			Cycle 7 - Phase 1 Abstracts
				1/19/06 AFB



	 Prop ID:        G001  Proposer:       Wang   
	 Institution:    University of Massachusetts   
	 Proposal Title: OVI Emission from Galactic Disk-Halo Interaction 

	 We propose FUSE observations to sample the OVI line emission
      from the disk-halo interaction of the nearby galaxies NGC2841 and
      NGC7090. The OVI 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 deep Chandra observations, and with the
      mechanical energy input from supernovae in these galaxies. The 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 study
      the line-of-sight size and dynamics of the gas. The results will have
      strong implications for understanding the role of the disk-halo
      interaction in galactic eco-systems.  endabstract
      

	Prop ID:        G002  Proposer:       Meyer   
	Institution:    Northwestern University   
	Proposal Title: High-Velocity Molecular Gas Toward M81       
                                                                                                          
	 Multiwavelength observations of the M81 galaxy group have discovered several
      dwarf galaxies and molecular complexes that may be associated with the
      intergalactic gas in this interacting system.  Although HI 21cm
      observations have found no evidence of such gas toward the M81 nucleus,
      opticalUV spectroscopy has revealed high-velocity atomic
      absorption in this region.  We have recently found a
      strong NaI component at +217kms^-1 that stretches over 400pc
      WSW of the nucleus.  In order to probe the molecular
      content of this high-velocity gas, we propose to obtain  FUSE
      observations of the H_2 absorption in the central AGN sightline.
      Our anticipated N(H_2) detection threshold of 5x10^15cm^-2
      is five orders of magnitude more sensitive than that inferred
      from the lack of CO 2.6mm absorption toward
      the central source.  If we fail to find H_2 at this
      sensitivity, it would imply that the
      high-velocity gas toward M81 is entirely atomic and thus
      analagous in content to the non-Magellanic-Stream HVCs
      in the Galactic halo.  On the other hand, the detection of an
      appreciable H_2 column would indicate that this gas has formed or is
      forming molecules and is most likely tidally-stripped material from M82.
      

	 Prop ID:        G003  Proposer:       Oliveira   
	 Institution:    Johns Hopkins University   
	 Proposal Title: HI, DI and other abundances along three extended sightlines 
                                                                                       
	 Measurements of the DH and DO ratios have been shown to be
      remarkably constant up to log N(H) 19.2, which corresponds roughly to
      the limits of the Local Bubble. Between 19.2 < log N(H) < 20.6, these
      ratios present a large scatter, while for log N(H) > 20.6 DH and DO
      seem to be constant again, albeit with values roughly half that of the
      Local Bubble. Although several mechanisms have been proposed to
      explain these variations, a global consistent picture of these
      abundance patterns is still missing. The low yield of high column
      density sightlines suitable for accurate DH measurements has been a
      major barrier to progress in this area. This derives from the extreme
      difficulty of finding suitable targets at these high N(H), both in
      terms of DI not being obscured by either HI or H_2 absorption and
      having data available to determine reliable N(HI) from Lyman alpha.
      This proposal requests additional observing time to obtain
      signal-to-noise ratios adequate for determining the column densities
      of DI, NI, OI, and FeII, along three high N(H) sightlines that have
      been previously observed by FUSE. Preliminary analyses of the current
      datasets show that these sightlines are suitable for DI measurements
      and that they may have high DH ratios (> 1E-5).
      Existing high resolution HST/STIS data for the three sightlines will 
      be used to determine N(HI) along two of the sightlines (N(HI) has been
      published for the other one) as well as to model the velocity
      structure along the sightlines. These datasets will also allow us to
      determine the abundances of species that do not have unsaturated
      transitions in the FUSE bandpass (SI, NiII, etc.). Additionally, N(OI)
      derived from the weaker, but with a more reliable f-value, 1356AA
      transition in the STIS bandpass will be compared to the one derived
      from the 974AA transition in the FUSE bandpass.
      

	 Prop ID:        G004  Proposer:       Lauroesch   
	 Institution:    Northwestern U.   
	 Proposal Title: Prospecting for Rare Elements in the Interstellar Medium 

	 The complex history and evolution of element production is reflected
      in the abundance ratios.  The distinctive abundance
      patterns produced by nucleosynthesis in supernovae and stars can be used to
      explore the history of star formation and evolution in galaxies.  Recent
      observations of damped Lyman-alpha absorbers suggest
      that observations of r- and s-process elements at high redshifts will soon
      provide a new window to explore chemical evolution.  Paradoxically, we may
      soon have more detections of some elements in
      high redshift galaxies than in the Galactic ISM.  However,
      without an understanding of the depletion behavior of these elements based upon
      observations of nearby sightlines we will be unable to correctly disentangle the
      effects of dust depletion and nucleosynthesis.  We therefore propose to
      determine the depletion of r- and s-process elements in two Galactic sightlines
      with relatively mild depletion patterns on nearly opposite parts of the sky.  In
      addition to providing a baseline for studies at high redshift, the long
      pathlength studied allows us to search for abundance variations within
      our Galaxy.  Absorption lines of the dominant ionization state of
      these elements can only be detected in the UV, and  FUSE is the only
      current instrument that can make progress in this field.
      

	 Prop ID:        G005  Proposer:       Schmidtke   
	 Institution:    Arizona State University   
	 Proposal Title: BeX-ray Pulsars in the Small Magellanic CLoud                                                                                                     

	 BeX-ray pulsars are the most numerous type of high-mass X-ray binary
      HMXB) found in the SMC, with over thirty known.  Yet, not one of this
      important class has been observed by FUSE.  We propose to obtain FUSE data
      for two of these systems which are well studied optically the classical
      source SMCX-3 and AXJ0049.4-7323.  Our FUSE spectra will not only be the
      first far-ultraviolet spectra of SMC BeX-ray pulsars, but will also have
      sufficient pulse-phase resolution to investigate the behavior of the
      material in the vicinity of the neutron star as the pulsar beam sweeps
      through it.  We will study variations in strength and profiles of the
      expected He II and O VI emissions from this gas to understand how the
      ionization and excitation changes through the pulse period. 
      AXJ0049.4-7323 is particularly well suited to such a study with its very
      long X-ray pulse period (755 sec).  SMCX-3 has a much shorter pulse
      period (7.8 sec), but it is sufficiently bright that we can bin the raw
      data into pulse-phase resolved spectra.  This study will provide FUV
      spectra of the important but unobserved HMXB and will give unique
      information about the environs of the neutron stars. 
      

	 Prop ID:        G006  Proposer:       Gull   
	 Institution:    Goddard Space Flight Center   
	 Proposal Title: Separating Binary Orbital Variations in Eta Carinae from Secular Changes                                                                            

	 Eta Carinae has long been suspected to be a massive binary
system, but the hot companion has eluded detection until now. Our FUSE
Cycle 4 observations have revealed the hot companion of eta Car for
the first time. FUV spectra show that the companion is consistent with
a late O or WR star, possibly nitrogen rich. FUSE observations of eta
Car 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 two Cycle 7
observations 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 by spectral analysis of
STIS observations from 1998.0 - 2004.5 that are yielding radial
velocity curves for the wind-wind interaction in the binary system.
      

	 Prop ID:        G007  Proposer:       Henry   
	 Institution:    The Johns Hopkins University   
	 Proposal Title: Diffuse UV Background web site.                                                                                                                   

	 We show that FUSE is capable of providing unique data on the diffuse
      ultraviolet background radiation shortward of Lyman Alpha.  This is the only
      way of confirming previous Voyager measurements of the diffuse
      background, which are contaminated with Lyman Beta because of the poor (28
      AA) spectral resolution of Voyager.  Confirmation of the Voyager
      measurements is important in its own right, but also may be of unique
      importance to cosmology, as the Voyager measurements show a drastically
      different picture of the diffuse ultraviolet background short of Lyman Alpha,
      compared with what is seen longward of Lyman Alpha, suggesting the possibility
      that the general diffuse background longward of Lyman Alpha is at least
      partially of cosmological origin (intergalactic hydrogen recombination
      radiation).  While we have just, once again, been successful in
      obtaining GALEX observing time longward of Lyman Alpha, FUSE provides our
      only opportunity to test the strength of our case shortward of Lyman Alpha.
      

	 Prop ID:        G008  Proposer:       Ignace   
	 Institution:    East Tennessee State University   
	 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 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 to derive the possible rotation velocity of the
      central stars.  We expect to probe the faster polar wind with higher
      ionization lines (SIV, FeIII, PV) and lower ionization lines to probe
      the disk flow (OI, NI, FeII).  The presence of OVI would also be a 
      tracer of hot gas in system, a common feature of line-driven flows. 
      

	 Prop ID:        G009  Proposer:       Welsh   
	 Institution:    UC Berkeley   
	 Proposal Title: The W4 Superbubble 

	 We propose to examine the high velocity ionized and neutral
      interstellar gas associated with the expansion of the W4
      superbubble. The massive young star clusters of IC 1805 & IC 1848
      appear to be to be powering an outflow of gas, such that the
      interstellar cavity has reached the classic bubble blow-out
      evolutionary phase and is now in the stage of ejecting gas through a
      galactic chimney into the overlying galactic halo. By comparing the
      interstellar sight-lines towards two early-type stars associated with
      underlying IC 1805 & IC 1848 clusters with a sight-line that
      intersects the arching chimney of expanding gas that has blown out
      into the lower halo, we shall be able to investigate the physical,
      chemical and dynamic conditions of the disturbed atomic and molecular
      gas associated with a classic blow-out phenomenon.
      

	 Prop ID:        G010  Proposer:       Wakker   
	 Institution:    University of Wisconsin   
	 Proposal Title: Studying the Warm-Hot Ionized Medium in Groups 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 medium
      WHIM) which can be observed through intervening OVI and NeVIII
      absorption line systems; about 50 of these have now been found.
      However, it remains unclear whether these systems are truly
      intergalactic or whether they are associated with galaxies andor
      galaxy groups. This relation is best studied at very low redshift
      v<6000kms, z<0.02), where we have a good galaxy inventory
      and can also study the 21-cm and X-ray properties of the
      IGM. Associated OVI and Lyman beta is seen in about 60
      with AGN-galaxy impact parameter <300kpc, but we find just one
      detection in seven sightlines with SN>10 that pass through a nearby
      loose group. We propose to search for OVI and CIII absorption toward
      RX,J1830.3+7312, which is one of just two known targets with flux
      >1.3tfu that pass through the inner half of a nearby group. Lyman
      Alpha has already been detected in its HST spectrum, including a broad
      line that may originate in hot gas.
      

	 Prop ID:        G011  Proposer:       Wakker   
	 Institution:    University of Wisconsin-Madison   
	 Proposal Title: Hot Gas in the Central Region of the Milky Way                                                                                                

	 Understanding the distribution, kinematics and origin(s) of the hot
      T>dex5K) interstellar gas in our Galaxy is one of the major goals of the
      FUSE mission. A large amount of hot gas is expected to be present in the
      Galaxys central region, as a result of stellar winds from OB stars, supernovae,
      and possibly even activity in the central black hole. The expected levels of
      activity may even produce an outflow of gas. We have a program to investigate
      OVI in the central few kpc of our Galaxy, by pairing extragalactic sightlines
      with galactic targets at known distances. This strategy allows us to
      differentiate between hot gas in the foreground and gas in the central region or
      beyond. We have identified several such pairs. High-positive and high-negative
      velocity OVI is seen in most extragalactic targets but not in the stellar
      targets, suggesting the presence of gas associated with the Center. However, the
      data are not good enough to be confident of this conclusion. We thus request
      additional data for four of the targets at declination >-50deg, as well as
      an exposure on a new target.
      

	 Prop ID:        G012  Proposer:       Crenshaw   
	 Institution:    Georgia State University   
	 Proposal Title: Variable Absorption in the Seyfert Galaxy NGC 3516                                                                                                 

	 The most popular models for the intrinsic UV and X-ray absorption
      lines in AGN invoke accretion-disk winds that are driven outward by
      radiation pressure, magnetocentrifugal forces, andor thermal
      pressure. However, recent observational evidence suggests that most of
      the UV absorption in Seyfert galaxies arises from much further out
      than predicted by these models, at distances of tens of parsecs (in
      the inner narrow-line region). Is there any evidence for absorption
      close to the nucleus, providing at least indirect evidence for
      accretion-disk winds NGC 3516, with high-column UV and X-ray
      absorbers at distances less than 0.2 pc from its active nucleus, is a
      prime candidate for detecting accretion-disk outflows, possibly due to
      a special viewing angle with respect to its accretion-disk axis. We
      propose new FUSE observations of NGC 3516 over a range of time scales
      days to months) much smaller than previously obtained (years) to pin
      down the distances, dynamics, and physical conditions of its UV
      absorbers, and thereby test the accretion-disk wind scenario. NGC 3516
      provides multiple opportunities to obtain four 20 ksec CVZ
      observations over a range of time scales during Cycle 7.
      

