FUSE French Guaranteed Time Observing Programs (Cycles 1, 2, and 3) ---------------------------------------------------------------------------- Prog ID: Q101 Title: H_2 Associated with Dust Color Variations PI: Gry Institution: Laboratoire d'Astrophysique de Marseille and ISO Data Center We propose to study the H_2 excitation, as well as the H_2 abundance and velocity distribution in nearby diffuse clouds in the Chamaeleon complex. The selected lines of sight present a wide variety in infrared colors, E(B-V), Rv and molecular abundances so that we can check the dependence of H_2 properties with these characteristics. After IRAS data revealed spatial variations in the dust emission color of these clouds, these variations have been correlated with changes in the shape of the UV part of the extinction curve, showing that they are due to variations in the size distribution of small dust particles. Comparative studies in the millimeter, visible and UV ranges have shown that highly energetic processes are present in the cloud presenting mid-IR excess. Magnetohydrodynamic shocks and intermittent dissipation of turbulence have been considered. The proposed study of H_2 in these clouds will help characterize these processes which should be of great significance for the evolution of dust particles and of the gas itself. ---------------------------------------------------------------------------- Prog ID: Q103 Title: He I in Local ISM PI: Vidal-Madjar Institution: Institut d'Astrophysique de Paris An attempt will be made on the brightest EUVE source showing emission in the 600 Angstrom EUVE band (410 c/ksec), to try to detect some second order absorption signature corresponding to He I in the local ISM. ---------------------------------------------------------------------------- Prog ID: Q105 Title: Lyman Break in Star-Forming Galaxies PI: Deharveng Institution: Laboratoire d'Astronomie Spatiale We wish to observe a star-forming galaxy shortward of its (rest frame) Lyman limit in order to measure or set limits on the Lyman continuum escape fraction. An object with a redshift large enough to get rid of residual galactic gas absorption (lyman series) is selected. Another related goal is to use the spectrum longward of the Lyman limit for better understanding the star, dust and gas content of the galaxy. ---------------------------------------------------------------------------- Prog ID: Q106 Title: O VI Phase in Galactic Haloes PI: LeBrun Institution: Laboratoire d'Astronomie Spatiale We propose to make low resolution (R=2000 and S/N~20) observations of two quasars, 3C 351 and Mark 205. Their sightlines cross the near environment of already known and identified galaxies or groups of galaxies, at impact parameters in the range 40-700 kpc (H0 = 50 km/s/Mpc). We will be able to detect the O VI doublet lines in absorption down to a limiting equivalent width of 0.2 Angstrom. We thus plan to determine whether a highly ionized phase exists in the close galactic environment in which the cooler and denser MgII absorbers would be embedded. These observations will also help in determining whether collisional excitation is present in these clouds and also to study the evolution of the shape and intensity of the intergalactic UV flux at low redshift. ---------------------------------------------------------------------------- Prog ID: Q107 Title: H_2 in the Small Magellanic Cloud PI: Ferlet Institution: Institut d'Astrophysique de Paris The star Sk 143 in the SMC has most peculiar properties: its extinction curve in the far-UV is of Galactic type, contrary to all the other SMC stars which have a small or absent extinction bump and a very strong rise in the extinction at shorter wavelength. It also has an apparently Galactic ratio of E(B-V) to atomic hydrogen column density. Still, the interstellar lines are at the SMC velocity, and suggest that the extinction is due to a molecular cloud in the SMC. However a deep integration in the CO(1-0) line with the Swedish-ESO submillimeter telescope has given a null result. FUSE will help solve this mystery by observing the H_2 lines and other lines which might yield a detection of the absorbing gas. ---------------------------------------------------------------------------- Prog ID: Q108 Title: Central Stars of Planetary Nebulae PI: Vidal-Madjar Institution: Institut d'Astrophysique de Paris Several investigations will be done simultaneously by observing the central stars of some bright Planetary Nebulae (PN): (a)The wavelength range is particularly appropriate to study the continuum, the temperature and the wind of the PNe central stars; (b)In addition to the stellar continuum, the spectra will yield information concerning the nebula. The CIII line at 977A should be easily observable. Its intensity will be an additional independent measurement to resolve the controversy about the carbon abundance in PN; (c)FUSE will offer the possibility to detect molecular hydrogen lines in absorption against the stellar continuum. In several cases, the velocity separation of that component formed in the vicinity of the nebula and that formed in the general ISM will be possible. It should then be possible to determine how much additionnal H_2 is formed by shocks in the