FUSE PI Team Science Program Abstracts This appendix summarizes the FUSE PI Team Science Program IDs, contact scientists, and program titles. This is followed by a text section with abstracts for each science program. FUSE PI Team Science Program Summary Listing Program ID Program Contact Program Title ----------- --------------- ---------------------------------------------- Major Programs P101 Sembach The Properties of Hot Gas in the Milky Way and Magellanic Clouds (Galactic Halo) P102/P122 Sembach The Properties of Hot Gas in the Milky Way and Magellanic Clouds (Galactic Disk) P103/P203 Sembach The Properties of Hot Gas in the Milky Way and Magellanic Clouds (Magellanic Clouds) P104/P204 Sembach Deuterium Abundances and the D/H Ratio (Local ISM) P105/P205 Sembach Deuterium Abundances and the D/H Ratio (Galactic Disk) P106 Sembach Deuterium Abundances and the D/H Ratio (Galactic Halo) P107/207 Sembach Deuterium Abundances and the D/H Ratio (Snapshot Survey) P108 Sembach Deuterium Abundances and the D/H Ratio (Extragalactic) P109 Sembach Deuterium Abundances and the D/H Ratio (Solar System) P110/P210 Kriss FUSE Studies of the Intergalactic Medium ------------------------------------------------------------------------------ FUSE Science Team Small and Medium Programs P111 Kriss Active Galactic Nuclei P112 Oegerle O VI in Cooling Flow Clusters P113 Sonneborn Circumstellar Interaction in SN 1987A P114 Blair Supernova Remnants P115 Shull Diffuse Molecular Hydrogen P116 Snow Molecular Hydrogen in Translucent Clouds P117 Hutchings Hot Stars P118 Linsky FUV Spectroscopic Survey of Cool Stars P119 Vidal-Madjar Circumstellar Disks P120 Feldman Solar System Objects P123 Sonneborn Supernovae as Probes of Galactic Halos ------------------------------------------------------------------------------ FUSE/Johns Hopkins Univ. Instrument and Operations Team Projects P131 Friedman Small-Scale Structure in the ISM P132 Kruk PG1159 Stars P133 Bianchi Planetary Nebulae Central Stars P134 Murphy Search for O VI Emission in the Halo of NGC4631 P135 Ake Epsilon Aurigae ------------------------------------------------------------------------------ FUSE/U.C. Berkeley Instrument Team Projects P151 Welsh Supernova Remnant Absorption Studies P152 Welsh Herbig Be stars P153 Griffiths Active Late-Type Stars P154 Siegmund Flare Activity in Cataclysmic Variable Systems ------------------------------------------------------------------------------ FUSE/Univ. of Colorado Instrument Team Projects P163 Wilkinson T Tauri Stars P164 Wilkinson Zeta Aur Systems P166 J. Green X-ray Binaries ------------------------------------------------------------------------------ FUSE Co-Investigator Projects P179 Dupree Atmospheres of Cool Star Binaries P180 Feldman Target of Opportunity Observations of Comets P184 Hutchings Stellar Winds and CVs P186 Linsky Transition Regions of PMS and Pleiades Age Stars P187 Malina Pulsar and CV Observations P191 Shull Lyman Break in Star-Forming Galaxies P192 Siegmund T-Tauri Stars P193 Snow Studies of IS and CS Gas and Dust P198 Vidal-Madjar Blue Compact Galaxy and CSPN ------------------------------------------------------------------------------ FUSE PI-Team Cycle 2 Programs P211 Green Monitoring Variable Active Galactic Nuclei P213 Sonneborn Circumstellar Interaction in SN 1987A P214 Blair Balmer Supernova Remnants in the LMC P215 Shull Two High-Extinction Stars in the LMC P216 Snow Molecular Hydrogen in Translucent Clouds P217 Fullerton Less Luminous Hot Stars in the LMC and SMC P218 Dupree Cool Stars P219 Vidal-Madjar Circumstellar Disks P220 Feldman Solar System Objects P221 Hutchings Far UV extinction curve in the SMC P222 Iping The ISM near eta Carina P223 Massa Phase-resolved spectroscopy of HD 5980 P224 Willis The Enigmatic WR Star HD 45166 P231 Andre O I Abundance and D/O P232 Hoopes The HII Region N44C P233 Catanzaro Magnetical chemically peculiar stars P234 Sankrit Extended Grid in the Northeast Cygnus Loop P235 Sonnentrucker H2, metals and DIBs in Reflection Nebulae P241 Lehner FUSE Observations of the Magellanic Bridge P242 De Marco Thermonuclear Runaways on Dwarf Novae P243 Hoopes WR Star AV336a in the HeII Nebula N76-A P247 Young 44i Bootis (HD 133640) P248 Young The Symbiotic Star AG Draconis P249 Andre HD in a Translucent Cloud P250 Roberge Circumstellar Disk Target HD 141569 P251 Oliveira D/O ratio toward WD2247+583 P252 Pellerin Young Stellar Populations and the Starburst-AGN Connection P263 Wilksinson Pre-Main Sequence Stars P267 Green Extragalactic Hot Gas along the MRK1383 sightline ------------------------------------------------------------------------------- FUSE PI-Team Cycle 3 Programs P203 Sembach The Properties of Hot Gas in the Milky Way and Magellanic Clouds (Magellanic Clouds) P204 Sembach Deuterium Abundances and the D/H Ratio (Local ISM) P205 Sembach Deuterium Abundances and the D/H Ratio (Galactic Disk) P207 Sembach Deuterium Abundances and the D/H Ratio (Snapshot Survey) P209/P309 Sembach Deuterium Abundances and the D/H Ratio (Solar System) P301 Blair D/H in the Vela-Puppis Region P302 Blair Expanded Sub-dwarf Program for Determining D/H P303 Williger Deuterium Abundances toward Hot Stars P304 Friedman D/H and O/H Toward Mu Col (HD 38666) P306 Kriss 1700+64 Followup P323 Sembach Supernovae as Probes of Galactic Halos ===================================================================================== Abstract listings: Major Program: The Properties of Hot Gas in the Milky Way and Magellanic Clouds The FUSE PI and Science Team will study the physical properties and distribution of hot gas in the interstellar media of the Milky Way and Magellanic Clouds through comprehensive absorption line studies of the O VI doublet and lower ionization lines in the FUSE bandpass. O VI is the best diagnostic of hot (log T = 5-6) gas in the ultraviolet spectral region. These observations will be covered under Team programs P101 (O VI Galactic Halo), P102/122 (O VI Galactic Disk), and P103 (O VI Magellanic Clouds). The Team D/H and O VI programs will share data. Note that the exposure times given in this NRA listing for sight lines toward hot stars in P101, P102/122, and P103 are appropriate for S/N ~ 30 at full resolution (0.03 A) at 1032 A. Extragalactic sight line integrations in P101 will have S/N ~ 12-30. D/H observations of some objects in the O VI program will be several times longer than the listed integrations. ------------------------------------------------------------------------------ Prog ID: P101 Title: The Properties of Hot Gas in the Milky Way and Magellanic Clouds (Galactic Halo) Program_contact: Sembach This portion of the O VI program will focus on understanding the character of the O VI absorption in the Galactic halo along sight lines toward stars and extragalactic continuum sources such as AGNs and QSOs. Regions to be explored include the Galactic poles, the inner Galaxy, and the outer regions of the Milky Way halo. The data obtained for this program will be integrated with existing information from previous space missions to provide a global picture of the hot gas content of the Milky Way halo. A portion of the time for this program will be used to make measurements of the O VI emission from the diffuse halo gas, though this is a secondary objective since such measurements depend sensitively on instrument performance. There will be a large amount of auxiliary information obtained as part of the O VI halo program. The Science Team will rely heavily upon these data to undertake additional investigations of the chemical composition and physical properties of the ISM, the properties of hot stars and their winds, and the far-UV continua and absorption line properties of AGNs and QSOs. Data from this program will also be used as a snapshot for determining which extended sight lines are best suited for follow-up studies of the D/H ratio. (See abstracts for programs P104, P105, P111, P115, and P117 for additional details.) ------------------------------------------------------------------------------ Prog ID: P102 Title: The Properties of Hot Gas in the Milky Way and Magellanic Clouds (Galactic Disk) Program_contact: Sembach This portion of the O VI program will focus on understanding the character of the O VI absorption in the Galactic disk at distances greater than ~ 1 kpc from the Sun. The survey will provide information for a statistical study of the O VI absorption properties as well as detailed studies of regions already known to contain hot gas through X-ray emission measurements (e.g., SNRs, radio continuum loops). Local interstellar medium data from the D/H program will be used to understand the properties of the hot gas in the solar neighborhood. There will be an additional "mini-survey" of several binary systems at multiple epochs to search for the presence of broad shallow O VI absorption due to very hot interstellar gas through a precise tomographic reconstruction of the stellar absorption in the vicinity of the O VI lines. The Team will also check for variability in the stellar O VI lines by observing several objects with a range of spectral types several times during the mission. There will be a large amount of auxiliary information obtained as part of the O VI disk program. The Science Team will rely heavily upon these data to undertake additional investigations of the chemical composition and physical properties of the ISM and the properties of hot stars and their winds. Data from this program will also be used as a snapshot for determining which extended sight lines are best suited for follow-up studies of the D/H ratio. (See abstracts for programs P104, P105, P115, and P117 for additional details.) ------------------------------------------------------------------------------ Prog ID: P122 Title: The Properties of Hot Gas in the Milky Way and Magellanic Clouds (Galactic Disk)--continuation Program_contact: Sembach Program P122 is a continuation of program P102. ------------------------------------------------------------------------------ Prog ID: P103/P203 Title: The Properties of Hot Gas in the Milky Way and Magellanic Clouds (Magellanic Clouds) Program_contact: Sembach This portion of the O VI program will focus on understanding the character of the O VI absorption in the Magellanic Clouds. Approximately 20 sight lines will be investigated in the two galaxies. The sight lines will include superbubble structures with strong X-ray emission and field positions with little X-ray emission. The hot gas properties of the LMC and SMC will be compared to those derived for the Milky Way. There will be a large amount of auxiliary information obtained as part of the O VI Magellanic Cloud program. The Science Team will rely heavily upon these data to undertake additional investigations of the chemical composition and physical properties of the ISM in the Milky Way and Magellanic Clouds, as well as the properties of hot stars and their winds (See abstract for programs P115 and P117 for additional details.) ===================================================================================== Major Program: Deuterium Abundances and the D/H Ratio The FUSE PI and