# Data extracted from the ASC AXAF Observing Catalog on 2/19/1998 proposal_id proposal_number submission_date abstract title status type multiwave_simul observatories request_extra_flag rank normalized_rank archive_flag coi_contact coi_phone total_time num_targets description catcode name authority ao_str piid ----------- --------------- --------------- -------- ----- ------ ---- --------------- ------------- ------------------ ---- --------------- ------------ ----------- --------- ---------- ----------- ----------- ------- ---- --------- ------ ---- 176 01100045 Aug 28 1997 3:03PM Auroral phenomena in Jupiter are diagnostic of the structure, processes and energetics of its magnetosphere. Past X-ray observations have revealed latitudinal and longitudinal asymmetries, with spectra consistent with a model of sulfur and oxygen ions precipitating onto the Jovian atmosphere. This observation will provide a clear image of the X-ray emission during a full Jovian rotational period with spectral resolution sufficient to detect the expected emission lines. Galilean moons immersed in the magnetosphere may emit X-rays due to particle bombardment, auroral activity or other process. ACIS OBSERVATION OF JUPITER AND THE GALILEAN SATELLITES APPROVED GTO Y HST S Y 814-865-0162 40.0 1 SOLAR SYSTEM AND MISC 10 . . 01 18 202 01100077 Sep 15 1997 10:32AM Determine the on-axis PSF for the HRC-I and ACIS-I. CALIBRATION OBSERVATIONS OF 2RE J1032+532 APPROVED CAL N N N 10.0 1 NORMAL STARS AND WD 20 DICK VANNELLI HARVEY TANANBAUM 01 81 212 01200001 Sep 15 1997 1:58PM The bright A1 star Vega is used to measure UV sensitivity (or insensitvity) of the HRC I and S detectors. TEST OF UV SENSITVITY APPROVED CAL N N N 18.0 6 NORMAL STARS AND WD 20 HARVEY TANANBAUM DIRECTOR OF ASC 01 87 18 01200018 Aug 26 1997 2:08PM Algol is a bright eclipsing binary which is well suited to study the geometry, the differential emission measure distribution, and the electron density distribution of the coronal components. OBSERVATIONS WITH LETGS OF THE ECLIPSING BINARY ALGOL APPROVED GTO N S N 80.0 1 NORMAL STARS AND WD 20 COR SCHOONENBERG SRON 01 7 28 01200028 Aug 26 1997 2:08PM HETGS spectra will reveal a wealth of information on the temperature and density structure of stellar coronae and winds. The Trapezium in Orion contains many hot and cool young stars. HETGS observations of Orion will simultaneously obtain dispersed spectra of the brightest objects (hot stars), and CCD PHA spectra of young cool stars. This observation will also test the abilities of multiple source spectroscopy with HETGS. STELLAR CORONAL SPECTROSCOPY OF STAR-FORMING REGIONS: ORION APPROVED GTO N S N 73.0 1 NORMAL STARS AND WD 20 PATRICIA K. GREER ASSOC. DIRECTOR, OFFICE OF SPONSORED PROGRAMS 01 13 29 01200029 Aug 26 1997 2:08PM HETGS spectra will reveal a wealth of information on the temperature and density structure of stellar coronae. In addition, rotational or eclipse modulation can be used to further determine geometric structure. Two RS CVn stars will be observed with HETG and ACIS-S: AR Lac, and II Peg. AR Lac data will be taken through primary eclipse to map emitting structures. One pre-main-sequence star, TW Hya, which is a nearby, isolated, classical T Tauri object, will provide detail on the nature of young-star X-ray emission. STELLAR CORONAL SPECTROSCOPY OF COOL STARS APPROVED GTO N S N 200.0 3 NORMAL STARS AND WD 20 PATRICIA K. GREER ASSOC. DIRECTOR, OFFICE OF SPONSORED PROGRAMS 01 13 31 01200031 Aug 26 1997 2:08PM We propose to obtain a single, 60 ksec, ACIS-I exposure of the core of the 100 million year-old Pleiades open cluster. The 16x16 arcmin ACIS-I field of view will contain at least 20 known ROSAT PSPC sources for which ACIS-I will provide simultaneous, high signal-to-noise 0.5-7 keV light curves and low-resolution spectra. The ACIS-I image will also reveal 100-200 previously unknown X-ray sources. Most will be associated with low-mass cluster members including a few candidate brown dwarfs. The ACIS data will be used with recently derived rotational periods to test rotation-activity at the low end of the zero-age main sequence. The ACIS spectra and light curves will allow modeling of X-ray flares and coronal heating for these young, active stars. DEEP ACIS IMAGING OF THE CORE OF THE PLEAIDES CLUSTER APPROVED GTO N S Y 303 492 0389 60.0 1 NORMAL STARS AND WD 20 CAROL B. LYNCH ASSOCIATE VICE CHANCELLOR FOR RESEARCH 01 14 142 01200032 Aug 26 1997 2:19PM We propose to observe two active binaries with the AXAF HETGS and LETGS. TZ CrB is a G0 V + G0 V RS CVn binary. The HETGS observation will span an entire 1.14-d orbital period and will probably include one large flare. The HETGS line profiles may reveal high-velocity material ejected at the onset of a flare. Density and temperature-sensitive line ratios obtained at different orbital phases will be used to map the coronal geometry of TZ CrB. 44 Boo is an eclipsing, W UMa-type contact binary. The LETGS observation of 44 Boo will span no less than two 0.27-d orbital periods and will be used to perform coronal eclipse mapping and to investigate flares. Moreover, 44 Boo's maximum radial velocity separation of 230 km/s should be resolved in the longer wavelength LETG line profiles. AXAF GRATING SPECTROSCOPY OF ACTIVE BINARIES APPROVED GTO Y GROUND (VLA) S Y 303 492 0389 136.0 2 NORMAL STARS AND WD 20 CAROL B. LYNCH ASSOCIATE VICE CHANCELLOR FOR RESEARCH 01 14 34 01200034 Aug 26 1997 2:09PM We propose to observe two active late-type single dwarfs with the AXAF HETGS. AB Dor is a Pleiades-age K2 V rapid rotator at a distance of 15 pc. AB Dor exhibits large-amplitude long-duration flares and rotationally modulated activity at many wavelengths. The HETGS observation of AB Dor will span an entire 0.51-d rotational period. AU Mic is a very active M1 V flare star at a distance of 10 pc. AB Dor and AU Mic are prototypes for extreme main-sequence magnetic activity. The principal objectives of the HETGS observations are (i) to obtain time-resolved X-ray spectra of flares and (ii) to obtain high signal-to-noise, high-resolution spectra of very hot coronal sources to test optically thin collisional ionization equilibrium plasma codes. Supporting ground-based observations are planned. AXAF GRATING SPECTROSCOPY OF ACTIVE SINGLE STARS APPROVED GTO Y GROUND S Y 303 492 0389 120.0 2 NORMAL STARS AND WD 20 CAROL B. LYNCH ASSOCIATE VICE CHANCELLOR FOR RESEARCH 01 14 174 01200039 Aug 28 1997 3:02PM The Orion Trapezium cluster is the richest and densent cluster of pre-main sequence stars in the solar neighborhood, and the nearest region of high-mass star forming region. It is a superb laboratory for study of X-ray emission from protostars, classical and weak-lined T Tauri stars. The proposed observation should detect hundreds of stars, dozens of powerful magnetically-induced flares. X-ray emission from embedded protostars and massive OB stars will also be studied. The relationaships between X-ray emission and other stellar properties, and the influence of magnetic activity on star and planet formation, will be investigated. YOUNG STARS IN THE ORION TRAPEZIUM CLUSTER APPROVED GTO N S Y 814-865-0162 50.0 1 NORMAL STARS AND WD 20 . . 01 18 43 01200043 Aug 26 1997 2:09PM Low-mass pre-main sequence stars from protostars to post-T Tauri stars have X-ray emission considerably above that seen in older stars. Powerful flares from Class I protostars are particularly important and poorly understood. The core of the nearby star forming cloud in Corona Australis contains several X-ray emitting protostars as well as T Tauri and Herbig Ae/Be stars with associated outflows. X-RAYS FROM THE YOUNGEST STARS IN THE CORONA AUSTRALIS CLOUD APPROVED GTO N S Y 814-865-0162 20.0 1 NORMAL STARS AND WD 20 . . 01 18 50 01200050 Aug 26 1997 2:10PM The Orion molecular cloud contains a wide range of star forming environments, from rich high-mass clusters to distributed low-mass star formation. This observation focuses on the latter. The field includes a number of T Tauri stars, the Herbig Ae/Be star V380, and the high-velocity Herbig-Haro objects HH-1 and HH-2. Soft X-rays from the outflow, or hard Fe-K emission from a diffuse plasma, may also be detected. A short exposure will resolve the whether the B9 star HD 37001 or a nearby M4 star is responsible for the ROSAT source RX0535-0633. YOUNG STARS AND OUTFLOWS IN LYNDS 1641 APPROVED GTO N S Y 814-865-0162 22.0 2 NORMAL STARS AND WD 20 . . 01 18 51 01200051 Aug 26 1997 2:10PM 30 Doradus is a bright star-forming region in the LMC. It contains over 100 OB stars and has been observed to be a source of diffuse X-rays. This AXAF observation will measure spectra of young stars and of the diffuse emission. Energy balance and emission processes in the nebula will be studied. ACIS OBSERVATION OF 30 DORADUS APPROVED GTO N S Y 814-865-0162 30.0 1 NORMAL STARS AND WD 20 . . 