	 Prop ID:        G013  Proposer:       Iping   
	 Institution:    Catholic University of America   
	 Proposal Title: Probing the Halo and ISM of Low-Redshift Galaxies with Young Supernovae                                                                         

	 We propose a Target of Opportunity program to study the halo and ISM
      of a low-redshift galaxy hosting a bright new supernova (V lesssim
      3).  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:        G014  Proposer:       Hebrard   
	 Institution:    Institut dAstrophysique de Paris   
	 Proposal Title: Surveying the sight lines of subdwarfs beyond the Local Bubble                                                                              

	 Deuterium abundance measurements allow constraints to be put on the
      Big Bang Nucleosynthesis, the baryonic content of the Universe, and
      the chemical evolution of galaxies. Such measurements in a variety of
      astrophysical environments was one of the main justifications for
      FUSE.  This program is dedicated to the interstellar deuterium
      abundance, representative of the Present Epoch, noted DH_PE.
      The first FUSE results show that DH_ISM likely has a single value in
      the Local Bubble, near 1.5times10^-5.  Beyond 100pc, however,
      analyses of more than 10 sight lines show a range of DH values that
      disagree with the local value. Two interpretations are proposed.  One
      assumes deuterium is depleted onto dust grains and finds DH_PE above
      2times10^  -5 . The second emphasizes the DO measurements and finds
      dshpe below 1times10^:  -5 .  Both would challenge models of
      deuterium evolution.
      Definitive conclusions are prevented by the limited number of
      measurements. We propose here to increase the sample of deuterium
      measurements along distant sight lines. Subdwarfs are targets that are
      especially well adapted for this purpose.  This survey program will
      allow deuterium abundances to be measured toward new distant sight
      lines, as well as extra candidates for deuterium measurements outside
      the Local Bubble to be selected for futureobservations.
      

	 Prop ID:        G015  Proposer:       Redfield   
	 Institution:    McDonald Observatory, University of Texas   
	 Proposal Title: Variations in the Ionization Structure within the Local Interstellar Cloud and Neighboring Clouds                                 

	 We propose to observe six nearby high latitude stars to measure the
      variation in ionization structure within the Local Interstellar Cloud
      LIC) and other neighboring clouds.  Of particular interest are the
      first three ionization stages of carbon and nitrogen, which are
      controlled by the (partially shielded) interstellar radiation
      field. FUSE is the optimal instrument for this kind of study because
      only FUSE can access the resonance lines of CIII (977.020AA), NII
      1083.99AA), and NIII (989.789AA). Since all of our targets have high
      resolution STIS or GHRS spectra, the velocity structure of all
      components are well characterized.  With both the HST and FUSE
      spectra, we can measure column densities of several ions, including CI
      FUSE and HST), CII (FUSE and HST), CIII (FUSE), NI (FUSE and HST),
      NII (FUSE), and NIII (FUSE), sampling many important ionization
      stages.  These observations will detect differences in the ionization
      structure within the LIC and other nearby clouds, and we will test
      whether these differences can be explained by different amounts of
      hydrogen continuum shielding of photoionizing radiation from bright
      sources like betaCen.  The ionization structure of the Local
      Interstellar Medium (LISM) is vital to understanding the formation,
      energy balance, and evolution of the LISM.
      

	 Prop ID:        G016  Proposer:       Rauch   
	 Institution:    Eberhard-Karls-Universitat   
	 Proposal Title: On the Evolutionary Status of Extremely Hot Helium Stars - are O(He) Stars Successors of RCrB Stars?                                                
	 
       95% of all stars end their lives as white dwarfs. About 20% of the 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 10-20
      O(He) stars, is 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:        G017  Proposer:       Jenkins   
	 Institution:    Princeton University   
	 Proposal Title: Why is Some Neutral Hydrogen in Interstellar Atomic Clouds so Extraordinarily Cold     

	 We propose to observe 2 stars 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:        G018  Proposer:       Knauth   
	 Institution:    Northwestern University   
	 Proposal Title: The Enigma of the Interstellar N_2 Abundance                                                                                                          

	 N_2 is the most abundant molecule in environments as diverse as the
      atmospheres of Earth and Titan.  Yet, until recently, little was known
      about its abundance in the ISM since the only accessible N_2
      transitions lie in the far-UV.  Utilizing the high-sensitivity of the
      FUSE detectors, Knauth and collaborators reported on the first
      detections of interstellar N_2 toward the stars HD124314 and 20Aql.
      The observed N_2 fractional abundances are almost two orders of
      magnitude larger than expected from models of interstellar nitrogen
      chemistry for diffuse clouds and do not agree with predictions from
      dark cloud chemistry either.  Here, we propose high SN (30), SiC
      only, FP-SPLIT observations toward four carefully chosen
      moderately-reddened stars which have substantial amounts of
      interstellar CO (spanning almost two orders of magnitude in column
      density).  The N_2 detection threshold N(N_2) > 6x10^12 cm^-2 is a
      factor of five more sensitive than previous measurements.  Our
      proposed observations will set stringent limits on the N_2 abundance
      along sightlines with substantial amounts of molecular material and
      provide clues toward either new N_2 production routes or for
      modification of the poorly known production andor destruction
      reaction rates.  
      

	 Prop ID:        G019  Proposer:       Knauth   
	 Institution:    Northwestern University   
	 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 Osmall 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 Nsmall I doublet at
      160AA in order to derive accurate nitrogen abundances and provide a
      direct comparison with the existing data.  All stars in our sample
      have high-precision STISHST measurements of the weak Osmall I
      356AA line for a variety of stellar distances (0.2 leq d leq
      .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:        G020  Proposer:       Bowen   
	 Institution:    Princeton University   
	 Proposal Title: A Search for Hot Baryons in the Halos of Nearby Galaxies     

	 We propose searching for OVI (and Lyman beta) absorption lines from
      the halos (simeq 8-280h radii) of five nearby galaxies, using
      background QSOs or AGN as probes. The detection of OVI around
      galaxies is likely to have important implications for our derstanding
      of how galaxies form and evolve. Models predict that gas creting to
      galaxies from the formation of galactic large scale structure (or om,
      g., the assimilation of dwarf satellites) should be shock-heated to
      mperatures at which oxygen would be detectable as OVI. At the same
      me, galaxies should also be feeding hot gas back into the
      intergalactic medium via winds driven by supernovae. Some of these
      processes may well be responsible for the High Velocity Cloud
      complexes seen in the Milky Way.  Despite the importance of such
      mechanisms, however, we have very little direct evidence of how hot,
      metal-enriched gas behaves close to a galaxy, or even that it exists
      beyond a few kpc. With this proposal, we seek to search the halos of
      various types of galaxies for OVI-absorbing gas, using the few probes
      which are bright enough to be observed by FUSE and which are at
      declinations above 50 deg.  Although the number of galaxies probed
      will be small, our observations will provide a first estimate of how
      far OVI extends from a galaxy, its covering fraction, whether the
      column density declines with distance, and whether the absorption
      complexes show unusual velocity structure, as might be expected from
      the more dynamical processes such as galactic outflows.
      

	 Prop ID:        G021  Proposer:       Skillman   
	 Institution:    University of Minnesota   
	 Proposal Title: The True Chemical Abundances of Dwarf Galaxies                                                                                                      

	 FUSE has discovered a putative offset between the neutral and ionized
      gas phase chemical abundances of nearby dwarf starburst galaxies.
      This important and intriguing result is in the sense that the neutral
      gas phase abundances are significantly (approx 1 dex) lower than
      the HII region abundances.  Thus, the starburst environment may be
      surrounded by a lower metallicity halo.  This could be a result of
      either chemical pollution of the medium closely surrounding the
      starburst or a metallicity gradient from the inner (relatively) metal
      rich galaxy to an outer metal poor halo.  This potentially high impact
      result is not yet secure because the neutral gas absorption lines may
      yield underestimates of the abundances due to ionization, depletion,
      andor saturation effects affecting the various chemical elements.
      For several reasons, oxygen is the ideal element to concentrate on,
      and by observing multiple OI lines with different oscillator
      strengths - and thereby addressing saturation concerns - we can obtain
      a secure absorption line oxygen abundance for the neutral gas phase
      for the first time.  A deep FUSE integration of a carefully selected
      and previously observed target (NGC3353 equiv Haro3 equiv
      Mrk35) will allow us to measure neutral oxygen lines over a range in
      oscillator strength, and thus support or question this very important
      FUSE discovery.
      

	 Prop ID:        G022  Proposer:       Blair   
	 Institution:    Johns Hopkins University   
	 Proposal Title: FUSE Survey of Magellanic Cloud Supernova Remnants Continued 
                                                                               
	 We propose to continue an unbiased ultraviolet survey of supernova
      remnants in both Magellanic Clouds that was begun in FUSE Cycles 4 and
      .  In these earlier programs, we have successfully detected at least
      5 Magellanic remnants, 14 of which had no previous FUV observations.
      This work indicates that optical andor X-ray characteristics of
      supernova remnants are not always good predictors of the objects that
      will be bright and detectable in the UV.  This survey proposal will
      add to this unique database by obtaining spectra of additional
      Magellanic Cloud remnants with a range of radio, optical, and X-ray
      properties.  A standard request of 10 ks per object using the LWRS
      aperture is used for the survey, reaching a limiting flux in OVI
      lambda 1032 about a factor of 100 below the flux observed for the
      bright LMC remnant N49.  In this proposal, we request time to observe
      any or all of the previously proposed targets that have not yet been
      observed (10 SMC objects plus 1 LMC object), and 11 new LMC remnants
      identified only recently as part of the MCELS project.  As a survey
      program, the time and number of targets listed is effectively an upper
      limit to the actual request.
      

	 Prop ID:        G023  Proposer:       Ayres   
	 Institution:    University of Colorado (CASA)   
	 Proposal Title: High-Declination Late-Type Supergiants in the Mass Range 5-7 Suns                                                                                

	 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 Mg 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 (T 10^5K) emission lines.  Even among these
      active supergiants, however, L_XL_CIV 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 active
      class, are important issues in stellar high-energy astrophysics; where
      the diagnostic power of FUSE spectroscopy can be put to good use.  We
      propose to add to the mix two key late-type supergiants---Beta Cam
      G0Ib) and Beta Ind (K1II)---not previously observed by FUSE; and a
      new pointing on the archetype hybrid chromosphere star Alpha TrA
      K2II), recorded by FUSE in 00 and 02, but now a planned target (as
      is Beta Ind) for an upcoming joint ChandraHST imaging program.
      vskip 0mm
      

	 Prop ID:        G024  Proposer:       Friedman   
	 Institution:    Space Telescope Science Institute   
	 Proposal Title: Probing Small-Scale ISM Variations with Multi-Epoch FUSE Observations                                                                     

	 The existence of small scale structures in the interstellar medium
      ISM) has now been verified using a variety of techniques, including
      optical, radio, and ultraviolet instruments.  They have been observed
      on scales ranging from tens of AU to parsecs.  One of the best ways to
      probe the smallest scales is with multi-epoch observations, in which
      one discerns spectral changes arising from material between an
      observer and a background source.  The number of such observations in
      dominant species in the ISM, as revealed by absorption line studies in
      the ultraviolet, is very small.  In addition, the physics of these
      structures, including their confinement mechanisms, lifetimes,
      pressures, and composition, is not well-understood.
      We propose a survey program to re-observe 18 stars already observed
      with FUSE more than 3 years earlier to search for time dependent
      changes in their spectra.  We will do profile fitting,
      curve-of-growth, and apparent optical depth analyses to search for
      changes in H2 and a variety of other species, such as CI, FeII, PII,
      ClI, and ClII.  These will allow estimates of electron temperatures,
      volume densities, and depletions.  The stars were selected on the
      basis of early spectral type, and existing high SN FUSE spectra
      obtained in TTAG mode, which will allow the best opportunity to detect
      subtle changes in the spectral features.  The newly obtained data will
      be useful for a variety of investigations beyond those described here,
      by providing a dataset of multi-epoch, high SN spectra of early-type
      stars.
      