Science Team will determine the abundance of deuterium and the D/H ratio in a variety of galactic environments through comprehensive absorption line studies of the D I and H I Lyman series lines in the FUSE bandpass. The sight lines studied will have varying degrees of metallicity and different evolutionary histories. Various metallicity markers (e.g., Oxygen, Iron) and ancillary ISM information (elemental abundances, physical conditions, and gas kinematics) will be integral components of all D/H analyses undertaken by the Team. The sky coverage of these observations will be maximized to the greatest extent possible. The D/H program encompasses Team programs P104 (D/H Local ISM), P105 (D/H Galactic Disk), P106 (D/H Galactic Halo), P107 (D/H Snapshot Survey), P108 (D/H Extragalactic), and P109 (D/H Solar System). ------------------------------------------------------------------------------ Prog ID: P104/P204 Title: Deuterium Abundances and the D/H Ratio (Local ISM) Program_contact: Sembach This portion of the D/H program will provide information for sight lines confined to the local interstellar medium to determine the extent to which the D/H ratio varies within a few hundred parsecs of the Sun. These observations will significantly increase the amount of information available for local deuterium abundance determinations and will enhance the information for the local interstellar medium available from earlier Copernicus satellite studies. Objects to be used as background sources include cool stars, white dwarf stars, the central stars of planetary nebulae, and a few A-type stars. Auxiliary uses for the data will include general ISM studies and a survey of hot gas within the Local Bubble. (See abstracts for programs P102/122 and P115 for additional details.) ------------------------------------------------------------------------------ Prog ID: P105/P205 Title: Deuterium Abundances and the D/H Ratio (Galactic Disk) Program_contact: Sembach This portion of the D/H program will provide information for sight lines that extend beyond the local interstellar medium of the Galactic disk. The sight lines covered will sample gas in spiral arm and interarm directions several kiloparsecs from the Sun. Most of the objects observed will be OB-type stars. Data from program P102/122 (O VI disk survey) will provide an initial far-UV observation of a large number of sight lines. Many of these sight lines will be re-observed for longer integration times (a factor of 3-5x) as part of this program. All of the P102/P122 sight lines should be considered potential candidates for this study. ------------------------------------------------------------------------------ Prog ID: P106 Title: Deuterium Abundances and the D/H Ratio (Galactic Halo) Program_contact: Sembach This portion of the D/H program will provide information for sight lines that extend into the Galactic halo. The directions to be studied include sight lines toward stars at the Galactic poles as well as toward stars in the inner and outer regions of the Galaxy. Most of the objects observed will be OB-type stars. Data from program P101 (O VI halo survey) will provide an initial far-UV observation of a large number of sight lines. Many of these sight lines will be re-observed for longer integration times (a factor of 3-5x) as part of this program. All of the P101 sight lines should be considered potential candidates for this study. ------------------------------------------------------------------------------ Prog ID: P107/P207 Title: Deuterium Abundances and the D/H Ratio (Snapshot Survey) Program_contact: Sembach This portion of the D/H program will provide short observations of many AGNs and QSOs to check far ultraviolet flux levels and suitability of the objects as background continuum sources for extended integrations. The data produced from this snapshot survey will be used extensively as part of program P111 to study the flux distribution and intrinsic absorption properties of the AGNs and QSOs observed. (See abstract for program P111 for more information.) The Team will also use this data for studies of extragalactic O VI and H I absorption at low redshift. ------------------------------------------------------------------------------ Prog ID: P108 Title: Deuterium Abundances and the D/H Ratio (Extragalactic) Program_contact: Sembach This portion of the D/H program will provide extended observations of extragalactic continuum sources for measurements of the D/H ratio in the distant Galactic halo, high velocity clouds, and low redshift (z < 0.3) absorption systems. These observations will provide unique opportunities to measure the deuterium abundance in places that are difficult to observe through absorption line studies of sight lines toward hot stars. Data from this program will be used by program P111 for high quality measurements of the far-UV continuum and absorption properties of AGNs and QSOs. (See abstract for program P111 for more information.) ------------------------------------------------------------------------------ Prog ID: P109 Title: Deuterium Abundances and the D/H Ratio (Solar System) Program_contact: Sembach This portion of the D/H program will focus on determining the D/H ratio on Jupiter. The observation will consist of several planetary limb pointings. The Jupiter D/H measurement will provide a reference value for the ratio at the time the solar system was formed about 5 billion years ago. ------------------------------------------------------------------------------- Major Program: FUSE Studies of the Intergalactic Medium Prog ID: P110/P210 Title: FUSE Studies of the Intergalactic Medium Program_contact: Kriss FUSE will provide an opportunity to explore absorption by He II in the intergalactic medium (IGM) over the redshift range z=2-3. The planned observations will measure the mean opacity of the IGM in coarse bins over this redshift interval to study the patchiness of the IGM over different lines of sight as a function of redshift. Deep observations of one or more candidate QSOs will attempt to resolve the He II Ly alpha forest. These observations will discriminate between discrete structures and distributed gas as sources of the He II opacity. Detailed comparisons of the He II forest lines and the H I Ly alpha forest lines will be used to determine the ionization state of the absorbing structures and the shape of the ionizing UV background spectrum. ===================================================================================== FUSE Science Team Small and Medium Programs Prog ID: P111 Title: Active Galactic Nuclei Program_contact: Kriss The nearest, brightest active galaxies have inspired our current vision of the AGN paradigm. These same galaxies have been imaged with HST, have the highest S/N HST and IUE far-UV spectra, and have the best X-ray spectra. Prime goals for FUSE observations are the shape of the far-UV continuum, the strength and velocity of the O VI emission line, strengths of other far-UV lines such as C III 977 and N III 991, and the prevalence of intrinsic absorption and Lyman limits. FUSE observations will resolve velocity structure in the O VI absorbing gas, and in any neutral hydrogen gas. Observations of Seyfert 2s (in addition to NGC 1068) will search for strong line emission in O VI, C III, and N III indicative of shock-heated gas. FUSE will also be sensitive to any molecular gas (visible as H_2 absorption) along the line of sight. In BAL QSOs, FUSE will be able to measure the absorption in the EUV transitions of high ionization ions such as Si XII. The detailed observations of selected objects in this program will supplement the more general surveys of AGN being used to explore O VI absorption and the D/H ratio in the galactic halo. ------------------------------------------------------------------------------ Prog ID: P112 Title: O VI in Cooling Flow Clusters PI: Oegerle We will search for the O VI 1032/1038 emission lines produced in the warm (300,000 K) intracluster gas in the cooling flow clusters A2597, A2199 and A1795. The existence of this warm component of the ICM has never been detected convincingly, although its presence is expected in the conventional models of cooling flows. These 3 clusters have strong cooling flows derived from their X-ray emission (>100 Msun/yr), as well as strong H-alpha emission from cool (10,000 K) gas in their cluster cores. Detection of the intermediate temperature gas at 300,000 K will provide a strong link between these temperature regimes, and important information on the thermal history of the gas in cooling flows. ------------------------------------------------------------------------------ Prog ID: P113 Title: Circumstellar Interaction in SN 1987A PI: PI: Sonneborn FUV emission from SN 1987A in the Large Magellanic Cloud will be observed to characterize the shock interaction between the high-velocity ejecta and circumstellar gas. We will attempt to observe O VI emission and the full blueward extent of the blue wing of Lyman-alpha, only part of which is observable with STIS because of the high expansion velocity of the ejecta (V>15,000 km/sec). Emission from recombination lines from the inner circumstellar ring may also be present. The nearest companion star (Star 3) will also be observed. ------------------------------------------------------------------------------ Prog ID: P114 Title: Supernova Remnants PI: Blair The FUSE Team Project on supernova remnants includes an absorption study of the young Type 1a SN remnant SN1006 and studies of selected filamentary emission regions in evolved galactic SNRs. Observations of the "Schweizer-Middleditch" star behind SN1006 will be used to search for a broad absorption from Fe III 1123, using FUSE's high dispersion to resolve contaminating stellar photospheric lines from the broad line. The presence of this line would indicate iron in the cool ejecta of the supernova. Observations of key, well-studied SNR emission filaments will be used to study different kinds of shock wave-ISM interactions, including nonradiative and radiative shocks, and thermally unstable regions. FUSE coverage of a range of ions and ionization stages at high spectral resolution will provide a unique capability to diagnose the thermal, chemical, and kinematic properties of these interactions. Observations of an X-ray bright region will be used to search for faint, high-ionization lines never observed previously in spectra of SNRs. ------------------------------------------------------------------------------ Prog ID: P115 Title: Diffuse Molecular Hydrogen PI: Shull The FUSE PI team will study interstellar H_2 absorption spectra of OB-stars in the Galactic halo, SMC, and LMC. The H_2 lines will be used to derive molecular abundances, the CO/H_2 and HD/H_2 ratios, rotational populations, rotational temperatures, gas densities, and UV radiation field in diffuse clouds. We will measure the molecular abundances, including CO/H_2 and HD/H_2, as a function of metallicity, and estimate the gas pressure (nT) in the low halo. We will also observe H_2 in planetary nebulae toward hot central stars. ------------------------------------------------------------------------------ Prog ID: P116 Title: Molecuar Hydrogen in Translucent Clouds PI: Snow The FUSE PI team will observe 31 stars which lie behind translucent clouds (i.e. clouds having total visual extinctions of around 2 magnitudes or greater), in order to determine the H_2 column densities (for all stars on the list) and the H_2 rotational excitations (for the brighter stars on the list). The total H_2 column densities will be applied to studies of gas-phase depletions and chemistry, while the rotational excitations will be used to analyze the physical conditions (e.g. cloud densities, temperatures, and radiation fields). In addition, the FUSE spectra will be used to determine far-UV extinction curves for the program stars, and data on lines of atoms and ions, as well as molecular transitions of species other than H_2, will be used in a comprehensive analysis of cloud abundances, depletions, and chemistry. ------------------------------------------------------------------------------ Prog ID: P117 Title: Mass Loss and Stellar Winds of Hot Stars PI: Hutchings This program is intended to a) enable modelling of stellar winds from FUSE spectra combined with HST/IUE range spectra, which will yield proper determination of the wind ionization balance. The program stars are selected mainly from the LMC and SMC and will be combined with the Galactic star sample from other programs, to b) enable a comparison of winds in stars with matched spectral type and luminosity in the 3 different environments, since abundance is known to be an important parameter in driving winds. Spectral types range through WR, and O3 to B2. Exposures are designed to provide a minimum S/N of 30 over 0.2 Angstroms; in many cases this is exceeded. ------------------------------------------------------------------------------ Prog ID: P118 Title: Spectroscopic Survey of Cool Stars PI: Linsky This program will obtain far-UV spectra of cool stars that span a broad range of spectral type and luminosity class. It is our intention to obtain these spectra early in the FUSE program and to provide the spectra quickly to the user community in order to guide potential guest investigators in designing their observing programs. The specific science objectives include: (1) studying transition region dynamics (winds and downflows), (2) modeling the thermal structure of transition regions, (3) measuring electron densities, (4) search for low temperature coronae, (5) studying molecular excitation and fluorescence processes, and (6) inferring how the transition regions of spectroscopic binary systems differ from those of single stars. ------------------------------------------------------------------------------ Prog ID: P119 Title: Circumstellar Disks Around Main-Sequence and Pre-Main-Sequence Stars PI: Vidal-Madjar The purpose of this program is to provide new insight on the signatures of circumstellar gas around main-sequence and pre-main-sequence stars. For some stars, the already detected gas may be the by-product of some activity (like evaporation and/or collision of kilometer-sized bodies) in a young planetary system in its clearing out phase. Spectroscopic variations observed around the targets stars (PMS, Herbig AeBe) present strong similarities with the already observed ones, but the origin of the circumstellar gas within these systems is still unclear. Detection of deuterium may help in identifying the origin of the gas. These observations are expected to allow the identification of the main form of the gaseous phase (H_2, CO, OI, NI, CII ?) and provide information on the ionization equilibrium of the zero radial velocity as well as of the accreting gas. Analysis of multiplet ratios will allow to probe the sizes of the inflowing gas structures. Also, in order to better understand the evolution of circumstellar gas from young stellar objects to main sequence stars, a few very young B-type stars are included as being members of a binary system with a T-Tauri companion. ------------------------------------------------------------------------------ Prog ID: P120 Title: FUSE Solar System Studies PI: Feldman H_2 emissions from both Jovian auroral regions measured with the high-throughput aperture (MDRS) will determine temperatures and self-absorption. Atomic H emissions from the bulge region measured by the high resolution aperture (HIRS) will determine the dynamics of the bulge and anti-bulge regions. The high-throughput aperture will be used to search for HD fluorescently pumped by solar Lyman-beta as well as to determine if there is a correlation of the H_2 Lyman and Werner bands with Lyman-alpha in the bulge region. The excitation of H_2 in the atmosphere of Saturn will be similarly studied. Io Torus emissions will be measured using the high-throughput aperture (MDRS) to determine ion velocity profiles and with the large science aperture to search for minor constituents. Observations of Venus will address the question of the atmospheric D/H ratio. ------------------------------------------------------------------------------ Prog ID: P123 Title: Supernovae as Probes of Galactic Halos PI: Sonneborn FUSE observations of a newly discovered, bright (V<14) core-collapse supernova (Types II or Ib) will be used to study interstellar properties of the sightline. The full range of interstellar species present in the FUSE wavelength range will be utilized to examine kinematics, depletions, and abundances of foreground gas, the Milky Way halo, the ISM of the supernova's host galaxy, and the intergalactic medium. Any data obtained from this program will be made available to other FUSE programs to study the properties of the supernova outburst. ===================================================================================== FUSE/Johns Hopkins Univ. Instrument and Operations Team Projects Prog ID: P131 Title: Small-Scale Structure in the ISM PI: Friedman The properties of the interstellar medium on scale sizes of about 1 pc are not well understood. Even as fundamental a parameter as the range of cloud sizes has not been measured properly. Some data suggest only weak opacity variations on scales of ~1 pc, and essentially none below 0.2 pc. Other data, especially in the UV and radio, suggest absorption line equivalent width variations as great as 25-50% toward targets with separations smaller than 3000 AU (~0.01 pc) at a distance of ~200 pc. The goal of this program is to observe closely spaced lines of sight toward spatially adjacent targets in an open cluster (NGC2264, distance=750 pc) in order to measure or place limits on various properties of clouds in the local interstellar medium. Among these properties are the sizes of the clouds and possible anomalous abundances. In addition, these observations may provide measures of metallicity and depletion gradients across the face of the cluster. ------------------------------------------------------------------------------ Prog ID: P132 Title: PG1159 Stars PI: Kruk The hot metal-rich hydrogen-deficient white dwarfs known as PG1159 stars provide a unique probe of the late stages of stellar evolution. Present theories of stellar evolution do not yet produce stars that match the properties of PG1159 stars. FUSE observations will provide improved data on the surface compositions of these stars; in addition, the O VI resonance line profiles will be searched for evidence of ongoing mass-loss. The long exposure on WD2117+341 is used to search for the effects of the pulsations on certain diagnostic line profiles. The 2000s exposure on HS2324 is a snapshot: if the spectrum shows sufficient flux then some time will be reallocated within the program. ------------------------------------------------------------------------------ Prog ID: P133 Title: Planetary Nebulae Central Stars PI: Bianchi Central stars of Planetary Nebulae (CSPN) are among the hottest stars in the H-R diagram. IUE and HST observations show that CSPN have significant supersonic winds and mass loss. Accurate measurements of the wind velocity and mass loss rate in CSPN are a crucial to test of whether current theories of radiation pressure accelerated winds apply to evolved, high gravity stars, and to understand the formation and evolution of the nebular shell, since the photons from the hot central star, and the momentum of its supersonic wind are responsible for the ionization of the visible nebula, and influence the dynamics of the expanding shell. IUE and HST data give only partial information about mass loss, since they can only observe the (often saturated) resonance lines of CIV, SiIV and NV. FUSE can observe wind lines in a greater spread of species and ionization states, especially the hot O VI 1032,1037 doublet, from which the wind ionization can be determined accurately. UV (IUE/HST) and optical spectra are already available for a consistent analysis of photospheric and wind lines. The line profiles will be analyzed with different methods (SEI, SSBAL, EMISSEI) to derive wind velocity, mass loss rate, gravity, temperature and luminosity. Moreover, measurements of the stellar continuum in the FUSE range will yield better determinations of temperature and luminosity, both because of the hot temperatures of the stars, and because nebular continuum emission contaminates the flux of CSPN longwards of about 1400 Angstroms, but drops drastically below 1300 Angstroms. Therefore, FUSE spectra of CSPN can help our understanding of mass loss mechanisms, PN formation and evolution (physical interpretation of the morphology), nebular ionization, and post-AGB evolution. ------------------------------------------------------------------------------ Prog ID: P134 Title: Search for O VI Emission in the Halo of NGC 4631 PI: Murphy We propose to look for the O VI 1032/1038 emission lines from hot gas in the disk and halo of the edge-on spiral galaxy NGC 4631. ROSAT observations of NGC 4631 clearly show a concentration of soft X-ray emission north of the galaxy's plane directly above an area of high star formation activity. The X-ray spectrum implies the presence of a soft X-ray gas component at a temperature of less than 1 million degrees. Since O VI is the best diagnostic of gas at this temperature in the FUSE bandpass, our measurements of the O VI emission strength will help us to understand the physical state, total content, and scale height of hot gas in the halo of NGC 4631. These quantities can then be directly compared to values derived for the Milky Way through the O VI Program. ------------------------------------------------------------------------------ Prog ID: P135 Title: Epsilon Aurigae PI: Ake FUSE will be used to study the nature of the unusual eclipsing spectroscopic binary, epsilon Aurigae. The most favored model of this system is that the secondary object is a large, cold disk seen nearly edge-on. IUE and GHRS observations indicate the existence of a far-UV excess compared to other A-F type supergiants, presumably from a hot star in the center of the disk. The main difficulty in interpreting the UV data is that the primary star still contributes significant flux down to 1400-1500 Angstroms. FUSE observations will perform a more direct