01 18 59 01200059 Aug 26 1997 2:10PM Our proposed program to understand the X-ray emission from late-type stars will address three important issues: i) establish whether the ``solar analogy'' is invariably appropriate (and under what circumstance it may not apply), ii) determine coronal characteristics and their dependence on the properties of the underlaying stars (including rotation, color, and metallicity), and iii) understand the variation of activity levels at the low-mass end of the main sequence, where the convection zone may penetrate to near the stellar center. EMISSION FROM LATE-TYPE STARS APPROVED GTO N S N 40.0 2 NORMAL STARS AND WD 20 IRWIN SHAPIRO DIRECTOR 01 24 60 01200060 Aug 26 1997 2:10PM These observations will investigate the origin of X-ray emission from early-type stars and seek to discriminate between existing models which can be grossly characterized as either ``coronal'' or ``shocked wind''. For the nearest examples of this stellar class, the HRC-I should be able to distinguish between X-ray emission from within the stellar wind ``bubble'' and that emanating from the surrounding interstellar medium. High resolution spectroscopic observations with the HRC-S+LETGS can determine the variation of the soft X-ray absorption as a function of bolometric luminosity, spectral type, and mass loss rate. This absorption holds the observational key to understanding the relative position of the X-ray source(s) and the ambient massive cool winds which emanate from OB stars. EMISSION FROM EARLY-TYPE STARS APPROVED GTO N S N 25.0 1 NORMAL STARS AND WD 20 IRWIN SHAPIRO DIRECTOR 01 24 190 01200061 Sep 4 1997 12:23PM Our observations of star formation regions and young compact clusters will address: i) stellar collapse and commencement of nuclear burning - associated high X-ray activity makes such observations one of the best techniques for selecting young stars in molecular clouds for detailed study; and ii) the question of the existence of the X-ray activity in low mass stars at the onset of full convection - the problem of conflicting evidence arising from studies of field M dwarfs can be addressed by observing young open clusters cores over a range of ages and by examining the behavior of Lx and Lx/L_bol with spectral type and/or rotation. STAR FORMING REGIONS AND YOUNG CLUSTERS APPROVED GTO N S N 118.0 2 NORMAL STARS AND WD 20 IRWIN SHAPIRO DIRECTOR 01 24 90 01200090 Aug 26 1997 2:13PM An O star with count rate of about 0.5 c/s is observed on-axis and at 3 off-axis angles. Roll angles are set to image other weaker nearby stars, both on and off-axis. Stars are in the Cyg OB2 association. At least 4 bright stars will be useful for boresights. OFF-AXIS PILEUP AND BORESIGHT USING CYG OB2 APPROVED CAL N N N 28.0 4 NORMAL STARS AND WD 20 HARVEY TANANBAUM DIRECTOR OF ASC 01 37 155 01200103 Aug 26 1997 2:24PM The F5 star Procyon is a strong source of soft x-ray emission lines. This observation will be used to determine the LSF for the HRC-I/LETG at many energies and orders. This observation will be conducted simultaneously with an EUVE observation to cross calibrate in the 100-160A region. EUVE can observe Procyon anytime between Oct. 18 and April 10. The integration time reflects an additional 50 ksec required by the Emission-Line Project. GRATINGS CALIBRATION OBSERVATION OF AN EMISSION LINE SOURCE: PROCYON APPROVED CAL N N N 150.0 1 NORMAL STARS AND WD 20 RICHARD VANELLI DR. HARVEY TANABAUM 01 47 118 01200118 Aug 26 1997 2:15PM The Pleiades open star cluster contains many X-ray bright stars over an area of more than a degree. Using the optical positions of these stars as determined by Hipparcos, we will be able to determine the boresight off-sets and plate scale for each detector. These exposures should result in the detection of 10-15 stars with more than 100 counts. CALIBRATION OBSERVATION OF PLEIADES FOR BORESIGHTING AND PLATE SCALE APPROVED CAL N N N 40.0 4 NORMAL STARS AND WD 20 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 128 01200128 Aug 26 1997 2:16PM 5 targets are selected: 2 bright nearby solar-type stars (Procyon and alpha Cen), 1 eclipsing binary of two dM stars (YY Gem), 1 active RS CVn-type binary (II Peg), and 1 nearby active pre-main-sequence star (AB Dor) OBSERVATIONS OF STELLAR CORONAE WITH LETGS APPROVED GTO N S N 160.0 2 NORMAL STARS AND WD 20 COR SCHOONENBERG SRON 01 7 165 01200142 Aug 28 1997 9:49AM H1504+65 is the hottest white dwarf star known. Its atmosphere appears to be devoid of H or He, perhaps from mass loss during several cycles through the red giant phase. If so this star reveals directly the products of nuclear burning in the core of its progenitor. A high resolution spectrum can identify the elements in the photosphere. If present, the detection of Ne and its abundance will provide important information on the physical conditions in the core. HIGH RESOLUTION SPECTROSCOPY OF WHITE DWARFS APPROVED GTO N S N 25.0 1 NORMAL STARS AND WD 20 IRWIN SHAPIRO DIRECTOR 01 27 225 01200155 Sep 18 1997 11:30AM Secondary standard candle for LETG. Secondary standard candle for LETG APPROVED CAL N N N 20.0 1 NORMAL STARS AND WD 20 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 214 01300102 Sep 15 1997 1:58PM The white dwarf HZ43 a strong source of soft x-rays. The X-ray spectrum of HZ43 is well modeled as a black body with kT=18 eV. This source will be used to measure the relative efficiency of the LETG/HRC-S and the HESF. These observations will be done simultaneously with EUVE observations to cross calibrate in the 100-160A region of the spectrum. GRATINGS CALIBRATION OBSERVATIONS OF A SOFT CONTINUUM: HZ43 APPROVED CAL N N N 26.399999999999999 2 NORMAL STARS AND WD 20 DICK VANNELLI HARVEY TANANBAUM 01 88 206 01300104 Sep 15 1997 10:33AM The RS CVn star HR1099 is a strong source of hard x-ray emission lines. This observation will be used to determine the LSF for the ACIS-S/HETG at many energies and orders. This observation will be conducted simultaneously with an EUVE observation. The observing window for EUVE is 8/14 through 2/1. GRATINGS CALIBRATION OBSERVATION OF AN EMISSION LINE SOURCE: HR 1099 APPROVED CAL N N N 200.0 1 NORMAL STARS AND WD 20 RICHARD VANELLI DR. HARVEY TANABAUM 01 47 186 01300149 Sep 4 1997 12:21PM White dwarf used to determine on-axis PSF White dwarf used to determine on-axis PSF APPROVED CAL N N N 20.0 2 NORMAL STARS AND WD 20 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 210 01300152 Sep 15 1997 10:34AM 9th magnitude G3V star used to plate focus all 4 detectors. 9th magnitude G3V star for focusing APPROVED CAL N N N 20.0 4 NORMAL STARS AND WD 20 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 5 01300005 Aug 26 1997 2:07PM RE0751+14 is the brightest of a new class of intermediate polars discovered by ROSAT. Its soft X-ray spectrum is dominated by a blackbody-like component with a temperature of about 50 eV, reminiscent of that seen in the strongly magnetic polars. In analogy the soft component probably originates from an accretion-heated surface region around the white dwarfs magnetic pole(s). We propose to do high resolution X-ray spectroscopy of RE0751+14 to investigate in detail the soft spectral component. Resolving spectral features will provide very valuable information on the emission mechanism and the white dwarf atmosphere. It will be vital to find the physical parameters which rule the production of the soft X-ray component in soft intermediate polars. X-RAY SPECTROSCOPY OF THE SOFT INTERMEDIATE POLAR RE0751+14 APPROVED GTO N S N 50.0 1 WD BINARIES AND CV 30 COR SCHOONENBERG SRON 01 5 9 01300009 Aug 26 1997 2:07PM The standard model of supersoft X-ray sources (SSS) adopts a WD burning accreted H stably on its surface. These LETG observations of both the prototype SSS CAL83 and the brightest ROSAT SSS (2c/s) will test this model by resolving for the first time the predicted absorption edges of heavy elements (mainly C+O) in the WD atmosphere. ASCA/SAX observations give first hints for edges, but have too poor sensitivity below 0.5 keV. Also, the XMM grating can only be used for RX J0925.7-4758, a particularly hard SSS in the galactic plane. CAL83 is a bright LMC source with a predicted 0.09 cts/s. RX J0019.8+2156 is the brightest galactic SSS with HRC-S-LETG, giving 0.2 cts/s. (both sources have kT=35 eV bbdy, logNH=20.6-20.8 approximately). OBSERVATIONS OF SUPER SOFT X-RAY SOURCES WITH LETGS APPROVED GTO N S N 100.0 2 WD BINARIES AND CV 30 COR SCHOONENBERG SRON 01 7 208 01300100 Sep 15 1997 10:34AM The RS CVn star Capella is the brightest coronal emission line source in the sky. The X-ray spectrum of Capella exhibits strong emission lines over most of the LETG and HETG energy bands. These observations will be used to determine the LSF for the HRC-I/LETG and ACIS-S/HETG at many energies and orders. These observations will be conducted simultaneously with EUVE observations which can observe Capella anytime between 9/14 and 3/7. The integration times reflect an additional 100 ksec required for the emission-line project. GRATINGS CALIBRATION OBSERVATION OF AN EMISSION LINE SOURCE: CAPELLA APPROVED CAL N N N 330.0 4 WD BINARIES AND CV 30 RICHARD VANELLI DR. HARVEY TANABAUM 01 47 197 01300129 Sep 4 1997 12:25PM We propose a deep initial study of the CV population and dim x-ray sources in two globular clusters, NGC 6397 and 47 Tuc. Both clusters have extensive dim (Lx ~ 10^31-33 erg/s) x-ray source populations which our ROSAT/HST studies have shown are likely dominated by CVs although the brightest sources in 47 Tuc may also include quiescent LMXBs. The HRC-I (47Tuc) and ACIS-S (NGC 6397) images will allow the luminosity function, variability, and source identifications (with planned HST followup) to be measured and constraints on the origin of cluster WDs and NSs as well as compact binaries in these two contrasting globulars (differing in metallicity, halo vs. disk, and mass) to be derived. A complementary ACIS-S study of 47Tuc will measure spectra of both dim sources and the diffuse emission. NATURE AND ORIGIN OF CATACLYSMIC VARIABLES AND DIM X-RAY SOURCES IN GLOBULAR CLUSTERS APPROVED GTO N S N 49.0 1 WD BINARIES AND CV 30 IRWIN SHAPIRO DIRECTOR 01 79 130 01300130 Aug 26 1997 2:16PM The nature of a large subset of luminous supersoft X-ray sources (SSSs) has not yet been established. Although they are thought to be white dwarfs steadily burning accreted matter, there is no definitive evidence that this picture is correct: in particular we do not have direct evidence that any of the systems contain an accreting white dwarf. The observations we propose will provide good spectral information for all of the SSSs that are candidates for the nuclear-burning white dwarf model. We will be able to extract values of the temperature, luminosity and N_H, and to see evidence of absorption edges that may be associated with the white dwarf's atmosphere. SUPER-SOFT X-RAY SOURCES APPROVED GTO N S N 51.0 7 WD BINARIES AND CV 30 IRWIN SHAPIRO DIRECTOR 01 63 7 01400007 Aug 26 1997 2:07PM We propose to use Cyg X-2 as a bright 'candle' behind a sufficient dense column of interstellar matter in order to study absorption and scattering effects. Energy resolved scattering halos provide a clue to the chemistry of interstellar dust including the question if grains have a Silicate core and an organic mantle. Since haloes are not completely observable with a dispersive instrument, we will use the brightness distribution in cross dispersion direction for measuring the energy dependent scattering cross section. Cyg X-2 is the brightest among reasonably absorbed sources (NH > 10**21 cm**-2). We expect about 18 cts/s with HRC-S + LETG more than 500.000 cts within a 30ksec observation, respectively. CHEMISTRY OF INTERSTELLAR DUST APPROVED GTO N S N 30.0 1 BH AND NS BINARIES 40 COR SCHOONENBERG SRON 01 4 151 01400042 Aug 26 1997 2:22PM Cyg X2, a bright accretion-powered binary is observed with both gratings and 2 ACIS modes. This is a "science calibration"; data are to be placed in the public archive immediately. DEMONSTRATION SPECTRA OF AN ACCRETION-POWERED BINARY APPROVED CAL N N N 6.0 2 BH AND NS BINARIES 40 HARVEY TANANBAUM DIRECTOR OF ASC 01 65 46 01400046 Aug 26 1997 2:10PM Study of the X-ray scattered halo around obscured Galactic X-ray sources can provide insights into the size, density, composition and spatial distribution of interstellar grains. Eclipsing X-ray binary systems offer unique advantages, as the evolution of the halo following an abrupt eclipse depends on the distance and distribution of clouds. A high-resolution spectrum will further provide rich information on the interstellar matter composition. ECLIPSING BINARY X-RAY HALOS AND INTERSTELLAR GRAIN PROPERTIES APPROVED GTO N S Y 814-865-0162 44.0 4 BH AND NS BINARIES 40 . . 