, and thereby place tight constraints on the changing physical conditions (ionization parameters, column densities), kinematics (transverse velocities, radial velocities), and geometry covering factors) of the outflowing absorbers. We will then use these constraints to identify the dynamical forces (radiation pressure, magnetocentrifugal acceleration, andor thermal expansion) responsible for driving the gas outward and thereby investigate the nature and origin of the mass outflows. PROP ID: H005 PROPOSER: Iping PROPOSAL TITLE: Probing the Halo and ISM of Low-Redshift Galaxies with Supernovae proposal site. We propose a Target of Opportunity program to study the halo and ISM of a low-redshift galaxy hosting a bright new supernova (V lesssim 13). 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 nearby galaxies 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. 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. Our team has the experience and extensive ground-based support to promptly assess the suitability for this program of each newly-discovered supernova. PROP ID: H006 PROPOSER: Fox PROPOSAL TITLE: Far-UV Spectra of the Brightest X-ray Sources Within the next fifteen years a new generation of X-ray satellites These facilities will have the sensitivity to measure intergalactic ionO7 and ionO8 absorbers toward sim100 AGN. Of the ten brightest X-ray sources, three do not yet have good fuse data. We propose to obtain the spectra of Mrk180, the only high-declination target among these three, and of NGC863, the brighter of the two low-declination targets. This will provide a legacy of os data that can in the future be compared to resolved osev and oeig profiles. Such a dataset will enable the full investigation of the warm-hot intergalactic medium from z0--0.05, namely its phase structure, physical conditions, and baryonic and metallic content. The data will be placed in the context of cosmological structure formation and will thus be able to constrain aspects of these models such as supernova feedback and intergalactic metal enrichment. Studies of associated os systems, intervening os systems, foreground galactic haloes, and high-velocity clouds will also be possible with this data. PROP ID: H007 PROPOSER: Ehrenreich PROPOSAL TITLE: A combined search for H_2 in the Sagittarius dwarf spheroidal galaxy and O, sc vi in the Milky Way The Sagittarius dwarf spheroidal galaxy (Sgr dSph) is located sim 6kpc below the Galactic plane and is 3times closer to the Galaxy than the Large Magellanic Cloud (LMC). Numerous studies and surveys were done to characterize the stellar population and the dynamics of this galaxy---explorations of its orbital history are all consistent with a total mass > 10^9 solar masses, 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 Sgr dSph plays 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-H_2 conversion factor is more than 30times 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 H_2. 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 enlighten the Sgr dSph ISM is extremely difficult. We propose to observe the globular cluster M54 (NGC 6715), which has been proven to be physically associated with the center of Sgr dSph. Luckily enough, the line-of-sight towards M54 does not only give the unique opportunity to investigate the ISM of our closest neighbor, but it is also one of the very few FUSE line of sight that probe the close neighborhood of the Galactic center. The expected flux of M54 in the FUV along with a relatively reduced reddening will allow us to detect a large amount of diffuse O,sc vi near the Galactic center. This program was accepted for Cycle 5 but was never achieved due to the target declination. This is the very last opportunity to observe M54 in the FUV. PROP ID: H008 PROPOSER: Jenkins PROPOSAL TITLE: Why Are Some Interstellar Atomic Clouds so Extraordinarily Cold We propose to observe a star behind a complex of unusually cold HI clouds that produce shadows in the background 21-cm line radiation. These clouds are not the classical dense molecular clouds that are known for their strong CO line emission. Our objective is to learn how this material arrives at temperatures well below those given by standard theoretical predictions. By measuring the ortho-to-para ratio of H_2, which equilibrates very slowly with the local kinetic temperature, we can determine if the gas has been cold for a long time, as one might expect if the clouds are stable and heating rate is abnormally low, or, alternatively, if the coldness is a very temporary condition brought about by rapid responses to turbulent expansions and compressions. In addition to using FUSE to measure the abundances and rotational excitations of H_2 and CO, we plan to compare the gas-phase abundances of Fe and O, so that we can test the proposition that there might be a deficiency of grains that emit energetic photoelectrons that would normally heat cold clouds. PROP ID: H009 PROPOSER: Shull PROPOSAL TITLE: Mixing of the Metals in Galactic Infall In this final FUSE observing cycle, we propose to obtain significant additional exposures on two important sight lines through ComplexC, an infalling, low-metallicity HVC located in the low halo. These Galaxy and focus on mixing of the infalling HVC with disk gas and the Galactic fountain. Additional FUSE data on PG1626+554 and Mrk876 will allow us to obtain much better abundances of O, Si, Fe, N, and C, particularly from short-wavelength OI lines in the SiC channel. Our program goals are 1) To measure accurate metallicities of OI and other species NI, SiII, FeII) indicative of the HVC nucleosynthetic origin; 2) To examine correlations of OIHI and NIOI with NHI to understand how infalling clumpy gas mixes with the Galactic disk and fountain. Infalling, low-metallicity gas can affect the Galactic chemical nucleosynthetic) history, as well as the thermodynamics (cooling) of halo gas. In our recent study of ten sight lines through Complex C Collins, Shull, & Giroux 2006) we showed that OIHI varies from 18.1 < logNHI < 20.1 NHI in cd. Our two sight lines with logNHI < 19.5 should be particularly sensitive to the interfaces between gas in the halo and fountain. PROP ID: H010 PROPOSER: Shull PROPOSAL TITLE: Multiphase Intergalactic Baryons and Metals One of the important discoveries of FUSE and HST was the detection of intergalactic OVI absorbers at low-z, possibly associated with the warm-hot intergalactic medium (WHIM) at 10^5-6K. Our FUSE surveys of OVI absorbers along 31 sightlines Danforth & Shull 2005; Danforth etal 2006) showed that 5--10 the local baryons reside in OVI-bearing gas with sim10 metallicity, and that the extent of metal transport at z leq 0.1 is leq 800 h^: -1 kpc from L^* galaxies (Stocke etal 2006). Owing to the steep column-density distribution, N (N_ OVI )propto N_ OVI ^ -2.2 pm 0.1 , weak absorbers may contain much of the OVI mass. This new survey could confirm those extra baryons. We propose a major program to obtain additional FUSE exposures of 10 high-declination AGN (300 ks on 6 type-A targets and 200 ks on 4 type-B targets). We will measure OVI absorbers (EW geq 12.5mAA, Nosix geq 10^13cd) that may contain a significant portion of the WHIM baryons. We will also probe multiphase ions (CIII, FeIII) and search for broad Lybeta and OVI absorption from hot gas. Our overall goals are to 1) Obtain an accurate baryon census of the hot IGM; 2) Test the predictions of cosmological simulations for WHIM redshift evolution; 3) Measure the metallicity distribution of the low-z IGM relative to the large-scale distribution of galaxies at z leq 0.1. We will search carefully for broad, shallow absorbers against the power-law continua of two bright BL Lac objects. FUSE data will be combined with STISE140M data on other ions to greatly improve the accuracy of our multi-phase baryon census at z leq 0.15. Galaxy redshift surveys will allow us to study the connections between OVI absorbers and the large-scale filamentary structure of galaxies, complete down to sim 0.2L^* at low redshifts, z leq 0.15, to determine whether outflows from dwarf galaxies are major sources of these metals. PROP ID: H015 PROPOSER: Brown PROPOSAL TITLE: Stellar Activity on Stars in the 7 Myr Old Eta Cha Cluster The young (7 Myr), nearby (97 pc), sparse eta Cha cluster provides a very special opportunity to understand the processes controlling protoplanetary system evolution. Within this cluster 40 low mass stars retain primordial disks and are still accreting, while the more massive stars have dissipated their inner disks. The most massive member now has a debris disk that indicates advanced protoplanetary system development. We propose FUSE observations of the most active, unobserved, low mass members of the cluster and the remaining unobserved intermediate mass member. This will provide an improved quantification of the evolution of stellar activity at this particularly critical and poorly sampled evolutionary phase, and give a better picture of the conditions under which this interesting set of primordial disks, potential disks with inner holes, and debris disks are undergoing the process of planetary system formation. PROP ID: H017 PROPOSER: Ignace PROPOSAL TITLE: Non-Spherical Winds and Disks around Rapidly Rotating, Luminous Stars The role of rotation for the mass loss from massive stars, with relevance for their evolution, is an important topic for which a number of outstanding questions persist. Chief among the puzzles is the creation and maintenance of disks and bipolar winds observed around some evolved massive stars -- the supergiant Be (sgBe) stars and Luminous Blue Variables (LBVs). We are seeking FUSE time to observe 4 stars of these types in the Magellanic Clouds. The goal will be to analyze the wind lines to further our understanding of the wind structure, to restrict the inclination of the systems, and possibly to derive the rotation velocity of the central stars. We expect to probe the faster polar wind with higher ionization lines (e.g., Nsc iii, Csc iii) and, potentially probe the equatorial or disk flow with lower ions (e.g., Sisc ii, Nsc ii, Fesc ii). PROP ID: H018 PROPOSER: Jeffery PROPOSAL TITLE: Far Ultraviolet Observations of Extreme Helium Stars We propose the first exploration of the far ultraviolet spectra of the rare extreme helium stars (EHes). These are O- and B-type stars in which atmospheric hydrogen is generally less than one part in 10,000 and carbon is enriched to sim1 The consequences of the absence of hydrogen opacity are severe for the far ultraviolet spectrum. Neutral and ionized helium, carbon and other line opacities become