examination of the secondary, free from contamination by from the photosphere of the primary star. Measurements will be made to determine the physical parameters of the central star, and study variability and gas motions in the disk. ===================================================================================== FUSE/U.C. Berkeley Instrument Team Projects Prog ID: P151 Title: Supernova Remnant Absorption Studies PI: Welsh We will observe 4 early-type stars in the line-of-sight towards the Monoceros Loop supernova remnant in order to investigate the dynamics, ionization state and elemental abundances of the disturbed, absorbing interstellar gas associated with the remnant. ------------------------------------------------------------------------------ Prog ID: P152 Title: Herbig Be stars PI: Welsh We will repeatedly observe 4 early-type Herbig Be stars which are thought to possess gaseous circumstellar disks. Our investigation will focus on the strong stellar FUV line profiles to determine the extent of time variability due to mass loss and accretion processes. We will also analyze the physical state of the molecular absorption lines sampled in the interstellar gas serendipitously observed in the line-of-sight to these objects. ------------------------------------------------------------------------------ Prog ID: P153 Title: Active Late-Type Stars PI: Griffiths We will complete repeated exposures of the active late-type RS CVn stars AR Lac and HR 1099, and perform an extended exposure of the G8V star Xi Boo A. We will obtain a better description of the transition regions of these stars by completing the full emission measure distribution and accurately measuring the plasma electron density. We hope to gain a detailed understanding of the connection between magnetic activity at the photospheric and transition region levels, and will search for solar-like coronal mass streamers using O VI (1032,1038 Angstrom) line profiles. ------------------------------------------------------------------------------ Prog ID: P154 Title: Flare Activity in Cataclysmic Variable Systems PI: Siegmund We will repeatedly observe one pre-CV and one normal CV eclipsing binary system to monitor the level of FUV flare activity that is routinely observed in these systems in other wavelength bands. We will observe the FUV emission from the surrounding gas disk and wind, the white dwarf companion, and a possible hot disk corona produced by EUV/X-ray radiation from the white dwarf that photoionizes and heats the disk surface. ===================================================================================== FUSE/Univ. of Colorado Instrument Team Projects Prog ID: P163 Title: T-Tauri Stars PI: Wilkinson FUV spectra of pre-main sequence (PMS) stars show high temperature emission lines from magnetically heated regions and excited molecular lines from the circumstellar environment. The FUSE region is still largely unexplored for PMS stars and contains unique diagnostics such as the O VI doublet, H Lyman lines, and the H_2 Lyman bands. Our targets are the Classical T Tauri star T Tau and the Herbig Ae star HD104237. T Tau shows a rich UV spectrum of a wide range of ionic and H_2 lines, while the UV spectrum of HD104237 shows wind-dominated emission lines below 1500 A. ------------------------------------------------------------------------------ Prog ID: P164 Title: Zeta Aurigae Systems PI: Wilkinson Zeta Aurigae/VV Cep eclipsing binary systems offer the most detailed method of studying mass loss from cool supergiant stars. The FUV continuum from the hot main-sequence secondary star provides a probe through the outer atmosphere and wind of the evolved primary star. The absorption spectra obtained will allow detailed investigation of the flow properties and ionization structure of these binaries, leading to improved mass-loss rates and wind energy budgets. ------------------------------------------------------------------------------ Prog ID: P166 Title: X-ray Binaries PI: J. Green Observations of bright X-ray binaries will be used to determine the physical conditions in the companion star's wind and the effects of the high energy spectrum on the wind environment. ===================================================================================== FUSE Co-Investigator Projects Prog ID: P179 Title: Atmospheres of Cool Star Binaries PI: Dupree The densities, mass motions, and emission measures will be evaluated for a selection of single stars and binary systems containing cool stars with various rotation periods to assess the effects of rotation upon the structure and energy balance of a stellar atmosphere. Most systems will be observed 3 times. ------------------------------------------------------------------------------ Prog ID: P180 Title: Target of Opportunity Observations of Comets PI: Feldman FUSE will attempt to determine the argon/oxygen ratio in a target of opportunity comet whose activity level and orbit are suitable for the observation. In addition, we will search for molecular hydrogen released directly by the cometary nucleus and for neutral and singly ionized nitrogen. These measurements will be normalized to a water production rate derived from the observed hydrogen Lyman series. ------------------------------------------------------------------------------ Prog ID: P184 Title: Stellar Winds and CVs PI: Hutchings Three stars in M33/M31 will be observed to study their stellar winds. The disk-dominated supersoft binary X-ray source 0513-69 in the LMC will be observed. Three CV binaries will be observed, with readouts at intervals which will sample their orbital and other variations. These targets are highly variable - maximum visible magnitude is given. ------------------------------------------------------------------------------ Prog ID: P186 Title: Transition Regions of PMS and Pleiades-Age Stars PI: Linsky The objectives of this program are to study the dynamics, thermal structure, and energy balance in the transition regions of young stars, including pre-main sequence and Pleiades age stars. The observations will address these questions by measuring the far-UV fluxes, line widths, and Doppler shifts of the O VI and other far-UV transition region lines. We will be studying some young A-type stars to determine whether their transition regions differ from those of cooler stars, and will analyze any flares observed in these young stars and a reference late-M star. ------------------------------------------------------------------------------ Prog ID: P187 Title: Pulsar and CV Observations PI: Malina PSR_0656+14: Measurement of surface thermal emission from neutron stars (NS) is essential to theories regarding the condensed matter state equation, the thermal evolution of NS, and of NS atmospheres. We propose to conduct 50 Ang band FUV photometric observations of PSR B0656+14, an X-ray, SXR and EUV bright isolated NS with an optical counterpart. FUV photometry will provide critical characterization of the NS's surface thermal radiation. Higher energy observations may be effected by poorly established effects including magnetized atmospheres, chemical compositions, temperature gradients and gravitational effects. Optical observations may be subject to non-thermal effects. V3885 Sgr: V3885 Sgr is one of the brightest nonmagnetic cataclysmic variables. We propose to observe V3885 Sgr for 5 to 6 contiguous FUSE orbits, achieving a S/N of about 12 at full resolution even at the troughs of the source's O VI absorption lines in each spectrum (assuming 2000 sec visibility per orbit). The primary purpose of the observations is to use the source as a bright continuum against which to study local interstellar absorption lines. Although observed on Malina's Co-I Program, the data will be analyzed in collaboration with members of the O VI Project. ------------------------------------------------------------------------------ Prog ID: P191 Title: Lyman Break in Star-forming Galaxies PI: Shull We will observe a blue, metal-poor, star-forming galaxy, Mrk 357 (z = 0.053) shortward of its (rest-frame) Lyman limit to measure or set limits on the Lyman continuum escape fraction. This fraction constrains the HI opacity and topology of gas layers in the parent galaxy and its halo, and it gauges the potential contribution of starbursts to the metagalactic (IGM) radiation field. A related goal is to use the spectrum longward of the Lyman limit for better understanding the star, dust and gas content of the galaxy. ------------------------------------------------------------------------------ Prog ID: P192 Title: T Tauri Stars PI: Siegmund We shall observe two relatively unobscured T Tauri stars to investigate the emission from accreting hot gas known to be present in these systems from previous IUE data. Observations of these emission processes will help in understanding the role of circumstellar disk gas in these pre-main sequence systems. ------------------------------------------------------------------------------ Prog ID: P193 Title: Studies of Interstellar and Circumstellar Gas and Dust PI: Snow Studies under this program fall into three distinct categories: (1) a detailed analysis, with enhanced S/N, of the spectra of two stars (HD 24534 = X Persei; and HD 23180 = o Per) for interstellar lines, with emphasis on weak molecular features and lines below 1000 Angstroms; (2) a study of absorption and emission in the spectra of three planetary nebula central stars; and (3) a search for UV diffuse bands as stationary features in the spectra of high- amplitude spectroscopic binaries. ------------------------------------------------------------------------------ Prog ID: P198 Title: Blue Compact Galaxy and CSPN PI: Vidal-Madjar IZW18 is known to be a blue compact galaxy presenting a very low metallicity. The purpose of this investigation is to search for H_2 in the context of such a low metallicity, probably dust free object. A high velocity cloud is also present along this line of sight. These observations will allow the precise evaluation of a much longer exposure to further study both the galaxy and the intervening high velocity cloud. Several programs can also be done simultaneously by observing the central stars of some bright Planetary Nebulae (PN): (a) The wavelength range is particularly appropriate to study the continuum, the temperature and the wind of the PNe central stars; (b) In addition to the stellar continuum, the spectra will yield information concerning the nebula; (c) FUSE will offer the possibility to detect molecular hydrogen lines in absorption against the stellar continuum. It should then be possible to determine how much additional H_2 is formed by shocks in the stellar winds. (d) Finally, the non-detection of deuterium should allow a direct check of its evolution within stars since these PN were selected for their different 3He environment. ===================================================================================== FUSE PI Team Major Programs for Cycles 2 and 3 Prog ID: P203 Title: The Properties of Hot Gas in the Milky Way and Magellanic Clouds (Magellanic Clouds) Program_contact: Sembach This portion of