	 Prop ID:        G025  Proposer:       Iping   
	 Institution:    Catholic University of America   
	 Proposal Title: FUV Study of the Extreme Wolf-Rayet Binary CQ Cephei                                                                                            

	 We propose a series of FUSE observations of the Wolf-Rayet + O star
      binary CQ Cephei to determine the structure of the bow shock zone
      formed when the winds of the two hot stars collide.  CQ Cephei has the
      shortest period of all the known WR+O binaries and would be the first
      WN+O binary to be studied in this way by FUSE.  Analysis of the FUSE
      spectra will lead to improved constraints on orbital parameters and on
      characteristics of the WR star itself (wind momentum, mass-loss rate,
      and abundances). Of particular importance in the FUSE wavelength range
      is the large number of emission lines with different ionization
      potentials from abundant elements, ranging from OVI, S IV, P V, C III,
      to N II.  The S and P lines are important because these elements are
      produced only in SN explosions and are not enhanced by CNO processes.
      The proposed observations will cover a significant part of the
      .64-day orbital period to map the wind interaction zone from
      phase-dependent spectral variations.
      

	 Prop ID:        G026  Proposer:       Iping   
	 Institution:    Catholic University of America   
	 Proposal Title: Mass Loss Processes in Luminous Blue Variables and Late-Type Wolf-Rayet Stars                                                                   

	 We propose a FUV survey of evolved massive stars in the Galaxy, LMC,
      and SMC.  The targets include Luminous Blue Variables (LBVs) and
      late-type Wolf-Rayet (W-R) stars.  LBVs, a transition stage between O
      and W-R stars, are in the early stages of post-main sequence
      evolution. They undergo brief, high mass-loss-rate episodes that bring
      processed material from deep within the stars to the surface.  The
      far-UV spectra will be used to determine stellar wind mass-loss rates
      and terminal velocities at different metallicities.  The role of
      rotation, asphericity and clumping in the wind will also be
      investigated.  Spectral features tracing a range of wind ionization
      states will be modelled with the latest version of the non-LTE, line
      blanketed, geometrically extended, expanding atmosphere code CMFGEN.
      The FUSE spectral range is ideally suited to test these models and
      determine metallicity effects connected with the complex mass loss
      from LBVs and W-R stars.
      

	 Prop ID:        G027  Proposer:       Giroux   
	 Institution:    East Tennessee State University   
	 Proposal Title: An Abundance Study of the Magellanic Stream                                                                                                   

	 We propose FUSE observations of the Seyfert Galaxy Fairall 9.  This
      sightline probes the Magellanic Stream, the most prominent example of
      the class of high velocity clouds (HVCs).  While the origins of the
      HVCs in general are still unclear, progress in the understanding of
      the Magellanic Stream has been made possible by the SII abundance
      measurements and SiII limits made using Hubble Space Telescope (HST)
      spectra of Fairall 9 (Gibson, Giroux, et al. 2000).  Preliminary FUSE
      observations toward Fairall 9 have also been used to characterize the
      H_2 abundances in the Magellanic Stream, as well as detect the
      presence of collisionally ionized gas in the form of OVI.  Extended
      observations in the FUSE band, however, promise to open up transitions
      of the dominant ionization stages of N, O, Si, Fe, Ar, and P in the
      neutral phase of the Stream.  This will allow both measurement of the
      metallicity of the Magellanic Stream and an estimate of the relative
      abundances of these elements.  This information will allow an initial
      assessment of the depletion of refractory elements as well as the
      nucleosynthetic history and possibly the dynamic history of the gas.
      Further, this observation will permit a detailed study of a multiphase
      region associated with the Stream, whose properties can be compared
      with regions associated with sightlines through the Galactic Halo.
      Such tidally-stripped gas may also be a local example of multi-phase
      absorbers in the intergalactic medium.
      

	 Prop ID:        G028  Proposer:       Korpela   
	 Institution:    University of California   
	 Proposal Title: Atomic and molecular gas toward the north ecliptic pole                                                                                             

	 SPEAR observations of the North Ecliptic Pole (Korpela, 2005) have
      resulted in a number of detections of atomic emission and molecular
      fluorescence lines, including a possible detection of fluorescent
      emission from molecular nitrogen. It is difficult to reconcile some of
      these emission feature with collisional processes at the abundances
      thought to be typical of the ISM. We will use two short-duration
      absorption observations of early type stars, one of a star with low
      reddening (E(B-V)0.04), one with higher reddening (E(B-V)0.5) to
      confirm line identifications and constrain our models of the emission
      seen by SPEAR.
      

	 Prop ID:        G029  Proposer:       Leighly   
	 Institution:    The University of Oklahoma   
	 Proposal Title: Tropical Storm to Hurricane The Emergence of a BAL Wind                                                                                           

	 We propose a 60 ks FUSE observation to quantify the outflow properties
      of the unusual Narrow-line Seyfert 1 Galaxy WPVS007.  Observed to
      have a miniBAL with maximum velocity v_max sim 1000  , km,
      s^-1 in an HST observation from 1996, it was discovered to have
      developed an additional BAL flow by the time of the FUSE observation
      seven years later.  The BAL flow has a maximum velocity of at least
      ,000  , km, s^:  -1 , and the unambiguous presence of ion P  5 
      indicates that it is very optically thick.  In addition, it was found
      to have normal X-ray flux during the ROSAT All Sky Survey, but in
      subsequent observations from 1993 to 2003 it was observed to be X-ray
      weak, suggesting that the X-rays were absorbed by the emerging BAL.
      This observation is remarkable, because the emergence of a BAL flow
      has never been observed before.  Furthermore, the observation of a BAL
      flow in such a low luminosity object (M_V-19.7) is unprecedented.  We
      propose another FUSE observation to look for further variability and
      development of the BAL flow. We will study the ionP5 lines which
      may not be saturated and therefore may be sensitive to changes in the
      BAL flow.  We expect that these observations will place strong
      constraints on the kinematics, energetics, and physical conditions of
      BAL outflows, as well constraints on the geometry and stability of the
      outflows.
      

	 Prop ID:        G030  Proposer:       Dupke   
	 Institution:    University of Michigan   
	 Proposal Title: The North Ecliptic Pole Supercluster A Window to Detect the Local Missing Baryons 

	 Simulations predict that nearly half of the baryons in the local
      universe are in a moderately hot phase, 10^5-10^7 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 50
      discovered 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 contraints of FUSE, which is, with the demise of STIS,
      the only satellite that is able to detect the key absorption lines for
      this study.
      

	 Prop ID:        G031  Proposer:       Irwin   
	 Institution:    University of Michigan   
	 Proposal Title: Can FUSE Tell Us if Intermediate Mass Black Holes Exist    

	 Ultraluminous X-ray sources (ULXs) are the brightest non-nuclear X-ray
      point sources in galaxies, and are second only to AGNs in bolometric
      luminosity.  However, despite a concerted effort in the last few years
      to determine the nature of these enigmatic objects, it is still
      unclear exactly what they are. If they are accreting 10 M_odot black
      holes X-ray binaries like those found in our own Galaxy, then they are
      emitting at luminosities approaching 100 times their Eddington
      luminosity (most probably through beaming of the X-ray emission).
      Alternatively, it has been suggested that these ULXs harbor
      intermediate mass black holes with masses 100--10000 M_odot, whose
      exist would bridge the gap between normal stellar-mass black holes and
      supermassive black holes.  At the same time, the existence of
      intermediate mass black holes would challenge our notions of how black
      holes form. The expected flux and velocity structure of OVI emission
      from the accretion disk of the black hole could provide an important
      diagnostic for distinguishing between beaming and intermediate mass
      black hole scenarios.  We propose the first far-ultraviolet
      observation of any ULX, a 70 ksec observation of a ULX in Holmberg II
      as a test case for using OVI emission as an indicator of the presence
      of intermediate mass black holes within ULXs.
      

	 Prop ID:        G032  Proposer:       Brown   
	 Institution:    University of Colorado   
	 Proposal Title: Magnetic Fields on Alien Dwarfs -- Stellar Activity in the Arcturus MG         

	 The Arcturus Moving Group is very likely a remnant of the merger of a
      dwarf galaxy with the Milky Way Galaxy in the distant (7- 8 Gyr)
      past. This kinematically distinct group has members that are located
      very close to the Sun, allowing study of stellar magnetic activity on
      very old stars that typically would not be possible. We propose to use
      FUSE spectra to study three dwarf members of the Arcturus Moving Group
      with the aim of determining their transition region (UV emission line)
      activity levels, and the effects of low metallicity on the transition
      region radiative losses. Our targets have metallicities of 20
      spectral types G1 - K0, and are at distances less than 35 pc from the
      Sun. Our aim is to measure fluxes for the O VI 1032, 1038AA and C III
      77, 1175AA emission lines, which are excellent diagnostics of the
      radiative losses from 0.5 - 3 10^5 K plasma. The measured optical
      chromospheric Ca II emission levels of the targets are comparable to
      or higher than that of the quiet Sun.
      

	 Prop ID:        G033  Proposer:       Bianchi   
	 Institution:    Johns Hopkins University   
	 Proposal Title: The UV-brightest Milky Way hot stars detected by GALEX                                                                                              

	 We propose to observe with FUSE the hottest, UV-brightest stellar
      objects selected from the UV sky surveys produced by GALEX and
      overlapping with the SDSS optical survey. We analyzed a total of 744
      GALEX fields with a unique overlapping area to the SDSS of over 400
      square degrees.
      We classified the UV sources, and estimated their physical parameters,
      by comparing their multi-band photometry (two GALEX bands, FUV and
      NUV, and five SDSS optical bands (u, g, r, i, z) to model colors
      Bianchi et al. 2005a, b).  The number density of some classes of
      astrophysical objects is increased by factors up to 100 with respect
      to previous catalogs, in particular very hot stars such as white
      dwarfs (single and in binaries). We selected the 20 UV-brightest hot
      objects from the fields at the high declinations accessible by FUSE.
      FUSE spectra, with GALEX and optical follow-up spectra already
      available or under way, will uniquely enable us to accurately model
      the atmospheres and winds (when present) of these hot stars, extending
      the -so far very limited - detailed measurements of stellar
      parameters, that led to a number of important results such as a
      revised Teff - spectral type calibration for pop-I O stars
      e.g. Garcia and Bianchi 2004), and the discovery of highly ionized
      neon in post-ABG objects, a crucial diagnostic for very hot stars with
      weak winds (Herald et al. 2005).  Determing neon abundances in WD
      stages where the winds are fading is an important diagnostic for
      stellar evolution.
      The proposed sample will also significantly augment the potential of
      the FUSE archive with new high Galactic latitude sight lines for ISM
      studies, and provide an unprecedented FUSE-GALEX legacy data-base of
      UV-selected MW objects.
      

	 Prop ID:        G034  Proposer:       Bianchi   
	 Institution:    The Johns Hopkins University   
	 Proposal Title: Far-UV extinction by dust in unexplored LMC environments                                                                                        

	 We propose to study the far-UV extinction in selected sightlines in
      the LMC, sampling three environments with differing levels of star
      formation activity, including the general field, hitherto
      unexplored. Extinction properties in the far-UV will give information
      about the distribution of small dust grains.  The investigation is
      important to understand the role of dust in the star formation and ISM
      enrichment history of galaxies, and the relations of extinction to
      global galaxy properties such as metallicity and starburst intensity.
      It will be ultimately useful to interpret integrated properties of
      distant galaxies, such as those measured by the GALEX UV surveys.
      We will derive extinction curves using pairs of stars in the
      LMC. Studies of extinction in the UV range (> 1200AA) indicate a
      complex dependence of the dust properties with environment, where
      metallicity and starburst activity are relevant factors.  Therefore,
      we have chosen pairs of stars inside, and far from, bright OB
      associations, to explore relations of dust properties with
      environment. 
      acquired complementary HST STIS and ACS spectra (1200-3200AA) of the
      proposed targets (HST cycle 12 GO9827). 
      properties The combined HST (UV) and FUSE (far-UV) results will
      provide a unique opportunity to study the properties of small grains.
      