01 18 150 01400049 Aug 26 1997 2:22PM The angular momentum of a black hole with an accretion disk may reveal itself in the X-ray spectrum through the profile of emission lines generated in regions where general relativistic frame dragging distorts the disk. This effect can be sought in both AGN and Galactic black hole binary systems; the latter give stronger signals and a variety of disk inclination angles. However, line profiles can be complicated by reflection effects. The excellent sensitivity and energy resolution of the ACIS/HETG may resolve some of the existing ambiguities and clearly detect relativistic frame dragging. MEASURING BLACK HOLE SPIN APPROVED GTO N S Y 814-865-0162 50.0 3 BH AND NS BINARIES 40 . . 01 18 195 01400071 Sep 4 1997 12:24PM Comparisons of the luminosities of Black Hole (BH) and Neutron Star X-ray Nova (XN) provide the first direct observational evidence that black holes have event horizons. Central to the interpretation of this evidence is the understanding of the accretion flow in X-ray Nova as Advection Dominated Accretion Flows (ADAFs) when the systems are "quiescent". These observations will allow qualitative improvement in our ability to test the ADAF (or any other) model by providing the second high-quality spectrum of a quiescent BHXN, and the first high-quality spectrum of a short-period BHXN. BLACK HOLE EVENT HORIZONS APPROVED GTO N S N 74.0 3 BH AND NS BINARIES 40 IRWIN SHAPIRO DIRECTOR 01 29 76 01400076 Aug 26 1997 2:12PM We propose to obtain HRC-S LETG spectra of the shortest period binary system know: the11 min WD-NS binary in the globular cluster NGC 6624. This prototype for the double degenerate binaries is bright enough to obtain high S/N spectra with the LETG such that phase-resolved spectra can neasure the abundances in this extreme example of stellar/binary evolution as well as provice the first measure of a NS mass in an actively accreting LMXB in a globular. Comparison with statistical measures will allow constraints on both cluster potential and formation and evolution of thsi exotic system. SPECTRA AND MASS MEASURE FOR THE ULTRACOMPACT BINARY IN NGC 6624 APPROVED GTO N S N 10.0 1 BH AND NS BINARIES 40 IRWIN SHAPIRO DIRECTOR 01 31 125 01400125 Aug 26 1997 2:16PM Comparisons of the luminosities of Black Hole (BH) and Neutron Star X-ray Nova (XN) provide the first direct observational evidence that black holes have event horizons. Central to the interpretation of this evidence is the understanding of the accretion flow in X-ray Nova as Advection Dominated Accretion Flows (ADAFs) when the systems are "quiescent". These observations will allow qualitative improvement in our ability to test the ADAF (or any other) model by providing the second high-quality spectrum of a quiescent BHXN, and the first high-quality spectrum of a short-period BHXN. BLACK HOLE EVENT HORIZONS APPROVED GTO N S N 43.0 1 BH AND NS BINARIES 40 IRWIN SHAPIRO DIRECTOR 01 60 170 01400127 Aug 28 1997 9:51AM 3 bright compact low-mass X-ray binaries (Cyg X-3, X 0614+091, and 4U 1627-67) are selected to study the structure of the accretion region. OBSERVATIONS OF ACTIVE, COMPACT, LOW-MASS X-RAY BINARIES WITH LETGS APPROVED GTO N S N 46.0 2 BH AND NS BINARIES 40 COR SCHOONENBERG SRON 01 7 171 01400137 Aug 28 1997 9:51AM Observe lines from the relativistic jets of SS 433; measure elemental abundances in 4U1626-67, Vela X-1, GX301-2 to test evolutionary scenarios; measure ISM opacity ; measure the iron line structure in Cyg X-1; and obtain spectra of X-ray bursts and a possible accretion disk corona in 4U1636-53. HETG OBSERVATIONS OF X-RAY BINARIES APPROVED GTO N S Y 617-258-5767 185.0 6 BH AND NS BINARIES 40 PATRICIA K. GREER ASSOC. DIRECTOR, OFFICE OF SPONSORED PROGRAMS 01 12 163 01400140 Aug 28 1997 9:49AM Her X-1 is a neutron star in a binary system, accreting matter from its stellar companion. The X-ray emission is modulated with the 1.24 s spin period of the neutron star, the 1.7 d orbital period and an additional 35 d cycle. The hard X-ray pulses of the neutron star irradiate plasma trapped in its magnetosphere, where they are partially absorbed and re-emitted at energies less than 1 keV. We propose to utilize the high spectral resolving power of the AXAF LETG for detailed phase-resolved spectral studies of the soft X-ray radiation during the 35 d on-state. The observation should start shortly before eclipse egress, when the X-rays of the neutron star are penetrating the atmosphere of the stellar companion, to get also information on its structure and ionisation stage. SPECTROSCOPY OF THE SOFT COMPONENT OF THE X-RAY SPECTRUM OF HER X-1 APPROVED GTO N S N 30.0 1 BH AND NS BINARIES 40 COR SCHOONENBERG SRON 01 4 167 01400144 Aug 28 1997 9:50AM This is an observation of the dust-scattered halo from a bright, strongly-absorbed source. X-RAY SCATTERING HALO APPROVED GTO N S N 7.0 1 BH AND NS BINARIES 40 COR SCHOONENBERG SRON 01 7 226 01400156 Sep 18 1997 11:30AM Measure of PSF wings. Measure of PSF wings APPROVED CAL N N N 10.0 1 BH AND NS BINARIES 40 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 2 01500002 Aug 26 1997 2:07PM The 50 ms pulsar is used to verify the ability to do fast timing with the HRC and with ACIS-I in continuous-clocking mode. VERIFICATION OF AXAF TIMING CAPABILITY APPROVED CAL N N N 30.0 2 SN, SNR AND ISOLATED NS 50 HARVEY TANANBAUM DIRECTOR OF ASC 01 2 3 01500003 Aug 26 1997 2:07PM The very soft (57 eV blackbody) and very bright (3.67 ROSAT PSPC cts/sec) ROSAT source RXJ1856.5-3754 was identified recently by HST as a near-by, isolated, old, non-pulsating neutron star. The PSPC spectral blackbody fit indicates a low absorbing column density (correponding to A_V below 0.1 mag), so that this object most certainly is foreground to the R CrA dark cloud at 130 pc. With the LETG spectrum, we plan to perform photospheric spectroscopy, i.e. to check for deviations from a blackbody, e.g. due to a cyclotron emission feature in the Wien tail, or either a H, He, or Fe atmosphere. From the PSPC count rate, we can estimate that a 50 ksec AXAF LETG observation will provide sufficient S/N for distinguishing between these alternatives. SOFT X-RAY SPECTRUM OF THE OLD NEUTRON STAR RXJ1856.5-3754 APPROVED GTO N S N 50.0 1 SN, SNR AND ISOLATED NS 50 COR SCHOONENBERG SRON 01 3 143 01500021 Aug 26 1997 2:20PM We will perform a deep ACIS observation of Cas A. The goals of the observation are to: 1. Produce a broad band map to AXAF's 0.5" intrinsic resolution. 2. Obtain a hard band continuum map with sufficient signal-to-noise to determine the morphology of the synchrotron radiation from the shell. 3. Map out emission from Si, S, Fe lines; look for clumps, or evidence of stratification. 4. Create detailed Doppler map. 5. Measure the expansion rate of the X-ray gas by comparison with ROSAT images. 6. Search for neutron star remnant. ACIS OBSERVATION OF CAS A APPROVED GTO N S N 50.0 1 SN, SNR AND ISOLATED NS 50 S.S. HOLT DIRECTOR OF SPACE SCIENCES 01 9 144 01500022 Aug 26 1997 2:20PM We will perform deep ACIS-I observations of the young SNR's Tycho and Kepler. The goals of these observations are to: 1. Map out emission from the Si, S, and Fe lines and search for evidence of stratification. 2. Perfrom line diagnostics to characterize properties of ejecta. 3. Provide a baseline for proper motion studies. For Tycho, additional goals are: 4. Isolate and characterize the spectrum of the blast wave. 5. Measure the flux and spectrum of the hard tail. ACIS OBSERVATIONS OF TYCHO AND KEPLER APPROVED GTO N S Y (301) 286-3632 125.0 2 SN, SNR AND ISOLATED NS 50 S.S. HOLT DIRECTOR OF SPACE SCIENCES 01 9 149 01500023 Aug 26 1997 2:22PM We will perform a 50 ks observation of the supernova remnant W49B using ACIS-I. The goals of this observation are as follows: 1. Measure the flux and spectrum of the hard tail. 2. Map out the emission from Si, S, Fe and thereby search for the stratification suggested by ASCA. 3. Determine progenitor type by measuring relative abundances of observable metals. 4.Obtain the first high spatial resolution, broad band image. 