the O VI program will focus on understanding the character of the O VI absorption in the Magellanic Clouds. Approximately 20 sight lines will be investigated in the two galaxies. The sight lines will include superbubble structures with strong X-ray emission and field positions with little X-ray emission. The hot gas properties of the LMC and SMC will be compared to those derived for the Milky Way. There will be a large amount of auxiliary information obtained as part of the O VI Magellanic Cloud program. The Science Team will rely heavily upon these data to undertake additional investigations of the chemical composition and physical properties of the ISM in the Milky Way and Magellanic Clouds, as well as the properties of hot stars and their winds. ------------------------------------------------------------------------------ Prog ID: P204 Title: Deuterium Abundances and the D/H Ratio (Local ISM) Program_contact: Sembach This portion of the D/H program will provide information for sight lines confined to the local interstellar medium to determine the extent to which the D/H ratio varies within a few hundred parsecs of the Sun. These observations will significantly increase the amount of information available for local deuterium abundance determinations and will enhance the information for the local interstellar medium available from earlier Copernicus satellite studies. Objects to be used as background sources include cool stars, white dwarf stars, the central stars of planetary nebulae, and a few A-type stars. Auxiliary uses for the data will include general ISM studies and a survey of hot gas within the Local Bubble. (See abstracts for programs P102/122 and P115/P215 for additional details.) ------------------------------------------------------------------------------ Prog ID: P205 Title: Deuterium Abundances and the D/H Ratio (Galactic Disk) Program_contact: Sembach This portion of the D/H program will provide information for sight lines that extend beyond the local interstellar medium of the Galactic disk. The sight lines covered will sample gas in spiral arm and interarm directions several kiloparsecs from the Sun. Most of the objects observed will be OB-type stars. Data from program P102/122 (O VI disk survey) will provide an initial far-UV observation of a large number of sight lines. Many of these sight lines will be re-observed for longer integration times (a factor of 3-5x) as part of this program. All of the P102/P122 sight lines should be considered potential candidates for this study. ------------------------------------------------------------------------------ Prog ID: P207 Title: Deuterium Abundances and the D/H Ratio (Snapshot Survey) Program_contact: Sembach This portion of the D/H program will provide short observations of many AGNs and QSOs to check far ultraviolet flux levels and suitability of the objects as background continuum sources for extended integrations. The data produced from this snapshot survey will be used extensively as part of program P111 to study the flux distribution and intrinsic absorption properties of the AGNs and QSOs observed. (See abstract for program P111 for more information.) The Team will also use this data for studies of extragalactic O VI and H I absorption at low redshift. ------------------------------------------------------------------------------ Prog ID: P209/P309 Title: Deuterium Abundances and the D/H Ratio (Solar System) Program_contact: Sembach This portion of the D/H program will focus on determining the D/H ratio on Jupiter which will provide a reference value for the ratio at the time the solar system was formed about 4.5 billion years ago. The observation will consist of several planetary limb drift scans. In this mode, the center of the MDRS or HIRS will move, perpendicular to the long dimension of the slit, from 0.80 R_j to 1.2 R_j along a jovian radius during a single orbit, and this scan will be repeated for 5 contiguous orbits during a single visit. The data will be obtained in time-tagged mode allowing separate extractions of the disk and limb spectra. The disk spectrum will show electron excited dayglow spectra of H_2 and HD and permit a determination of the vibrational temperature of the H_2, needed for modeling of observed HD and D Lyman-beta emission which should be enhanced at the limb. The contiguous orbits will make it possible to take into account any effects of the equatorial hydrogen bulge which is centered on 90 degrees in System III longitude. ===================================================================================== FUSE PI Team Cycle 2 Programs Prog ID: P211 PI: Green, Richard Institution: NOAO Title: Monitoring Variable Active Galactic Nuclei We will monitor the highly variable O VI emission and associated absorption in three bright Seyfert galaxies. The screening observations for good AGN sightlines are, of course, taken at arbitrary times with respect to AGN light curves. In several cases of well-known Seyfert galaxies, FUSE caught them in a low state. To our surprise, the typical broad emission line expected for O VI had nearly vanished, leaving a narrower line component that was essentially invisible when observed in a high state by HUT. The emission velocity widths fall in the range of 400-800 km/s. Two different scenarios may explain the observations, and both may be operative to some degree. There may be an extended narrow-line region in O VI. When the broad line region fades as ionizing flux drops, the narrow-line component remains more nearly constant but gains prominence in the observed spectrum. Alternatively, there may be bi-conical outflow as in NGC 4151. As the accretion state changes, the structure of this focused wind changes both in ionization and density. The velocity spread and strength of O VI depends on the physical details of where in the flow the line is produced. An additional diagnostic is provided by the associated absorption. The degree to which it covers the broad line, narrow line, and continuum places the absorbing gas geometrically and constrains the location of the emission-line gas. The extent to which the strength of absorption varies with the continuum and emission components gives further information about its location in the nuclear region. ------------------------------------------------------------------------------ Prog ID: P213 Title: Circumstellar Interaction in SN 1987A PI: Sonneborn FUV emission from SN 1987A in the Large Magellanic Cloud will be observed to characterize the shock interaction between the high-velocity ejecta and circumstellar gas. We will study observe O VI emission and the full blueward extent of the blue wing of Lyman-alpha, only part of which is observable with STIS because of the high expansion velocity of the ejecta. Emission from recombination lines from the inner circumstellar ring may also be present. The nearest companion stars (Star 2 and 3) will also be observed. ------------------------------------------------------------------------------ Prog ID: P214 PI: Blair, William P. Institution: Johns Hopkins University Title: FUSE Observations of Balmer Supernova Remnants in the LMC We propose to observe the four Balmer-dominated (Type Ia) SNRs in the Large Magellanic Cloud. These objects will all be observed with Chandra, so FUSE observations will provide information on OVI line intensities for comparison with OVII and OVIII from the soft X-ray region. The combined data will provide strong constraints on the dominant emission mechanism operating in young SNRs arising from Type Ia supernovae. The LMC set of objects is unique in permitting reasonable estimates of the total OVI emission from each object with relatively little foreground extinction. ------------------------------------------------------------------------------ Prog ID: P215 PI: Shull, Michael Institution: University of Colorado Title: Two High-Extinction Stars in the LMC The fundamental physical and chemical processes at work in molecular clouds are key objects of FUSE science. Preliminary results on H2 in the LMC, based on available PI Team data, suggest a reduced molecular fraction in the low-metallicity LMC gas. Although this result provides the first direct evidence of a metallicity dependence in the formation rate of interstellar H2, the available FUSE targets do not sample the high-extinction regime where the correlation between E(B--V) and molecular fraction is strong. Therefore, we cannot test whether the apparent reduction in molecular fraction is due to reduced formation rates, high radiative destruction rates, or selection effects. We propose observations of 7 LMC stars and 2 SMC stars with E(B--V) = 0.20 -- 0.42, which will allow us to test cloud models that incorporate different assumptions about the formation rate of H2 as a function of metallicity. We will also obtain CO emission maps in these selected regions to assess the CO/H2 ratio in this gas. As a key goal of FUSE H2 science, this test can be applied only to sight lines for which the variation of molecular fraction with extinction can be tightly controlled. ------------------------------------------------------------------------------ Prog ID: P216 PI: Snow, Theodore P. Institution: University of Colorado Title: FUSE Team Project on Molecular Hydrogen in Translucent Clouds This Cycle 2 program plans observations of 11 stars (in addition to the original list) as an add-on to our medium project to study molecular hydrogen in translucent clouds. The new stars have been selected on the basis of reddening, known extinction and interstellar line parameters, and inclusion in the comprehensive survey of diffuse interstellar bands being carried out by group member Don York and collaborators (e.g. Snow, Welty et al.). ------------------------------------------------------------------------------ Prog ID: P217 PI: Fullerton, Alex Institution: University of Victoria Title: Less Luminous Hot Stars in the LMC and SMC The primary goal of the FUSE P117 Hot Star program is to characterize the stellar winds of a representative sample of early-type stars in the Galaxy, Large Magellanic Cloud (LMC), and Small Magellanic Cloud (SMC), in order to study the properties of mass-loss via stellar winds as a function of metallicity. Information about the ionization balance, velocity law, and mass-loss rates associated with these winds can be derived from modeling. However, in order to understand the behavioral trends of these properties, good coverage of the relevant temperature and luminosity classes is required. Through P117 and other PI-team programs, this spectral domain is well covered for Galactic OB and WR stars. However, the existing coverage of parameter space for the LMC and SMC is biased toward supergiants and hotter stars. With this proposal, we seek to mitigate these biases by supplementing the original sample of PI and GI targets in the LMC and SMC with objects of lower luminosity. This additional coverage of the H-R diagram will enable us to determine where the stellar wind turns off, and the dependence of this point on metallicity. Objects in the SMC are particularly interesting, since their abundances reflect