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Chandra proposals are divided into the following categories:
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SOLAR SYSTEM
--------------------------------------------------
===================================================================================
Proposal Number: 02100065
Proposal Title: ASTEROID OBSERVATION
PI: GORDON GARMIRE
Subject Category: SOLAR SYSTEM
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:03:50.98 +12:34:32.52 1998 WT24 ACIS-S NONE 3.30
08:04:21.04 +12:23:44.99 1998 WT24 ACIS-S NONE 3.30
08:04:50.29 +12:11:54.56 1998 WT24 ACIS-S NONE 3.30
===================================================================================
Proposal Number: 02100129
Proposal Title: GRB OBSERVATION
PI: GORDON GARMIRE
Subject Category: SOLAR SYSTEM
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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GRB ACIS-I NONE 80.00
===================================================================================
Proposal Number: 02100164
Proposal Title: MARS - A PLANETARY ANALOG TO A COMET
PI: KONRAD DENNERL
Subject Category: SOLAR SYSTEM
Abstract: The discovery of unexpectedly bright X-ray emission from comets has led
to increased interest in X-ray studies of solar system objects. It has
demonstrated that even in our immediate astronomical environment surprises may be
waiting to be discovered. With its carbon and oxygen rich atmosphere and the
absence of a strong magnetic field, Mars represents a planetary analog to a
comet. Soft X-ray observations provide a sensitive tool to study the tenuous
outer regions of such atmospheres for outgassing effects and interactions with
the solar wind. Chandra is the first imaging X-ray satellite which is able to
observe Mars at opposition, when it is closest to Earth.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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17:00:33.95 -26:56:00.13 MARS ACIS-I NONE 30.00
===================================================================================
Proposal Number: 02100148
Proposal Title: THE MORPHOLOGY OF JOVIAN X-RAYS AND SUPPORT OF THE CASSINI FLYBY
OF JUPITER
PI: G. GLADSTONE
Subject Category: SOLAR SYSTEM
Abstract: We propose HRC-I observations of Jupiter's x-ray emissions. At 10 times
the spatial resolution of existing observations, the Chandra data will allow: 1)
latitudinal location of the x-ray relative to far-ultraviolet auroral emissions,
which will allow confirmation of the x-ray magnetospheric source region; 2)
separation of the two sources of low-latitude x-rays (radiation-belt particle
precipitation and solar x-ray fluorescence), establishing their relative
importance, and the mapping of high-order B-field components; 3) a search for
lightning-generated x-ray emissions from high-shear zones in the lower
atmosphere. The observations will be part of an extensive campaign during the
Cassini flyby of Jupiter, including 35 HST orbits, which will greatly enhance the
science yield of the data.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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04:06:39.20 +20:00:08.65 JUPITER HRC-I NONE 36.00
===================================================================================
Proposal Number: 02100340
Proposal Title: X-RAY SPECTROSCOPY OF COMET C/1999 T1
PI: VLADIMIR KRASNOPOLSKY
Subject Category: SOLAR SYSTEM
Abstract: The generation of X-rays in comets is a new puzzling phenomenon. We
propose a spectroscopic study of X-rays in comet C/1999 T1 at E>0.15 keV using
ACIS-S for 19 ksec. We have obtained the EUVE spectra of comet Hyakutake (that
was powerful and exceptionally close) up to 0.15 keV with resolving power of 10
and signal-to-noise ratio of 15. Comets are very extended sources, therefore the
resolving powers of ACIS-S and HRC-S/LETG are similar (3.5 and <6 for C/1999
T1)in the range of 0.15-0.85 keV, while the ACIS-S effective area is better by a
factor of 30. This proposal is directly related to NASA's programs for both X-ray
astronomy and solar system science and is a continuation of our study of X-ray
emission from comets which has engendered a broad response in scientific
community and public
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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15:17:51.30 -06:57:30.42 C/1999 T1 ACIS-S NONE 3.40
15:21:48.97 -05:46:43.32 C/1999 T1 ACIS-S NONE 3.40
15:29:06.91 -03:35:28.86 C/1999 T1 ACIS-S NONE 3.40
15:32:26.79 -02:35:50.93 C/1999 T1 ACIS-S NONE 3.40
15:34:27.99 -01:56:55.50 C/1999 T1 ACIS-S NONE 3.40
***********************************************************************************
NORMAL STARS AND WD
--------------------------------------------------
===================================================================================
Proposal Number: 02200030
Proposal Title: HIGH-RESOLUTION SPECTRUM OF UX ARI
PI: ALBERT BRINKMAN
Subject Category: NORMAL STARS AND WD
Abstract: We plan to study the soft X-ray spectrum of the stellar coronal source
UX Ari and its time variability.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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03:26:35.40 +28:42:54.50 UX ARI HRC-S LETG 120.00
===================================================================================
Proposal Number: 02200045
Proposal Title: COLLIDING STELLAR WINDS IN IOTA ORIONIS.