substantially more important than that due to the Lyman series in normal stars. FUSE spectra will allow us to make crucial tests of the latest H-deficient model atmospheres, and will improve the overall temperature diagnostics for these stars. We will also be able to test the treatment of the atomic physics, particularly line-broadening, in light ions and investigate interstellar Lyman beta profiles over a range of hydrogen column depths without stellar Lyman contamination. PROP ID: H019 PROPOSER: Blair PROPOSAL TITLE: A New Galactic Balmer-Dominated SNR, G156.2+5.7 The galactic supernova remnant G156.2+5.7 was discovered by ROSAT in 1991, and optical emission was only recently reported by Gerardy & Fesen 2006). Faint, thin filaments located along the remnants X-ray emission boundaries show only H-Balmer line emission in the optical, making this object a new member of the small class of SNRs likely attributable to Type Ia precursors, such as Tychos SNR and SN 1006 in our Galaxy. Combined UV-optical data on such objects provide a powerful tool for determining the shock velocity and physical parameters and more generally studying shock physics, including electron-ion and ion-ion energy equilibration in the post-shock region and cosmic ray acceleration processes. Unfortunately, however, few of these objects are available for FUV observation. Both X-ray and optical data suggest that G156.2+5.7 is relatively nearby with only modest foreground extinction in its eastern and northern sections, making it an extremely valuable new object for study with FUSE. We request two-20 ks LWRS pointings at Balmer-dominated filaments in this SNR, using FUSEs excellent diffuse source sensitivity to observe broad Lybeta andor OVI lambdalambda1032,1038 lines from this important new supernova remnant. PROP ID: H020 PROPOSER: Gull PROPOSAL TITLE: Eta Carinae Separating Binary Orbital Variations from Secular Changes Eta Carinae has long been suspected to be a massive binary system, but the hot companion has, until now, eluded detection. Our FUSE Cycle 4 observations revealed evidence of the hot companion for the first time. FUV spectra show that the companion is consistent with a late O or WR star that may be nitrogen rich. FUSE observations of ecar now span one complete binary orbit (5.54 years). Future FUSE spectra will allow us to begin to separate cyclical binary orbit variability from long-term secular changes. We propose three Cycle 8 observations, each about six months apart to place further constraints on the hot companion, perhaps obtaining spectral classification and radial velocity measurements which could lead to direct mass estimates for the system. These objectives are supported (1) by spectral analysis of STIS observations from 1998.0 - 2004.2 that have yielded radial velocity curves for ion: He 1 , ion H 1 and ion Fe 2 wind lines in the binary system and (2) VLTIAMBER spectroscopic interferometric observations of ion He 1 2.06 and ion H 1 2.12 micron wind lines that support wind-wind interactions in a binary system. PROP ID: H021 PROPOSER: Cheng PROPOSAL TITLE: CS Gas in the Newly Discovered Edge-On Dust Disk Around HD 32297 Recently, Schneider et al.(2005) discovered an extensive circumstellar dust disk 400 AU in radius) around HD 32297 using HSTNICMOS. Subsequent optical coronagraphic images of HD 32297 revealed a larger and more asymmetric circumstellar nebulosity Kalas 2005) than shown by the HSTNICMOS results. This young (sim30 Myr) A0 star joins beta Pic (A5V; 12 Myr), HR4796A A0V; 8 Myr), and alpha PsA (A3V; 200 Myr) as an additional example of A-type stars with circumstellar dust disks imaged in scattered light. If HD 32297 is indeed a beta Pic analog with similar age, could also have a dynamic circumstellar gas diskenvelope. Although the presence of circumstellar gas can be diagnosed by visual absorption features in CaII K, such absorption features could also be of interstellar origin. Fortunately, many pure circumstellar absorption lines such as Fe II, Fe III, O I (^1D), N I (^2D), N I (^2P), and SII (^2D) can be observed with FUSE. To understand the evolution and interaction of the dust and gas in the debris disks, we propose to observe the possible circumstelar gas in HD 32297 system. The new FUSE observation will further constrain theories of debris disk evolution and planet formation. PROP ID: H023 PROPOSER: Bianchi PROPOSAL TITLE: Revising the fundamental parameters of massive stars We analysed FUSE, HSTIUE and optical 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 relevant implications for our understanding of massive stars evolution, and of the energy balance of HII regions. Although modeling of optical lines with line-blanketed atmospheres also indicates lower effective temperatures than classical calibrations, the hitherto still quantitatively discrepant (between optical and UV diagnostics) results on Teff and especially mass loss rates could be reconciled with a revised inclusion of X-rays from shocks and clumping in the wind modeling. These effects can only be constrained by lines in the FUSE range e.g. Bianchi, Herald, and Garcia 2006). Such analysis for a representative number of stars covering the early spectral types will 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 rate. We propose to observe a final sample of four Milky Way stars, to remedy remaining gaps in the coverage of early spectral types in the list of FUSE observed or approved Galactic stars. 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). The data will have additional value as an archival resource for population synthesis work, and ISM studies. PROP ID: H024 PROPOSER: Rauch PROPOSAL TITLE: On the Evolutionary Status of Extremely Hot Helium Stars - are O(He) Stars Successors of RCrB Stars Hot post-AGB stars are hydrogen deficient. Most of these are the result of a late helium-shell flash, but the evolutionary status of a fraction of about 0-20 as yet unexplained. They could be the long-sought hot successors of RCrB stars, which have not been identified up to now. If this turns out to be true, then a third post-AGB evolutionary sequence is revealed, which is probably the result of a double degenerate merging process. More generally, understanding details of merging double degenerate stars is of interest in the context of SN,Ia events and hence cosmology. PROP ID: H025 PROPOSER: Dixon PROPOSAL TITLE: FUSE Observations of Hot Horizontal Branch Stars in the Globular Cluster NGC 6752 We propose fuse observations of three extended horizontal-branch (EHB) stars spectral type sdB) in the globular cluster NGC6752 to determine their photospheric abundances. With effective temperatures ranging from 20,000 K to 35,000 K and surface gravities ranging from log g 5.0 to 6.2, EHB stars occupy the high-temperature extension of the normal horizontal branch; their hydrogen envelopes are too thin to trigger nuclear fusion of hydrogen. The atmospheres of field EHB stars are chemically peculiar and show unusual and puzzling abundance patterns. Diffusion processes such as gravitational settling, radiative levitation, and possibly weak stellar winds are believed to be responsible for the abundance anomalies. Our goal is to compare EHB stars in NGC 6752 with theoretical models to identify the mechanisms at work in the atmospheres of these stars, to understand their abundance patterns, and ultimately, to constrain their atmospheric structure. Because EHB stars and their progeny may contribute significantly to the UV excess seen in elliptical galaxies, an understanding of their abundances, opacities, and resulting EUV and FUV spectra is important for studies of both galactic evolution and the intergalactic medium. PROP ID: H026 PROPOSER: Ayres PROPOSAL TITLE: The Beta Project Late-type supergiants represent the terminal evolutionary stage of short lived, high mass stars. We shouldnt expect their coronal magnetic behavior to be anything like the long lived, low mass Sun. Many GK supergiants fulfill that expectation by displaying prominent cool wind absorptions in Mgsmall II, and little if any coronal X-ray emission. Yet, a number of early-G supergiants do exhibit symptoms of solar-type coronal behavior, down to details like redshifted transition zone (Tsim 10^5K) emission lines. Even among these active supergiants, however, L_ X L_ C,IV ratios curiously are depressed an order of magnitude below solar-like stars. The winds of the inactive supergiants, and the X-ray deficiency of the class as a whole, are important issues in stellar high energy astrophysics; where the can be put to good use. We propose to add to the mix two key late-type supergiants---betaCam (G1Ib) and betaAqr (G0Ib)---not previously observed by An important objective is to collect fluxes of Csmall III lambda977 and the O: small VI doublet near 1035AA. These are three of the ten strong FUV emissions in the so-called CNOSi sum, which comprises fully two thirds of the total radiative losses of the 0.3--3times 10^5K plasma and is more resistant to compositional anomalies in evolved stars than the commonly used Csmall IV flux index. Equally important, the FUV profiles carry an imprint of the dynamical state of the stellar outer atmosphere, a likely key to understanding the nature and origin of hot coronae in such objects. vskip 0mm PROP ID: H027 PROPOSER: Sembach PROPOSAL TITLE: A FUSE Search for Ne VIII in the Warm-Hot Intergalactic Medium The H,1821+643 sight line provides a final unique opportunity for FUSE to measure ionNe8 absorption in the warm-hot intergalactic medium (WHIM), the respository for approximately half of the baryons in the low-redshift universe. Ne 8 is the best ultraviolet tracer of gas in the WHIM at temperatures of T5times10^5 - 1times10^6,K. In conjunction with measures of ionO6, its detection or restrictive upper limit is a strong indicator of how much hot gas is present. However, useful constraints on ionNe8 require long integrations, even on bright sources. Consequently, only a few measures of redshifted ionNe8 in intergalactic O 6 systems have been possible to date, and only one solid detection of intergalactic ionNe8 exists so far. We propose to alleviate this problem by obtaining a long FUSE observation of QSO H,1821+643, the first sight line for which intergalactic O 6 absorption was studied in detail. H,1821+643 is one of the brightest QSOs in the sky at ultraviolet wavelengths, is in an optimal region of the sky for FUSE observing, and the sight line contains four intergalactic ionO6 absorption systems at z 0.21-0.25 with corresponding wavelength intervals for redshifted ionNe8 that are clear of foreground Galactic contamination. By