5. Map temperature and ionization structure ACIS OBSERVATION OF W49B APPROVED GTO N S Y (301) 286-1587 50.0 1 SN, SNR AND ISOLATED NS 50 S.S. HOLT DIRECTOR OF SPACE SCIENCES 01 9 162 01500024 Aug 26 1997 2:27PM We will perform ACIS-I observations of some of the bright, young supernova remnants in the Magellanic Clouds. Two of these, 0519-69.0 and N103B have Type Ia progenitors; the other two, E0102-72 and 0540-69.3 are the results of core collapse explosions. For 0519-67.5, 0102-72, and N103B, our goals are: i. Measure nucleosynthesis yields via spectral fitting. ii. Look for evidence of stratification and ionization variation via high resolution, narrow band maps. For 0540-69.3, are goals are: i.) Obtain spatially resolved spectrum of the shell, and search for enhanced abundances of Type II nucleosynthesis products. ii.) Measure the extent of the central plerion. ACIS OBSERVATIONS OF EJECTA DOMINATED MAGELLANIC CLOUD SNR'S APPROVED GTO N S Y (301) 286-3844 85.0 2 SN, SNR AND ISOLATED NS 50 S.S. HOLT DIRECTOR OF SPACE SCIENCES 01 9 36 01500036 Aug 26 1997 2:09PM E0102-72 and N132D are the brightest remnants in the SMC and LMC (respectively) and are the best SNR candidates for grating observations as they are distant enough to subtend a small angular size yet bright enough to allow reasonable integration times. The ASCA spectrum of E0102-72 shows lines of He-like emission from O, Ne, and Mg. The line ratios of these elements cannot be explained using models with uniform abundances. Previous high-resolution studies of N132D using the Einstein Focal Plane Crystal Spectrometer (FPCS) have shown an oxygen overabundance. We plan to use plasma diagnostics of individual emmission lines to map the temperature, ionization and abundance structures of these two remnants. HIGH RESOLUTION SPECTRA OF EXTRAGALACTIC SUPERNOVA REMNANTS APPROVED GTO N S N 240.0 2 SN, SNR AND ISOLATED NS 50 PATRICIA K. GREER ASSOC. DIRECTOR, OFFICE OF SPONSORED PROGRAMS 01 16 38 01500038 Aug 26 1997 2:09PM Over the next decade, the shock front from the supernova explosion SN 1987A in the Large Magellanic Cloud will interact with a comlex environment. The X-ray emission is likely to brighten and change in various ways as the shock encounters the dense ring, HII region and red giant wind. Regular monitoring of the source throughout the duration of the AXAF mission is needed to test models of remnant evolution, nonequilibrium ionization processes and elemental abundances. MONITORING OF SN 1987A APPROVED GTO N S Y 814-865-0162 10.0 1 SN, SNR AND ISOLATED NS 50 . . 01 18 175 01500044 Aug 28 1997 3:03PM The Galactic supernova remnant RCW 103 contains a central object that appears to be a member of the class of radio silent neutron stars. ASCA observations show that it has a temperature that could be as high as 7 million degrees, making it the hottest surface seen so far. The data from ASCA are difficult to interpret unambiguously, however, because the neutron star is not well separated from the diffuse emission. This ACIS observation will clearly resolve the neutron star and determine its surface temperature. THE SUPERNOVA REMNANT AND NEUTRON STAR RCW 103 APPROVED GTO N S Y 814-865-0162 40.0 1 SN, SNR AND ISOLATED NS 50 . . 01 18 47 01500047 Aug 26 1997 2:10PM The nearby supernova SN 1987A provides an unprecedented opportunity to study the formation of a supernova remnant as the supernova shock front interacts with the surrounding circumstellar medium. The spectrum obtained here should give unique information concerning the physical conditions, composition and (through Doppler broadening) bulk velocity of the X-ray emitting gas. Repeated observations through the duration of the AXAF mission will trace the complex evolution of the shock. HIGH RESOLUTION SPECTROSCOPY OF SN 1987A APPROVED GTO N S Y 814-865-0162 100.0 1 SN, SNR AND ISOLATED NS 50 . . 01 20 179 01500054 Aug 28 1997 3:04PM N103B = SNR 509.0-68.7, one of the radio and X-ray brightest supernova remnants (SNRs) in the LMC, is a remnant of a Type Ia supernova explosion (carbon deflagration of a white dwarf). One side encounters a giant HII complex while the other side is freely expanding. With a known distance and low absorption, it provides an excellent oportunity to explore early SNR evolution. This ACIS observation will give spatially-resolved spectra. The elemental abundances and ionization state of the bright X-ray clumps (ejecta?) will be resolved from the more diffuse shell (blast wave?) emission. ACIS STUDY OF THE LMC SUPERNOVA REMNANT N103B APPROVED GTO N S Y 814-865-0162 40.0 1 SN, SNR AND ISOLATED NS 50 . . 01 18 55 01500055 Aug 26 1997 2:10PM G292.0+1.8, one of the radio-brightest supernova remnants (SNRs) in the sky, has a shell-type exterior with a plerionic core. Optical high-velocity O- and Ne-rich filaments are seen near the center. The X-ray morphology is also composite with a large barlike structure bisecting the shell. The X-ray spectrum shows both a non-equilibrium ionized plasma with excess metal abundances expected from a 25 solar mass progenitor, and a hard power-law component likely associated with the central synchrotron nebula. This ACIS image will elucidate the spatial distribution of elemental excesses, study dynamics of the X-ray bar with Doppler shifts, and confirm the presence of a nonthermal nebula. G292.0+1.8: A REMARKABLE OXYGEN-RICH SUPERNOVA REMNANT APPROVED GTO N S Y 814-865-0162 40.0 1 SN, SNR AND ISOLATED NS 50 . . 01 18 73 01500073 Aug 26 1997 2:12PM The pulsar PSR B0833-45 inside the Vela supernova remnant is the youngest and brightest source of thermal X-ray radiation from a neutron star. It thus provides an important laboratory for study of several expected components: continuous soft thermal X-ray emission from the cooling neutron star surface, pulsed hard thermal X-rays from the hot magnetic polar caps, and absorption features from the highly magnetized atmosphere. This observation will resolve the Vela pulsar from the surrounding synchrotron nebula, and give a high resolution spectrum that may reveal the chemical composition of its outer layers, its surface magnetic field, mass/radius ratio, and polar cap properties. The HRC detector is used to obtain spectra at different phases within the 89 ms rotational period. THE VELA PULSAR APPROVED GTO N S Y 814-865-0162 30.0 2 SN, SNR AND ISOLATED NS 50 . . 01 18 203 01500088 Sep 15 1997 10:32AM The SNR E0102-72.3 is positioned close to the aim points on the principle FI and BI chips to measure absolute sensitivity and response to low energy lines. The source will be used as a standard candle to monitor chip performance. ACIS CHIP RESPONSE TO LINES WITH E=0.6-1.5 KEV APPROVED CAL N N N 240.0 8 SN, SNR AND ISOLATED NS 50 HARVEY TANANBAUM DIRECTOR OF ASC 01 82 217 01500089 Sep 15 1997 1:59PM This target is a Standard Candle with well known continuum spectrum. It is used to measure absolute sensitivity and to monitor detector performance. HRC RESPONSE TO CONTINUUM SOURCE. APPROVED CAL N N N 240.0 8 SN, SNR AND ISOLATED NS 50 HARVEY TANANBAUM DIRECTOR OF ASC 01 91 91 01500091 Aug 26 1997 2:13PM This target is a standard candle with well known continuum spectrum. It is positioned close to the aim points on the principle FI and BI chips and at the center of the other ACIS chips to measure absolute sensitivity and to monitor performance ACIS CHIP RESPONSE TO A CONTINUUM SOURCE APPROVED CAL N N N 140.0 10 SN, SNR AND ISOLATED NS 50 HARVEY TANANBAUM DIRECTOR OF ASC 01 38 99 01500099 Aug 26 1997 2:14PM The spectrum of the Crab nebula and pulsar have been studied by virtually every X-ray astronomy mission in the last 20 years. The spectrum is stable and is relatively well known, so we propose to use it to calibrate the HETGS system, looking primarily for an overall agreement with other X-ray telescopes. The ACIS continuous clocking mode will be used so that the pulsar can be time resolved. CALIBRATION OF HETGS USING THE CRAB PULSAR AND NEBULA APPROVED CAL N N Y 617-253-8573 10.0 1 SN, SNR AND ISOLATED NS 50 HARVEY TANANBAUM DIRECTOR OF ASC 01 46 156 01500106 Aug 26 1997 2:24PM The bright SNR, Cas A, is centered on each HRC MCP to measure relative sensitivity and response to a line source. CasA emits bright lines over the range 1.8 to 6.5 keV. This target will serve as a standard candle for monitoring purposes. HRC RESPONSE TO CASA APPROVED CAL N N N 14.0 4 SN, SNR AND ISOLATED NS 50 HARVEY TANANBAUM DIRECTOR OF ASC 01 67 112 01500112 Aug 26 1997 2:14PM The bright SNR, Cas A, is centered on each chip to measure relative sensitivity and response to a line source. CasA emits bright lines over the range 1.8 to 6.5 keV. Response to individual lines from individual features should be above 1 count/s. If suitable, this target will serve as a standard candle for monitoring purposes. ACIS CHIP RESPONSE TO CASA, SEP. 98 APPROVED CAL N N N 10.0 10 SN, SNR AND ISOLATED NS 50 HARVEY TANANBAUM DIRECTOR OF ASC 01 55 215 01500113 Sep 15 1997 1:59PM The bright SNR, Cas A, is centered on each chip to measure relative sensitivity and response to a line source. CasA emits bright lines over the range 1.8 to 6.5 keV. Response to individual lines from individual features should be above 1 count/s. If suitable, this target will serve as a standard candle for monitoring purposes. ACIS CHIP RESPONSE TO CASA, MONITORING APPROVED CAL N N N 54.0 6 SN, SNR AND ISOLATED NS 50 HARVEY TANANBAUM DIRECTOR OF ASC 01 89 216 01500114 Sep 15 1997 1:59PM The bright SNR, Cas A, is centered on each HRC MCP to measure relative sensitivity and response to a line source. CasA emits bright lines over the range 1.8 to 6.5 keV. This target will serve as a standard candle for monitoring purposes. HRC RESPONSE TO CASA, MONITORING APPROVED CAL N N N 14.0 1 SN, SNR AND ISOLATED NS 50 HARVEY TANANBAUM DIRECTOR OF ASC 01 90 200 01500136 Sep 4 1997 12:26PM Use the high spatial resolution of AXAF/HRC to separate possible pulsars from surrounding nebula emission. Accurately measure the pulse fraction and shape of any detected puslars. SEARCH FOR PULSARS APPROVED GTO N S N 29.0 1 SN, SNR AND ISOLATED NS 50 IRWIN SHAPIRO DIRECTOR 01 80 164 01500141 Aug 28 1997 9:49AM We propose to observe two isolated neutron stars which are known to be pulsars at other wavelengths and are moderately strong X-ray sources. The objective is to observe spectral absorption features due to Fe atoms in the stellar atmosphere. The locations and strengths of the absorption features will be determined in large part by the strength and orientation of the magnetic field at the neutron surface. The features will be modulated as the star rotates, so we desire to measure the spectrum as a function of pulse phase. HETG OBSERVATIONS OF ISOLATED PULSARS APPROVED GTO N S Y 617-253-8573 80.0 2 SN, SNR AND ISOLATED NS 50 PATRICIA K. GREER ASSOC. DIRECTOR, OFFICE OF SPONSORED PROGRAMS 01 12 224 01500154 Sep 18 1997 11:30AM First-light picture First-light picture APPROVED CAL N N N 5.0 1 