	 Prop ID:        G035  Proposer:       Gaetz   
	 Institution:    Smithsonian Astrophysical Observatory   
	 Proposal Title: Dynamics of a Young, O-Rich Supernova Remnant in the Small Magellanic Cloud                                                       

	 The supernova remnant 1E0102.2-7219 in the Small Magellanic Cloud is
      the best studied O-rich remnant after Cas-A, having been observed in
      bands from radio through X-ray.  In spite of its simple appearance
      round remnant, bright reverse shock) the remnants structure is
      complex.  X-ray kinematics suggest an expanding toroid viewed nearly
      on-axis, while optical kinematics suggest an expanding shell with a
      bubbly internal structure.  We will use FUSE to examine the
      velocity structure on sight-lines through the center of the remnant
      which will complement our Cycle 3 observations of the bright X-ray
      ring.  These observations will provide OVI kinematic data for
      comparison to the optical OIIIf and X-ray grating kinematic data.  The
      MDRS slit samples a significant fraction of the projected area, but is
      small enough to isolate interesting structure.  Recent OIIIf proper
      motion data yield an expansion center near the X-ray knot in a central
      X-ray filament, and the kinematic center is included in all the
      proposed observations.  This will allow a search for evidence (such as
      variability) for a compact central object which should have been
      produced by the collapse of a massive star.
      

	 Prop ID:        G036  Proposer:       Moffat   
	 Institution:    Universite de Montreal   
	 Proposal Title: Does Metallicity Affect Clumping in Hot-Star Winds                                                                                                     

	 All hot, luminous stars drive strong winds, that have a major impact
      on their evolution and their surroundings. This was especially
      important in the early Universe, that was dominated by massive stars
      with very low metallicity. But what were the actual mass-loss rates
      then  Small-scale structures (clumps) are considered as the main
      factor which can reduce the observed mass-loss rate, by a factor of at
      least 3.  No one knows whether and how clumping changes with the
      decreasing fraction of wind-driving metals.  We propose to approach
      this important question by detecting clumps in hot-star winds of 2
      selected single WN stars in the SMC, where metallicity is one-tenth
      solar.
      

	 Prop ID:        G037  Proposer:       Pellerin   
	 Institution:    Space Telescope Science Institute   
	 Proposal Title: FUV Spectral Variations of Wolf-Rayet Type Stars                                                                                          

	 The understanding of Wolf-Rayet type stars is fundamental since they
      are involved in chemical enrichment processes of interstellar and
      intergalactic medium by releasing a lot of metals produced during the
      CNO cycle. The FUSE spectral range includes several spectral
      transitions from highly ionized atoms in the far-ultraviolet range
      that can improve the understanding of massive star evolution. However,
      the wavelengths below 1200AA remains a range quite unexplored for
      these stars.
      Recent far-ultraviolet spectra from FUSE show, for the first time,
      strong evidences for important stellar line profiles variations for a
      given WR subtype, which are not seen at optical wavelengths. These
      variations may be related to evolutionary stages of Wolf-Rayet stars.
      Unfortunately, the number of Wolf-Rayet stars observed below 1200AA is
      actually too small to study and characterize these variations within a
      spectral class. Using FUSE, we propose to observe additional
      Wolf-Rayet stars of WN-types to better characterize these spectral
      variations. A quantitative analysis of these spectra will be performed
      using the NLTE model atmosphere code CMFGEN.
      

	 Prop ID:        G038  Proposer:       Herald   
	 Institution:    The Johns Hopkins University   
	 Proposal Title: Investigating the Neon Abundance of LMC WO stars                                                                                                 

	 WO stars represent the most evolved sub-type of Wolf-Rayet class,
      which are believed to descend from the most massive of the O-stars.
      WOs are the hottest (T>100,000K) and also the rarest; only seven are
      known among the Local Group, out of hundreds of known WR stars.  Their
      spectra are characterized by strong oxygen and carbon emission lines,
      which form in their fast (4000kms) stellar winds.  Despite their
      evolutionary importance, only two of these rare objects have been
      observed by FUSE; Sanduleak 2, a WO3, and Sanduleak 1, a WO4+O binary.
      Unfortunately, during the observation of Sanduleak 2, the SiC detector
      was misaligned, resulting in no useful data for the short wavelengths
      of the FUSE range.  As these stars represent the only WO stars
      currently observable by FUSE, we request a re-observation of Sanduleak
      .  The SiC detectors cover the wavelength range where the important
      SVI lambda lambda 933,944 doublet lies, as well as NeVII lambda973.
      This neon feature has been recently identified in the FUSE spectrum of
      a rare transitional WO-PG1159 central star of a planetary nebula.
      If it appears in the spectrum of Sanduleak 2, it may allow the neon
      abundance, an important evolutionary diagnostic, to be determined for
      a star in the most advanced WR phase.  We shall use stellar atmosphere
      codes to model the FUSE spectrum of Sanduleak 2 to better determine
      parameters such as mass-loss rate, stellar temperature, and chemical
      abundances, allowing a better evolutionary understanding of this rare
      class of objects and WR stars in general.
      

	 Prop ID:        G039  Proposer:       Herald   
	 Institution:    The Johns Hopkins University   
	 Proposal Title: Wolf-Rayet Stars in Environments of Different Metallicity                                                                                        

	 Wolf-Rayet (WR) stars, thought to descend from the most massive stars,
      are important drivers of galactic evolution through their injection of
      mechanical energy, chemically enriched material and ionizing photons
      into their surroundings.  They are a key to understanding massive
      stellar and galactic evolution, as well as nucleosynthesis processes.
      An important aspect in the understanding of WR stars is the influence
      of the metallicity of their environment on their parameters and
      evolution.  To shed light on this question, we wish to study and
      compare two like samples of WR stars from environments of differing
      metallicity; the Milky Way and Small Magellanic Cloud (SMC).  FUSE
      observations provide crucial diagnostic lines for measuring mass-loss
      parameters, effective temperatures, and certain abundances.  We will
      model the FUSE spectra to derive the stellar parameters of these
      objects, which will help answer the following outstanding questions;
      i) What effect does metallicity have, if any, on the wind properties
      of WR stars  (ii) Do wind clumping parameters (which directly affect
      derived mass-loss rates) determined from far-UV diagnostics agree with
      those derived from IR diagnostics  (iii) Do observed WR parameters
      agree with predictions of theoretical evolutionary models  (iv) Do
      observed SMC WR properties agree with those currently adopted in
      low-metallicity stellar synthesis models  (v) Do X-ray parameters
      derived from stellar atmosphere models agree with observed X-ray
      fluxes
      

	 Prop ID:        G040  Proposer:       Godon   
	 Institution:    Villanova University   
	 Proposal Title: FUSE Survey of DN basic characteristics of the WD and accretion disk                                                                                      
	 The white dwarfs (WDs) in cataclysmic variables (CVs) are probes of
      cataclysmic evolution and accretion physics because 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 dwarf nova (DN) systems (a class of CVs
      in which the WD can easily be observed) for which FUV spectra in
      quiescence have never been obtained before.  These systems have not
      been studied in detail (only five have a known period) and little is
      known about their accreting WD. We propose to determine the WD surface
      temperature, gravity, rotation rate and composition and probe their
      innermost disk accretion flows (e.g. detect and characterize accretion
      belts) 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 and determine the orbital period of those systems
      for which it is unknown.
      

	 Prop ID:        G041  Proposer:       Godon   
	 Institution:    Villanova University   
	 Proposal Title: BZ UMa an Intermediate Polar Candidate  

	 We propose FUSE observations of the Dwarf Nova (DN) BZ UMa which is a
      candidate for Intermediate Polar (IP).  In quiescence, BZ UMa has an
      apparently large N,sc vC,sc iv which is atypical of most DNe
      and its FUV spectrum is dominated by the white dwarf (WD). High
      frequency QPOs, high excitation lines and strong X-ray emission have
      been detected suggesting it is an IP.
      The truncated inner disk helps lower the luminosity and exposes the WD
      in the FUSE range, therefore allowing us to estimate the temperature
      of the WD (Teff) and the chemical abundances (to check signs of
      elevated N and depleted C as well as elevated abundances of odd
      numbered nuclei from proton capture during CNO burning).
      Currently, there are only two IPs with known Teff and the present FUSE
      proposal aims at adding an additional object in order to better
      understand the accretion geometry and evolutionary history of these
      systems.
      

	 Prop ID:        G042  Proposer:       Godon   
	 Institution:    Villanova University   
	 Proposal Title: FUSE Observation of the eclipsing Dwarf Nova IY UMa 

	 IY UMa is a recently-discovered double-lined eclipsing CV with an
      extremely high inclination. The orientation allows us a view into a
      narrow shock-heated cavity driven into the disc edge by the accretion
      stream from the mass donor star. This (literal) probe is so far
      unique.  At the orbital phase when we look into the hot cavity, the
      emission from the cavity should be a significant fraction of the total
      UV flux. Comparison with our hydrodynamic simulations of the
      stream-disc impact will allow us to determine the structure of the
      cool quiescent outer disc.  We will fully characterize the white
      dwarf, measuring its rotation rate, surface gravity, effective
      temperature, chemical abundances and accretion rate.  The obscuration
      of the inner UV emitting regions by vertical structure associated with
      spiral density waves will be measured and interpreted by comparison
      with our simulations.
      

	 Prop ID:        G043  Proposer:       Shull   
	 Institution:    University of Colorado   
	 Proposal Title: Interstellar H_2 near the Lockman Hole 

	 We propose to observe 3C263, a bright, high-latitude AGN located at
      high declination (+65.8 deg) near the Lockman Hole.  This sightline is
      part of an extended region of low H2 column densities identified in
      our FUSE survey of high-latitude H2 (Gillmon et al. 2006).  The
      regions of low NH2 appear at Galactic latitudes b > 55 deg and extend
      from 60 deg < l < 180 deg.  The Lockman Hole (low NHI) and
      Northern Galactic Chimney (low N_NaI) are both contained within
      this extended H2 Hole, identified in 8 AGN sightlines (b > 50 deg)
      with NH2 < 10^15 cm^-2 in our FUSE survey.  The 3C263 sightline
      probes a low NHI region toward the edge of the Lockman Hole.  With
      this and other data, we will characterize the structure and extent of
      infalling high-velocity clouds (HVCs) in the Galactic halo and
      cross-correlate H2 with the presence and strength of OVI, which is
      also patchy at high latitude.  Low-H_2 sightlines may be associated
      with low NHI and N_NaI and with IR cirrus emission (Gillmon & Shull
      006).  At SN > 6 per resolution element, our spectra will be
      sensitive to log NH2 > 14.0 with line-stacking of several Lyman
      bands. High-latitude sightlines with low NH2 are also valuable for
      studies of the IGM, owing to their low H2 line contamination.
      Together with previous high-latitude, low-NH2 sightlines, our target
      will better define the H2 and Lockman hole, the mass of high-latitude
      H2, and the relation of this gas to the distributions of HI, OVI,
      infrared cirrus, and other large-scale Galactic halo structures.
      Models of H2 rotational excitation will be used to derive the gas
      temperature, density n_H, and UV radiation field and at high Galactic
      latitude, in a new regime of optically-thin, low-NH2 gas inaccessible
      to FUSE in the Galactic disk.
      

	 Prop ID:        G044  Proposer:       Shull   
	 Institution:    University of Colorado   
	 Proposal Title: Detecting the Elusive Hot Baryons in OVI   

	 One of the important discoveries of FUSE and HST was the detection of
      intergalactic OVI absorbers, possibly associated with the warm-hot
      intergalactic medium (WHIM) at 10^(5-6)K.  Danforth & Shull (2005)
      found 40 OVI absorbers in 31 sightlines, spanning Delta z approx 2.2,
      and estimated that 5-10
      gas. With a steep column-density distribution calN (N_OVI)
      proportional to N_OVI^-2.2 pm 0.1, weak absorbers contain much of the
      total mass. Thus, it is important to measure OVI absorbers down to
      weak levels (Nosix approx 10^13 cd) in order to (1) obtain an
      accurate baryon census of the hot IGM; (2) test the predictions of
      cosmological simulations for WHIM redshift evolution; (3) probe the
      distribution of IGM metals; (4) compare the metallicities with the
      large-scale distribution of galaxies.  We propose to observe 6
      high-declination AGN to probe OVI, CIII, and HI absorbers. Danforth &
      Shull (2005) estimated that 5--10
      OVI-bearing gas, and they estimated the metallicity at sim0.1 solar.
      Previous OVI surveys are highly incomplete in these weak absorbers
      W_lambda < 80mAA) that contain a significant fraction of WHIM
      baryons. We will also measure HI Lyman beta and CIII lambda 977 to
      improve the multi-phase baryon census at z < 0.15.  FUSE and HST
      archival OVI data will be compared to test simulation predictions that
      the WHIM mass fraction increases at lower redshifts.  Galaxy redshift
      surveys will allow us to study the connections between OVI absorbers
      and the large-scale filamentary structure of galaxies, complete down
      to approx 0.2L^* at low redshifts, z < 0.15.  We will use the
      combined absorber and galaxy data to estimate the extent of metal
      dissemination in the IGM.  
      