PI: CLAUDE CANIZARES
Subject Category: NORMAL STARS AND WD
Abstract: IOTA Orionis is an early type binary system consisting of two O-type
stars. This system is one of the prototypes for the possible existence of
colliding winds. The X-rays are thought to be generated in cooling zones behind
shock fronts in the winds. Models show that X-ray emission is extremely dependent
on the amount of cooling in the shock flow. Fits to ROSAT data show that
post-shock temperatures assuming cooling layers behind the shocks instead of
isothermal shocks result in significantly higher post shock temperatures. The
highly resolved X-ray spectrum of IOTA Orionis will provide direct measures for
post shock tempertures and densities to test current models. It may also help to
understand the unusually hot spectrum observed previously in Theta Ori.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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05:35:26.00 -05:54:35.00 IOTA ORIONIS ACIS-S HETG 11.00
05:35:26.00 -05:54:35.00 IOTA ORIONIS ACIS-S HETG 39.00
===================================================================================
Proposal Number: 02200047
Proposal Title: HIGH-RESOLUTION SPECTROSCOPY OF ACTIVE COOL STARS
PI: CLAUDE CANIZARES
Subject Category: NORMAL STARS AND WD
Abstract: The cool, active binary stars have a forest of coronal emission lines.
These prominent features, along with any continuum emission, are diagnostics of
the temperature and density structure of coronae, abundances, and geometric
extent. Eclipse modulation can provide a direct measurement of coronal geometry.
TY Pyx is a 3-day period near-totally eclipsing RS CVn system. We will obtain
HETG spectra through the primary eclipse to obtain phase-resolved coronal
diagnostics.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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08:59:42.70 -27:48:58.70 TY PYX (HD77137) ACIS-S HETG 50.00
===================================================================================
Proposal Number: 02200056
Proposal Title: OBSERVATION OF MASSIVE BINARY
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:35:08.28 +09:56:03.00 LAMBDA ORIONIS ACIS-I NONE 10.00
===================================================================================
Proposal Number: 02200057
Proposal Title: OBSERVATION OF BROWN DWARF
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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11:31:55.40 -34:36:27.00 TWA-5 ACIS-S NONE 10.00
===================================================================================
Proposal Number: 02200061
Proposal Title: OBSERVATION OF M17
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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18:20:29.90 -16:10:45.50 M17 ACIS-I NONE 40.00
===================================================================================
Proposal Number: 02200064
Proposal Title: OBSERVATION OF M-DWARF SYSTEM
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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19:53:54.80 +44:24:54.00 G208-45 ACIS-I NONE 5.00
===================================================================================
Proposal Number: 02200073
Proposal Title: HETG OBSERVATIONS OF THE K GIANT BETA CETI
PI: JEFFREY LINSKY
Subject Category: NORMAL STARS AND WD
Abstract: Beta Ceti (HD 4128) is the brightest K giant as seen in X-rays. This K0
III post helium flash star is unusually luminous in X-rays compared to other
clump giants. The high X-ray luminosity may be due to its age or to a rejuvenated
dynamo as a result of angular momentum redistribution in its core. We propose a
deep (88 ks) HETG observation to measure the coronal temperature structure,
coronal densities, and coronal abundances of this unusual star.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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00:43:35.40 -17:59:11.80 BETA CETI ACIS-S HETG 88.00
===================================================================================
Proposal Number: 02200080
Proposal Title: EMISSION FROM LATE-TYPE STAR AD LEO
PI: STEPHEN MURRAY
Subject Category: NORMAL STARS AND WD
Abstract: 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 rotations, 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.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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10:19:36.92 +19:52:12.20 AD LEO HRC-S LETG 50.00
===================================================================================
Proposal Number: 02200099
Proposal Title: IS THE HOT DO WHITE DWARF KPD0005+5106 REALLY A CORONAL X-RAY
SOURCE?