the metallicities - and hence the behavior of stellar winds - in the early universe. ------------------------------------------------------------------------------ Prog ID: P218 PI: Dupree, Andrea Institution: Harvard-Smithsonian Center for Astrophysics Title: Cool stars This program will obtain far-UV spectra of cool stars that span a broad range of spectral type and luminosity class. The specific science objectives include: (1) studying transition region dynamics (winds and downflows), (2) modeling the thermal structure of transition regions, (3) measuring electron densities, (4) search for low temperature coronae, (5) studying molecular excitation and fluorescence processes, and (6) inferring how the transition regions of spectroscopic binary systems differ from those of single stars. All five targets have been previously observed with FUSE, and their spectra assessed. They indicate that FUSE will identify the source of the stellar coronal holes and define the acceleration and transition region densities over the cool half of the HR diagram. However, further observations are required to improve the quality of the line profiles from which conclusions can be drawn. In particular we require observations during orbial night-time to remove any uncertainties due to solar and airglow contamination. ------------------------------------------------------------------------------ Prog ID: P219 PI: Vidal-Madjar, Alfred Institution: Institut d'Astrophysique de Paris Title: Circumstellar Disks Extension Program The purpose of this program is to obtain new spectra of the most important targets of the Circumstellar disk program (P119, Q119, Q219) which aims to observe the signatures of circumstellar gas around main-sequence and pre-main-sequence stars. The objective of this program is to monitor the spectroscopic variabilities of the targets for which FUSE spectra have already been obtained or will be obtained in the coming months. The selected targets have already shown signature of spectroscopic variations in the UV or the visible. Although these variations are often interpreted in terms of proto-planetary activity, a clear understanding is still to be established. Further observations and studies are thus needed. ------------------------------------------------------------------------------ Prog ID: P220 PI: Feldman, Paul D. Institution: The Johns Hopkins University Title: FUSE Team Project on Solar System Objects The original P120 proposal requested observations of Jovian aurora with the MDRS and the Io plasma torus with both LWRS and MDRS apertures. Because of anticipated difficulties in achieving pointing at specific regions of the torus or polar aurora and problems in maintaining co-alignment of the four channels, the initial observations of these targets were made with the LWRS. However, there remains a strong desire to observe both targets at the higher spectral resolution afforded by the MDRS aperture. For example, one of the initial objectives for the Io torus was to determine the velocity distribution (expected to be non-Maxwellian) of the principal sulfur ions, S II, S III and S IV. Higher resolution would also make the analysis of the multitudinous lines of H_2 seen in the auroral spectrum much more tractable. We propose to use the MDRS in a short raster scan for both targets. This will alleviate the pointing and co-alignment problems cited above and additionally will provide, in the case of the Io torus, information about the radial distribution of electron temperature and density, relative ion abundances and ion temperature, with which to test current models. ------------------------------------------------------------------------------ Prog ID: P221 PI: Hutchings, John Institution: HIA, NRC of Canada Title: Far UV extinction curve in the SMC The observation is of reddened stars in the SMC which will yield an far UV extinction curve for this galaxy. UV extinction in galaxies of low metal abundance are of high interest in current cosmology research as well as in understanding the evolution of our neighbour galaxy. The early universe is seen at rest UV wavelengths because of redshifting, but the energy budget and completeness will not be known until proper allowance is made for extinction. It is known that the SMC UV extinction curve is steeper and different in shape from that seen in the more evolved environment of our Galaxy. The extension of this to the Lyman limit is not known and of high importance as it rises with decreasing wavelength. ------------------------------------------------------------------------------ Prog ID: P222 PI: Iping, Rosina Institution: CUA, NASAGSFCLASP Title: FUSE OBSERVATIONS IN SUPPORT OF ETA CARINAE Eta Carinae, located in the association Trumpler 16 in the Carina Nebula (NGC 3372), was observed by FUSE in February and March 2000 and was found to have surprisingly bright far uv fluxes and strong H2 absorption. If circumstellar nature of H2 can be established, this would be the first detection of molecules in the eta Car nebulosity. Do the large FUV fluxes provide evidence for or against a binary companion of eta Car or constrain the mass of this object? In an effort to clearly distinguish between the interstellar and circumstellar material, three OB stars close (within 1 arcmin) to Eta Carinae, Trumpler 16 will be observed. Additional lines of sight close to eta Car should help to better understand the ISM near eta Car. To complement the observation of eta Carinae, three other luminous blue variables, P Cygni, AG Carinae and HR Carinae will be observed. Comparison of additional LBVs with eta Car will help to establish in what way they are similar and/or different. P Cygni is especially important because it is widely regarded as an eta Car analog in terms of its UV properties (Ebbets et al. 1997, ApJ, 489, L161). These observations will give us a better understanding what LBV's look like in the FUV. ------------------------------------------------------------------------------ Prog ID: P223 PI: Massa, Derck Institution: Raytheon STX Title: Phase-Resolved FUV Spectroscopy of the Binary HD 5980 HD 5980 is the brightest star in the SMC and indicative of the luminous objects which dominate the light from distant, metal poor, young galaxies (Koenigsberger et al., 2000, ApJ, 542, 428). HD 5980 is also an eclipsing WN+O binary with an eccentric orbit and a period of 19.26 days (Breysacher & Perrier 1980, A&A, 90, 207). In addition, in 1994 one component of the system underwent a Luminous Blue Variable (LBV) outburst of the sort experienced by the most luminous stars in the universe (Moffat et al. 1998, ApJ, 497, 896). The binary nature of HD 5980 is fortuitous, since it allows us to determine far more about the object than we could ever glean from a single star. Because the two components have different temperatures, observations of the eclipses at different wavelengths reveal different aspects of the stars. To probe the massive winds of the binary, to attempt to disentangle the contributions of the two components and to make unambiguous identifications of the ISM lines along the line of sight, better phase coverage of the orbit is essential. Three observations near each of the two eclipses (phases 0.00 and 0.36) and one near each opposition (phases 0.13 and 0.78), where the line of sight to the system does not intersect the interacting winds. ------------------------------------------------------------------------------ Prog ID: P224 PI: Willis, Allan Institution: University College London Title: The Enigmatic WR Star HD 45166 It is proposed to secure FUV spectra of the qWR star HD45166. These data will provide measurents of qWR emission lines in important species like CIII, CIV, SIV, SVI, OVI, NIII. Their analysis using state of the art, nLTE model atmosphere techniques will determine the fundamental properties of the low mass, qWR star, and fix its evolutionary status. ------------------------------------------------------------------------------ Prog ID: P231 PI: Andre, Martial Institution: John Hopkins University Title: OI Abundance and D/O The Oxygen abundance is a critical point for D/H measurements with FUSE since D/O can be determined with greater accuracy. Using the Copernicus data, astronomers found a depletion of Oxygen in the gaz phase (com pared to solar abundance) and started to investigate the O/H(total) ratio in the LISM. From Deboer et al (1981) to Keenan et al(1985), the determination of this ratio proved to be difficult and nothing could been said about possible variations because of the scatter of data and the error bars. Then, using GHRS data, Meyer at al (1998) tried to set a Definitive Oxygen Abundance and found 50 % depletion in the LISM (gaz phase). Still, the survey implied only 13 targets so that nothing can be said as to variation or gradient. In particular, distant targets are required to test the metal poor infall scenario (to explain the LISM depletion) but such targets show strong H2. The next step would be to improve the statistic but to do so means to be able to choose a large sample of targets for which a non negligible fraction of H may be in H2 molecules. The most useful sample of targets comes from the Lauroesch survey (STIS 1998) where lines of sight were selected to show 1356 A OI transition. From this survey, I extracted 19 very nice lines of sight, showing clear velocity structure and no blending. Actually, 14 of them are planned FUSE target or already in the FUSE archive. Among the 5 other targets, 3 have a E(B-V) greater than .2 and FUSE is the only instrument able to give their H2 column density. ------------------------------------------------------------------------------ Prog ID: P232 PI: Hoopes, Charles G. Institution: Johns Hopkins University Title: The HII Region N44C I am proposing to observe the central star of the HII region N44C in the LMC, as well as the surrounding ionized gas. This HII region contains HeII emission, but the central star has been classified as type O7, not hot enough to produce the 54 eV photons necessary to ionize HeII. With a FUSE spectrum we can search for other highly ionized elements requiring photon energies similar to that of HeIII. The recombination time of these elements can constrain and perhaps eliminate the hypothesis that the ionization source has turned off. We can also determine the metallicity in the region to see whether enrichment by an evolved companion has occurred, and use the stellar spectrum to refine the spectral classification. ------------------------------------------------------------------------------ Prog ID: P233 PI: Catanzaro, Giovanni Institution: Johns Hopkins University Title: Vertical abundance stratification in the atmospheres of Chemically Peculiar stars Magnetic Chemically Peculiar (CP) stars are characterised by spectral, photometric and magnetic variations with a common period. In the oblique rotator model, proposed by Stibbs (1950), chemical elements are not homogeneusly distribuited on the stellar surface, and the observed variations are due to the stellar rotation. The anomalous abundances are caused by diffusion process (Michaud, 1970). Magnetic fields