SN, SNR AND ISOLATED NS 50 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 30 01600030 Aug 26 1997 2:08PM We propose to observe two elliptical galaxies NGC1399 and NGC4486 with the HETGS. Hot gas trapped in the potential well of elliptical galaxies is known to emit X-rays with a temperature that is characteristic of the depth of the potential. Cool (~1 keV) X-ray plasmas are rich in emission lines which will allow us to determine the physical state of the ISM. The temperature and abundance of the hot gas will be determined. The relative abundances of Fe and the alpha-process elements will allow us to determine the relative rate of Type I & Type II SNe supernova. In addition, X-ray emission from any nuclear sources will also be examined. THE DETAILED X-RAY SPECTRA OF ELLIPTICAL GALAXIES APPROVED GTO N S Y 617-258-7254 98.0 2 NORMAL GALAXIES 60 PATRICIA K. GREER ASSOC. DIRECTOR, OFFICE OF SPONSORED PROGRAMS 01 11 148 01600040 Aug 26 1997 2:22PM The Galactic Center is an extremely complex region with extremely high stellar densities, high-mass star formation, highly sheared motions and magnetic fields, and probably a massive black hole. Past X-ray observations have not had sufficient resolution or sensitivity to clearly discriminate the various emitting structures. This ACIS observation has the high energy response to penetrate the large column densities, the resolution to achieve extremely high sensitivity to an active galactic nucleus and detect a variety of stellar sources. ACIS IMAGING OF SGR A* AND THE GALACTIC CENTER APPROVED GTO N S Y 814-865-0162 50.0 1 NORMAL GALAXIES 60 . . 01 18 41 01600041 Aug 26 1997 2:09PM M82 is the prototype starburst galaxy, the closest galaxy with L(FIR)>L(V). Its inner kpc is experiencing a violent episode of star formation with a top-heavy initial mass function following a recent passage by M81. The result is a rich complex of OB stars, giant HII regions, supernovae and supernova remnants all driving a hot galactic wind. This observation should detect and resolve a considerable number of supernovae, young remnants, OB star clusters and X-ray binaries in addition to the X-ray luminous hot interstellar medium. ACIS IMAGING OF THE STARBURST GALAXY M82 APPROVED GTO N S Y 814-865-0162 25.0 1 NORMAL GALAXIES 60 . . 01 18 184 01600053 Aug 29 1997 1:55PM The X-ray spectra of Seyfert galaxies can be very complex with combinations of thermal emission from the accretion disk, Compton upscattering of disk photons, Compton reflection continuum, nonthermal jet continuum, ultrasolf component, neutral and ionized absorbers. This study concentrates on high resolution spectroscopy of one bright Seyfert 1 (NGC 3783) and one bright Seyfert 2 (Circinus galaxy). NGC 3783 is a particularly good laboratory for study of the ionized `warm absorbers' in AGNs; numerous absorption edges are expected which will strongly constrain the geometry of material around the AGN. Circinus is expected to show a rich emission line spectrum superposed on a reflection continuum. ACIS GRATING SPECTROSCOPY OF SEYFERT GALAXIES APPROVED GTO N S Y 814-865-0162 135.0 2 NORMAL GALAXIES 60 . . 01 18 57 01600057 Aug 26 1997 2:10PM By monitoring M31 on a monthly basis we will be able to detect transients and follow thier evolution. Follow-up visits to newly discovered transients will be planned in order to monitor their spectral evolution during decay. These observations will provide a detailed look at the transient population of the nearest galaxy similar to the milky way. MONITORING M31 APPROVED GTO N S N 60.0 5 NORMAL GALAXIES 60 IRWIN SHAPIRO DIRECTOR 01 22 58 01600058 Aug 26 1997 2:10PM By monitoring M31 on a monthly basis we will be able to detect transients and follow thier evolution. Follow-up visits to newly discovered transients will be planned in order to monitor their spectral evolution during decay. These observations will provide a detailed look at the transient population of the nearest galaxy similar to the milky way. M31 MONITORING (FOLLOWUP) APPROVED GTO N S N 60.0 1 NORMAL GALAXIES 60 IRWIN SHAPRIO DIRECTOR 01 23 191 01600062 Sep 4 1997 12:23PM We will obtain an ACIS-S spectral image of the Antennae (NGC4038/NGC4039). This interacting galaxy pair shows complex ROSAT HRI emission, and contains 12 sources. ASCA shows that at least two spectral components are present. ACIS-S spectra and imaging will determine the nature of these sources and of the diffuse emission. This exposure will give 500 counts in each HRI source, sufficient for a spectrum. THE ANTENNAE APPROVED GTO N S N 74.0 1 NORMAL GALAXIES 60 IRWIN SHAPIRO DIRECTOR 01 25 194 01600065 Sep 4 1997 12:24PM NGC5128, the host galaxy of the Cen A, is the nearest elliptical galaxy, and the only one in which individual binary X-ray sources can be detected (and then only by AXAF). This allows a unique way to discriminate the hot ISM from the binary source contribution to elliptical galaxy emission. The absorption of the nuclear spectrum by the dust lane will provide diagnostics of the composition and ionization state of the absorber. The X-ray/radio jet is the closest powerful example of its kind. A detailed X-ray map will explicate jet physics, and will again serve to study the galaxy ISM through the jet interaction. NGC5128: BINARY SOURCES IN THE NEAREST ELLIPTICAL GALAXY APPROVED GTO N S N 74.0 1 NORMAL GALAXIES 60 IRWIN SHAPIRO DIRECTOR 01 77 180 01600067 Aug 28 1997 3:04PM Previous X-ray imaging studies have revealed that the optically flattened lenticular galaxy NGC 720 contains a massive flattened dark halo. The X-ray distribution also shows an isophotal twist misaligned from the stellar distribution, indicating a complex gravitational potential. Models for this galaxy, and implications for dark matter halo and galaxy formation in general, will be further constrained by the surface brightness and temperature distributions revealed by this observation. ACIS STUDY THE ELLIPTICAL GALAXY NGC 720 APPROVED GTO N S Y 814-865-0162 40.0 1 NORMAL GALAXIES 60 . . 01 18 198 01600133 Sep 4 1997 12:25PM A study of the mass distribution, gas, dark halos, and elemental abundances of early type elliptical galaxies. EARLY TYPE GALAXIES APPROVED GTO N S N 58.0 2 NORMAL GALAXIES 60 IRWIN SHAPIRO DIRECTOR 01 27 168 01600145 Aug 28 1997 9:50AM The program consists of 1) detailed spatially resolved spectra of bright elliptical galaxies and 2) deep images of high redshift cluster candidates NGC4472,NGC4636 and NGC 4472 are 3 of the brightest x-ray elliptical galaxies. The AXAF exposure times with ACIS-S are set to derive temperature and abundance profiles for >3 annuli inside the deVacouleurs radius allowing a direct comparison of the gas and stellar abundances and the gas and stellar temperatures. These deep exposures should also detect numerous x-ray binaries in these galaxies. 3C324 is a z~1.2 cluster that is the most distant x-ray cluster known. The S-Z cluster 1312+42 is one of two objects for which a significant Sunyaev-Zeldovich decrement is measured but for which there is no optical cluster visible. BRIGHT ELLIPTICAL GALAXIES AND HIGH REDSHIFT CLUSTERS APPROVED GTO N S N 325.0 8 NORMAL GALAXIES 60 S. HOLT GSFC 01 71 211 01600153 Sep 15 1997 1:53PM M51, the Whirlpool Galaxy, has a nuclear source and several point sources associated with spiral arms. Extent of the galaxy is 7 arcminutes so the entire system will be in good focus. The X-ray image will make an interesting contrast to the optical picture. DEMONSTRATION IMAGE OF M81 APPROVED CAL N N N 25.0 1 NORMAL GALAXIES 60 HARVEY TANANBAUM DIRECTOR OF ASC 01 86 6 01700006 Aug 26 1997 2:07PM Within a 30 day ROSAT HRI monitoring observations we have detected the strongest persistent X-ray variability known in a Seyfert galaxy. At least 5 giant amplitude variations with a factor of about 60 are visible. Unusually strong relativistic boosting effects provide the most plausible explanation of the X-ray data. We propose to use AXAF for a precise measurement of the position of the source of the strong variability to further proof that the X-rays we measure are associated with the distant galaxy. We expect about 500 HRC photons within 10 ks observing time. We may further improve the HRG position using serendipitous X-ray sources detected previously with the HRI that have counterparts in the Optical. A PRECISE MEASUREMENT OF THE POSITION OF THE SOURCE OF GIANT AND RAPID VARIABILITY IN THE NLS1 13224-3809 APPROVED GTO N S N 10.0 1 ACTIVE GALAXIES AND QUASARS 70 COR SCHOONENBERG SRON 01 6 8 01700008 Aug 26 1997 2:07PM 3 relatively bright AGNs are selected: 1 bright Seyfert 1 galaxy (NGC 5548) with strong soft X-ray excess and with indications for a warm absorber and line (EUV) emission 1 Seyfert 2 galaxy (NGC 1068) of which the continuum is blocked so that only reprocessed radiation is seen PKS 2155-304, the brightest BL Lac object on the sky. A broad absorption feature is tentatively identified as discrete absorption by O VIII Lyman alpha. OBSERVATIONS OF BRIGHT ACTIVE GALACTIC NUCLEI WITH LETGS APPROVED GTO N S N 220.0 3 ACTIVE GALAXIES AND QUASARS 70 COR SCHOONENBERG SRON 01 7 27 01700027 Aug 26 1997 2:08PM Observe 1 BL Lac to see absorption from relativistic jets, 1 AGN to resolve a possibly broad Fe-K line, 1 Sy 2 to detect and measure emission lines from hot gas near the nucleus, 1 high z QSO to find Fe-K emission and possible absorption, 1 high z QSO with damped Ly alpha absorption to see evidence for X-ray absorption, 1 narrow line Sy 1 galaxy to determine the nature of spectral features at 1 keV, 1 Sy 1 AGN to measure the emission and resolve absorption due to warm absorption, and 1 AGN in a cluster of galaxies to find absorption due to the hot cluster gas. HETG OBSERVATIONS OF VARIOUS ACTIVE GALACTIC NUCLEI APPROVED GTO N S Y 617-253-8573 355.0 6 ACTIVE GALAXIES AND QUASARS 70 PATRICIA K. GREER ASSOC. DIRECTOR, OFFICE OF SPONSORED PROGRAMS 01 12 159 01700035 Aug 26 1997 2:25PM The X-ray emission of radio jets and of the narrow line regions of active galaxies will be investigated with AXAF. Images and spectra will be obtained to define the morphologies, X-ray powers, emission mechanisms and physical conditions of both unresolved nuclear and extended emission. Detection of non-thermal X-rays (inverse Compton or synchrotron emission) will probe the properties of the magnetic fields and cosmic ray spectra. If thermal X-ray emission is detected, the density, temperature and chemical abundances of hot gas can be derived and the relationship to other components (radio emission, narrow line region) studied. Hot gas can be associated with hot radiatively driven winds, shocks driven by mass outflow or cooling accretion flows. STUDIES OF RADIO JETS AND THE NARROW LINE REGIONS OF ACTIVE GALAXIES WITH THE AXAF APPROVED GTO N S N 325.5 20 ACTIVE GALAXIES AND QUASARS 70 ERICA MAGRUM DIRECTOR 01 69 182 01700052 Aug 28 1997 3:05PM The ability to observe a distant quasar subject to gravitational lensing by a foreground cluster of galaxies provides unique insight into dark matter in clusters, cosmological parameters H_o and q_o, Ly-alpha absorption systems, and more. ACIS imaging can simultaneous resolve the emission of the AGN components and the intracluster medium of the lensing cluster, if present. Repeated observations can measure time delays and ACIS grating spectroscopy can measure differences in absorption along different lines of sight. ACIS STUDY OF GRAVITATIONALLY LENSED QUASARS APPROVED GTO N S Y 814-865-0162 160.0 4 ACTIVE GALAXIES AND QUASARS 70 . . 