PI: STEPHEN MURRAY
Subject Category: NORMAL STARS AND WD
Abstract: We will observe the hot DO white dwarf KPD0005+5106 with the Chandra
LETG to conclusively show whether or not the X-ray emission arises from a coronal
plasma. If the emission is merely photospheric, then the spectrum will form a
continuum possibly including absorption features from heavy elements in the
atmosphere. In contrast, a coronal plasma will generate an emission line
spectrum. If this hypothesis is finally prove, this white dwarf will be
completely unique as the only coronal degenerate star detected in the soft X-ray
band. Such a source probably arises from a hot wind, or interaction of a wind
with surrounding circumstellar material. A detailed analysis of the line emission
will reveal the physical conditions within the plasma and allow examination of
alternative models.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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00:08:17.00 +51:22:54.00 KPD0005+5106 HRC-S LETG 20.00
===================================================================================
Proposal Number: 02200081
Proposal Title: STAR FORMING REGION NGC 6530
PI: STEPHEN MURRAY
Subject Category: NORMAL STARS AND WD
Abstract: 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.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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18:04:24.00 -24:21:20.00 NGC 6530 ACIS-I NONE 61.00
===================================================================================
Proposal Number: 02200137
Proposal Title: THE M 16 STAR-FORMING REGION
PI: JEFFREY LINSKY
Subject Category: NORMAL STARS AND WD
Abstract: The Eagle Nebula (M 16, NGC 6611) is a giant H II region with an
optically visible cluster of very young MS OB stars and low-mass pre-main
sequence stars. The fingers of the Eagle Nebula also contain some of the youngest
known embedded mm and infrared protostars. We will obtain an 80-ks ACIS-I image
of the core of the Eagle Nebula to look for X-ray emission and flares from the
stars and protostars of M 16. To our knowledge, this is the first pointed X-ray
observation of M 16. Given the distance to M 16 (2.1 kpc) and the high density of
stars (2200 catalogued stars within 20 arcmin of the cluster center), a
long-exposure Chandra image is needed to reliably detect and identify the X-ray
sources.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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18:18:44.72 -13:47:56.50 M 16 ACIS-I NONE 80.00
===================================================================================
Proposal Number: 02200059
Proposal Title: OBSERVATION OF SCO-CEN OUTLYERS
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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11:33:25.40 -70:11:41.00 HD100546 ACIS-I NONE 3.00
11:33:25.40 -70:11:41.00 HD100546 ACIS-I NONE 3.00
11:33:25.40 -70:11:41.00 HD100546 ACIS-I NONE 3.00
12:00:05.10 -78:11:35.00 HD104237 ACIS-I NONE 3.00
12:00:05.10 -78:11:35.00 HD104237 ACIS-I NONE 3.00
12:00:05.10 -78:11:35.00 HD104237 ACIS-I NONE 3.00
15:49:57.80 -03:55:16.00 HD141569 ACIS-I NONE 3.00
16:40:17.90 -23:53:45.00 HD150193 ACIS-I NONE 3.00
16:54:44.90 -36:53:19.00 HD 152404 ACIS-I NONE 3.00
===================================================================================
Proposal Number: 02200175
Proposal Title: A SEARCH FOR CORONAL X-RAYS FROM WHITE DWARFS BY CHANDRA
PI: Zdzislaw Musielak
Subject Category: NORMAL STARS AND WD
Abstract: Observations of DA and DB white dwarfs have not been successful in
detecting coronal X-ray emission, but observations of late-type dwarfs and giants
show that coronae are common for these stars. To produce coronal X-rays, a star
has to have a well-developed convection zone and a dynamo-generated magnetic
field. There is strong evidence that the DB star GD 358 and the DA star LHS 1038
have weak and variable surface magnetic fields. Theory suggests that these fields
are generated by dynamo action, and that both stars have well-developed
convection zones. These stars are among the most promising white dwarf candidates
for having coronal X-ray emission at level detectable by CHANDRA. Its discovery