	 Prop ID:        G045  Proposer:       Cheng   
	 Institution:    California State University, Fullerton   
	 Proposal Title: Circumstellar Absorption Lines in the Far-UV Spectra of Ae and A-Shell Stars                                                            

	 A-shell stars are characterized by the coexistence of two types of
      line profiles in their spectra, one originating in the stellar
      photosphere and the other originating in the cooler shell. These stars
      are of great interest because shell characteristics appear in three
      important types of A stars (1) Those with infrared excess arising from
      circumstellar dust (Vega-like objects), (2) beta Pic-like objects, and
      2) lambda Bootis stars (metal-deficient A stars with infrared
      excess).  Snow et al. (1979) used Copernicus data to study 17 Be and
      B-shell stars, which have a rich shell absorption spectrum between
      120 and 1140 AA.  We propose to carry out a similar far-ultraviolet
      study of the slightly cooler Ae and A-shell stars. Among the 14 bright
      Ae and A-shell stars observed in the visual and the near infrared by
      Jaschek and Andrillat (1998), only 2 stars (HD 103287 and HD 112028)
      can be observed with FUSE during cycle 7 due to the new pointing
      constraints.  Our new FUSE data will add important information to our
      previous FUSE studies (cycle 2, 4, and 5) of protoplanetaryplanetary
      debris disks.
      

	 Prop ID:        G047  Proposer:       Blake   
	 Institution:    MC California Institute of Technology   
	 Proposal Title: Evaluating the UV Energy Distribution of the Nearby T Tauri Star T Cha                                                                   

	 The UV and X-ray energy distribution generated by a young
      pre-main-sequence (PMS) star can have a profound effect on the
      excitation conditions in its circumstellar environment. High energy
      photons can play an important role in photoexciting molecules and dust
      grains in both the accretion disk and the lower density circumstellar
      gas. We propose FUSE spectroscopy of the nearby (66 pc), G8, PMS star
      T Cha, which has not been successfully observed in the UV
      previously. UV spectra provide vital information on the stength of the
      high temperature UV emission lines that are a dominant feature of PMS
      stellar spectra. This star shows an IR energy distribution that
      suggests that transiently heated (most likely by UV photons) dust may
      be present. We intend to use the measured O VI and C III emission line
      fluxesprofiles to estimate the likely overall UV spectrum and to
      model the photo-excitation effects of this spectrum on the
      circumstellar gas and dust.
      

	 Prop ID:        G048  Proposer:       Dupree   
	 Institution:    Smithsonian Astrophysical Observatory   
	 Proposal Title: A Test of Wind Dynamics in Accreting Young Stars                                                                                        

	 Young stars can not only undergo accretion but also drive fast hot
      winds.  The winds revealed by FUSE spectra in 2 T Tauri stars (TW
      Hya and T Tau) viewed pole-on can affect the evolution of angular
      momentum in a system, define the geometry of the stellar magnetic
      field, cause ablation of a surrounding accretion disk, and serve as an
      acceleration site for optical jets.  We propose to determine the
      configuration and characteristics of the fast wind with FUSE spectra
      of 2 edge-on T Tauri stars in the nearby Eta Cha cluster (RECX-11 and
      ECHA J0843.3-7905) that are well-matched in age to TW Hya. If the
      outflow is collimated from the stellar polar region, the shape of the
      O VI and C III lines in high inclination systems should differ
      markedly from those in systems viewed pole-on.  Additionally,
      signatures of H_2 can indicate its presence (or not) in the
      circumstellar environment.
      

	 Prop ID:        G049  Proposer:       Aracil   
	 Institution:    University of Massachusetts   
	 Proposal Title: The Large-Scale Distribution and Physical Properties of Gas in the Cosmic Web                                                                     

	 Hydrodynamic simulations of large-scale structure growth predict that
      at low redshifts, low-density shock-heated gas at T  10^5 - 10^7 K
      should be distributed in large-scale gaseous filaments that are
      correlated with the filaments observed in the galaxy distribution, the
      so-called cosmic web. To test this fundamental prediction of the
      cosmological simulations, we propose to study OVI, HI, and ancillary
      absorption lines in the spectra of QSOsAGNs that penetrate
      large-scale galaxy filaments revealed by the 2MASS survey.  Our target
      3C204) is well beyond the redshifts of the 2MASS galaxy structures.
      We will combine the new observation of 3C204 with high quality sight
      lines already observed with FUSE and HST. Very few existing
      observations probe the highest density regions in the 2MASS survey,
      and the proposal observation will bolster the statistics for these
      crucial regions. We will be able to statistically address the
      following questions- (1) Does the distribution of gas track the galaxy
      distribution in the filaments (2) What are the physical conditions of
      gas inside the filaments, and how do these compare to gas on sight
      lines through low-density regions and voids Is the gas predominantly
      collisionally ionized and hot, or is it photoionized and cold  Does
      this depend on environment as expected (3) What is the metallicity of
      the gas in these different environments (4) How do the observed
      properties of the absorption lines compare to the properties predicted
      by the simulations such as the clustering of the lines
      

	 Prop ID:        G050  Proposer:       Howk   
	 Institution:    University of Notre Dame   
	 Proposal Title: Far-Ultraviolet Study of the Magellanic Bridge                                                                                                         

	 Galaxies are known to interact with each other.  These interactions
      can have profound effects on the gaseous components of galaxies, often
      by inducing star formation or stripping material from the main bodies
      of the interacting systems.  Thus, these interactions have a
      significant connection to the manner in which galaxies evolve with
      time and pollute the intergalactic medium with non-primordial
      material.  The Magellanic Bridge, gas that links the Small and Large
      Magellanic Clouds (SMC, LMC), is believed to result from a recent
      close encounter between the SMC and LMC.  The Bridge provides an
      unique opportunity to study tidally-stripped, star-forming gas
      inasmuch as its proximity to our own Galaxy and the absence of sight
      line confusion with material from the Milky Way allow us to study it
      using UV absorption lines.  We propose to obtain new FUSE spectra of
      ESO31-8, a Seyfert galaxy situated behind the Bridge near the SMC, and
      DGIK975, a B2V star within the Bridge near the LMC.  Our observations
      will provide absolute interstellar Magellanic Bridge abundances.
      These abundances will be compared to those of the SMC and LMC to
      determine the origins of the Bridge and the source of its chemical
      enrichment. We will study and compare the kinematics and column
      densities of FUV absorptions such as OVI, CIII, SIII, FeIII, PII,
      SiII, FeII, ArI, and H_2, between several lines of sight within the
      Bridge and with sightlines within the Clouds to further understand the
      interaction and evolution of the Magellanic system.
      

	 Prop ID:        G051  Proposer:       Howk   
	 Institution:    University of Notre Dame   
	 Proposal Title: Tidal Debris and Halos about the Magellanic Clouds                                                                                                     

	 The Large and Small Magellanic Clouds represent the closest gas-rich
      galaxies to our own Milky Way.  The feedback of energy and matter from
      massive stars has created gaseous halos about these galaxies, as
      revealed by FUSE observations of OVI in both Clouds.  At the same
      time, the gravitational interactions between the Clouds have stripped
      gas from their outer regions to form the Magellanic Stream and other
      prominent gaseous features of the southern hemisphere.
      Tidally-stripped material such as this may plan an important role in
      the evolution of galaxies.
      We propose to observe two UV bright AGNs behind the periphery of the
      Magellanic Clouds in order to study gas in the far reaches of these
      galaxies.  These objects are drawn from our Cycle 4 survey to identify
      UV bright objects behind the Clouds.  Our proposed observations will
      allow us to 1) study the hot gas content of the very extended coronae
      and tidal material of the Clouds through the OVI absorption doublet;
      ) study the relative abundances and metallicity of gas in the distant
      reaches of these galaxies; and 3) compare the physical conditions and
      the large-scale energy content of this distant gas with sight lines
      within the Clouds.  We will compare the absorption properties of the
      gas in the outer reaches of these low-redshift, low-mass,
      low-metallicity galaxies with the low-redshift quasar absorption line
      systems.
      

	 Prop ID:        G052  Proposer:       Sankrit   
	 Institution:    Johns Hopkins University   
	 Proposal Title: OVI Emission from Conductive Interfaces in the Local Interstellar Medium                                                                            

	 We propose observations of OVI emission from conductive interfaces in
      the local interstellar medium.  These interfaces have been identified
      by their OVI absorption lines in the spectra of nearby white dwarfs.
      The OVI column densities in the interfaces have been measured.  We
      will target regions at small angular separations from the white dwarfs
      to ensure that the emission and absorption sample the same gas.  The
      target sight lines were chosen to have high background interstellar
      extinction, so the probability of contamination by emission from
      regions further away is minimized.  The combination of emission and
      absorption data for OVI will allow us to obtain the densities of the
      emitting regions, and the path length through them.  This detailed
      characterization of the interfaces between hot and warmcool gas will
      allow a greater understanding of the physical processes at work in
      creating and maintaining them.  Our understanding of OVI production in
      the local interstellar medium can then be applied to the general case,
      since such interfaces are likely to be ubiquitous in the Galaxy and
      beyond.
      

	 Prop ID:        G053  Proposer:       Danforth   
	 Institution:    University of Colorado at Boulder   
	 Proposal Title: OVI and CIII Emission from LMC Superbubble N70                                                                                            

	 Superbubbles are a major mechanism of feedback between massive stars
      and the ISM and are thought to be the primary means through which
      coronal gas flows from the disk into the halo.  Many are seen to be
      bright in soft X-rays and photoionized optical emission.  Between
      these two phases should exist a warm-hot (T  10^5 K) component formed
      either through shock heating or thermal conduction.  OVI lambda lambda
      032,1037 is an ideal tracer of this warm-hot gas as it is not formed
      through photoionization in the ISM.  However, absorption from the
      diffuse OVI in the LMC halo tends to overwhelm any absorption seen
      within a superbubble.  We have observed four sight lines toward LMC
      superbubble N70 and see an excess of OVI absorption in comparison to
      four nearby, field sight lines.  We interpret this excess OVI
      absorption, which amounts to log N_OVI14.05 or approx 60 percent
      greater than is seen in the comparison sight lines, as the signature
      of hot gas within N70, however, it is possible that this reflects
      normal variation in the halo of the LMC.  A detection of OVI in
      emission from N70 would seal the case for a warm-hot component in
      superbubbles.  Emission and absorption data together will constrain
      physical density and the mechanism through which OVI is produced in
      superbubbles.  We propose to place two LWRS apertures on N70 and
      attempt to measure diffuse OVI and CIII emission from the superbubble.
      

	 Prop ID:        G054  Proposer:       Gruendl   
	 Institution:    University of Illinois   
	 Proposal Title: Hot Gas in the Starburst Carina Nebula                                                                                                                

	 The Carina Nebula is the nearest example of a starburst region.  At a
      distance of approx 2 kpc, its stellar content and interstellar
      structure can be resolved and studied in detail. The mechanical
      energies injected by massive stars have yielded a large amount of hot,
      X-ray-emitting gas in the Carina Nebula. Optical and X-ray
      observations reveal a complex relationship between 10^4 K and 10^6 K
      gas components.  We request FUSE observations of the Carina Nebula to
      use emission lines to study both the physical conditions and kinematic
      properties of the hot gas in X-ray-emitting regions. In particular, we
      will use the OVI emission lines, in conjunction with complementary
      X-ray and optical data, to study SNR shocks and interfaces between hot
      >10^6 K) gas and the surrounding cooler (10^4 K) shell gas. The
      results will aid in our understanding of the generation and conditions
      of hot gas in distant, unresolved starburst regions.
      

	 Prop ID:        G055  Proposer:       McCandliss   
	 Institution:    Johns Hopkins University   
	 Proposal Title: Far-Ultraviolet Observations of N11B -- Searching for Extragalactic Molecular Hydrogen Emission                                                  

	 Recent studies of galactic reflection nebulae have revealed strong
      variations in the relative contributions from dust scattered starlight
      and fluorescent molecular hydrogen 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 fluorescence of molecular hydrogen.  We
      propose to extend this study beyond the Milky Way with FUSE
      observations of the star-forming nebula N11B in the Large Magellenic
      Cloud.  With several stars of spectral type B1 and earlier, we suggest
      that N11B is an external analog to the Orion Nebula (M42).  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 molecular hydrogen emission outside the Milky Way.
      These observations will complement our ongoing study of galactic
      nebulae by probing new environmental variables such as grain
      composition and metallicity.
      