observing this one rich sight line, we will nearly double the number of ionO6 systems with data good enough to carry out a meaningful search for ionNe8 in the WHIM. The proposed observation will be a lasting legacy of the FUSE program since it will not be possible to search for ionNe8 at z lesssim 0.5 with HSTCOS. PROP ID: H029 PROPOSER: Danforth PROPOSAL TITLE: Assessing the Hot Gas Content of LMC Superbubbles Early FUSE work on sight lines towards the LMC indicated that OVI absorption at LMC velocities was nearly ubiquitous and varied substantially between sight lines (Howk et al. 2002a). These variations had no obvious correlation with ISM morphology. This was taken as evidence for a patchy hot halo in the LMC, and was thought to preclude significant studies of hot gas from isolated ISM structures in this nearby galaxy. We have revisited this problem recently and in the LMC is detectable with FUSE by making careful comparisons between sight lines toward superbubbles and nearby comparison stars. Unfortunately, at this late date in the FUSE mission, several important superbubbles still have no observed sight lines with FUSE, and many of the existing data for superbubbles have marginal or no usable comparison sight lines nearby. We propose to correct these problems by observing a carefully selected set of previously unobserved LMC stars. The new data will allow us to leverage the existing LMC data sets and extend the study of OVI to a statistically meaningful number of LMC superbubbles. The requested data will allow us to a) verify the result that superbubbles contain measurable excess OVI content, b) better assess internal variations within individual superbubbles, and c) shed additional light on the production mechanisms behind the hot phase of the ISM in the LMC, and by extension, other galaxies including our own. PROP ID: H032 PROPOSER: Grady PROPOSAL TITLE: The Source of Activity on a Young Vega Analog HD 169142 An emerging body of data point to A stars harboring planetary systems. As for lower-mass young planetary systems, the stellar radiation field is critical in the chemical evolution of the disk, through photodissociation of the molecular gas which is the bulk of a protoplanetary disks mass, and in modifying the atmospheric chemistry of young planets. If the star is extremely rapidly rotating, the radiation field experienced by bodies in the disk differs significantly from that of slowly rotating stars Vega and Altair have approx2000K pole-to-equator temperature gradients. By combining inclination measurements with v sin i data, we have identified a similarly rapidly rotating, 8 Myr-old Herbig Ae star. The UV data for this star, HD 169142, indicate a mass loss like TW Hya, and that the inner disk is gas-depleted. However, strong UV line emission and L_x at the upper end of beta Pictoris Moving Group (BPMG, t12 Myr) F stars are consistent either with accretion or with rotationally-enhanced activity. FUSE FUV spectra of HD 169142 and a rapidly rotating BPMG FOV star, 51 Eri, will definitively establish the UV emissions origin, and allow us to characterize the radiation field of a young Vega-analog. PROP ID: H034 PROPOSER: Wang PROPOSAL TITLE: OVI Emission from Galactic Chimneys We propose sl FUSE observations to sample the O,VI line emission from the galactic chimneys of the nearby massive galaxy NGC2841. 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), as detected in our sl Chandra observation. The O,VI line intensity measurements will help to determine the temperature distribution and cooling mechanism of the hot gas, whereas the line centroids and widths of the emission will further enable us to constrain the dynamics of the gas. The results will have strong implications for understanding the role of the disk-halo interaction in a galactic eco-system. PROP ID: H036 PROPOSER: Wesemael PROPOSAL TITLE: Trace Elements at the Photospheres of DB White Dwarfs The DB white dwarfs belong to the subgroup of white dwarf stars which possess an atmosphere dominated by helium. Their optical spectra are characterized by the transitions of neutral helium, and their effective temperatures range from 30,000 K to approximately 13,000 K. Trace elements are also occasionally seen in the atmosphere, principally hydrogen, but also a handful of heavy elements like carbon and silicon. To explain the abundance patterns of both dominant and trace elements, several processes must be called upon, namely upward diffusion of hydrogen left over from previous evolutionary phases, downward settling of heavy elements, convective dredge-up from deeper layers, convective mixing, accretion from the ISM, radiative element support, and stellar winds. Because the abundances of heavy elements have been determined in so few DB stars, our picture of the abundance trends remains sketchy and the potential to test theoretical models remains largely unfulfilled. We thus propose to secure spectra for four DB stars spanning the effective temperature range between 16,000 and 3,000 K with the specific aims of obtaining abundances of several elements (principally C and Si, but also N, Fe, P, and S) and of testing the reliability of our model atmospheres in that wavelength range. The FUSE observations will provide us with a unique opportunity to study the competing physical processes which affect the photospheric abundance of heavy elements in DB stars. PROP ID: H038 PROPOSER: Wang PROPOSAL TITLE: A Joint FUVX-ray Emission and Absorption Study of the Galactic Corona The Galactic corona is believed to play an essential role in the eco-system of the Galaxy. But the extent as well as the physical properties of the corona are yet to be determined. We request sl FUSE observations of the ovi line emission in adjacent fields of LMC X-3, toward which we have already detected ovi, ovii, and neix absorption lines and have obtained Suzaku measurements of the local X-ray background. We have also developed a software tool to jointly fit the far-UVX-ray absorption and emission spectra, allowing for serious tests of various models (e.g., diffuse hot gas vs. conductive layers) and for tight constraints on spatial and thermal properties of the hot gas over a broad temperature range. The results will provide a unique calibration of our understanding of the corona. PROP ID: H039 PROPOSER: Andersson PROPOSAL TITLE: The Interstellar NO Ratio - Evidence for Local Infall Sophisticated nucleosynthesis models exploring the infall of low-metallicity high-velocity clouds on the chemical evolution of the host galaxy can account for the observed NO variations in metal-poor and metal-rich external galaxies. Subtle variations of the interstellar O: small I abundance in the Solar neighborhood suggest that infall of low-metallicity gas may have occurred within the Solar neighborhood. Precise observations of the NO abundance ratio are essential to test this hypothesis. Recent FUSE measurements of NH_: tot reveal variations with N(H_ tot ), but with significant scatter due to observational uncertainties. Here, we propose to obtain additional high SN observations of the weak interstellar N: small I doublet at 1160 AA in order to derive accurate nitrogen abundances and provide a direct comparison with the existing data. All stars in our sample have high-precision STIS: HST measurements of the weak O small I 1356 AA line for a variety of stellar distances (0.2 leq d leq 3.5 kpc) from the Sun. This proposal is designed to investigate an intriguing trend with distance detected in the best published NO data available. If verified, these NO variations provide direct evidence for different nucleosynthetic histories within and around the Solar neighborhood. PROP ID: H040 PROPOSER: Guinan PROPOSAL TITLE: Completing the FUSE dM Star Database We have extended our ongoing Sun in Time Program on solarstellar dynamo physics and X-rayFUV irradiance (and effects on planetary atmospheres) of solar-type (G0--K5 V) stars to cooler, more numerous dM stars with deep convective zones (CZs). These later goals are motivated by the upcoming Kepler, SIM, and DarwinTPF missions that will search for Earth-like planets in the habitable zones (HZs) of nearby cool stars. The major aims of this proposal are to complete the parameter space of agerotationFUV-emission of dM stars in the FUSE archive. Here we propose FUSE observations of two additional stars GJ 685 -- an intermediate age (sim1--3 Gyr; P_ rot approx 18.6-d) dM1 star -- & Kapteyns Star -- a high velocity and very old (sim12--14 Gyr), slowly rotating P_ rot approx 198-d) dM1 star. GJ 685 (delta approx 62deg) was selected because it bridges the critical agerotationactivity gap now present in the archive between sim300 Myr and sim6 Gyr. Kapteyns Star is noteworthy as the nearest genuine Pop. II star and serves as a proxy for very old metal poor dM stars. Also, Kapteyns Star has a V_ R sim+245 ^ km_ sec that has the major advantage of Doppler shifting its FUV emissions (such as C sc iii and H sc i Lyman series), thus avoiding possible contaminations from geocoronal and ISM lines. Having a full range of P_ rot and FUV fluxes for dM stars (with similar masses and CZs) is important for studying dynamos and heating effects. We also wish to explore the effect of the CZ depth on magnetic activity by comparing dwarf G, K, and M stars with similar rotation periods and ages. This program has a major impact on studies of FUV radiation and its effects on the environments of extrasolar planets that may be hosted by dM stars and on the possible origin and evolution of life on such planets. We will combine the FUSE FUV observations with existing X-ray (ROSATChandraXMM) and UV IUEHST) to form spectral irradiance tables (flux at 1 AU) of dM stars. With FUSE nearing the end of its usable lifetime, this will be the last chance to complete this important FUV dataset. PROP ID: H041 PROPOSER: Blair PROPOSAL TITLE: FUSE Magellanic Supernova Remnant Survey -- The Small Cloud Sample We propose to complete an unbiased ultraviolet survey of supernova remnants in the Magellanic Clouds that was begun in FUSE Cycles 4, 5 and 7. In these earlier programs, we successfully detected at least 17 Magellanic remnants, 16 of which had no previous FUV detections. However, almost 90 of the observations from these earlier programs were for LMC remnants. A cycle 7 survey program includes objects in the SMC, but only three objects have been observed to date, with two detections.) With Cycle 8 likely being the last proposal round for FUSE, we propose here for the remaining SMC supernova remnants as a STANDARD proposal, to ensure that a representative sample of SMC remnants is obtained for