would confirm the existence of a new class of objects with convection-dynamo
driven X-rays.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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00:12:17.50 +50:25:52.90 LHS 1038 ACIS-S NONE 5.00
16:47:18.30 +32:28:25.50 GD 358 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 02200178
Proposal Title: X-RAYS FROM THE NEAREST PROTOSTARS: L1551
PI: JOHN BALLY
Subject Category: NORMAL STARS AND WD
Abstract: The discovery of hard X-ray emission from protostars may have profound
implications for the astrophysics of star formation the earliest phases of
stellar evolution. The Lynds 1551 cloud in the Taurus-Auriga complex is the
closest group of actively forming stars with several Class 0/I protostars and
outflows lying in a single ACIS-I field. The proposed observation will give an
extremely sensitive measurements of these protostars and other young stars, and
will search for X-rays emission from Herbig-Haro shocks.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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04:31:32.50 +18:07:49.00 LYNDS 1551 ACIS-I NONE 80.00
===================================================================================
Proposal Number: 02200185
Proposal Title: STELLAR CENSUS OF THE CHAMAELEON I NORTH CLOUD
PI: ERIC FEIGELSON
Subject Category: NORMAL STARS AND WD
Abstract: Unbiased and complete samples of pre-main sequence stars in star
forming regions are essential for determining the initial mass function, star
formation history and efficiency of clouds, magnetic activity evolution, and the
longevities of circumstellar disks (and thereby timescales for planet formation).
Infrared samples select preferentially stars with hot disks while X-ray surveys
are unbiased in this respect. The nearby, rich Chamaeleon I-North star forming
region offers a superb opportunity to detect several dozen pre-main sequence
stars and brown dwarfs down to extremely low masses in a single Chandra field to
address these issues.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:10:12.00 -76:34:30.00 CHA I NORTH CLOUD ACIS-I NONE 70.00
===================================================================================
Proposal Number: 02200208
Proposal Title: HIGH ENERGY PROCESSES AT THE EARLIEST STAGES OF MASSIVE STAR
FORMATION
PI: HENRIK BEUTHER
Subject Category: NORMAL STARS AND WD
Abstract: We propose to observe with CHANDRA ACIS-S the youngest sites of high
mass star formation. Recent ASCA observations suggest, that the earliest
evolutionary states of massive star formation are associated with hard X-ray
emission. A systematic proof of this finding can only come from the superior
resolution achievable with CHANDRA. The observations will allow us to resolve the
protostellar cluster and, supplemented with high resolution IR and radio data, to
identify the nature of the detected objects. The X-ray spectral information will
give us important clues on the X-ray production mechanism in high mass
protostars, which is up to now unexplored. The observations will also permit to
evaluate the impact of X-rays on star formation and chemistry within dense
molecular cores.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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19:43:11.40 +23:44:06.00 19410+2336 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 02200221
Proposal Title: A HIGH RESOLUTION X-RAY SPECTRUM OF THE INTERMEDIATE ACTIVITY
STAR $\EPSILON$ ERI
PI: JURGEN SCHMITT
Subject Category: NORMAL STARS AND WD
Abstract: We propose to obtain a high-spectral resolution and a high
signal-to-noise X-ray spectrum of the intermediate activity star $\epsilon$ Eri
with the Chandra LETG. $\epsilon$ Eri is nearby (d = 3.29 pc), hence the full
spectral range of the Chandra LETG can be utilised. Further, the star is unusual
in the sense that it has both low temperature (Fe IX) and high temperature (Fe
XXI) lines in its soft X-ray spectrum, all of which can be simultaneously
studied. The LETG spectrum of $\epsilon$ Eri will be of unprecedented quality and
allow us to study the detailed coronal temperature distribution, densities and
possible abundance anomalies in $\epsilon$ Eri. $\epsilon$ Eri is a {\bf key