stellar winds. (d)Finally, the non detection of deuterium should allow a direct check of its evolution within stars since these PN were selected for their different 3He environment. ---------------------------------------------------------------------------- Prog ID: Q109 Title: Peculiar White Dwarfs PI: Vidal-Madjar Institution: Institut d'Astrophysique de Paris The standard post-AGB evolution theory predicts that throughout the whole post-AGB phases the chemical surface composition of the star remains essentially unchanged, because hydrogen shell burning ceases when the surface H-rich layer has been thinned down to about 1.e-4 Msun. However about 25% of the spectroscopically observed post-AGB stars in the planetary nebula stage are hydrogen-deficient and the origin of their peculiar surface abundances is still unclear. Among the hydrogen deficient post-AGB stars the class of the PG1159 stars are the most peculiar. They cover the hottest part of the post-AGB evolution (65000 - 180000K) and their surface is composed of carbon, helium, and oxygen (typically 50/30/20% by mass). Since mass loss could also be responsible for the observed peculiarities, we need a determination of the mass-loss rate to be conclusive. The O VI line at 1034 Angstroms is best suited since it is the most sensitive indicator for mass-loss in these stars. In that frame we will observe PG1159-035 the prototype as well as H1504+65 which is the most extreme one of this class. Deuterium evaluations will be also made on the line of sights towards these stars. ---------------------------------------------------------------------------- Prog ID: Q110 Title: Quasi-Molecular Satellite Lines in Lyman Beta PI: Vidal-Madjar Institution: Institut d'Astrophysique de Paris Our purpose is to detect in the wing of Lyman Beta the signatures of absorptions due to the quasimolecular satellites of H_2+ and H_2 in, respectively, photospheric spectra of a white dwarf and a Lambda Boo star where they have been observed in wing of Lyman Alpha. These targets are suitable for such detection: the white dwarf WD1620-391 has a pure hydrogen atmosphere and that of HD125162 is depleted in metals. ---------------------------------------------------------------------------- Prog ID: Q111 Title: The Symbiotic Binary IX Velorum PI: Ferlet Institution: Institut d'Astrophysique de Paris The profiles of the absorption and emission lines, particularly of the O VI doublet for the symbiotic binary AG Peg, will enable information to be obtained on the kinematics of the regions of line formation. The very high ionization O VI doublet may in particular be produced very near the compact hot component. A wind from the cool component of the binary should be present; signs of the continuing existence of a wind from the hot component seen on older IUE spectra as well as a possible region where the winds collide, will be looked for. ---------------------------------------------------------------------------- Prog ID: Q112 Title: Cataclysmic Binaries PI: Ferlet Institution: Institut d'Astrophysique de Paris We propose to observe the highly mass-accreting cataclysmic binary IX Vel in the far UV, for the first time at a very high spectral resolution (R~30000), to infer the physics of the accretion very close to the white dwarf. A detailed analysis of the absorption resonance lines of O VI, PV and SVI by means of phase-resolved spectra (exposure time of 1/8 Porbital) will bring important clues to probe the structure of the wind (geometry, velocity law, inhomogeneities). When combined with the study of the continuum distribution in the far UV, this will allow us to test the still unknown mechanism of wind formation and to distinguish between different proposed models for the boundary layer which plays a major role in the dynamical evolution of these systems. ---------------------------------------------------------------------------- Prog ID: Q113 Title: The Old Nova V603 Aql PI: Ferlet Institution: Institut d'Astrophysique de Paris The absorption and emission line profiles of the old nova V603 Aql will be observed with FUSE in order to further study the properties of what appear to be an accretion disk and wind coming from this disk, also studied at longer wavelengths. Rapid line profile variations already seen for other lines in HST spectra, will in be searched for and examined, this being the case in particular for the O VI doublet. ---------------------------------------------------------------------------- Prog ID: Q114 Title: Be Stars PI: Ferlet Institution: Institut d'Astrophysique de Paris The study of high excitation line transitions in the wavelength range observed by FUSE will bring important information on the nature of activities taking place in the outermost layers of Be stars. The Lyman energy distribution predicted by thermal models of stellar atmospheres, which does not even agree with observations of normal B stars, will probably produce larger disagreements in Be stars, where, as highly rotating objects, the atmospheric structure remains quite unknown. A young B star in a binary system with a T-Tauri star will also be observed for the purpose of comparison. This program is also conducted in the frame of other observing programs toward