comparison with the LMC sample. As with our earlier requests, a standard 0 ks per object using the LWRS aperture will be used for these observations, reaching a limiting flux in OVI lambda1032 about a factor of 100 below the flux observed for the bright LMC remnant N49. With lower mean abundances in the SMC compared with the LMC, and a less complicated ISM environment, the systematics of FUV detections of SMC remnants may be different between the two Clouds. The only way to tell is to look. PROP ID: H043 PROPOSER: Walborn PROPOSAL TITLE: Stellar-Wind Variations in the Ofp Magnetic Oblique Rotator 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. In 2004, with the aid of Hipparcos photometry, a 538d period was found in both light and spectral variations; while in 006, the detection of a magnetic field was announced, strongly suggesting an interpretation as an oblique rotator, only the second known with an O spectral type. The optical behavior suggests that the UV wind features should vary drastically, as they do in the other known O-type magnetic oblique rotator, theta^1OrionisC. We propose to investigate to provide further physical constraints on a model of this remarkable star. This program was approved in Cycle6 but subsequently deferred because of spacecraft problems, now partially resolved. PROP ID: H045 PROPOSER: Wisniewski PROPOSAL TITLE: Massive Stars with Dusty Disks A FUSE Survey of the Most Metal Poor Be Supergiants Massive OB stars are among the most dominant influences on the regions of the galaxies in which they live. Consequently, the understanding of their evolutionary paths is crucial to many aspects of astronomy. Be supergiants represent one of the post-main-sequence evolutionary phases of OB stars, yet they are one of the least well understood. We propose to triple the number of SMC Be supergiants observed to date by FUSE and complete the FUSE survey of all bright LMC Be supergiants. We will model these FUV data, along with ancillary optical spectra, UV spectra, and optical polarimetry, to probe the temperature, density, velocity structure, and geometry of Be disks. These fundamental disk parameters will be compared to predictions from the two leading models which seek to explain the mechanism responsible for the creation of Be disks. Additionally, we will probe the role metallicity may play in the formation and evolution of the Be phenomenon. PROP ID: H048 PROPOSER: Ayres PROPOSAL TITLE: FUSE Observations of an Extragalactic Red Giant We examined a list of potential extragalactic red giant targets environmental conditions---such as metallicity---might influence the development of hot 1--10MK X-ray emitting coronae. Of the 10^20 possible candidates, however, only one survived our feasibility tests--- Arcturus (alphaBoo; K1III). Although its distance (10^-5Mpc) might seem a bit close by normal extragalactic standards, in fact Arcturus belongs to an eponymous moving group thought to be a relic of a merger between a dwarf irregular galaxy and the Milky Way, some billions of years ago. Beyond its intriguing alien heritage, Arcturus has the dubious distinction of being the faintest---but positively detected---coronal X-ray source known, and one of very few red giants to Arcturus, and related Aldebaran (alphaTau; K5III), are centerpieces of a controversial idea to explain the ostensible lack of X-ray activity among red giants by the smothering of coronal loops in extended chromospheric envelopes. Arcturus was Science Team cool star targets. However, because of a variety of unfortunate circumstances, it was not successfully observed prior to the guidance system problems that subsequently have thwarted further attempts. mission nevertheless drawing to a close, it would be extremely valuable to secure an FUV spectrum of Arcturus; not only because its ionO6 lambda1031 and ionC3 lambda977 features can contribute in a unique way toward testing the buried corona hypothesis, but also to provide the sorely needed shortwavelength complement to the 1150--50,000AA spectral Atlases already available for the archetype red giant. vskip 0mm PROP ID: H049 PROPOSER: Walter PROPOSAL TITLE: Absorption Lines in the V471 Tau System The eclipsing DAK2V system V471 Tau affords a unique opportunity to probe the extended atmosphere of an active K dwarf. UV spectra obtained between orbital phases 0.75 and 0.25, with the K star in the foreground, show the transition region lines of C II through N V in absorption against the white dwarf. The scale heights, line velocities, and time variability suggest confinement in large-scale magnetic loops reaching up to heights of at least K star radii. These lines probe the emission measures and temperatures along this line of sight. HST spectra show that the atmosphere is asymmetric, clumpy, hot, and time-variable. We do not know the maximum temperature of this confined gas. Therefore we propose to observe this system with FUSE to see the O VI lines and study the higher temperature gas. We propose to observe for about 30ksec, long enough to ensure a good liklihood of observing at all interesting orbital phases. The lessons learned will be generally applicable to investigations of the atmospheric structures in very rapidly rotating stars. In addition, the lack of absorption lines in the DA photophere casts doubts on the prevalent theory for the DA rotational modulation we will search for temperature variations by studying the stability of the Lymanbeta line profile. PROP ID: H053 PROPOSER: Martin-Zaeidi PROPOSAL TITLE: Characterization of the circumstellar gaseous component around the Herbig B9 star HD97048 HD97048 is a Herbig B9 star known to possess an extended circumstellar (CS) disk supposed to be associated with an enveloppe. It is the only Herbig star for which the flaring of the disk has been directly observed by imaging (VLTVISIR observations). Such a flaring geometry is supposed to be an evidence for the presence of large amounts of gas and is generally a probe of the evolutionnary status of the star. In order to better characterize its gaseous circumstellar environment, we propose to obtain a FUSE spectrum of HD97048. Especially, we wish to observe circumstellar H_2 absorption lines, and study the excitation of this molecular gas. On the other hand, signs of activity and wind have been already observed in the spectrum of this star at longer wavelengths. As a consequence, emission lines of CIII and OVI, which are linked to the activity of the star, are highly expected in the FUSE spectrum. The analysis of H_2 circumstellar lines in the FUSE spectrum will allow us to quantify the gaseous content in the inner planet-forming regions of the disk around the star, and determine the possible correlation between the stellar activity and the excitation of the gas. The proposed FUSE observations, combined with observations at other wavelengths already obtained, will allow us to definitively characterize the circumstellar environment of HD97048 and its evolutionary status. PROP ID: H054 PROPOSER: Wakker PROPOSAL TITLE: OVI in the inner halos of galaxies 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. They may be hiding in the warmhot intergalactic matter (WHIM), evidence for which is provided by the detections of redshifted intervening OVI absorption lines. These OVI absorbers appear to be associated with the extended halos of galaxies. We have searched for intergalactic OVI absorption with v<3500kms (z<0.012), and find a galaxy within 500kpc of each OVI absorber, with the fraction of detections increasing with decreasing impact parameter, although we find just a few targets at low impact parameter (rho<100kpc). Only three FUV targets with rho<100kpc to a nearby galaxy have good FUSE data (Mrk,205, ESO,185-IG13, PG,1259+593). We propose to observe the three remaining targets that can still be observed with FUSE (MCG+10-16-111, RX,J1706.1+7239, RX,J1736.6+7205), in order to determine whether the fraction of OVI detections keeps increasing at the smallest impact parameters. PROP ID: H056 PROPOSER: McCandliss PROPOSAL TITLE: Characterizing H_ 2 Fluorescence, Dust and Diffuse Stellar Populations in the Magellanic Clouds Recent studies of galactic photodissociation regions have revealed strong variations in the relative contributions from dust scattered starlight and fluorescent H_2 emission in their far-ultraviolet spectra. These differences are seen to be correlated with the environmental characteristics of the nebulae and have led to improved models of the ultraviolet H_2 fluorescence. We propose to extend this study beyond the Milky Way with FUSE observations of star-forming regions in the Magellanic Clouds. N66 is the most massive star-formation site in the SMC, with extensive regions of gas and dust excited by far-ultraviolet photons from cluster O-stars. N11B is a region of massive star formation in the LMC, with several stars of spectral type B1 and earlier illuminating bright nebular filaments, suggesting that is an external analog to the Orion Nebula. The unique bandpass and spectral resolution of FUSE will enable an unprecedented study of extragalactic dust and may provide the first detection of far-ultraviolet H_2 emission outside the Milky Way. Combining observations of dust-scattered light from these clusters with stellar observations in the FUSE archive, we can constrain the ultraviolet grain properties of the Magellanic Cloud dust. The scattered light spectra will also be used to constrain the relative contribution of dust-scattered cluster light to the emission from a diffuse population of stars, as observed in starburst galaxies. PROP ID: H058 PROPOSER: McCandliss PROPOSAL TITLE: Expanded Lyman Continuum Search, 19 Far-UV Bright Galaxies Above z0.017 The goal of this proposal is to quantify the star-forming galaxy contribution to the ionization history of the universe. We propose to build on the recent successes in finding Lyman continuum (Lyc) leakage from three blue compact galaxies (BCG) with FUSE, showing estimated leakage of between 4 -- 35 Leitet et al. (2006). We have developed a pool of nineteen far-UV bright candidate objects spanning a variety of starburst morphological types -- spirals, irregulars (Irr), BCG, mergers and interacting galaxies (IG) -- in the redshift range 0.017 le z le 0.043. For these nineteen objects we will be able to detect or limit the escape fraction of lyman continuum photons from star forming galaxies at the 5 detection threshold. By characterizing f_esc at low redshift across a wide spectrum of galaxy types, we obtain data that can be used to constrain the fraction of ionizing radiation originating in starburst galaxies