01 18 192 01700063 Sep 4 1997 12:23PM We will obtain ACIS-S spectra of quasars at high redshifts to investigate their: emission spectra to ~30keV (rest); Fe-K emission; low energy cut-offs. A search for extended emission around the quasars will limit any hot atmosphere associated with the surrounding galaxy/cluster in formation. PKS2126-158 is the brightest of the absorbed high z quasars. HE1104-1805 is a radio quiet quasar lensed to be bright. The lens contains a damped Lyman-alpha absorber that should affect the X-ray spectrum, and the two lens components are readily resolved by AXAF at 3 arcsec separation. HIGH REDSHIFT QUASAR SPECTRA APPROVED GTO N S N 74.0 2 ACTIVE GALAXIES AND QUASARS 70 IRWIN SHAPIRO DIRECTOR 01 76 193 01700064 Sep 4 1997 12:24PM B2 0738+313 is a Gigahertz Peaked Spectrum (GPS) radio source. Our ROSAT HRI observations show that the X-ray source is extended. This probably indicates a group or cluster of galaxies with a hot ICM is present. Such a high pressure environment may limit the expansion of the radio source and may cause its low frequency absorption. An AXAF image will allow the determination of the properties of this environment- scale size, temperature, pressure - separately from the quasar emission. EXTENDED EMISSION AROUND A GIGAHERTZ PEAKED RADIO SOURCE APPROVED GTO N S N 29.0 1 ACTIVE GALAXIES AND QUASARS 70 IRWIN SHAPIRO DIRECTOR 01 27 66 01700066 Aug 26 1997 2:11PM We propose a series of onservations of M82 spread over 1 year to investigsate the variability of sources in the nuclear region to a limiting luminosity of 1E37 ergs/sec. This will allow us to determnine if the hard x-rays ion M82 come from a low luminosity AGN and to investigate the properties of x-ray binaries and luminous SNR in the galaxy. Co-adding the data will allow studies of extended emission and a super-wind halo. THE ORIGIN OF HARD X-RAYS FROM M82 APPROVED GTO N S N 25.0 1 ACTIVE GALAXIES AND QUASARS 70 IRWIN SHAPIRO DIRECTOR 01 27 181 01700068 Aug 28 1997 3:04PM The rapid cosmic evolution of the QSO population predicts that a substantial fraction of massive galaxies today chould contain supermassive black holes. A recent optical emission line survey finds that over 40% of all nearby bright galaxies may harbor LLAGNs. These sources may contribute substantially to the X-ray background radiation. This snapshot survey provides brief ACIS images of the nuclei for a volume-limited sample of 25 candidate LLAGN plus several prototype galaxies of different classes. LOW-LUMINOSITY ACTIVE GALACTIC NUCLEI IN NEARBY GALAXIES APPROVED GTO N S Y 814-865-0162 68.0 34 ACTIVE GALAXIES AND QUASARS 70 . . 01 18 69 01700069 Aug 26 1997 2:11PM Time delays between components of gravitationally lensed quasars provide a unique and potentially accurate determination of the cosmological quantities H_o and q_o. Quasars generally have stronger and more rapid variations in the X-ray band than at lower frequencies so that reliable time delay measurements should be achievable. High resolution X-ray images are needed both to resolve the quasar images and to study the mass distribution of the intervening lensing structure. This observation surveys promising candidates for later intensive monitoring to obtain time delay measurements. A SURVEY OF GRAVITATIONALLY LENSED QUASARS APPROVED GTO N S Y 814-865-0162 120.0 8 ACTIVE GALAXIES AND QUASARS 70 . . 01 18 204 01700097 Sep 15 1997 10:32AM Mkn 421 is a bright BL lac object with a simple absorbed power-law continuum. This source will be used to measure the relative throughput of the gratings. Mkn 421 was the primary in-flight spectroscopic calibration source for the ROSAT PSPC. The LETG/HRC-S observation will be done simultaneously with a EUVE observation to allow a cross calibration of LETG/HRC-S in the 100-160A spectral region. The EUVE observing window for Mkn421 is between 11/22 and 5/17. GRATINGS OBSERVATIONS OF A FEATURELESS CONTINUUM: MKN 421 APPROVED CAL N N N 110.3 5 ACTIVE GALAXIES AND QUASARS 70 RICHARD VANELLI DR. HARVEY TANABAUM 01 83 205 01700101 Sep 15 1997 10:33AM The targets 3C 273 and Cyg X-2 are well-studied continuum sources that we propose to observe as calibration targets. The QSR 3C 273 has been observed for calibration purposes by XTE, SAX and ASCA simultaneously, so a cross-calibration with these missions would be possible if any of them can be available when AXAF observes 3C 273. In the case of Cyg X-2, its spectrum is relatively well known and it is known to be point-like, so that cross dispersion profiles can be measured. IN FLIGHT CALIBRATION OF THE HETGS EFFECTIVE AREA AND CROSS DISPERSION PROFILE APPROVED CAL N N Y 617-253-8573 150.0 4 ACTIVE GALAXIES AND QUASARS 70 HARVEY TANANBAUM DIRECTOR OF ASC 01 84 108 01700108 Aug 26 1997 2:14PM CenA, the nearest active galaxy, has both AGN and a jet, both demonstrated X-ray emitters. This observation will thus show emission from a black hole, the jet, and probably other bright sources in the CenA galaxy. The X-ray image will also make an interesting contrast to the optical picture. DEMONSTRATION IMAGE OF CENA APPROVED CAL N N N 10.0 1 ACTIVE GALAXIES AND QUASARS 70 HARVEY TANANBAUM DIRECTOR OF ASC 01 52 110 01700110 Aug 26 1997 2:14PM M82 is a starburst (formerly exploding) galaxy with sources and diffuse emission in the central region. DEMONSTRATION IMAGE OF M82 APPROVED CAL N N N 10.0 1 ACTIVE GALAXIES AND QUASARS 70 HARVEY TANANBAUM DIRECTOR OF ASC 01 54 124 01700124 Aug 26 1997 2:15PM Observe 1 BL Lac to see absorption from relativistic jets, 1 AGN to resolve a possibly broad Fe-K line, 1 Sy 2 to detect and measure emission lines from hot gas near the nucleus, 1 high z QSO to find Fe-K emission and possible absorption, 1 high z QSO with damped Ly alpha absorption to see evidence for X-ray absorption, 1 narrow line Sy 1 galaxy to determine the nature of spectral features at 1 keV, 1 Sy 1 AGN to measure the emission and resolve absorption due to warm absorption, and 1 AGN in a cluster of galaxies to find absorption due to the hot cluster gas. HETG OBSERVATIONS OF VARIOUS ACTIVE GALACTIC NUCLEI APPROVED GTO N S Y 617-253-8573 125.0 1 ACTIVE GALAXIES AND QUASARS 70 PATRICIA K. GREER ASSOC. DIRECTOR, OFFICE OF SPONSORED PROGRAMS 01 59 201 01700131 Sep 9 1997 11:24AM ROSAT and ASCA have revealed a rich variety of quasars and AGN with highly obscured nuclei. In many cases X-ray spectra are sensitive to material that is otherwise invisible. We shall obtain prototype spectra of the brightest source of each type. PHL5200, a Broad Absorption Line Quasar (BALQSO), z=1.98; PHL 6625 is a z=0.38 Quasar absorbed by the foreground galaxy NGC247; 3C212 is a red quasar with a weakly ionized absorber; 3C351 has a high ionization absorber. OBSCURED QUASARS AND AGN APPROVED GTO N S N 30.0 2 ACTIVE GALAXIES AND QUASARS 70 IRWIN SHAPIRO DIRECTOR 01 25 132 01700132 Aug 26 1997 2:16PM We will obtain ACIS-S images of nearby Seyfert galaxies known to have extended X-ray emission. The alignment of the X-ray structures with the optical and/or radio features, and the amount of line emission present in the ACIS spectra, will determine the emission mechanism(s) at work. EXTENDED X-RAY EMISSION AROUND NEARBY SEYFERTS APPROVED GTO N S N 20.0 1 ACTIVE GALAXIES AND QUASARS 70 IRWIN SHAPIRO DIRECTOR 01 25 199 01700134 Sep 4 1997 12:25PM We will use the power of AXAF to resolve the AGn from the surroundiong starburst in composite nuclei, to study the x-ray properties of discrete starforming regions in hot spot galaxies and hence the evolution of the starburst. STUDIES OF STARBURST GALAXIES APPROVED GTO N S N 39.0 2 ACTIVE GALAXIES AND QUASARS 70 IRWIN SHAPIRO DIRECTOR 01 27 209 01700151 Sep 15 1997 10:34AM AGN used to determine on-axis PSF AGN used to determine on-axis PSF APPROVED CAL N N N 40.0 4 ACTIVE GALAXIES AND QUASARS 70 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 169 01100146 Aug 28 1997 9:50AM These observations form part of a systematic determination of H0 and q0 by combining X-ray observations of distant galaxy clusters with radio measurements of the Sunyaev Zel'dovich effect. DETERMINATION OF H0/Q0 APPROVED GTO N S N 750.0 37 CLUSTERS OF GALAXIES 80 DR. HARVEY TANANBAUM ASC DIRECTOR 01 72 10 01800010 Aug 26 1997 2:07PM To determine the structural and spectral properties of the cooling flow in the cluster A1795 (Allen & Fabian, MN, 286, 583, 1997; Fabian et al ApJ, 436, L63, 1994). The use of both FI and BI spectra should enable the level of excess absorption and its covering factor to be well quantified. THE COOLING FLOW IN A1795 APPROVED GTO N S N 40.0 2 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 11 01800011 Aug 26 1997 2:07PM To determine the structural and spectral properties of the cooling flow around A1835 (Allen et al, MN, 283, 263, 1996). This includes measurement of the temperatures of the multiphase