B and Be stars. ---------------------------------------------------------------------------- Prog ID: Q119 Title: Circumstellar Disks PI: Deleuil The purpose of this program is to give new insights on the signatures of circumstellar gas around main-sequence and pre-main-sequence stars. For the stars Beta Pic (HD39060) and 51 Oph (HD158643), the gas already detected may be the by-product of some activity (like evaporation and/or collision of kilometer-sized bodies) in a young planetary system in its clearing out phase. These observations are expected to allow the identification of the main form of the gaseous phase (H_2, CO, OI, NI, CII ?) and to give information on the ionization equilibrium of the zero radial velocity as well as accreting gas. Analysis of multiplet ratios will allow to probe the sizes of the inflowing gas structures. ---------------------------------------------------------------------------- Prog ID: Q201 PI: Gry, Cecile Institution: Laboratoire d'Astrophysique de Marseille and ISO Data Center Title: IS Studies : H2 associated with dust color variations We propose to study the H2 excitation, as well as the H2 abundance and velocity distribution in nearby diffuse clouds. This is to complement the study started with Q101 for clouds in the Chamaeleon complex. The selected lines of sight present a wide variety in infrared colors, E(B-V), Rv and molecular abundances so that we can check for correlations between these characteristics and H2 properties. After IRAS data have evidenced spatial variations in the dust emission color of these clouds, these variations have been correlated with changes in the shape of the UV part of the extinction curve, showing that they are due to variations in the size distribution of small dust particles. Comparative studies in the millimeter, visible and UV ranges have shown that highly energetic processes are present in the cloud presenting mid-IR excess. Magnetohydrodynamic shocks and intermittent dissipation of turbulence have been considered. The proposed study of H2 in these clouds will help characterize these processes which should be of great significance for the evolution of dust particles and of the gas itself. ---------------------------------------------------------------------------- Prog ID: Q206 PI: Le Brun, Vincent Institution: Laboratoire d'Astronomie Spatiale Title: O VI Phase in Galactic Haloes This program is the continuation of the Q106 program on the study of the OVI phase in galactic halos. We have selected a third quasar, Q0026+1259 (Bowen & Blades, 1997). Two galaxies lie close to the quasar sightline, which could give rise to OVI absorption lines, which FUSE only would be able to detect. The quasars has a flux of 2x10^-14 erg/s/cm^2/A. ---------------------------------------------------------------------------- Prog ID: Q210 PI: Hebrard, Guillaume Institution: Institut d'Astrophysique de Paris Title: Quasi-Molecular Satellite Lines in Lyman Beta Quasi-molecular satellites provide an important source of opacity in the DA white dwarf atmospheres not only in the red wing of Lyman alpha, but also in the red wing of Lyman beta. The recently discovered line satellites in the red wing of Lyman beta due to the close collisions of atomic hydrogen with protons fall right on the range of maximum sensitivity of FUSE (1050 - 1100 A). This spectrum region has a great potential for determining basic stellar parameters, provided that the physics underlying its formation is well described. This is exactly what we are able to achieve. We propose to observe one DA cool white dwarf in order to study the temperature sensitivity of the Lyman beta spectrum and deduce the lower limit of appearence of these line satellites. ---------------------------------------------------------------------------- Prog ID: Q219 PI: Lecavelier, Alain Institution: CNES, Institut d'Astrophysique de Paris Title: Circumstellar Disks The purpose of this program is to obtain spectra of a new target for the circumstellar disk program (P119, Q119) which aims to observe the signatures of circumstellar gas around main-sequence and pre-main-sequence stars. The selected target HD 163296 is a well known active HAeBe star. It is surrounded by a circumstellar dust and gas. Episode of accretion and outflows have been discovered with HST. A remnant H2 similar to the one detected with FUSE toward AB Aur (Roberge et al. 2001) could be observed. In any case, the comparison with AB Aur will be very fruitful. ---------------------------------------------------------------------------- Prog ID: Q221 PI: Andre, Martial Institution: The John Hopkins University Title: Red Rectangle Nebula The Red Rectangle is a remarkable bipolar nebula associated with the star HD 44179. First studied by Cohen et al (1975), the nature of this nebula is still not well understood. High-resolution infrared imaging Mekarnia et al (1998) showed that the nebula is produced by a compact equatorial disk of dust. Far ultraviolet observation of this nebula may be an enormous benefit to the study of evolving disk systems, leading to the best source information along with previous spectroscopic studies. ---------------------------------------------------------------------------- Prog ID: Q222 PI: Deleuil, Magali Institution: Laboratoire Astrophysique de Marseille Title: The H2 molecular gas in the center of M100 We propose to observe the central region of the nearby spiral galaxy M100 in order to properly measure the column density of the molecular hydrogen gas via its absorption lines (Lyman and Werner bands). CO (J=1-0) data are available for this galaxy as well as metallicity measurments within the same aperture as that of FUSE. Therefore we will be able to perform a direct measure of the CO to H2 conversion factor in a normal spiral galaxy. ---------------------------------------------------------------------------- Prog ID: Q223 PI: Ferlet, Roger Institution: CNRS, Institut d'Astrophysique de Paris Title: Study of Mkn36 Mkn36 is known to be a blue compact galaxy presenting a relatively low metallicity. The purpose of this investigation is to search for H_2 in the context of an intermediate metallicity object. These observations should also give access to a more precise evaluation of the elements abundances within such a galaxy as well as the physical state of the absorbing gas. If the stellar component responsible for the UV light is well placed behind absorbing material presenting a small enough spread of the velocity distribution including thermal, turbulent and large motion broadening, then possibly an estimation of the deuterium abundance in such a low metallicity object could be attempted. In such a case possible follow up observationbs will have to be considered. ---------------------------------------------------------------------------- Prog ID: Q224 PI: Lemoine, Martin Institution: CNRS Title: ISM in IZW36 IZW36 is known to be a blue compact galaxy presenting a relatively low metallicity. The purpose of this investigation is to search for H_2 in the context of an intermediate metallicity object. These observations should also give access to a more precise evaluation of the elements abundances within such a galaxy as well as the physical state of the absorbing gas. If the stellar component responsible for the UV light is well placed behind absorbing material presenting a small enough spread of the velocity distribution including thermal, turbulent and large motion broadening, then possibly an estimation of the deuterium abundance in such a low metallicity object could be attempted. In such a case possible follow up observationbs will have to be considered. ---------------------------------------------------------------------------- Prog ID: Q225 PI: Vidal-Madjar, Alfred Institution: Institut d'Astrophysique de Paris Title: Star formation in the atypical S0 galaxy NGC 5102? NGC 5102 is a very atypical giant lenticular galaxy: (1) its ultraviolet emission is much stronger than in other early-type galaxies observed by the IUE satellite; (2) it is a gas-rich galaxy where HII regions have been detected; (3) individual observations of blue stars near the center of the galaxy with the FOC/HST suggest they are young massive stars (Deharveng et al. 1997). All these results are evidences of a recent star-forming event. As shown by HUT observations of other early-type galaxies (Brown et al. 1995), NGC 5102 should also have a population of hot old stars (post-AGB, hot horizontal branch, AGB manque stars) contributing to the ultraviolet emission. Between 900 and 1200 A, the spectrum is very sensitive to the temperature of the hottest stars: FUSE data should therefore be especially efficient to disentangle the young hot stellar populations from older ones. To this purpose, the spectral energy distribution will also be connected to IUE data and optical and near-infrared colors. The global spectrum (continuum and stellar lines) will finally be analyzed with our evolutionary synthesis model PEGASE (Fioc & Rocca-Volmerange 1997, 2000) in terms of star formation history and metallicity. Modeling the spectral energy distribution of NGC 5102 is essential to understand both the star-forming process in ellipticals and S0's and to analyze observations of such galaxies at high redshift, when they underwent star formation. This will put important constraints on cosmological models of galaxy formation. ---------------------------------------------------------------------------- Prog ID: Q301 Title: Extra-solar Planet Aurorae PI: Vidal-Madjar Institution: Institut d'Astrophysique de Paris We will search for extra-solar planet aurorae emission (HI, H2) in the spectrum of stars with known extra-solar planets. The selected targets harbor "hot Jupiter" type planets or/and multiple systems. The observations will be performed during the quadrature to optimize the chance of detection using the velocity Doppler shift of the planets. ---------------------------------------------------------------------------- Prog ID: Q302 Title: Quasi Periodic Oscillations in the accretion disk of Black holes. PI: Andre Institution: Institut d'Astrophysique de Paris Quasi Periodic Oscillations (QPOs) in the X-ray brightness of neutron star and black hole X-ray binaries provide a useful probe into the inner accretion flows. Since the discovery in 1985 (Van der Klis) numerous neutron star QPOs have been observed with properties that depend on the spectral type of the sources (high or low luminosity). In