during, and after, the era of reionization of the universe. This parameter is of great importance for understanding the formation of structure in the early universe. At present, direct spectroscopic measurements of Lyc leak in specific galaxy types at low redshift can only be made by FUSE. PROP ID: H061 PROPOSER: Barstow PROPOSAL TITLE: Pollution of White Dwarf Atmospheres by Asteroids and Comets There is clear evidence from Spitzer (and other) observations for the presence of circumstellar debris, in the form of dusty disks, around white dwarfs. Indeed, such debris disks might be composed of cometary or asteroidal remnants, providing source material that might explain the peculiar metal abundance patterns seen in some white dwarfs.If discrete objects such as comets or asteroids are being accreted, then accretion will be a stochastic process. Since the residence times of many elements against gravitationallly driven downward diffusion are rather short, any abundance enhancements would be expected to decay between events on timescales of days, weeks or months. Therefore, we might expect to see variations in measured abundances or even disappearance of certain elements on these timescales. We proposed repeat FUSE observations of a number of white dwarfs with known peculiar abundances to search for any such changes. PROP ID: H063 PROPOSER: Vennes PROPOSAL TITLE: The Iron Abundance Pattern in Hot DA White Dwarfs The iron abundance in hot DA white dwarfs with temperatures between approx 30,000 and approx 64,000 K varies over two orders of magnitudes between the highest and the lowest temperatures probed, however considerable variations (over one order of magnitude) between objects with similar temperatures and surface gravities are observed. These abundance measurements are based on FUSEHSTIUE spectra which covered the ionFe3 to Fe 6 absorption lines, enabling a detailed iron abundance analysis over a wider range of effective temperatures than previously afforded. The observed iron abudance variations may be imputed to accretion from unseen companions or so-called circumstellar debris although the effect of residual mass-loss and selective radiation pressure in the hottest objects in the sample may remain dominant. We propose to obtain high-quality FUSE spectra of a select group of white dwarfs which show evidence of photospheric opacities in EUVsoft X-ray measurements and to accurately determine the iron abundance in their photospheres. The results of this investigation will contribute to a better understanding of abundance variations in hot DA white dwarfs. PROP ID: H064 PROPOSER: Dupke PROPOSAL TITLE: The North Ecliptic Pole Supercluster A Window into the Missing Baryons Simulations predict that nearly half of the baryons in the local universe a re in a moderately hot phase, 1E5--1E7 K, largely in the form of giant cosmic filaments that connect the denser virialized clusters of galaxies. Since they are tenuous and have low overdensities these missing baryons evade detectability and are missing from census of the baryonic content of the local universe. They, however, can be detected through absorption lines they produce in the spectra of background AGNs. The highest covering fraction of such filaments occurs in superclusters and an initial study of AGNs projected behind superclusters has shown absorption systems ( in LyalphaLybetaOVI) at the supercluster redshifts. Here we propose to build upon our initial successful detections and expand our sample by nearly 40 in the ROSAT North Ecliptic Pole survey. This is best known supercluster to study the Cosmic Web because it is entirely selected in X-rays, which defines the real potential well best, but also has the largest number of bright background AGNs among all cataloged superclusters. Furthermore, it matches very well the current observational constraints of FUSE, which is, with the demise of STIS, the only satellite capable of detecting the key absorption lines for this study. PROP ID: H065 PROPOSER: Neff PROPOSAL TITLE: Active Region Evolution on AB Dor Magnetic activity in the chromospheres, transition regions, and coronae of late-type stars has been studied at every wavelength, from radio to x-ray. Outer atmospheres are very dynamic, with short-term flare-like variability, variations produced by the rotation of a non-uniformly bright star, variations produced by the evolution of surface structures, and long-term variations similar to solar cycles. Short-term variations have been extensively studied, with maps of surface structure (Doppler Images) obtained at many epochs. Year-to-year variations in these maps suggest that the active regions evolve on intermediate timescales. Because of observational constraints from the ground and previous spacecraft, these intermediate time domains have been very poorly studied. The unique capabilities of the FUSE spacecraft provide us an unprecedented opportunity to study stellar activity over these scientifically critical, intermediate timescales. We will observe ABDor for 90 ksec (2 rotational period) during each of its CVZ windows during Cycle 8. This will provide full sampling of timescales between 2 and 16 months, the equivalent of observing solar activity on timescales from 8 to 67 years. We will organize contemporaneous observations at other wavelengths, and we will use the archival FUSE observations of ABDor to extend our study to longer timescales. PROP ID: H066 PROPOSER: Dupree PROPOSAL TITLE: Wind Evolution in the Eta Cha Association FUSE spectra of 2 accreting T Tauri stars reveal similar asymmetric profiles of O VI 1032AA indicative of fast winds. Since one star is observed pole-on and the other observed at high inclination, this important result indicates that the winds are not highly collimated from the pole but originate from the whole Cha and EO Cha, are needed (a) to test whether the O VI emission flux results from accretion, or from the enhanced magnetic activity in a young star, (b) to determine whether massive winds vanish in young stars, once the accretion stops, thus giving credence to an accretion-driven wind in the classical T Tauri stage, and (c) to assess the presence of mass loss in the young Sun. The Category B targets, also in the Eta Cha association, will determine O VI emission and wind characteristics of an extreme accretor and a transition object experiencing disk clearing. PROP ID: H069 PROPOSER: Long 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 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 common envelope 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 four WDMSs (HS1316+6747,GD,543, DE,CVn, and SDSSJ1724+5620) in order to accurately measure the effective temperatures, masses, photospheric abundances, and rotation rates of their white dwarf primaries. These observations will double the number of well-observed WDMSs in our ongoing FUSE programme, and will result in a sufficiently large sample for a detailed assessment of the evolutionary state of these stars. PROP ID: H070 PROPOSER: Iping PROPOSAL TITLE: Search for O VI Emission from the Shocked Ring of SN1987A We propose to observe sna to measure the O VI flux from the shock interaction zones produced by the collision of high-velocity supernova ejecta with the dense inner circumstellar ring. Since the shock interaction with the inner ring began in 1997, broad (FWHMsim300 kms) emission from optical coronal lines (e.g. Fe X, Fe XI, and Fe XIV) has emerged and increased exponentially in strength. O VI 1032-1038 emission is expected to track the coronal lines. O VI is also expected to be the primary cooling transition for the million-degree shocked gas. A measure of the O VI line strength will significantly improve current models of the shock interaction. Earlier attempts to detect broad O VI from sna were inconclusive due to spectral contamination from two early-type stars within a few arc seconds of the SN. The proposed observation will use the narrowest FUSE slit (HIRS) to significantly reduce this effect. PROP ID: H074 PROPOSER: Smith PROPOSAL TITLE: The transition to outflows among bright giants The aim of this proposal is to address a specific question concerning the incidence of winds among giant stars Do outflows in the transition region TR) occur among Luminosity Class II (LC II) bright giants of spectral types late-F through early-K The incidence of winds in such stars is significant for a number of reasons : i) LC II stars in this range of spectral type fall just faintward of a region in the H-R diagram within which circumstellar ionCa2 is detected. As such they may be in states of mass loss prior to, or in lieu of, the development of a cool wind. ii) Their chromospheric ion: Mg 2 emission profiles often show no evidence of outflow, thus if winds are present they must accelerate with altitude. iii) They may be relevant to the mechanism by which Population II red giants, which have --2.7 < Mv < --1.7 and similar effective temperatures, lose mass prior to becoming horizontal branch stars. High-altitude TR emission lines are well suited to test for accelerating winds. FUSE covers the key O 6 lambda1032 line that arises from altitudes where temperatures are sim 3 times 10^5 K, which is hotter than for TR lines typically observed by IUE and HST. Dupree et al. (2005) found evidence for wind opacity in the lambda1032 ionO6 line among a small sample of evolved giants observed with FUSE, but this only includes one LC II star, the relatively active binary beta Dra (B-V 1.0). We propose to analyze the O 6 lambda1032 and ion C 3 lambda977 line profiles for two single LC II giants of color B-V 0.8 and 1.2 in order to test more generally for the incidence of hot outflows among such stars. PROP ID: H076 PROPOSER: Bregman PROPOSAL TITLE: The Detection of Hot Gaseous Halos Around 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, is nearly black, which occurs only if the hot gas is optically thick and on the near side of the bulge. This absorbing gas, near 3E5 K, is either due to a bulge cooling flow or a galactic fountain-driven halo. We can determine if such hot halos are common around normal spirals, and distinguish between the two models through observations toward additional normal spiral bulges, as hardly any have been observed with FUSE. PROP ID: H078 PROPOSER: Savage PROPOSAL TITLE: Physical Conditions and Baryonic Content of the Highly Ionized IGM A FUSE snapshot observation reveals that HE,0153-4520 (z_ QSO0.451) is the third brightest moderate redshift (z>0.4) QSO at FUV wavelengths. Our proposed 200ksec integration provides an outstanding opportunity to add to our knowledge of the highly ionized