	 Prop ID:        G056  Proposer:       Brown   
	 Institution:    University of Colorado   
	 Proposal Title: Stellar Activity in the 30 Myr old Tucana-Horologium Association

	 We propose a FUSE survey of stellar activity among the members of the
      Tucana-Horologium Association with dec < -50 deg, using the O VI and
      C III transition region emission lines as diagnostics of the
      transition region (10^5 K) activity. This set of stars is a 30 million
      year old subgrouping within the Local Association.  These spectra will
      significantly expand the sample of young active,
      zero-age-main-sequence (ZAMS), F-M stars with measured transition
      region emission line fluxes, and allow direct comparision with the
      younger (12 Myr) beta Pic Moving Group stars, from our Cycle 6 FUSE
      Legacy program, and other older stars from the AB Dor (50 Myr) and
      Pleaides (100 Myr) Moving Groups. These spectra will allow detailed
      studies of the influence of stellar activity on the immediate
      circumstellar environment of young stars during the crucial phases of
      protoplanetary system formation, when the formation of gas giant
      planets and smaller terrestrial planets is underway. The sample chosen
      for this study have identical ages and formed together during the same
      star formation episode.  By studying such samples of low and
      intermediate mass stars with identical ages and formation history, a
      clearer determination of the factors controlling stellar magnetic
      activity can be obtained, thus enabling better characterization of the
      evolution in stellar activity during the crucial early phases of
      stellar, circumstellar disk, and protoplanetary system evolution.
      

	 Prop ID:        G057  Proposer:       Dunne   
	 Institution:    University of Illinois at Urbana-Champaign   
	 Proposal Title: OVI Emission from the Interface Layers in the Superbubbles DEML152 and DEML192                                                      

	 We are studying the interface between the the hot (approx 10^6K)
      interior and the cooler (approx 10^4K) swept-up shell of superbubbles.
      Heating and cooling processes operating in these interface layers
      determine the structure and evolution of the associated astronomical
      objects.  OVI lines are good tracers for the approx 10^5K gas of the
      interface layer.  Thus, FUSE is an excellent instrument with which to
      study such interfaces.  Previous studies of the interface layer have
      attempted to detect O^(+5) ions in absorption against probe stars
      within the superbubble s, but the OVI absorption from the interface is
      confused by hot halo gas and prevalent H_2 absorption lines.  These
      problems are mitigated by observing OVI in emission.  We therefore
      request new FUSE observations to search for OVI emission from the
      interface layers of two superbubbles in the LMC, DEM L 152 and DEM L
      92.  These FUV data will allow us to probe the 3E10^5K gas in the
      interface layer and, combined with previously obtained optical and
      X-ray data, to determine the physical parameters of the interface
      layer.
      

	 Prop ID:        G058  Proposer:       Espey   
	 Institution:    Trinity College Dublin   
	 Proposal Title: Understand Mass-loss in Cool Giants the Wind of SY Mus  

	 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 derive spatially 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,
      ionisation and dynamic information on the wind which can then be
      compared against predictions of hydrodynamical stellar atmosphere
      codes. We propose 6 observations of the symbiotic SY Mus utilizing the
      0 day periodicity inherent in FUSE scheduling to phase space the
      observations.  Results will be compared to PHOENIX hydrodynamical
      models and to similar observations of earlier spectral type symbiotic
      giants to constrain wind acceleration and chromospheric models.
      

	 Prop ID:        G059  Proposer:       Blair   
	 Institution:    Johns Hopkins University   
	 Proposal Title: The Enigmatic Magellanic Cloud Supernova Remnant N63A                                                                                                 

	 We propose follow-up FUSE observations of the supernova remnant N63A
      in the Large Magellanic Cloud.  This remnant is within an OB
      association whose main sequence turn-off mass is 30 solar masses, and
      yet no evidence of the stellar ejecta is obvious.  It was observed at
      one central position as part of the FUSE Magellanic Cloud SNR survey
      project.  The LWRS aperture position was dominated by a bright optical
      shocked cloud, and a strong signal was seen in OVI lambda lambda
      032,1038, but not in CIII lambda 977, the other strong line normally
      seen in strong radiative shocks. In this proposal, we request two
      short observations at offset positions to diagnose the eastern bright
      X-ray shock and the SW limb that shows two protrusions in the Chandra
      X-ray image of Warren et al. (2003) which are similar in appearance to
      ejecta-driven bow shock features seen in the Vela supernova remnant in
      our Galaxy.  This small investment of time will provide a much clearer
      picture of FUV-emitting characteristics of this unusual supernova
      remnant.
      

	 Prop ID:        G060  Proposer:       Guinan   
	 Institution:    Villanova University   
	 Proposal Title: Towards Completing the FUSE dM Star Database - FUV Observations of the Old High Velocity dM1 Star SZ 

	 We propose to extend and expand our ongoing Sun in Time Program on
      solarstellar dynamo physics and X-rayFUV irradiance (and effects on
      planetary atmospheres) of solar-type (G0-5 V) stars to cooler, more
      numerous dM stars with deep convective zones (CZs). This proposal is
      also motivated by the upcoming exoplanetary search missions
      e.g. Kepler, SIM, and DarwinTPF) that will search for earth-like
      planets in the habitable zones of nearby G-K-M stars.  Two years ago
      the program was extended to include FUSE Cycle 5 observations of a
      sample of dK0-5 stars of different ages. Here we propose a 40 ksec
      FUSE observation of a carefully selected representative old disk dM
      star -- SZ UMa -- which will help complete the parameter space of age,
      rotation, and FUV emission for dM stars. Also, we 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. Of particular
      interest is the determination of X-rayFUV emission flux evolution
      with age for dM stars. This is because of the critical roles that FUV
      TR and chromospheric emissions (dominated by HI Lyman series and CIII
      and OVI emissions) play on the photochemical and photoionization
      evolution (and possible erosion) of planetary atmospheres and
      ionospheres. This program will also have 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 extraterrestrial life on such planets. We plan to combine
      the FUSE FUV observations with X-ray and UV (from IUE or HST, where
      available) to form spectral irradiance tables (flux at 1 AU) of dM
      stars covering a wide range of ages. With FUSE nearing the end of its
      usable lifetime, this may be the last chance to complete this
      important FUV dataset.
      

	 Prop ID:        G061  Proposer:       Chayer   
	 Institution:    Johns Hopkins University   
	 Proposal Title: FUSE Observations of Hot Subdwarf B Stars                                                                                                            

	 We propose FUSE observations of a sample of hot subdwarf B stars (sdB)
      in order to carry out an abundance analysis of heavy elements and see
      how their abundance patterns emerge from the observations.  It is a
      well known fact that the atmospheres of these extreme horizontal
      branch stars exhibit abundance anomalies.  Diffusion processes such as
      gravitational settling, radiative levitation, weak stellar winds, and
      accretion have been proposed to explain the abundance anomalies.  Our
      goal is to identify which mechanisms operate in the atmospheres of
      these stars, study their interactions, understand the abundance
      patterns, and ultimately, constrain the structure of the atmospheres
      of sdB stars.  With this proposal we want to complete our FUSE
      proposals E152 and F909 with targets that are feasible with the new
      FUSE.  Only four sdB stars out of forty have been already observed
      within these two programs, and only three more targets are still
      feasible.  This is why we propose observations of a new sample of sdB
      stars that can be done with the new FUSE.  To study and interpret the
      abundance patterns in sdB stars, we need a large sample of stars with
      atmospheric parameters that cover the whole effective temperature and
      gravity domains (20,000 K < T_eff < 40,000 K ; 5.0 < log g < 6.5).
      To achieve a thorough abundance analysis we need FUSE observations,
      because many resonance lines of elements such as phosphorus, sulfur,
      chlorine, iron peak elements, and elements beyond the iron group are
      only visible in the FUV range for the effective temperatures of
      interest.  This study will not only provide new insights into the
      stellar atmosphere structure of sdB stars, but also to the evolution
      of galaxies since these stars are the most important candidates for
      the source of the UV excess in elliptical galaxies and early-type
      spiral bulges.
      

	 Prop ID:        G062  Proposer:       Wesemael   
	 Institution:    Universite de Montreal   
	 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, stellar winds etc. Our picture of the abundance
      patterns of trace elements remains sketchy, however, especially for the
      cooler DB stars. We propose to secure spectra for three DB stars spanning
      the effective temperature range between 14,400 and 17,900 K with the
      specific aims of obtaining abundances of several elements (principally
      C, but also Si, N, Fe) 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:        G063  Proposer:       Penny   
	 Institution:    College of Charleston   
	 Proposal Title: The Effect of Metallicity of the Rotation Rates of Massive Stars  

	 Recent theoretical predictions for low metallicity massive stars
      predict that these stars should have drastically reduced equatorial
      winds (mass loss) while on the main sequence, and as such should
      retain most of their angular momentum.  Observations of both the
      Be(B+Be) ratio and the blue-to-red supergiant ratio appear to have a
      metallicity dependence that may be caused by high rotational
      velocities.  But to date only two studies of the rotation rates of
      massive stars have been completed.  Their results differ, one finding
      that lower Z massive stars do rotate faster, one finding the opposite.
      In addition both studies have limitations.  The first observed only
      stars with masses lower than 12 M_sun, which are not predicted by
      theory to have rotation rates affected by metallicity.  The second had
      only a small sample, and one which may have been skewed to
      narrow-lined targets.  The Multimission Archive at Space Telescope
      MAST) contains FUSE archival spectra of over 140 O-type stars in the
      Magellanic Clouds.  This is a significantly large sample that can be
      used to address this question with directly measured projected
      rotational velocities in a low metallicity environment.  The method to
      employ is that used in previous studies on both IUE and STISHST
      spectra (Penny 1996, Howarth et al. 1997, Penny et al. 2004).  An UV
      spectrum of a test star is cross-correlated with a narrow-lined star
      to create a cross-correlation function (CCF).  The width of this CCF
      is related to the intrinsic width of the spectral lines of the star.
      To determine projected rotational velocities, an accurate calibration
      must be found between CCF widths and V sin i values, for a sample of
      stars for which these values are already known.  Archival FUSE spectra
      also exist for over 100 Galactic O-type stars with known projected
      rotational velocities.  However there is a paucity of narrow-lined
      targets from the Galaxy available.  This severely limits the
      calibration of CCF width to V sin i and results in overestimates of
      the latter from FUSE spectra.  The acquisition of five additional
      narrow-lined stellar spectra will complete the calibration of CCF
      width to V sin i.  And allow the huge archive of LMC and SMC O-type
      spectra to be used to its fullest potential.
     

	 Prop ID:        G064  Proposer:       Charpinet   
	 Institution:    Observatoire Midi-Pyrenees   
	 Proposal Title: Testing Mode Identification Techniques for sdB Pulsators with FUSE                                                                              

	 We propose to monitor the rapid pulsations of the hot subdwarf B (sdB)
      star Feige 48 in the Far UV using the Time Tag (TTAG) mode of
      FUSE. This star has recently been under detailed study using
      asteroseismic techniques based on standard optical white light
      photometry (Charpinet et al. 2005, A&A, in press). This analysis
      provided both very strong constraints on the fundamental structure of
      this star and a prediction of the nature of the pulsation modes being
      observed (i.e., the mode identification). This latter prediction can
      be checked independently using multi-waveband photometry. The apparent
      amplitude of a nonradial oscillation mode depends on both its geometry
      through the degree ell) and the wavelength at which it is
      observed. For hot sdB stars, calculations clearly indicate that the
      relative mode amplitudes as seen in the optical and in the Far UV
      strongly discriminates between values of the degree ell, allowing
      these to be easily determined. Such constaints on the mode
      identification are otherwise very difficult to obtain from optical
      multicolour photometry alone, as the discrimination between different
      ell values is weak when confined in this bandpass. The comparison of
      the FUV amplitudes of the modes detected by FUSE with their optical
      counterparts (from dedicated, simultaneous ground-based observations)
      will permit an independent determination of the degree ell of the
      pulsation modes of Feige 48. Our ultimate goal is to provide
      fundamental tests of the models that describe pulsating sdB stars and
      the techniques that are being developed to exploit their strong
      seismic potential. A consistency check of this kind offers a rare
      opportunity to validate asteroseismic tools that will be extensively
      used in the future to infer internal properties of subdwarf B stars.
      