current nomenclature, we distinguish 8 types of neutron star QPOs (from kHz to Hz and below). As to the black hole QPOs, a few cases have been observed in the same frequency range and show many similarities with neutron star QPOs. Nevertheless, at present the BH QPO studies are based on very few objects (Dimitrios 1999). Many theoretical models have been proposed for the different QPOs. Some of them identify the frequency with Keplerian orbital motion others suggest a hydrodynamic pulsation in the disk, others again imply general relativistic effects. But some of these models only apply to neutron star QPOs (hard surface, magnetic field) and some others only to BH QPOs. Opening the FUV window, FUSE will allow for the study of highly ionised species in the accretion disk. In particular, the O VI doublet ratio will help to put a limit on the density of these disk and the broadening of these lines should also put a constraint on the Keplerian model. Since BH QPO are found to be consistently lower than the neutron star QPOs, we suggest also the possiblity of time resolved spectroscopy (~.1 hz) in TTAG mode. The objects we propose to observe have been selected on a wide variety of criteria : weak stellar continuum, low distance and low frequency QPO. ---------------------------------------------------------------------------- Prog ID: Q303 Title: P cygni line variability in WR 140 PI: Gry Institution: Laboratoire d'Astrophysique de Marseille and ISO Data Center WR140 is going through periastron passage of its 7.94-year eccentric orbit in February 2001. X-ray monitoring with RXTE has shown that the heavy X-ray absorption expected as the Wolf-Rayet star moves into the line-of-sight to the O-star primary has started. Previous IUE observations have shown considerable extra absorption in P Cygni profiles was seen even months later. Nearer periastron these absorbtion effects should be much more pronounced. Although the interstellar absorbtion is quite high to WR140, the region longward of 1100 A has several lines of interest that should show heavy absorption through the WR wind. The object will be observed once during the periastron passage and once several months later to evidence the variations. ---------------------------------------------------------------------------- Prog ID: Q304 Title: The rapidly evolving planetary nebula Hen 3-1357 PI: Gry Institution: Laboratoire d'Astrophysique de Marseille and ISO Data Center Hen 3-1357 (known as the 'Stingray Nebula') is the youngest Planetary Nebula known in the sky. It has become ionized within the past few decades and its central star seems to be still rapidly evolving in the H-R diagram towards hotter effective temperatures. With this proposal we want to determine the current effective temperature of the central star and the characteristics of the stellar wind thirteen years after its discovery with IUE. This will enable us to determine whether the rapid spectral changes observed in the last few years are the consequence of an episodic post-AGB mass loss event or the result of a continuous evolution in the H-R digram. In any of these cases, the observations will help us to understand this short and, thus, still poorly known transition phase which leads to the formation of a new PN. ---------------------------------------------------------------------------- Prog ID: Q305 Title: Lyman continuum radiation from galaxies PI: Deharveng Institution: Laboratoire d'Astronomie Spatiale There is an on-going effort to measure the Lyman continuum radiation escaping from galaxies. Current data suggest a cosmic evolution of the escape fraction with implications on the contribution of star formation to the ionisation of the intergalactic medium. Measurements of nearby galaxies with FUSE should confirm the trend observed. ---------------------------------------------------------------------------- Prog ID: Q306 Title: Search for H2 in young circumstellar disks PI: Lecavelier Institution: Institut d'Astrophysique de Paris We will search for H2 absorption lines in the spectrum of stars surrounding by circumstellar disks in which H2 is already detected through quadrupole rotational transitions. By observing different inclination of disks, these observations will constrain the spatial distribution of the molecular gas. This should help to solve the issues raised by the observations of H2 in the Beta Pictoris disk. ---------------------------------------------------------------------------- Prog ID: Q319 Title: Circumstellar disks PI: Deleuil Institution: Laboratoire d'Astronomie Spatiale The purpose of this program is to obtain spectra of new targets for the circumstellar disk program (P119, Q119, P219, Q219) which aims to observe the signatures of circumstellar gas around main-sequence and pre-main-sequence stars. HD 141569 is a well-known pre-main sequence stars surrounded by a circumstellar disk for which images have been obtained, given information on the dust distribution and inclination of the disk. HD 36112 is a young pre-main sequence star surrounding by a huge amount of CO. The derivation of the CO/H2 ration will give important information on the gaseous content as well as on the origin and history of disk around stars more massive than the Sun.