IGM. The spectrum will cover redshifted EUV lines of OII, OIII, OIV, NIV, and NeVIII in addition to FUV lines of HI, CII, CIII, NII, NIII, OI, and OVI. Even though the existing data only have an SN ratio of sim5, we already find some interesting absorption line systems toward HE,0153-4520. Access to a range of ion states is crucial for determining the physical conditions, ionization and origin of IGM absorption-line systems, allowing 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: H079 PROPOSER: Howk PROPOSAL TITLE: Peering through the LMC -- Feedback in the Nearest Disk Galaxy The Large Magellanic Cloud (LMC) is the closest gas-rich disk galaxy to our own Milky Way. It has been the focus of intense study by FUSE and other instruments in a quest to better understand feedback processes in such galaxies. The feedback of energy and matter from massive stars has created a gaseous halo about this galaxy, revealed by FUSE observations of ovi toward stars in the LMC. Toward the LMC, absorption from ovi and strong low-ionization lines can be found over a velocity range -50 la v_: LSR la +350 kms. Our recent analysis of FUSE and STIS observations of the LMC suggests that much of the material at v_: LSR ga +100 kms is actually associated with the LMC. If truly associated with the LMC, this material is moving away from its disk at velocities in excess of the escape velocity and potentially represents a galactic wind. We propose to study this putative LMC wind and the general ISM of the LMC by observing a Seyfert galaxy (CALF, aka RXJ0503.1-6634) that lies behind the optical disk of the LMC, allowing us to probe gas throughout the potential of the LMC. We will also observe a WR star within the LMC projected sim7arcmin (100 pc) from CALF. With these observations we will 1) study the total column density of warm and hot ionized gases in the LMC, determining if the background sight line probes a significantly increased column compared with the stellar sight line; 2) study the kinematics of the low, intermediate, and high ionization gas to search for evidence of a two-sided wind coming out of the LMC; and 3) compare the outflow structure and kinematics with observations of outflows from starburst and distant star forming galaxies. Our observations will provide a unique legacy for FUSE, providing the only measurements of an entire path through the LMC. PROP ID: H080 PROPOSER: Lehner PROPOSAL TITLE: Origin and Structure of the Magellanic Bridge The Magellanic Bridge is a massive component of the nearby interacting Magellanic system. It joins the Small and Large Magellanic Clouds (SMC, LMC) forming a filament of gas with on-going star formation. It is an unique feature enabling detailed studies of tidal interaction between galaxies and star formation in a low metallicity environment. According to stellar studies, the Magellanic Bridge abundance is a factor 3 deficient with respect to the SMC. However, this contradicts the current numerical simulations predicting that the Bridge gas was pulled mostly from the SMC some 200 Myr ago during a close encounter with the LMC. An independent estimate of the present-day metallicity of the Magellanic Bridge is required to constrain spectra (SN,sim15 per 20 km resolution element) of ESO,31--8, a Seyfert galaxy situated behind the Bridge near the SMC. This is the only probe of the Bridge useful for gas-phase abundance. We will study the chemical abundance ratios, physical conditions, chemistry, and kinematics of the Magellanic Bridge. We will compare these Bridge properties with those derived along other lines of sight within the Bridge and Magellanic System in order to further discern the Bridge chemical history and interactions between the Magellanic complexes. Our proposed observations will be compared to higher-redshift absorbers such as the Lyman Limit systems or sub-DLAs observed in distant QSOs to determine whether or not galaxy interactions may produce the observed gas in these high redshift systems. PROP ID: H083 PROPOSER: Herczeg PROPOSAL TITLE: Accretion, outflows, and disk dissipation in FUSE spectra of CTTSs We propose to observe a range of CTTSs with FUSE to understand the structure of the accretion shock, estimate its contribution to disk photoevaporation, and analyze wind heating mechanisms. The ionO6 doublet, a unique tracer of 3times 10^5 K gas, will constrain the temperature structure of the shock. We can then use that temperature structure to indirectly infer the EUV emission from CTTSs, which may lead to substantial disk photoevaporation. H_2 absorption lines seen against O 6 emission will help to determine the hydrogen column density to the stars. The hydrogen column density measured from FUV spectra can then be compared with similar X-ray measurements, which appear to be discrepant for TW Hya. The strength of any ionN2 and ionFe3 wind absorption, relative to ionN1 and ionFe2, respectively, will determine whether the ionization equilibrium in the wind is controlled by photoionization or collisions. PROP ID: H084 PROPOSER: Massa PROPOSAL TITLE: Structure in the fast winds of PN central stars proposal site. We propose to secure two 18ks observations of the central star of the planetary nebula (CSPN) NGC6826 in order to study the structure and variability of its fast wind. Together with archival observations of IC2419 and pending observations of NGC 6543 (program F034 scheduled for 5 Sept. 2006) this observation will complete the first set of UV data suitable for probing the wind activity in CSPNs on key characteristic timescales, ranging from several hours to the mooted rotation periods sim 1 day). All of these stars have variable fast winds (based on the fragmented archival exposures), and they are also periodic photometric variables. This study will provide new constraints on the inhomogeneous and structured nature of the fast CSPN winds with a range of terminal velocities, and enable us to compare their winds to each other and to those of massive stars. Results from this study will provide information on (i) the role of fast winds in shaping the nebula, (ii) the origin of X-ray emission within PNe, and (iii) the nature of radiation-pressure-driven outflows through comparisons of the structures seen in CSPN winds to those in massive star winds. PROP ID: H085 PROPOSER: Paerels PROPOSAL TITLE: The Nature of the White Dwarfs in Hard-X-ray Symbiotics Although most symbiotic stars produce only soft X-ray emission, hard X-ray emission greater than 50 keV has recently been detected with INTEGRAL and Swift from several exceptional symbiotic stars. These objects are members of a subclass of symbiotics characterized by rapid optical flickering. This flickering subclass may also contain high-mass white dwarfs (WDs) headed toward supernova Type Ia explosion. However, the basic underlying properties that make these these accreting WDs different from those in other symbiotics are not known. Very little observational data in the UV range exist for this new class of objects. Since the far-ultraviolet regime gives the best view of the hot WDs in symbiotic stars and their immediate environs, FUSE observations will help us determine the nature of these objects - i.e., whether the WDs are indeed massive, whether they are magnetic as is the case for hard X-ray emitting cataclysmic variables), whether they are jet-producing, or whether they have some other feature that distinguishes them from other symbiotic stars. We propose to perform FUSE observations of the hard X-ray symbiotics RT Cru, CD-573057, and CH Cyg. The properties of these hard X-ray symbiotics may hold the key to the signatures of magnetism in symbiotic stars, how the WDs in some symbiotics can grow to large masses, and the nature of jets and jet production in accreting WDs. PROP ID: H087 PROPOSER: Massa PROPOSAL TITLE: Silicon wind lines in late O and early B supergiants We intend to address the issues of mass loss and clumping in OB star winds by observing a unique combination of resonance and excited state wind lines in 9 O9.5 -- B0 supergiants. The lines we propose to study are the Sisc ivlambdalambda 1393, 1400 resonance doublet (observed by iue and hst) and the sielambdalambda1122, 1128 excited state doublet, available only to fuse. What makes this pair unique is that sielambdalambda1128 is excited by Si: sc iv lambdalambda 400 (all other excited state wind lines are populated by resonance lines below 912AA). Stars in the very narrow spectral range we propose to observe have sie excited state lines that are clearly affected by a stellar wind situation allows us to test whether the excited state lines, and the assumptions used to predict their strengths, agree with the results obtained from the resonance lines. If so, then we can confidently use the excited state lines to infer mass loss rates in stars whose resonance lines are strongly saturated. In addition, we discuss how highly structured (clumped) winds can cause the ratio of the excited state to resonance line strengths to be larger than expected. Thus, if the two doublets yield consistent results, this provides an independent constraint on the nature of clumping in the winds of OB stars. PROP ID: H088 PROPOSER: Guinan PROPOSAL TITLE: The Secret Lives of Cepheids The major aim of this proposal is to solve an important puzzle that we have recently uncovered in the examination of FUSE spectra of two nearby cepheids. This study will have a major impact on understanding the structure, heating, dynamics and possible magnetic activity of Cepheid (and related Hybrid Star) atmospheres. This program focuses primarily on 3 bright Cepheids -- Polaris (F7 Ib--II; 132.28-pc; P 3.98-d), beta Dor (F6 Ia; 349-pc; P 9.84-d) and delta Cep (F5 Iab; 273-pc; P 5.37-d). These cepheids are bright and located at high absolute declinations, thus having large amounts of available FUSE exposure times. Previous FUSE spectra of Polaris and beta Dor show the presence of strong C sc iii 977AA, 1176AAemission lines as well as the O sc vi 10321038AAemission doublet, indicating the presence of 50,000--300,000 K plasma in their extended atmospheres. Surprisingly, the four spectra of beta Dor available from the FUSE archive show significant variations in the C sc iii and O sc vi emission lines that appear to be correlated with pulsation. Unfortunately, only one Polaris FUSE spectrum is currently available, and there are currently no observations of the Classical Cepheid prototype delta Cep. We propose a multi-visit program (4 visits -- Polaris; 3 visits -- beta Dor; 4 visits -- delta Cep; 18--20-ksec each) to secure FUSE spectra sampled over their respective pulations. We have extensive