	 Prop ID:        G065  Proposer:       Dupuis   
	 Institution:    Canadian Space Agency   
	 Proposal Title: Metals and Quasi-Molecular Satellites in Cooler DA White Dwarfs  

	 We are re-proposing a survey program of DA white dwarfs approved for
      cycle 6 with a list of targets more suited for the new pointing
      constraints caused by the loss of an additional reaction wheel on
      FUSE. This survey concentrates mainly on stars cooler than 20,000K but
      a couple of slightly hotter stars were included for increased
      flexibility of FUSE scheduling.
      Cooler DA white dwarfs have not been studied as extensively than
      hotter white dwarfs by FUSE as they tend to be fainter and are not
      good background sources for deuterium studies. We will search for the
      presence of trace elements such as C, N, Si, and Fe in the atmosphere
      of these cooler white dwarfs. Previous observations of white dwarfs in
      this temperature range have revealed surprisingly high metallicity in
      a subset of these stars. This is in spite of the dwindling of support
      by selective radiative acceleration at these temperatures. The current
      wisdom about this phenomenon is that these stars are accreting matter,
      either interstellar or circumstellar, which then pollutes their
      atmospheres. These observations will allow us to potentially discover
      new cool metal-enriched DAs and further our understanding of this
      peculiar phenomenon. These observations will also allow us to improve
      our understanding of quasi-molecular satellites which become prominent
      in the wings of Lyman beta and Lyman gamma profiles at these
      temperatures.
      

	 Prop ID:        G066  Proposer:       Tripp   
	 Institution:    University of Massachusetts - Amherst   
	 Proposal Title: Probing the Origin of O VI Emission from LMC X-3                                                                                         

      We propose to monitor the UV and X-ray emission of the persistent
      black hole X-ray binary (XRB) star LMC X-3 in a coordinated FUSE and
      RXTE program. In FUSE Cycle 5, we detected OVI emission from LMC X-3,
      and we observed velocity shifts of the OVI emission at different
      orbital phases by up to 200 km s^(-1), in agreement with earlier
      FUSE observations reported by Hutchings et al. (2003). However, while
      Hutchings et al. observed very broad OVI emission that could arise in
      the black hole accretion disk, during our more recent observation the
      broad feature was greatly suppressed and we detected an additional
      much narrower OVI emission feature. The narrow OVI emission is
      strongest at orbit phase approx 0.5 (inferior conjunction) and
      disappears at phase approx 0 (superior conjunction). In principle,
      these OVI emission features could provide important constraints on
      fundamental parameters of the XRB such as the inclination of the
      system. However, a variety of interpretations remain viable, and the
      current FUSE observations are too sparse to support firm
      conclusions. To improve our understanding of the nature and
      implications of the OVI emission, we seek ten short observations
      during the course of FUSE Cycle 7, with nearly-simulataneous X-ray
      observations from RXTE. With these data, we will (1) obtain better
      measurements of the OVI velocity variations, (2) study the dependence
      of the OVI emission strength on orbital phase, (3) study how changes
      in the X-ray spectrum affect the OVI emission, and (4) investigate
      how the X-ray and UV emission (both OVI and continuum) are
      correlated.


	 Prop ID:        G067  Proposer:       Ghavamian   
	 Institution:    Johns Hopkins University   
	 Proposal Title: The Nebular Shell Around the Ultraluminous X-ray Source Ho IX X-1 -- Supershell or Hypernova Remnant                                              

	 We propose FUSE observations of a large shell associated with the
      ultraluminous X-ray source Holmberg IX X-1 (a.k.a. M81 X-9).  The
      optical spectrum of the shell shows a classic shock spectrum, with
      strong SII relative to H alpha. The X-ray emission derives
      primarily from an embedded ultraluminous (approx 10^40 ergs s^-1)
      X-ray source (ULX).  The source is pointlike and may be an accreting
      intermediate mass (100-1000 M_odot) black hole.  Its relationship to
      the nebular shell is poorly understood. The shell may be a supershell
      blown by multiple stellar winds and SNe, or it may be the remnant of a
      single highly energetic (E > 10^53 ergs) explosion (i.e.,
      hypernova). Understanding the kinematics of the shell will provide a
      critical clue to the origin of the X-ray source Ho IX X-1.  We will
      search for CIII andor OVI and other FUV line emission from the shell
      and use the line ratios to constrain the shock speed.  As a bonus, we
      also plan to search for emission from the compact photoionization
      nebula around the ULX itself.  The measurement of OVI from this
      source would provide valuable information such as the absorbing column
      in the immediate vicinity of the compact object and the shape of the
      ionizing spectrum.  The Ho IX X-1 shell is likely the only ULX with
      low enough extinction to be observable in the FUV, and is well-matched
      to the diffuse source capabilities of FUSE.
      

	 Prop ID:        G070  Proposer:       Sankrit   
	 Institution:    Johns Hopkins University   
	 Proposal Title: Survey of OVI Emission towards Nearby White Dwarfs                                                                                                  

	 We propose a survey of OVI emission along sight lines at small
      angular separation from nearby white dwarfs that have been observed by
      FUSE.  The white dwarf spectra present a wide range of OVI absorption
      properties, ranging from no detectable OVI to circumstellar OVI.
      The results of our survey will allow us to characterize the
      relationship between emission and absorption along closely spaced
      sight-lines.
      In a companion (standard) proposal we have requested observations of
      the four best cases of emissionabsorption pairs of sight-lines.
      Those results will be used to obtain the physical properties of
      conductive interfaces in the local interstellar medium, which in turn
      will help us interpret the data obtained in this survey.
      

	 Prop ID:        G071  Proposer:       Dixon   
	 Institution:    The Johns Hopkins University   
	 Proposal Title: FUSE Observations of the High-Ionization Planetary Nebula around KPD 0005+5106                                                                    

	 A high-ionization planetary nebula (PN) around the hot white dwarf
      KPD0005+5106 was discovered serendipitously by its photoionized OVI
      emission in FUSE observations.  Because the data were taken as part of
      a calibration program, only two radii and a limited range of position
      angles are sampled by the discovery observations.  We propose
      additional FUSE observations of the nebula in order to study the
      distribution of the OVI emission.  Since the properties of the stars
      ionizing continuum and its distance are well constrained, the
      measurements will allow us to estimate the density of the emitting
      gas.  High-ionization PNe should exist around most hot white dwarfs
      but are difficult to identify and study because they are faint and
      extended in the optical.  Our proposed FUSE observations of one of the
      few known high-ionization PNe will yield important insights into the
      properties of this class of objects.
      

	 Prop ID:        G072  Proposer:       Dixon   
	 Institution:    The Johns Hopkins University   
	 Proposal Title: FUSE Observations of Hot Horizontal Branch Stars in the Globular Cluster NGC 6752                                                                 

	 We propose FUSE observations of eight stars in the globular cluster
      NGC 6752.  These stars span the full length of the clusters extended
      horizontal branch (EHB) and continue on into the post-EHB phase.  By
      comparing its FUV spectrum with synthetic spectra derived from non-LTE
      stellar atmosphere models, we will derive the effective temperature,
      surface gravity, and photospheric abundances of each star.  Our
      principal goal is to study the competing effects of gravitational
      settling and radiative levitation in the atmospheres of EHB stars by
      looking for variations in their abundances from the cluster mean and
      as a function of temperature.  While ground-based observers have
      measured the abundances of cooler (< 20,000 K) blue horizontal branch
      BHB) stars in several clusters, the abundance ratios of EHB stars are
      unknown.
      

	 Prop ID:        G073  Proposer:       Dixon   
	 Institution:    The Johns Hopkins University   
	 Proposal Title: FUSE Observations of the UV-Bright Star in 47 Tucanae                                                                                             

	 We propose FUSE observations of the hot post-asymptotic giant branch
      PAGB) star BS in the globular cluster 47Tuc.  The star has been
      observed with the Hopkins Ultraviolet Telescope (HUT) and from the
      ground, and we seek to answer questions raised by those observations.
      Models fit to the stars FUV and optical spectra vastly over-predict
      the flux at wavelengths shorter than that of Lyman beta.  What is the
      source of this excess opacity  According to stellar evolution theory,
      stars that have undergone first dredge-up on the RGB should be
      enhanced in nitrogen and depleted in carbon.  Its HUT spectrum
      suggests that the star is overabundant in nitrogen and underabundant
      in carbon, but the lines of both elements are are blended with
      interstellar features at the HUT resolution.  By comparing the stars
      FUSE spectrum with synthetic spectra derived from stellar atmosphere
      models, we can determine the stars photospheric abundances and
      reconstruct the history of its chemical evolution and mass loss.
      

	 Prop ID:        G074  Proposer:       Peters   
	 Institution:    University of Southern California   
	 Proposal Title: Mass Transfer in the Active Interacting Binary UCephei                                                                                      

	 Following the recent FUSE detection of a well-defined accretion hot
      spot in the Algol binary UCephei (P2fd493), an active system in
      which the gas stream strikes the mass gainers photosphere at a steep
      angle, we propose new observations to determine physical and
      geometrical parameters for the impact site and its apparently
      associated splash plasma. The capabilities of FUSE present us with an
      unparalleled opportunity to map a splash plasma in velocity and
      physical space, as many prominent shell-type absorption features are
      formed in this gas. Furthermore, the location, size, and temperature
      of the impact site can be well-determined because the flux contrast
      between the spot and the photosphere of the B7-8 mass gainer is large
      in the FUV.  We propose a series of randomly spaced observations, each
      with a duration of 5 orbits (approx 10 ksec of observing time) and
      spanning a phase interval of 0.13 in the 60 hr period. Statistically
      half of the observations should fall in important phase interval
      .63-0.13 that includes totality and the transit of the hot spot
      through our line of sight. Based upon the results from previous FUSE
      observations of Algol binaries during total eclipse (Peters & Polidan
      004) we expect that the stream impact produces a high-temperature
      circumstellar plasma abovebelow the orbital plane that emits in
      OVI. Totality observations of UCep would allow us to test a
      hypothesis that this bipolar flow is a result of an impact-produced
      splash of material.  To increase the chance of observing the 2.3hr
      total eclipse that will enable us to map the location of the expected
      high-temperature plasma, we request 10 visits.  The physical
      parameters that are obtained from the observations will constrain
      future 3-D hydrodynamical simulations of mass flow in Algols and
      enable an estimate of the amount of mass lost from the system during
      the Algol phase of evolution.
      

	 Prop ID:        G075  Proposer:       Peters   
	 Institution:    University of Southern California   
	 Proposal Title: A FUSE Survey of Be Stars in Galactic Clusters                                                                                              

	 We propose a survey of Be stars that reside in galactic clusters to
      determine the abundances of carbon and nitrogen in their photospheres.
      During the past two decades there has been a consensus that the
      rotation rates in Be stars are rapid but far short of their critical
      values (0.50 < VV_cr < 0.85). But recently there has been a renewed
      interest in the possibility that Be stars are critical rotators
      Townsend, Owocki, & Howarth 2004).  Abundance studies can provide a
      test for the latter hypothesis, as stellar evolution modeling by
      Meynet & Maeder (2000) has predicted a significant enhancement in the
      photospheric N abundances in very rapidly rotating OB stars due to
      mixing of CNO-processed material from their interiors. The FUV is the
      best spectral region for determining CN abundances in Be stars as the
      strongest lines of CII, III and NII, III fall in this region and the
      flux contribution from the disk is not important.  The survey will
      include Be stars in h & ChiPer, a galactic cluster that contains a
      large fraction of Be stars, NGC 3766, and NGC 4755, and provide an
      independent test of the critical rotation hypothesis and contemporary
      stellar evolution models that include stellar rotation.
      

	 Prop ID:        G076  Proposer:       Peters   
	 Institution:    University of Southern California   
	 Proposal Title: The Abundances of Carbon and Nitrogen in the Be Star NGC330-B12 in the Small Magellanic Cloud                                               

	 We propose a FUSE observation of the Be star B12 in NGC330 in the
      Small Magellanic Cloud to determine the abundances of carbon and
      nitrogen in its photosphere.  During the past two decades there has
      been a consensus that the rotation rates in Be stars are rapid but far
      short of their critical values (0.50 < VV_cr < 0.85). But recently
      there has been a renewed interest in the possibility that Be stars are
      critical rotators (Townsend, Owocki, & Howarth 2004).  Abundance
      studies can provide a test for the latter hypothesis, as stellar
      evolution modeling by Meynet & Maeder (2000) has predicted a
      significant enhancement in the photospheric N abundances in very
      rapidly rotating OB stars due to mixing of CNO-processed material from
      their interiors. The FUV is the best spectral region for determining
      CN abundances in Be stars as the strongest lines of CII, III and NII,
      III fall in this region and the flux contribution from the disk is not
      important. The Be star B12 in NGC330 is ideal for an abundance
      analysis as it has relatively sharp lines.  A recent abundance study
      from optical data (Lennon et al. 2005) suggested a low N abundance,
      but the result was inconclusive as it was based upon only one very
      weak line. The low N abundance in the SMC renders it an ideal
      environment in which to look for altered abundances due to rotational
      mixing.  We also propose an observation of a well-known, sharp-lined
      non-emission B star in NGC 330 (B30) in order to be able to compare
      the CN abundances in NGC330-B12 with benchmark values for the cluster.
      