target}, since it is the by far nearest and X-ray brightest star of {\bf
intermediate activity}.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:32:55.80 -09:27:30.00 EPSILON ERI HRC-S LETG 100.00
===================================================================================
Proposal Number: 02200227
Proposal Title: INTRINSIC X-RAY EMISSION FROM M-TYPE GIANTS
PI: MATTHIAS HUENSCH
Subject Category: NORMAL STARS AND WD
Abstract: We propose to observe five M-type giants detected in the course of the
ROSAT all-sky survey in order to confirm the detections and to obtain accurate
positions and count rates with the HRC-I. M-type giants are old, low-mass stars
to the right of the canonical X-ray dividing line and they are not expected to
show magnetic activity and hence X-ray emission at all. Thus, any X-ray
detections among such stars would challenge our ideas of coronal structures and
late stellar activity in giants, especially as possible companions are not a
reasonable explanation. Therefore, it is important to comfirm or reject the
preliminary detections and to find out whether they are intrinsic or
misidentified with background sources.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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02:35:47.00 +34:41:16.00 HR 750 HRC-I NONE 3.00
14:46:06.00 +15:07:54.00 HR 5512 HRC-I NONE 3.00
===================================================================================
Proposal Number: 02200277
Proposal Title: SEARCH FOR X-RAYS FROM COLLAPSING MAGNETIZED PRE-STELLAR
CONDENSATIONS
PI: NICOLAS GROSSO
Subject Category: NORMAL STARS AND WD
Abstract: X-rays from young protostars are likely, as is the VLA emission, a
reliable tracer of the start of an accretion process onto a central object. We
seek to assess whether or not X-ray emission is simultaneous with the very first
steps of star formation, or even precedes them. The main goal of this proposal is
to search for X-ray emission from collapsing pre-stellar condensations, and to
investigate the chronology between X-ray, VLA emission, and outflow phenomena
during protostar formation. We request 2 x 100 ksec to study the double NGC
2068/2071 complex in the Orion B giant molecular cloud at d~400 pc, containing
several young protostars, and many newly discovered pre-stellar condensations.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:46:43.50 +00:03:30.00 NGC 2068 ACIS-I NONE 100.00
===================================================================================
Proposal Number: 02200280
Proposal Title: BINARIES IN OLD OPEN CLUSTERS: M67
PI: TOMASO BELLONI
Subject Category: NORMAL STARS AND WD
Abstract: We propose to observe the old open cluster M 67 to study its population
of X-ray emitting objects. On the basis of our ROSAT campaigns we expect to see a
variety of objects. Many of these are stars currently undergoing tidal
interaction, or that have interacted tidally in the past. Some may be rapidly
rotating stars that are the product of a merger. These objects are X-ray sources
because of a very specific type of binary evolution, and by studying these
special systems in optical follow-up we can study little-understood details of
stellar evolution and of binary evolution. This provides new information on
initial parameter distributions of binaries in a well defined population.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:51:24.00 +11:49:48.00 M 67 ACIS-I NONE 50.00
===================================================================================
Proposal Number: 02200327
Proposal Title: STAR FORMATION IN THE ROSETTE MOLECULAR CLOUD
PI: LEISA TOWNSLEY
Subject Category: NORMAL STARS AND WD
Abstract: We propose to use an ACIS mosaic of the Rosette Molecular Cloud (RMC)
and its associated HII region as a testbed for understanding both high- and
low-mass star formation. Our goals are: to use X-ray-selected sources to decide
which infrared (IR) sources are actually RMC members; to determine if there is an
X-ray population distinct from the IR population; to study X-rays from
low/intermediate mass stars associated with CO clumps and embedded stellar
clusters; to examine the relationships between the X-ray luminosity function