observational material on Polaris. Recently we observed Polaris with Chandra (PI Evans) and found Polaris to be a very soft X-ray source (log L_ x 28.8 ergsec with virtually no counts above 1 keV). More X-ray observations are planned to discern whether the X-rays originate from the Cepheid itself or a ^ th mag dF5 companion. FUSE is ideally suited for this study because the FUV contains important diagnostic lines uncontaminated by the F-stars strong UV continua. FUSE also provides crucial information on the emission line fluxes, line profiles, and possible Doppler shifts that can be used to discern wind-driven mechanisms from magnetic activity effects. PROP ID: H092 PROPOSER: Kaiser PROPOSAL TITLE: Probing the Origin of High-ionization Emission Lines in AGN with BLRGs Radio galaxies with broad, double-peaked Balmer lines (BLRGs) occupy an important niche in our understanding of active galaxies because their profiles suggest that the emission occurs in the accretion disk. Observations in the UV, however, reveal that the high-ionization lines are not always double-peaked, implying perhaps that they are emitted in a weak wind. The ionO6 line, observable by FUSE in low redshift BLRGs, offers an important probe of the high-ionization line emission. The profile yields information about the kinematics of the line emitting region; the ratio of the ionO6 line with other high-ionization lines yields information about the ionization state and abundances in the emitting gas. Yet, despite the great promise that FUSE observations of BLRGs harbor, only one has been observed so far. We propose observations of three of the brightest double-peaked BLRGs that also have supporting UV spectra. Included in our sample is the prototype double-peaked BLRG 3C390.3. It harbors a massive black hole (M_BH,,2.9times,10^8M_sun) and exhibits a low accretion rate (.M.M_Edd,,0.02). Thus, 3C390.3 presents a test of the extreme end of Eigenvector 1, which is believed to be related to the fraction of the Eddington luminosity at which the object is emitted. PROP ID: H094 PROPOSER: Peters PROPOSAL TITLE: Elemental Abundances for the Iron Group in Early B Stars in the Large Magellanic Cloud From FUSE data obtained in earlier cycles, we are mapping the abundances of the Fe group elements in the Magellanic Clouds directly from the analyses of photospheric spectra of early B stars using the technique of spectrum synthesis. But currently we have spectra of only three B stars in two OB associations (NGC1818-D1, NCG2004-B15, and NGC2004-B30). To supplement these data, we propose FUSE observations of two additional sharp-lined main-sequence early B stars (LH10-3270 and LH104-39) that reside in other LMC regions. Both objects have significantly younger ages than the LMC stars that we have already studied and are sufficiently isolated and bright enough for FUSE observations with the LWRS aperture. The FUSE spectral region contains numerous lines of ionV3, ionCr3, ionMn3, and ionFe3, but the optical region is almost devoid of measurable features of these species. The abundances will be compared with those obtained from the interstellar gas and A supergiants. The FUSE observations will allow us to assess the chemical evolution of the LMC and the past history of Types Ia and II supernovae across this galaxy. PROP ID: H096 PROPOSER: DeWarf PROPOSAL TITLE: FUV Activity Cycles in the alpha Cen proposal site. Since 1990 we have been engaged in the Sun in Time project -- a program of coordinated multiwavelength observations of solar-type stars. These stars have been selected as proxies for the Sun at stages throughout its main-sequence lifetime, and are single, main-sequence G0-G5 stars of ages from sim70 Myr (representing the ZAMS Sun), to stars of approximately solar age, like alpha Cen A, together with older solar analogs with ages up to sim8.5 Gyr. These stars all have similar physical properties mass, radius, temperature, and depth of convection zone), differing only in age, or equivalently, rotation period. Specifically, we use these stars to investigate the decline in the level of solar magnetic activity as the Sun spins down, and also changes in the activity cycle with age. An important component of this Sun in Time project is the investigation of magnetic activity cycles that occur within these solar proxies, and the changes in the high energy coronal and transition region emissions. Recently, X-ray emission fluxes for one of our program stars, alpha Cen A, was observed to diminish by a factor of sim25 in only two years time, a phenomenon never before observed for any solar-aged star. The XMM observations imply that the chromospheric through coronal regions of alpha Cen A can be highly variable, with changes in both mean temperatures and the emission measures necessary to address these recent observations. We propose here to observe alpha Cen three times during Cycle 8 to delineate the evolution of this unprecedented, very deep magnetic inactivity state of this solar-type star. These new observations will be compared to the previously existing Cycle 2 spectra secured before this dramatic magnetic drop began, and the recent Cycle 7 observations obtained shortly after its X-ray minimum. We find that in this short span of five years alpha Cen A has exhibited a significant drop of approximately 2.5-3times in the key FUV emissions, which may indicate an activity cycle. PROP ID: H098 PROPOSER: Crowley PROPOSAL TITLE: Further Eclipse Mapping of Symbiotic Binaries For the majority of red giant stars the basic mass-loss processes at work are unknown. Indeed, for stars of spectral types between K0 III and M5-M6 III, much remains unknown about the regions above the visible photosphere and the transportation of the processed material outwards to the ISM. Theories and models are in need of observational constraint, and in particular it is vital to resolved information throughout the wind acceleration region within a few giant radii of the stars photosphere. Eclipsing symbiotic binary systems, consisting of an evolved giant in orbit with a white dwarf, provide an opportunity to take advantage of the finite size of the hot component to probe different levels of the chromosphere and wind acceleration region in absorption. This provides spatially resolved thermal, ionization and dynamic information on the wind which can then be compared against predictions of hydrodynamical stellar atmosphere codes. We propose FUSE observations of 2 eclipsing symbiotic systems, utilizing the 60 day periodicity inherent in FUSE scheduling to phase space the observations. Results will be compared to PHOENIX wind models and also to a successful analysis of other eclipsing systems (EG And and BF Cyg with FUSE) with different binary and giant parameters, with a view towards constraining the wind acceleration and chromospheric models. PROP ID: H099 PROPOSER: Peters PROPOSAL TITLE: The Abundances of the Iron Group Elements in Early B Stars in the Magellanic Inter-Cloud Region We propose FUSE observations of two sharp-lined main-sequence band early B stars that reside in the bridge region between the Large and Small Magellanic Clouds, to determine the abundances of the Fe group elements in these objects. From data obtained in earlier FUSE cycles, we are mapping the abundances of the Fe group elements in the Magellanic Clouds directly from the analyses of photospheric spectra of early B stars using the technique of spectrum synthesis. To compare the abundances in the LMC and SMC with those in their bridge, we are proposing FUSE observations of two early B bridge stars (DI1162 and DI1239) that have been found suitable for abundance analyses. Ground-based spectroscopic studies of these and two other objects have suggested extreme metal deficiencies in the Inter-Cloudbridge that are lower than those that prevail in both Magellanic Clouds and more than 1.0 dex smaller than in our galaxy. Unlike the optical region that is devoid of measurable lines from most Fe group ions, the FUSE spectral region contains numerous ionV3, ionCr3, ionMn3, and ionFe3 features. The FUSE observations will allow us to assess the chemical evolution of the bridge, that is believed to have been formed from a recent close tidal encounter between the SMC and LMC, and the past history of Types Ia and II supernovae in the region. PROP ID: H107 PROPOSER: Smith PROPOSAL TITLE: A Far ultraviolet observation of the unusual OB binary system NGC346-013 NGC346-013 is a peculiar binary discovered by the recent VLT-FLAMES Survey of Massive Stars. The primary is an early B-type star. Optical spectra of the He,II 4686AA line disclose two components, one arising from the secondary star that moves in anti-phase with respect to the primary and which further suggests that the optical secondary is both hotter and more massive than the primary. The flux from the secondary will significantly dominate in the FUV, so we propose FUSE observations of this object to determine the nature of this puzzling object. The FUSE spectra will be used to constrain the temperature and chemical abundances of the secondary as well as offer insight into the structure and intensity of any wind outflowmass transfer. Once both components are characterized, we will explore plausible evolutionary scenarios for this unique system. PROP ID: H110 PROPOSER: Wahlgren PROPOSAL TITLE: Synoptic study of the eruptive symbiotic AG Dra We propose to observe the eruptive S-type symbiotic star AG Dra -- which is the strongest supersoft x-ray source among these systems -- at intervals of four months to sample the far ultraviolet spectrum at five phases spanning the binary orbital period and to be coordinated with groundbased spectrophotometry. The FUV spectrum, which is dominated by the white dwarf (WD), has only sporadically been observed and only at quiescent phases, yet shows variability in the strengths and profiles of both the slow K-star wind and fast WD-outflow emission lines. The orbital modulation of the FUV spectrum has never been investigated nor has the WD wind been systematically monitored. Such monitoring is particularly important for providing information about the collision zone between the two winds and the accretion rate of material onto the WD that powers the luminosity and outbursts. The proposed FUSE observations will be part of a multiwavelength campaign to observe an anticipated major eruptive event for AG Dra that occurs approximately every 14 years. The next major eruption is likely to occur during 20072008, during the upcoming FUSE cycle; such an event for AG Dra has never been recorded at FUV wavelengths, where the bulk of the emission is expected