	 Prop ID:        G077  Proposer:       Thilker   
	 Institution:    The Johns Hopkins University   
	 Proposal Title: Probing Extranuclear Star-Forming Regions from SINGS                                                                                            

	 NASAs Spitzer Space Telescope and Galaxy Evolution Explorer (GALEX)
      now provide high-resolution MIR--FIR and FUV--NUV probes for the
      internal structure of nearby galaxies, effectively constraining the
      spatial distribution of dust and stars of varied age.  Both
      observatories have committed to a common Legacy project to ascertain
      the star formation activity and its effect on dust properties in a
      large representative sample of local targets. This effort is called
      SINGS -- the Spitzer Infrared Nearby Galaxies Survey.  Highlighted
      within SINGS are a collection of 75 optically- or IR-bright
      star-forming regions, for which dedicated high-resolution IR (5-37 mu
      m) spectroscopy will be obtained. In order to best capitalize on this
      opportunity to gauge the entire (stellar and dust) FUV--FIR SED for
      such intermediate luminosity starbursts, we propose FUSE
      observations for 14 optically-selected, extranuclear star-forming
      regions in three SINGS galaxies.  The proposed sample benefits from
      completed GALEX FUV and NUV imaging, which we have used to assess
      feasibility.  The extranuclear SINGS star-forming regions span a
      representative range of key physical parameters.  The FUSE spectra of
      these star-forming regions, when combined with GALEX and Spitzer
      observations, will constrain the massive stellar content in each
      object and permit determination of the UV attenuation law.  We will
      also explore the possibility of using the equivalent width of NIV,
      CIII, and PV winds lines as metallicity indicators, with application
      at high redshift.  Our FUSE dataset will have exceptional archival
      value, given the GALEXSINGS Legacy program.  This proposal is a
      resubmission of our approved Cycle 6 Survey project (F918) from which
      no targets have yet been observed.
      

	 Prop ID:        G078  Proposer:       Thilker   
	 Institution:    The Johns Hopkins University   
	 Proposal Title: FUSE Survey Observations of UV-Bright Stellar Complexes                                                                                         

	 GALEX has dramatically increased the number of galaxies in the local
      Universe for which sensitive, high-resolution UV imagery is available.
      In particular, our Nearby Galaxies Survey (NGS), Medium Imaging Survey
      MIS), and Deep Imaging Survey (DIS) have together provided FUV and
      NUV imaging observations at approx 5 arcsec resolution for 200+
      galaxies with v <2500 kms and delta > 50 deg.  In addition to
      establishing a benchmark for global UV galaxy morphology, these three
      core GALEX surveys have yielded an unprecedented sample of UV-bright
      stellar complexes which probe a diverse set of host environments.
      FUSE offers a superb opportunity to obtain FUV spectra for these
      stellar nurseries (intermediate-luminosity starbursts).  As a
      class they harbor much of the star formation in normal galaxies, yet
      remain under-represented within the FUSE archive.  We propose survey
      observations for a sample of 24 such UV-bright complexes in 12 nearby
      galaxies. FUSE spectra will constrain the massive stellar content in
      each object.  We will further determine the equivalent width of NIV,
      CIII, and PV winds lines as a function of metallicity, setting up for
      their use as a high redshift metallicity indicator. The combination of
      FUSE, GALEX, and infrared (Spitzer, eventually JWST) observations of
      our sample will prove particularly powerful, delineating variations of
      the UV attenuation law versus environment.  We have already initiated
      such panchromatic work. In a parallel effort approved for FUSE Cycle 6
      F918) and in a follow-up Cycle 7 proposal, we are investigating a
      small number of extranuclear star-forming regions highlighted by SINGS
      the Spitzer Infrared Nearby Galaxies Survey) for which we have
      IRACMIPS imaging and 5-37 mu m spectroscopy to complement the UV
      observations.  Similar Spitzer imagery is available for 10 of 12
      galaxies we focus on here. IR spectroscopy will be proposed, but FUSE
      and GALEX now present a chance which should not be missed.
      

	 Prop ID:        G079  Proposer:       Kaiser   
	 Institution:    Johns Hopkins University   
	 Proposal Title: Probing the Origin of High-ionization Emission Lines in AGN with BLRG, 3C390.3                                                                       

	 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 OVI 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 OVI 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 the prototype double-peaked BLRG 3C390.3. It
      is one of the brightest double-peaked BLRGs and it has archival UV and
      optical spectra.  In addition, it harbors a massive black hole (M_BH 
      .9E8M_sun) and exhibits a low accretion rate (MM_Edd0.02).  Thus,
      C390.3 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:        G080  Proposer:       Gabel   
	 Institution:    University of Colorado   
	 Proposal Title: Monitoring the Intrinsic Absorption in Mrk 817 Probing Feedback from AGN Outflows  


	 Recent theoretical models suggest AGN outflows may have a far-reaching
      global impact, playing a central role in the evolution of supermassive
      black holes, their host galaxies, the surrounding IGM, and cluster
      cooling flows.  The mass outflow seen as UV and X-ray blueshifted
      absorption in AGN spectra may be the observational signature of these
      feedback mechanisms. To test this, detailed studies at high spectral
      resolution are needed to determine the physical conditions and
      geometry of the outflow.  The Seyfert galaxy Mrk 817 is an ideal
      target for this.  It has a far higher outflow velocity (v approx 4000
      kms) than any other nearby AGN, thus providing a direct study of the
      energetic outflows likely to impact their environment.  It also
      provides a unique study of the link between the ubiquitous Seyfert
      intrinsic absorbers and the more extreme systems seen in distant QSOs.
      Furthermore, it is one of the brightest AGNs at UV wavelengths,
      thereby allowing precise measurements of the absorption parameters.
      Previous observations have shown the intrinsic absorption in Mrk 817
      is variable.  We propose two new FUSE observations of Mrk 817.  These
      will provide the constraints needed to isolate the variability
      mechanism (changes in ionic column density versus covering factor).
      Column densities, or limits, measured from the crucial O VI, H I, and
      C III lines in the FUSE bandpass will determine the total column
      density (N_H) and ionization of the outflow via photoionization
      modeling.  Variability in the ionization structure will give limits on
      the distance of the absorber from the central engine.  Variability in
      the covering factors or N_H will constrain the transverse velocities
      and geometry of the outflow.  These results will allow us to measure
      the total kinetic luminosity of the outflow, which is needed to assess
      AGN feedback models.  It will also provide important constraints on
      dynamical models of AGN outflows.
      

	 Prop ID:        G081  Proposer:       DeWarf   
	 Institution:    Villanova University   
	 Proposal Title: FUSE Observations of the Unprecedentedly Deep Quiescent Magnetic Activity State of alpha Centauri A  

	 A long standing problem and a central topic of solar-stellar
      connection studies is that of relating the Suns magnetic behavior to
      other stars.  Our Sun is used as a fundamental calibration and as a
      reference point for stellar theory.  This requires that the Suns
      expressions of activity (distribution of magnetic active regions,
      coronal densities, emergence of magnetic flux, etc.) are fundamentally
      normal for a star of its age and evolutionary history.  Direct
      comparison with true solar analogs is critical for both understanding
      the magnetic nature of the Sun as well as magnetic phenomena in other
      stars.  alpha Cen is the nearest stellar system to our Sun.  The G2V
      primary (alpha Cen A) is an almost perfect solar analog with regard to
      its mass, radius, temperature, and convection zone depth, but is
      slightly older (tau approx 5-6 Gyr) than our Sun.  These properties
      are well determined through extensive studies, making it an ideal
      Sun-as-a-star comparison to test solar concepts.  Recently, X-ray
      emission fluxes for alpha Cen A were observed to diminish by a factor
      of nearly 25(), a phenomenon never before observed for the Sun of 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, to a larger extent, the
      emission measures necessary to address these new observations.  The
      requested FUSE observations are crucial to a program to examine the
      long-term magnetic activity cycle of alpha Cen A.  We hope to observe
      alpha Cen A during Cycle 7 to obtain high quality FUV spectra during
      this unprecedented, very deep quiescent state of this up til now
      normal solar-type star.  These FUSE observations will be compared to
      the FUSE spectra secured in 2001 to search for differences in line
      strengthsprofiles along with carrying out detailed emission measure
      analysis.  We will coordinate these FUSE observations with the XMM
      observations of the target that are planned by a European group.
      

	 Prop ID:        G082  Proposer:       Malkan   
	 Institution:    University of California   
	 Proposal Title: Simultaneous Multiwavelength Spectra of High-Z Quasars--Physical Nature of the EUV Continuum                                                         

	 We propose FUSE spectroscopy of three newly discovered high-redshift
      Sloan quasars (1.5 < z < 2.2) and the only known EUV variable quasar
      HS 1700+6416 (at z  2.73).  These redshifts give us the ability to
      measure the EUV continuum below 400AA -- where only four quasars have
      ever been observed.  Combining these FUSE spectra with simultaneous
      observations by GALEX, XMM, and from the ground, we will obtain the
      first complete measurements of the quasar continuum SED across its
      energy peak, and over the range where most of its photoionizing power
      is emitted.  These determinations of the full ionizing spectrum of
      quasars have strong implications for the evolution of the IGM and the
      evolution of structure in the Universe, as well as for quasar emission
      lines and efforts to weigh their black holes through reverberation
      mapping.  By obtaining complete SEDs of 1700+6416 at two epochs, we
      will determine whether its surprisingly strong EUV variability is
      correlated with changes at higher andor lower energies.  These data
      will provide the strongest tests yet of competing physical models of
      the central engine, such as a black hole accretion disks with
      Comptonizing corona.  If we manage to detect the rest frame continuum
      down below 304AA, we will measure HeII Ly alpha absorptions.  These
      quasars are the brightest known in the u-band, and have extremely low
      levels of Milky Way extinction.  Only a handful of quasars have ever
      been detected in the EUV shortward of 600AA, and FUSE is the only
      operating spectrograph which can obtain any further such data.
      

	 Prop ID:        G083  Proposer:       Herczeg   
	 Institution:    Caltech   
	 Proposal Title: The Molecular Hydrogen Column Density In Our Line of Sight To CTTSs  

	 Estimating the extinction to CTTSs has historically been difficult
      because the accretion continuum complicates measurements of the
      photospheric emission.  We propose to use FUSE spectra of three
      CTTSs to measure the H_2 column density in our line of sight.  We
      will then use this measurement to infer a total hydrogen column
      density, thereby constraining the extinction in our line of sight to
      these CTTSs.  A low N(H_2) will strongly indicate that the
      extinction is negligible, while a high N(H_2) will yield a
      reasonable estimate for A_V that will ultimately need to be
      complemented with future N(HI) measurements with the next
      generation of UV spectrographs for an accurate extinction estimate.
      Previous studies of four CTTSs have demonstrated that the extinction
      estimates can differ by A_V>1.0 mag between this technique and
      previous, less reliable techniques.
      

	 Prop ID:        G084  Proposer:       Holberg   
	 Institution:    University of Arizona   
	 Proposal Title: FUSE Observations of the Pre-Intermediate Polar HS1136+6646 

	 HS1136+6646 is a close binary system consisting of a hot DAO primary
      and a secondary of spectral type K7.  It is classified as a
      post-common envelope pre-cataclysmic variable binary.  Recent FUSE and
      HST observations have shown this system to be one of only three known
      pre-intermediate polar systems known as well as the most massive
      pre-cataclysmic variable.  This system has been well observed from the
      ground, and the system parameters are now well known.  Spaced based
      FUV and UV spectra have revealed intriguing details of the magnetic
      nature of the hot white dwarf including correlations between the white
      dwarf spin phase and shape of the O VI line profiles.  We propose
      follow-up FUSE observations that focus on the discoveries regarding
      the magnetic nature of HS1136+6646.  The proposed observations, along
      with existing FUSE data, will increase our sensitivity, making
      possible our two main objectives.  One, a mapping of the O VI line
      shape variations with respect to the spin phase of the white dwarf as
      well as planned ground based spectropolarimetric observations.
      Second, an intensified search for spectroscopic evidence of
      photospheric abundance inhomogeneities and changing line shapes using
      phase resolved spectra.
      

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