(XLF), K-band luminosity function, and theoretical initial mass function (IMF)
over a wide range (tenths to tens of solar masses); and to search for extended
emission at the ionization front between the RMC and the Rosette Nebula.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:31:52.00 +04:55:57.00 ROSETTE FIELD 1 ACIS-I NONE 20.00
06:32:40.00 +04:43:00.00 ROSETTE FIELD 2 ACIS-I NONE 20.00
06:33:16.30 +04:34:57.00 ROSETTE FIELD 3 ACIS-I NONE 20.00
06:34:16.50 +04:28:01.00 ROSETTE FIELD 4 ACIS-I NONE 20.00
===================================================================================
Proposal Number: 02200366
Proposal Title: THE X-RAY VIEW OF ACTIVE STAR-FORMATION IN THE DENSE STELLAR
CLUSTER NGC 2024
PI: STEPHEN SKINNER
Subject Category: NORMAL STARS AND WD
Abstract: The molecular cloud associated with the HII region NGC 2024 contains
one of the richest young stellar clusters in the Orion region. More than 300 IR
sources have been detected within the cluster, and millimeter observations have
revealed a group of six protostellar condensations near the cluster center which
are thought to represent the earliest stages of star formation. We propose to
obtain a sensitive ACIS-I image of NGC 2024 centered on this protostellar
cluster. This observation will permit an accurate determination of the X-ray
luminosity function of NGC 2024, and will also serve as a sensitive search for
X-ray emission from protostars and from low-mass cluster members which have so
far escaped detection in infrared surveys.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:41:46.30 -01:55:28.70 NGC_2024 ACIS-I NONE 80.00
===================================================================================
Proposal Number: 02200371
Proposal Title: THE COOL AND HOT CORONAE OF HR 1099
PI: MANUEL GUEDEL
Subject Category: NORMAL STARS AND WD
Abstract: Chandra offers unique possibilities for the study of emission measure
distributions of stellar coronae over a wide range of temperatures. At the same
time, high-resolution spectroscopy determines unambiguously the abundances of
chemical elements. Previous solar/stellar observations have indicated `anomalies'
in the coronal elemental composition. The present investigation addresses the
question of whether abundance anomalies are dependent on the temperature of
coronal plasma in one and the same star. In particular, the observation
concentrates on the cooler part of the emission measure distribution of a very
active binary system (HR1099). The LETGS offers unique access to different
ionization stages of various elements not accessible by previous observations.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:36:47.30 +00:35:15.90 HR 1099, V711 TAU HRC-S LETG 100.00
===================================================================================
Proposal Number: 02200375
Proposal Title: FLARE ACTIVITY AND CORONAL HEATING ON THE ACTIVE FLARE STAR
BINARY UV CETI
PI: MARC AUDARD
Subject Category: NORMAL STARS AND WD
Abstract: Coronal heating on active stars has been related to magnetic flare
activity explicitly seen in these stars, or to microflaring concepts accessible
through flare energy distribution statistics and coronal parameters
(temperatures, emission measure distributions, densities, mass flows). We propose
to test these concepts in the extremely variable flare star binary UV Cet,
requesting an 80 ks exposure that will provide information on overall coronal
parameters, flare statistics, and flare heating mechanisms. A coordinated VLA
observation is planned. This exposure will probe two apparently identical stars
at the same time. Their separation of 1" does not split the spectral lines, while
the 0th order image in the proposed LETGS/HRC-S will clearly resolve the binary.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:39:01.88 -17:57:00.84 UV CETI,GLIESE 65 HRC-S LETG 80.00
===================================================================================
Proposal Number: 02200383
Proposal Title: THE NEARBY LOW METALLICITY STARBURST NGC~346: A HIGH REDSHIFT
STARBURST ANALOGUE
PI: MICHAEL CORCORAN
Subject Category: NORMAL STARS AND WD
Abstract: Hot stars form in groups in spiral and irregular galaxies.