to occur. In the event of a strong outburst we also propose a target of opportunity observation, to be made within the first month following maximum brightness. FUSE will be the only source for UV spectroscopy during this event, it is important to be able to correlate flux variations with those recorded at optical and infrared wavelengths, as for example the O VI lambda1032 line flux with known Raman scattering feature at lambda6825. These data will also be crucial inputs to our photo-ionization modeling to study the excitation and dynamics of the system as it evolves through the outburst. PROP ID: H111 PROPOSER: Ghavamian PROPOSAL TITLE: Collisionless Shock Physics in Fully Ionized Gas The existing FUV observations of non-radiative collisionless shocks have all focused on SNR blast waves propagating into partially neutral gas, identified by faint optical filaments dominated by hydrogen Balmer line emission. Multiwavelength studies of these Balmer-dominated objects suggest that the electron to proton temperature ratio T_eT_p at the shock transition declines as v_Shock^,,,-2, a tantalizing result which we have interpreted in terms of a simple plasma wave heating model. However, the vast majority of non-radiative, collisionless astrophysical shocks propagate into fully ionized gas. We cannot extend our model to these cases unless we know what role, if any, is played by the presence of partially neutral gas in equilibration at the shock fronts of Balmer-dominated SNRs. To clarify this issue, we propose FUSE observations of the Magellanic Cloud supernova remnants SNR 0534-69.9, SNR 0103-72.6 and SNR 0049-73.6, three remnants exhibiting non-radiative shocks in fully ionized gas. Combined with the Chandra observations, the OVI emission line widths and fluxes from these SNRs will enable us to make the most direct measurement of temperature equilibration in fully pre-ionized shocks. A comparison against our results from Balmer-dominated SNRs will provide invaluable insights for applying our equilibration model to more general collisionless shocks in SNRs, superbubbles and galaxy clusters. PROP ID: H901 PROPOSER: Bianchi PROPOSAL TITLE: Understanding Late Stages of Stellar Evolution; FUSE Survey of post-AGB Objects We propose to observe with FUSE a representative, UV-selected sample of post-AGB objects with the goal of clarifying some important issues in the late stages of intermediate-mass star evolution, including the abundance of neon, which has broad implications for the born-again scenario and yield of chemical elements, and the fading of supersonic winds when the hot late-post-AGB stars enter the WD cooling sequence. FUSE spectra, with corollary data at longer wavelengths, will uniquely enable precise determination of stellar parameters, especially Teff, mass loss (when present), and some abundances. FUSE spectra will also reveal possible circumstellar molecular hydrogen, yielding additional clues to the previous (red-giant) phases. Observations of binary systems will shed new light on evolutionary sequences predicted theoretically but which have previously been difficult to explore. The results are relevant in the context of stellar evolution but also of galaxy evolution, since these objects play a major role in the chemical enrichment of the ISM and their parent galaxy. The sample also includes sdB stars, which are thought to be the cause of the UV upturn in elliptical galaxies. The GALEX UV Sky Surveys provided the first unbiased and possibly complete census of such objects in the Milky Way (Bianchi et al. 2006a), that are elusive in optical surveys because of their high temperatures (to which optical colors are insensitive) and low optical luminosities. Targets for this proposal were chosen from our UV-selected catalogs (including WD, SD, PG1159 stars) to cover a range of physical parameters. In addition to our science goals, the sample will also augment the FUSE archive with new sight-lines for ISM studies. PROP ID: H902 PROPOSER: Dupuis PROPOSAL TITLE: The Spectral Evolution of Hot DA White Dwarfs Gravitational settling at the surface of white dwarfs is responsible for the purity of their atmospheres. Along their cooling phases, though, white dwarfs experience diffusion processes that prevent the downward diffusion of elements heavier than hydrogen. The goal of the spectral evolution theory of white dwarfs is to identify which mechanisms operate in the atmospheres of these stars, study their interactions, understand the abundance patterns, and constrain the stellar structure. We propose to pursuit our survey of hydrogen-rich atmosphere white dwarfs in order to build a representative sample of white dwarf spectra that can be compared to diffusion models. The selected stars in this proposal sample a wide range of effective temperatures and surface gravities that cover a cooling sequence from T_ eff approx 60,000K to 20,000K. FUSE is the only observatory that can probe with an unprecedented sensitivity the metallicity of the atmosphere of hot white dwarfs. PROP ID: H903 PROPOSER: Godon PROPOSAL TITLE: FUSE Survey of Nova-likes Characterizing the hot component The white dwarfs (WDs) and their accretion diskcolumn in cataclysmic variables (CVs) are probes of cataclysmic evolution and accretion physics, they bear the thermal, chemical and rotational imprint of their long term accretion and thermonuclear history. An understanding of the consequences of accretion in CVs is the first step in a global understanding of accretion-related phenomena throughout the universe including Young Stellar Objects, galactic binaries (accretion onto neutron stars and black holes) and AGN, which cant be easily observed. We propose a FUSE survey of 16 Nova-likes (NLs) systems (a sub-class of CVs) to characterize their hot component in the FUSE spectral range. These systems have not been studied in detail and little is known about their accreting WD : only approxhalf have a known period, only 3 have a STIS spectrum, and the classification of some is uncertain. We propose to determine the WD surface temperature, gravity, rotation rate and composition and probe their innermost disk accretion flowscolumn by applying multi-component synthetic spectral analyses to the FUSE data. We will use photometry to look for periodic signals in the FUSE time-tag data of the brightest targets that could be due to the spin or orbital periods of the systems. PROP ID: H904 PROPOSER: Iping PROPOSAL TITLE: Completion of the FUSE-IUE Survey of Galactic Early-Type Stars We propose a fuse Survey program to complete the sample of high-declination Galactic O and B stars previously observed in high dispersion in the 1150-2000 AA region with the iue satellite. About 1200 such stars were observed with iue across the entire sky, 363 of which are located at deltage 50^circ. About 180 have previously been observed by fuse, but 97 of these high-declination early type stars are within the fuse brightness limit and remain unobserved in the far ultraviolet. An archive of 900-2000 AA OB star spectra at 15-30 kms resolution is an invaluable resource for stellar population synthesis of galaxies, studying star formation in distant galaxies, interstellar abundance measurements, providing comparison stars for interstellar extinction studies and for peculiar objects or binary systems, studying the effects of temperature, gravity and metallicity on stellar UV spectra, and as a teaching aid. We propose to complete this sample of Galactic early-type stars in order to provide a stellar library as complete as practical, which will be available for astronomical research by the scientific community long into the future. The program stars covers a wide range of spectral types (WR, O, B0-5) and luminosity (V-Ia) and a sufficient number of stars to improve the calibration of effective temperature, gravity, and metallicity in a given spectral type-luminosity class combination. PROP ID: H905 PROPOSER: Smith PROPOSAL TITLE: A Complete Archive of Far-UV Spectra for B III-V Stars Because of their repsective instrumental constraints, there has been remarkably little overlap sharp-lined OB stars observed spectroscopically by both FUSE and IUE satellites. In this survey program of some 17 stars, we propose to more than double the sample of B stars near the main sequence that will have been observed in both the far-UV and the middle-UV. We outline the types of scientific investigations that can be conducted from spectra of B,V stars, ranging from the study of individual Galactic stars, including the structure, chemical composition, and kinematics of their atmospheres, to the population syntheses of highly redshifted galaxies. PROP ID: H906 PROPOSER: Desert PROPOSAL TITLE: Search for aurorae in close-in giant extra-solar planets and interactions with their hosting stars We propose to study the interactions between known extra-solar planets and their hosting stars. We will tackle this challenging subject by using two different approaches. Firstly, we propose to look for auroral emissions (e.g., H_2 and H,sc i lines) in the spectra of stars hosting known extra-solar planets. Secondly, the same sets of spectra will be used to analyze the modulation of the stellar emission lines as a function of the planetary orbital phase. The detection of extra-solar planets aurorae will provide a new and crucial step for understanding the structure of these extra-solar planets, and their relation with their nearby parent stars. Also, a mapping of planet-induced activity at varying stellar atmospheric depths will allow characterization and quantification of the physical interaction between the magnetically heated layers of the star and the planets magnetosphere. PROP ID: H907 PROPOSER: Brown PROPOSAL TITLE: An Extended Survey of Stellar Magnetic Activity on Young Stars Young stars have very high levels of stellar activity (e.g. UV and X-ray emission) that can strongly influence the formation and evolution of their protoplanetary systems. The high energy emission, both as radiation and particles, resulting from magnetic activity on the central star controls the thermal structure of disks, the formation process of planetesimals, and the photoexcitation and photoionization of protoplanets and young planetary atmospheres. The dwarfs of the Local Association, whose ages range from 7 Myr to 200 Myr, are a remarkable sample of young stars very close (typically nearer than 0 pc) to the Sun that permit the detailed study of the evolution of stellar activity. We propose a Cycle 8 Survey project to enlarge the sample of older Local Association dwarfs with measured transition region (100,000 K) emission line fluxes.