medium, excess absorption, any abundance gradients, interaction with the central.radio source, and the mass profile to compare with that deduced from lensing. THE MASSIVE COOLING FLOW IN A1835 APPROVED GTO N S N 30.0 2 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 12 01800012 Aug 26 1997 2:07PM To determine the structural and spectral properties of the cooling flow in the cluster A2199 (Allen & Fabian, MN, 286, 583, 1997). The use of both FI and BI spectra should enable the level of excess absorption and its covering factor to be well quantified. THE COOLING FLOW IN A2199 APPROVED GTO N S N 40.0 2 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 13 01800013 Aug 26 1997 2:07PM To determine the structural and spectral properties of the massive cooling flow in A2204 (Peres et al 1997 MN submitted). This includes measurement of the temperatures of the multiphase medium, excess absorption, and detailed mass dropout distribution. THE MASSIVE COOLING FLOW IN A2204 APPROVED GTO N S N 10.0 1 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 14 01800014 Aug 26 1997 2:07PM To determine the structural and spectral properties of the massive cooling flow in A2390 (Pierre et al, A&A, 311, 413, 1996; Allen, MN submitted). This includes measurement of the temperatures of the multiphase medium, excess absorption, detailed mass dropout distribution and mass profile for comparison with lensing models. THE MASSIVE COOLING FLOW IN A2390 APPROVED GTO N S N 20.0 2 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 15 01800015 Aug 26 1997 2:07PM To determine the structure and spectral properties of the cooling flow around NGC1275 in the core of the Perseus Cluster, A426 (Fabian et al ApJ 248, 47, 1981; Fabian et al 1994 ApJ 436, L63). This includes measurement of the temperatures of the multiphase medium, excess absorption, any abundance gradients and study of the interaction of the radio lobes with the surrounding gas (Bohringer et al MN 264, L25, 1993). THE COOLING FLOW IN THE PERSEUS CLUSTER APPROVED GTO N S N 50.0 2 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 16 01800016 Aug 26 1997 2:08PM To determine the structure and spectral properties of the cooling flow around NGC4696 in the core of the Centaurus Cluster (Allen & Fabian, 269, 409, 1994; Fabian et al, ApJ, 436, L63, 1994). This includes measurement of the temperatures of the multiphase medium, excess absorption, and the abundance gradients. THE COOLING FLOW IN THE CENTAURUS CLUSTER APPROVED GTO N S N 40.0 2 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 17 01800017 Aug 26 1997 2:08PM To determine the structural and spectral properties of the massive cooling flow in RXJ1347-114 (Schindler et al, A&A, 317, 646, 1996; Allen MN submitted). This includes measurement of the temperatures of the multiphase medium, excess absorption, and detailed mass dropout distribution. THE MASSIVE COOLING FLOW IN RXJ1347-114 APPROVED GTO N S N 20.0 2 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 19 01800019 Aug 26 1997 2:08PM To determine the structural and spectral properties of the cooling flow around PKS0745-191 (Fabian et al, 216, 923, 1985; Allen, Fabian & Kneib, MN, 279, 615, 1996). This includes measurement of the temperatures of the multiphase medium, excess absorption, any abundance gradients, the interaction with the central radio source and the mass profile for comparison with that determined by us using lensing data. THE MASSIVE COOLING FLOW IN PKS0745-191 APPROVED GTO N S N 30.0 1 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 20 01800020 Aug 26 1997 2:08PM To determine the structural and spectral properties of the massive cooling flow in IRAS09104+4109 (Fabian & Crawford, MN 274, L63, 1995; Fabian et al, ApJ, 274, L51, 1994). This includes measurement of the temperatures of the multiphase medium, excess absorption, detailed mass dropout distribution and structures at the centre of the flow. THE MASSIVE COOLING FLOW IN IRAS09104_4109 APPROVED GTO N S N 10.0 1 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 26 01800026 Aug 26 1997 2:08PM We propose to obtain HETGS data on two bright clusters of galaxies which show strong evidence for cooling flows. PKS 0745-191 (z=0.1028) and Abell 1835 (z=0.2523) exhibit large cooling rates of ~1400 M_sol/yr and ~2300 M_sol/yr, respectively. The HETG will allow us to measure a number of X-ray emission lines from the cooling gas. Each of these measurements will provide an independent test of the cooling rates. In addition, it will be possible to search for absorption features due to accumulated cold material. Determining the fate of the large amounts of cooling material predicted in these objects is currently the greatest challenge facing the cooling flow theory. HIGH RESOLUTION X-RAY SPECTRA OF CLUSTER COOLING FLOWS APPROVED GTO N S Y 617-258-7254 235.0 2 CLUSTERS OF GALAXIES 80 PATRICIA K. GREER ASSOC. DIRECTOR, OFFICE OF SPONSORED PROGRAMS 01 11 177 01800048 Aug 28 1997 3:03PM The mass of X-ray emitting gas in rich clusters can considerably exceed the mass in stars, and is enriched in heavy elements. The origin and evolution of this intracluster medium are not fully understood. This observation of an X-ray-bright cluster at z = 0.83 will give insight into the mass, temperature and metal distribution of the medium at an early epoch, as well as measurement of the gravitational potential. X-RAY PROPERTIES OF A HIGH-REDSHIFT CLUSTER APPROVED GTO N S Y 814-865-0162 90.0 1 CLUSTERS OF GALAXIES 80 . . 01 18 56 01800056 Aug 26 1997 2:10PM ROSAT PSPC image of A3667 suggests a shock wave located to the South-East of the cluster center. The X-ray surface brightness drops by a factor of 5 within 1' across the shock; the Hugoniot adiabat predicts a 50% temperature drop. A 100 ksec ACIS-I observation would enable an accurate measurement of the shock temperature profile (~1keV accuracy will be achieved in 15"x4.5' strips along the shock). The shock density profile will be resolved because the free path of electrons,15 kpc, corresponds to 10" at the cluster redshift. Important information about the ICM can be derived from these observations. For example, shaper shocks with milder temperature drop are expected if the magnetic fields are dynamically important. RESOLVING THE SHOCK WAVE IN ABELL 3667 APPROVED GTO N S N 50.0 1 CLUSTERS OF GALAXIES 80 IRWIN I. SHAPIRO DIRECTOR 01 21 70 01800070 Aug 26 1997 2:11PM A1367 is a unique cluster with multiple "clumps" first observed with the Einstein Observatory and then with ROSAT. Some of these clumps appear to be coincident with cluster galaxies, others do not. A high resolution image with CCD energy resolution will help determine what these clumps really are. A1367: A CLUSTER WITH STRUCTURE APPROVED GTO N S N 40.0 1 CLUSTERS OF GALAXIES 80 IRWIN SHAPIRO DIRECTOR 01 29 183 01800072 Aug 28 1997 3:05PM Clusters of galaxies are large gravitationally bound systems dominated by dark matter (DM). The amount and spatial distribution of DM in clusters are keys to understanding the development of cosmic structure and cosmography. The gravitational potential of clusters observed here can been mapped in various ways: strong or weak gravitational lensing of background galaxies, Sunyaev-Zel'dovich effect, and X-ray gas hydrostatic equilibrium. ACIS will measure the cluster X-ray surface brightness and temperature profiles, detect nonuniformities and substructure that will signficantly improve our understanding of their DM distribution. ACIS STUDY OF DARK MATTER IN CLUSTERS APPROVED GTO N S Y 814-865-0162 145.0 2 CLUSTERS OF GALAXIES 80 . . 01 18 83 01800083 Aug 26 1997 2:12PM To determine the structural and spectral properties of the massive cooling flow in the Virgo cluster (Stewart et al 1984, ApJ 278,536). This includes measurement of the temperatures of the multiphase medium, excess absorption, and detailed mass dropout distribution. THE COOLING FLOW IN THE VIRGO CLUSTER AROUND M87 APPROVED GTO N S N 10.0 1 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 92 01800092 Aug 26 1997 2:13PM Calibration Observation - The Coma cluster of galaxies is an extended, nearly isothermal (kT = 8 keV) source of X-rays. The extent of the Coma cluster is sufficient to completely cover all 4 detectors when observed on-axis. This source will be observed periodically by all 4 focal plane instruments throughout the AXAF mission to monitor any temperoal variations in the characteristics of the detectors. This observation is the first such measurement and needs to be carried out shortly after launch to establish a fiducial point from which subsequent observations will be compared. CALIBRATION OBSERVATION OF AN EXTENDED HARD SOURCE: THE COMA CLUSTER APPROVED CAL N N N 80.0 4 CLUSTERS OF GALAXIES 80 RICHARD VANELLI DR. HARVEY TANABAUM 01 39 213 01800096 Sep 15 1997 1:58PM Abell 1060 is an extended, nearly isothermal (kT=4 keV) source of X-rays. The X-ray spectrum of A1060 is dominated my strong emission lines from Fe, Ne, Mg, Si, S, Ca, and Ar. This source will be observed periodically by all 4 focal plane instruments throughout the AXAF mission to monitor any temperoal variations in the characteristics of the detectors. This observation is the first such measurement and needs to be carried out shortly after launch to establish a fiducial point from which subsequent observations will be compared. A1060 is well suited to monitor changes in the CTI of the CCDs due to radiation damage, since it is a good source of lines in addition to those avaiable with the internal ACIS calibration source. CALIBRATION OBSERVATION OF AN EXTENDED MEDIUM SOURCE: ABELL 1060 APPROVED CAL N N N 17.5 2 CLUSTERS OF GALAXIES 80 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 105 01800105 Aug 26 1997 2:14PM The radio galaxy Hydra A, is the central dominant galaxy in one of the strongest know cluster cooling flows with a mass accretion rate of 600 Mo/yr. This observation will generate two X-ray spectra (with both a front and back side illuminated ACIS chip) of a cooling flow for science calibration. The Hydra A cluster is also at a low enough redshift (z=0.5) that the central cooling flow region will be resolved with AXAF. DEMONSTRATION