are suspected to influence the diffusion by suppressing mass-motions and changing the path of ionised species (Michaud et al., 1981), so that diffusion in CP stars results in a non-homogeneous distribution of elements over the stellar surface. The vertical stratification of chemical elements in the atmospheres of CP stars was predicted from results of radiative diffusion processes. In order to study this phenomenon, one attempt we can make is to compute chemical abundances by measuring different lines of the same element, formed at different layers of the atmosphere. FUSE offers the possibility to look very deep in the atmosphere of these stars, so it is possible to select a number of spectral lines, that together with other lines observed in optical spectra, will furnish an unique opportunity to improve our knowledge about vertical stratification. ------------------------------------------------------------------------------ Prog ID: P234 PI: Sankrit, Ravi Institution: Johns Hopkins University Title: Extended Grid in the Northeast Cygnus Loop We will obtain MDRS spectra at two locations near a Balmer filament in the northeast region of the Cygnus Loop supernova remnant. The first position will be ahead of the filament and the second will be behind it. These observations will supplement the spectra taken at three locations on the filament (part of FUSE program P114). The OVI flux was found to decrease as a function of position downstream behind the shock front. Weak emission on the wings of the primary OVI 1032 component was detected at all three locations. The flux in these weaker components was about the same in all three spectra. The current observations are designed to measure the OVI flux in regions away from the filament. This will allow us to examine the OVI emission that may be present, arising from regions other than the shocked gas in the Balmer filament. We expect he same strength in each of the spectra. The current observations are designed to measure the OVI flux in regions away from the filament. From these measurements we will be able to estimate the contribution of sources other than the primary shock to the total OVI flux in the remnant. In addition to the spectra in the primary aperture (MDRS) we will obtain data in the LWRS aperture, from which we will obtain the OVI flux in regions about 3.5 arcminutes away, but still within the remnant. ------------------------------------------------------------------------------ Prog ID: P235 PI: Sonnentrucker, Paule Institution: Johns Hopkins University Title: H2, metals and DIBs in Reflection Nebulae Diffuse Interstellar Bands (DIBs) are absorption features detected mainly in the optical. Even though the DIB carriers have been proven to be most likely carbonaceous in nature and reside in the gas phase, their origin remains a complete mystery (Herbig, 1995 for a review). Former studies indicated that some (DIBs) are weaker in reflection nebulae than in diffuse clouds of equivalent reddening. Few attempts were made to explain the DIBs peculiar behavior toward those particular environments. However, this issue widely remains unexplored because the line of sight properties toward reflection nebulae are not always well constrained. I, therefore, propose to observe the reflection nebulae HD190603 and HD198478 to derive the column density of H2, CI, CI* and CI**, PII, ArI, FeII, NI, estimate the molecular fraction in order to study these lines of sight properties and relate them to the DIBs, CaI, CaII, NaI, CH and CH+ column densities measured in the optical. In addition, the extinction curves of HD190603 and HD198478 only differ in the FUV non-linear rise portion. Since the FUV non-linear rise is thought to be due to very small grains (or large molecules) in a neutral form, assessing the role of the FUV non-linear rise on to the DIBs, H2 and the metals in the FUSE passband will give further information on the properties of these two lines of sight and the DIB carriers survival/destruction conditions. ------------------------------------------------------------------------------ Prog ID: P241 PI: Lehner, Nicolas Institution: The Johns Hopkins University Title: FUSE Observations of the Magellanic Bridge Young B-type stars are known to exist in the Magellanic Bridge (MB) gas, a region of material between the Large and Small Magellanic Clouds, implying that star formation is still occurring in the MB. In all known environments star formation occurs within molecular clouds, but there is yet no direct evidence of star-forming clouds in the MB. FUSE will allow for the first time to make a direct sensitive search for molecular hydrogen in the MB and give more insights on the possible star formation mechanisms in low density and metallicity environments. The proposed targets are two young hot stars, DI1388 and DGIK975, and not only search for molecular hydrogen will be made possible, but a detailed investigation of the physical conditions within the MB gas will be studied in different spatial positon (DGIK975 is near the LMC while DI1388 is near the SMC). In particular, using our previous HST STIS, the FUSE observations will allow us to place limit or measurements on the ratios of C III/C II, S III/S II, N III/N II/N I, Fe III/Fe II, Si IV/O VI and C IV/O VI. Finally, an HVC was detected in the DI1388 STIS spectra and was found to be nearly fully ionized. FUSE observations will help to place a constrain on the ionization origin by studying the ionic ratio of several species. ------------------------------------------------------------------------------ Prog ID: P242 PI: De Marco, Orsola Institution: American Museum of Natural History Title: Thermonuclear Runaways on Dwarf Novae We are going to take an observation of the dwarf nova SS Cygni during quiescence to measure elemental abundances in the atmosphere of the exposed white dwarf component of this binary. We expect that the absolute abundances will yield clues about the past outbursting history of the system. In particualr, as is the case for the dwarf nova VW Hyi, we might detect abundaces characteristic of thermo-nuclear processing, which would indicate that SS Cyg experienced a nova outburst sometime in its past. Such finding would contribute substantially in unifying the dwarf nova and nova outburst scenarios. ------------------------------------------------------------------------------ Prog ID: P243 PI: Hoopes, Charles G. Institution: Johns Hopkins University Title: WR Star AV336a in the HeII Nebula N76-A I propose to obtain a 10 ksec LWRS spectrum of the WR star AV336a in the SMC. This star is surrounded by a HeII nebula (Garnett et al. 1991), one of only six known in the Local Group. The presence of HeII emission requires that the ionizing star emit photons with energy greater than 54 eV, which in turn requires a stellar effective temperature of 70,000 - 80,000 K. Wolf-Rayet stars have temperatures in the 30,000 - 60,000 K range (Conti 2000), and in fact no population I stars are known to have temperatures as high as those required by the HeII emission. Either AV336a is a very rare type of star, or else the ionization source in this HII region is not understood. The FUSE bandpass provides a unique opportunity to study both AV336a and the surrounding HeII nebula. The stellar spectrum will provide information on the stellar winds and abundances, which will shed light on the unusual nature of this star. Secondly, the absorption spectrum of the intervening material in the HeII nebula will provide information about other highly ionized elements. The adjacent ionization stages of PIII, IV, and V and S III, IV, and VI in the FUSE bandpass, as well as other ionized gas diagnostic lines, will be used to measure the luminosity of the star at energies well above the Lyman limit, providing a strict diagnostic of the stellar temperature. The spectrum will also be used to search for high velocity gas that would indicate shock ionization. ------------------------------------------------------------------------------ Prog ID: P247 PI: Young, Peter Institution: Harvard-Smithsonian Center for Astrophysics Title: 44i Bootis (HD 133640) 44i Boo is a W UMa type contact binary at a distance of 12.8 pc with an orbital period of 6.4 hours and an inclination of 72.8 degrees, so that there are two eclipses per orbit. X-ray and UV emission from highly-ionised ions have revealed that 44i Boo exhibits a corona, but that the emission levels are below those of rapidly rotating single stars or short-period, detached binaries, indicating that the dynamo is being inhibited by the physics associated with the contact. By categorising in detail the nature of the corona of 44i Boo, one may shed light on how the magnetic dynamo operates in stars. With FUSE it will be possible to use the high spectral resolution and sensitivity of the instrument to monitor line fluxes and profiles of the strong C III 977 and O VI 1032 emission lines during the orbit, as well as use the temperature coverage of these and weaker lines to compare with the atmospheric models made with previous instruments. ------------------------------------------------------------------------------ Prog ID: P248 PI: Young, Peter Institution: Harvard-Smithsonian Center for Astrophysics Title: AG Draconis (BD +67 922) Follow-up AG Draconis is a symbiotic star consisting of a K giant and white dwarf. The UV is dominated by emission lines from a nebula believed to be around the white dwarf. AG Dra was observed by FUSE on 16-March-2000 as part of the science verification program for FUSE. This short (~2400s) observation produced a high quality spectrum revealing emission lines from several species, including O VI, Ne V, Ne VI, S IV, S VI and He II. A further observation of AG Dra is planned to determine the geometry of the nebula, attribute the wind to one of the two stars, and to obtain a full exposure in the SiC channels which will be needed to obtain a density for the nebula. ------------------------------------------------------------------------------ Prog ID: P249 PI: Andre, Martial Institution: John Hopkins University Title: HD in a Translucent Cloud Deuterated molecules are another means of determining the Deuterium abundance. With Copernicus, H2 and HD nolecules were observed in absorption in the ultraviolet in diffuse clouds such as that toward Zeta Oph. Nevertheless, very low HD/H2 ratios were found, reflecting the atomic nature of these clouds. With FUSE, we can use denser molecular clouds within which one might expect H and D to be in their molecular form. In such cases, molecular fractionation correction is not required and direct measurement of D/H could result from HD/H2 ratios. Until recently, HD/H2 measurements were limited to these few good candidates where the velocity structure could allow for an isolated translucent intervening cloud, but saturation and low S/N of these detections implied large uncertainties on the result. For one of the translucent cloud's targets, however, high S/N detection of HD is present. The star HD206267 lies behind the translucent cloud DC 1107. Within a few arc min to the star, and showing the same reddening (E(B-V) ~.4) we found 2 fuv bright stars : BD+56 2617C and BD+56 2617D. These 3 stars could possibly illuminate the same cloud whose aera is grater than 10 deg steradian on the sky (very close). Such a configuration is what we need to argue for a HD reservoir inside the cloud. ------------------------------------------------------------------------------ Prog ID: P250 PI: Roberge, Aki Institution: Johns Hopkins University Title: Circumstellar Disk Target HD 141569 The circumstellar disks medium team projects (P119 and Q119) have produced remarkable spectra, showing emission and absorption features arising from gasses that have a wide range in temperature, from hot OVI emission to cold H_2 and CO absorption. The emission from the highly-ionized species was unexpected, as standard stellar theory predicts that these stars (with spectral types earlier than about F0) should not have convective outer layers, and therefore, should not have chromospheres, coronae, or strong stellar winds. While these stars clearly do show stellar activity, the exact nature is unclear. AB Aurigae shows strong stellar winds and it is thought that the highly-ionized species may be formed by shocks in the wind. Beta Pic, on the other hand, shows emission from OVI and CIII, but no trace of stellar winds. Since Beta Pic is older than AB Aur, this difference might indicate that the stellar activity is changing (possibly decreasing) with age. To demonstrate this, we need to study young stars with a variety of ages. Unfortunately, most of the targets in P119 and Q119 are younger than about 10 Myr; Beta Pic is the only one that is clearly older (age ~ 20-30 Myr). We therefore propose to observe another nearby young star with a CS disk, HD 141569 (spectral type B9 Ve, d=99 pc), that is thought to be a more evolved object (age > 10 Myr). This star's CS disk was imaged with NICMOS (Weinberger et al. 1999), which showed a remarkable gap in the dust disk. This gap may most easily be explained by the gravitational influence of one or more planets orbiting the star. (Go to http://oposite.stsci.edu/pubinfo/pr/1999/03/index.html to see the NICMOS image and HST press release). This makes HD 141569 a very interesting object, as well as providing additional evidence that it is a relatively evolved young star. ------------------------------------------------------------------------------ Prog ID: P251 PI: Oliveira, Cristina Institution: Johns Hopkins University Title: D/O ratio toward WD2247+583 I propose to observe the white dwarf WD2247+583 (Lan 23) and measure the D/O ratio along this line of sight. If the O/H ratio is ~ constant as the work of Meyer et al (ref 3) seems to indicate and the D/H is also ~ constant then we would expect that D/O is also ~ constant. Preliminary analysis of several lines of sight using FUSE data have not yet been able to show a definite correlation between N(DI) and N(OI) and so more measurements along different lines of sight are needed. Previous measurements using EUVE data (ref 1) have placed the HI column density at 716 < N(HI) < 1596 x10^17 cm^-2. Using a D/H ratio of 1.2x10^-5 this places the DI column between 8.6 x10^14 and 1.9x10^15 (cm^-2). This will be an interesting measurement since DI is typically measured in lines of sight with low HI column density (N(HI)~10^18 cm ^-2) and we'll be probing the D/O ratio in a regime that is not very explored. The effective temperature and gravity of this white dwarf indicates that the stellar continuum will be relatively smooth and continuum placement won't be a major uncertainty in measuring N(DI) as is the case with other types of white dwarfs. ------------------------------------------------------------------------------ Prog ID: P252 PI: Pellerin, Anne Institution: Universite Laval Title: Young Stellar Populations and the Starburst-AGN Connection I propose to study young stellar populations in the nuclear region of the starburst galaxy NGC 5430. This project is part of my thesis which adresses the question of an evolutionary relation between nuclear starbursts and AGN (based on Weedman et al. 1998 and Heckman et al. 1997). For my thesis, a large sample of starbursts and AGNs are to be considered in order to establish a scenario on how nuclear starbursts may evolve into an AGN based on the importance of a nuclear bar (Friedli et al. 1995). Although the FUSE archives already contain spectra for a variety of nuclear starbursts and AGN, none of them are characterized by a strong nuclear bar. The goal of this proposal is to obtain a FUV spectrum of the starburst galaxy NGC 5430, which does have such a bar. ------------------------------------------------------------------------------ Prog ID: P263 PI: Wilkinson, Erik Institution: University of Colorado Title: Pre-Main Sequence Stars HST/STIS GTO observations of HD104237 are being planned during 2001 using 4 HST orbits to observe the star using 2 orientations of coronagraphic imaging, and then obtaining two UV spectra, one a G140M spectrum at H Lyman alpha with an orientation determined from the coronography, and the other a G140L spectrum with the same orientation. We would like to obtain a second epoch FUSE observation of HD104237 contemporaneous with the STIS UV spectroscopy, in order to measure the full temperature structure of the circumstellar environment around this young intermediate mass star and to investigate whether the FUV spectrum of this star is as variable as the spectra from other Herbig Ae stars. This star has very few HST observing constraints and thus FUSE observation scheduling can be the primary driver for when these observations occur. ------------------------------------------------------------------------------ Prog ID: P267 PI: Green, Jim Institution: CASA, University of Colorado Title: Extragalactic Hot Gas along the MRK1383 sightline HST/STIS+G140M data of the MRK1383 sightline reveal an extremely broad, but relatively weak, low-z Ly-alpha absorber. We propose to use FUSE to search for OVI absorption associated with this absorber to search for hot gas in the very local universe. =============================================================================== Prog ID: P301 PI: Blair Title: D-to-H in the Vela-Puppis Region The D-to-H ratio toward the star gamma2Vel has been measured to be anomalously high by IMAPS, while the value toward zetaPup (about 8 degrees away) is apparently normal. We request observations of additional stars in the Vela-Puppis region in an attempt to either confirm or refute the high value toward gamma2Vel and to exercise various bright star observing techniques. Many of the stars are very bright and will require special techniques to observe. One is actually quite faint and will require a moderately long integration. Since bright target observing is not yet standard, planners should exercise considerable caution in scheduling these observations. Some hand scripting will be required. ------------------------------------------------------------------------------ Prog ID: P302 PI: Blair (LI: Williger) Title: Expanded Sub-dwarf Program for Determining D-to-H A major goal of the PI team program is to measure the D-to-H ratio (or its surrogate, D-to-O) in stars beyond the local ISM. Recent work indicates that subdwarf O stars may be the best type of target for accessing the intermediate region from ~100 to 1000 pc or more. This program strives to expand the sample of target stars in this distance range available for D-to-H analysis. In the process, excellent spectra of the subswarf stars themselves will also be obtained. ------------------------------------------------------------------------------ Prog ID: P303 PI: Williger Title: Deuterium Abundances toward Hot Stars The scatter in D/H values measured at high redshift suggests that the gas involved may have undergone some stellar processing. It is therefore important to understand the role of chemical evolution with respect to the deuterium abundance. The variatio ns in the Galactic ISM D/H ratio can shed light on the effects of star formation history and mixing processes. A comparison of the local D/H value, which appears to be stable aqt 1.5+-0.2e-4, can be compared to more distant regions which have undergone varyqing amounts of stellar processing. We request observations of OB stars with distances beyond the Local Bubble to explore the variation of D/H in a variety of environments. Some of the stars are very bright and will require special techniques to observe. Others are actually quite faint and will require moderately long integrations. ------------------------------------------------------------------------------ Prog ID: P304 PI: Friedman Title: D/H and O/H Along Sight Line to Mu Col (HD 38666) Mu Col is an excellent target for D/H studies. As a GHRS high- and intermediate-resolution radiometric standard it has been observed many times. There is a large literature on this star, and the properties of the sight line have been studied extensively. The component structure is well known. It is at a distance of 400 pc, beyond the wall of the local bubble, and where evidence of variability in D/H is growing. There is an exquisite measure of the HI column density, log N(HI)=19.86+/-0.015, and good measures of many other species, both depleted and non-depleted. However, there is *not* a good measurement of OI because the 1355 line is too weak, and the 1302 measurements only apply to low-column, intermediate velocity gas. Thus, we can expect this dataset to yield excellent values of both D/H and O/H. ------------------------------------------------------------------------------ Prog ID: P306 PI: Kriss Title: 1700+64 Followup In March 2003, the quasar HS1700+64 was found (as part of program C123) to be 2-3 times brighter than in the past. This quasar was used for the first measurements of He II opacity in the intergalactic medium by HUT. It is currently brighter than HE2347-4342, the quasar first observed by FUSE for resolving the He II Lyman alpha forest in the IGM, giving us a unique opportunity to obtain high quality measurements of the He II opacity along another sight line through the IGM. The data in this program, when combined with C123 and the Z012 DOT program, will give a final spectrum of the same quality as that obtained on HE2347-4342. These two quasars are the only ones known with clear lines lines of sight to the He II Ly-alpha foresy that can be observed with FUSE. ------------------------------------------------------------------------------ Prog ID: P323 Title: Supernovae as Probes of Galactic Halos PI: Sembach FUSE observations of a newly discovered, bright (V<14) core-collapse supernova (Types II or Ib) will be used to study interstellar properties of the sightline. The full range of interstellar species present in the FUSE wavelength range will be utilized to examine kinematics, depletions, and abundances of foreground gas, the Milky Way halo, the ISM of the supernova's host galaxy, and the intergalactic medium. Any data obtained from this program will be made available to other FUSE programs to study the properties of the supernova outburst. ------------------------------------------------------------------------------