SPECTRUM OF A COOLING FLOW CLUSTER: HYDRA A APPROVED CAL N N N 20.0 2 CLUSTERS OF GALAXIES 80 RICHARD VANELLI DR. HARVEY TANABAUM 01 47 207 01800109 Sep 15 1997 10:33AM A nearby and a distant cluster are used to show AXAF's capability. DEMONSTRATION IMAGES OF CLUSTERS APPROVED CAL N N N 50.0 2 CLUSTERS OF GALAXIES 80 HARVEY TANANBAUM DIRECTOR OF ASC 01 85 218 01800115 Sep 15 1997 1:59PM Abell 1060 is an extended, nearly isothermal (kT=4 keV) source of X-rays. The X-ray spectrum of A1060 is dominated my strong emission lines from Fe, Ne, Mg, Si, S, Ca, and Ar. This source will be observed periodically by all 4 focal plane instruments throughout the AXAF mission to monitor any temperoal variations in the characteristics of the detectors. This observation is the first such measurement and needs to be carried out shortly after launch to establish a fiducial point from which subsequent observations will be compared. A1060 is well suited to monitor changes in the CTI of the CCDs due to radiation damage, since it is a good source of lines in addition to those avaiable with the internal ACIS calibration source. CALIBRATION OBSERVATION OF AN EXTENDED MEDIUM SOURCE (DEC 1998): ABELL 1060 APPROVED CAL N N N 17.5 2 CLUSTERS OF GALAXIES 80 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 219 01800116 Sep 15 1997 2:00PM Abell 1060 is an extended, nearly isothermal (kT=4 keV) source of X-rays. The X-ray spectrum of A1060 is dominated my strong emission lines from Fe, Ne, Mg, Si, S, Ca, and Ar. This source will be observed periodically by both ACIS detectors throughout the AXAF mission to monitor any temperoal variations in the characteristics of the detectors. A1060 is well suited to monitor changes in the CTI of the CCDs due to radiation damage, since it is a good source of lines in addition to those avaiable with the internal ACIS calibration source. CALIBRATION OBSERVATION OF AN EXTENDED MEDIUM SOURCE (MAR 1999): ABELL 1060 APPROVED CAL N N N 54.200000000000003 4 CLUSTERS OF GALAXIES 80 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 220 01800117 Sep 15 1997 2:00PM Abell 1060 is an extended, nearly isothermal (kT=4 keV) source of X-rays. The X-ray spectrum of A1060 is dominated my strong emission lines from Fe, Ne, Mg, Si, S, Ca, and Ar. This source will be observed periodically by both ACIS detectors throughout the AXAF mission to monitor any temperoal variations in the characteristics of the detectors. A1060 is well suited to monitor changes in the CTI of the CCDs due to radiation damage, since it is a good source of lines in addition to those avaiable with the internal ACIS calibration source. CALIBRATION OBSERVATION OF AN EXTENDED MEDIUM SOURCE (JUNE 1999): ABELL 1060 APPROVED CAL N N N 17.5 2 CLUSTERS OF GALAXIES 80 RICHARD VANELLI DR. HARVEY TANABAUM 01 43 221 01800120 Sep 15 1997 2:00PM Calibration Observation - The Coma cluster of galaxies is an extended, nearly isothermal (kT = 8 keV) source of X-rays. The extent of the Coma cluster is sufficient to completely cover all 4 detectors when observed on-axis. This source will be observed periodically by the HRC-I and HRC-S throughout the AXAF mission to monitor any temperal variations in the characteristics of the detectors. CALIBRATION OBSERVATION OF AN EXTENDED HARD SOURCE (DEC 1998): THE COMA CLUSTER APPROVED CAL N N N 40.0 2 CLUSTERS OF GALAXIES 80 RICHARD VANELLI DR. HARVEY TANABAUM 01 39 222 01800121 Sep 15 1997 2:01PM Calibration Observation - The Coma cluster of galaxies is an extended, nearly isothermal (kT = 8 keV) source of X-rays. The extent of the Coma cluster is sufficient to completely cover all 4 detectors when observed on-axis. This source will be observed periodically by the HRC-I and HRC-S throughout the AXAF mission to monitor any temperal variations in the characteristics of the detectors. CALIBRATION OBSERVATION OF AN EXTENDED HARD SOURCE (MAR 1999): THE COMA CLUSTER APPROVED CAL N N N 40.0 2 CLUSTERS OF GALAXIES 80 RICHARD VANELLI DR. HARVEY TANABAUM 01 39 223 01800122 Sep 15 1997 2:01PM Calibration Observation - The Coma cluster of galaxies is an extended, nearly isothermal (kT = 8 keV) source of X-rays. The extent of the Coma cluster is sufficient to completely cover all 4 detectors when observed on-axis. This source will be observed periodically by the HRC-I and HRC-S throughout the AXAF mission to monitor any temperal variations in the characteristics of the detectors. CALIBRATION OBSERVATION OF AN EXTENDED HARD SOURCE (JUNE 1999): THE COMA CLUSTER APPROVED CAL N N N 40.0 2 CLUSTERS OF GALAXIES 80 RICHARD VANELLI DR. HARVEY TANABAUM 01 39 135 01800135 Aug 26 1997 2:16PM Study of the mass distributions in relatively relaxed, round, clusters of galaxies. Observe a set of bright clusters to derive the mass distribution, abundance distribution and compare with other mass estimates (e.g., lensing) MASS DISTRIBUTIONS OF RELAXED CLUSTERS APPROVED GTO N S N 60.0 2 CLUSTERS OF GALAXIES 80 IRWIN SHAPIRO DIRECTOR 01 29 138 01800138 Aug 26 1997 2:16PM To determine the structural and spectral properties of the massive cooling flow in A2597 (Crawford et al 1989, MN 236, 979). This includes measurement of the temperatures of the multiphase medium, excess absorption, and detailed mass dropout distribution. THE COOLING FLOW IN A2597 APPROVED GTO N S N 0.0 0 CLUSTERS OF GALAXIES 80 P ASLIN SECRETARY OF THE INSTITUTE OF ASTRONOMY 01 8 172 01800147 Aug 28 1997 3:00PM Clusters of galaxies are large gravitationally bound systems dominated by dark matter (DM). The amount and spatial distribution of DM in clusters are keys to understanding the development of cosmic structure and cosmography. The gravitational potential of clusters observed here can been mapped in various ways: strong or weak gravitational lensing of background galaxies, Sunyaev-Zel'dovich effect, and X-ray gas hydrostatic equilibrium. ACIS will measure the cluster X-ray surface brightness and temperature profiles, detect nonuniformities and substructure that will signficantly improve our understanding of their DM distribution. ACIS STUDY OF DARK MATTER IN CLUSTERS APPROVED GTO N S Y 814-865-0162 20.0 1 CLUSTERS OF GALAXIES 80 . . 01 73 185 01800148 Sep 4 1997 12:21PM The cluster 1E0657-56 is the highest temperature known cluster; an accurate determination of the temperature and structure of this distant cluster will place useful constraints upon cosmological parameters. TEMPERATURE AND STRUCTURE OF A VERY HOT CLUSTER APPROVED GTO N S N 28.0 1 CLUSTERS OF GALAXIES 80 DR. HARVEY TANANBAUM ASC DIRECTOR 01 75 25 01900025 Aug 26 1997 2:08PM We will perform a Deep Survey of the Lockman Hole to a depth of 1x10^-16 erg/cm^2/sec. Of order 400 sources are expected to be detected within the HRC "good" filed of view, and the CXRB may be fully resolved. The HRC-I provides accurate positions and extent information for the sources. Identifications should be unambiguous through correlations at other wavelengths. Existing questions about the contributions of NLXGs to the background should be resolved. DEEP SURVEY OF THE LOCKMAN HOLE APPROVED GTO N S N 350.0 1 EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS 90 IRWIN SHAPIRO DIRECTOR 01 10 173 01900037 Aug 28 1997 3:02PM This observation of the X-ray background will achieve unprecedented sensitivity to faint X-ray sources, particularly in the 2-10 keV band. Source counts and arcsecond positions for several hundred sources will be obtained with spectra and variability for the stronger sources. Combined with the superb optical images and spectroscopy available for the Hubble Deep Field and flanking fields, and new spectroscopy where needed, this study should considerably elucidate the composition and astrophysics of the high-energy cosmic background radiation. DEEP ACIS OBSERVATION OF THE HUBBLE DEEP FIELD APPROVED GTO N S Y 814-865-0162 237.0 1 EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS 90 . . 01 74 98 01900098 Aug 26 1997 2:14PM We propose to use ACIS-I to carry out an ultra-deep deep observation of the Hubble Deep Field South with the following objectives: 1) Further insight into the nature of the sources which constitute the the extra-galactic X-ray background; 2) The detection and source spectrum of the most luminous HDF-S galaxies ULTRA DEEP AXAF OBSERVATION OF THE HDF-S WITH ACIS APPROVED GTO N S N 325.0 1 EXTRAGALACTIC DIFFUSE EMISSION AND SURVEYS 90 RICCARDO GIACCONI DIRECTOR GENERAL 01 45 196 01910075 Sep 4 1997 12:25PM We propose a deep ACIS-S observation of 47 Tuc to confirm and map our ROSAT discovery of diffuse emission from a probable bow shock and possible non-thermal emission from the large population of millisecond pulsars. The bow shock emission will be mapped out to 5-10arcmin from the peak diffuse emission and measure the proper motion of the cluster in the Galaxy. The spectral distribution will constrain both the mass loss of cluster stars and the temperature-density of the hot gas in the galactic halo. The possible IC emission from low energy CR electrons accelerated in the bow shock will constrain the MSP population and particle production in the cluster, while the spectra of point sources will complement and extend our deep HRC-I survey for CVs and dim x-ray sources in this key cluster. DIFFUSE X-RAY EMISSION IN GLOBULARS: HOT GAS VS. NON-THERMAL EMISSION IN 47 TUC APPROVED GTO N S N 74.0 1 GALACTIC DIFFUSE EMISSION AND SURVEYS 91 IRWIN SHAPIRO DIRECTOR 01 78 93 01910093 Aug 26 1997 2:13PM This observation is a "science calibration", to illustrate the science capabilities of AXAF. It is to be done early and archived so the data are accessable to all without delay. There is no proprietary period. Eta Carinae is a diffuse source, 1 arcminute in diameter, surrounding a strongly absorbed central star. It is the brighest extrasolar source at a wavelength of 2 microns. Comparison of the AXAF image with the widely-distributed HST image should be of particular interest to the general public. The ACIS CC observation is to obtain a spectrum of the central source undistorted by pileup. DEMONSTRATION IMAGE OF ETA CARINAE APPROVED CAL N N N 30.0 2 GALACTIC DIFFUSE EMISSION AND SURVEYS 91 HARVEY TANANBAUM DIRECTOR OF ASC 01 40