Understanding the X-ray emission from starburst regions depends on disentangling
point source from diffuse emission. We request a 100 ksec ACIS-I observation of
an important nearby "starburst analogue", NGC 346 in the LMC. This observation
will allow us to study the extended emission, the emission from evolved O stars,
and to look for candidate collapsed objects and proto-stars in this
low-metallicity stellar group.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:59:05.00 -72:10:42.10 NGC 346 ACIS-I NONE 100.00
===================================================================================
Proposal Number: 02200420
Proposal Title: X-RAY EMISSION FROM HIGH MASS PRE-MAIN-SEQUENCE STARS
PI: KATSUJI KOYAMA
Subject Category: NORMAL STARS AND WD
Abstract: X-rays from high mass remain sequence stars have not been well studied
both in observation and theory. We propose an ASIC-I observation on a high mass
star forming region, the Monoceros R2 cloud, since ASCA has already found
variable hard X-ray sources embedded in the cloud. Our objectives are to resolve
the hard X-rays spatially and investigate which massive stars are responsible for
the hard X-rays. We then observe the plasma temperature, absorption column, time
variability including flare activity and chemical composition of the resolved
sources. These are key information for the X-ray emission mechanisms, hence the
evolution of the massive young stars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:07:49.50 -06:22:54.70 MONOCEROS R2 ACIS-I NONE 100.00
===================================================================================
Proposal Number: 02200424
Proposal Title: REVEALING THE MAGNETIC ACTIVITIES ON HERBIG AE/BE STARS
PI: SHIGEO YAMAUCHI
Subject Category: NORMAL STARS AND WD
Abstract: We propose ACIS-I observations on two intermediate-mass
pre-main-sequence stars (Herbig Ae/Be stars; HAEBE), MWC297 and EC95, because
ASCA found variable hard X-rays from these HAEBEs, but its limited spatial
resolution did not allow us to exclude possibility that the X-rays are due to
nearby low-mass young stars. With Chandra, we intend to (1) uniquely identify the
X-ray sources to the HAEBEs, (2) investigate the origin of the X-rays, (3) study
the dust-gas composition of the circumstellar medium, (4) search for a close
companion low-mass star and (5) discover X-rays from Class 0 protostars in a
small molecular cloud, the Serpence cloud.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:27:39.60 -03:49:52.00 MWC297 ACIS-I NONE 40.00
===================================================================================
Proposal Number: 02200379
Proposal Title: X-RAY SPECTROSCOPY OF THE SUN IN TIME: A STUDY OF CORONAL
PHYSICS OF SOLAR-TYPE STARS AT DIFFERENT AGES
PI: MANUEL GUEDEL
Subject Category: NORMAL STARS AND WD
Abstract: A comprehensive project on the ``Sun in Time'' has been set up over the
last few years, aiming at studying the physical properties, phenomenology, and
fundamental parameters of a solar-type star (G0-5 V) throughout its main-sequence
life. We propose a spectroscopic study with the LETGS/HRC-S to investigate in
detail coronal temperature and emission measure structuring, coronal densities,
elemental abundances, possible mass flows, and variability in selected targets.
We propose three stars regularly distributed in log(rotation period) over the
possible range, to be complemented by one GTO target that we will have access to.
This will provide a gross overview over the range of solar-type coronae. It is
anticipated that additional targets will be requested in later AOs.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
14:39:00.20 +64:17:30.00 EK DRA HRC-S LETG 70.00
===================================================================================
Proposal Number: 02200535
Proposal Title: CORONAL DYNAMICS OF THE FLARE STAR EV LAC
PI: RACHEL OSTEN
Subject Category: NORMAL STARS AND WD
Abstract: We request a 100 ks ACIS-S+HETG observation of the dMe flare star EV
Lac. EV Lac is an excellent candidate for dispersed spectroscopic studies with
Chandra due to its brightness and propensity for frequent and extreme
variability. EV Lac is the second brightest M dwarf X-ray source (the other, AU
Mic, has already been observed). HETG observations allow study of coronal
dynamics for the first time. The key physical parameters: abundances,
temperatures, and densities, which have been constrained poorly up until now, can
be determined accurately, leading to improved models and understanding of coronal
structure and variability. Coordinated observations with HST and radio and
optical observatories would extend our investigation into the dynamics of the
entire atmosphere of EV Lac.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:46:49.70 +44:20:02.40 EV LAC ACIS-S HETG 100.00
===================================================================================
Proposal Number: 02200558
Proposal Title: WHEN THE DYNAMO SPUTTERS:THE CORONA OF A AN EXTREMELY INACTIVE
(MAUNDER MINIMUM?) STAR
PI: STEVEN SAAR
Subject Category: NORMAL STARS AND WD
Abstract: The Wilson survey identified a group of stars with very low level,
near-constant Ca II emission. Weak UV and Xray emission in a few of these stars
implies that magnetic heating from a residual (probably turbulent) dynamo still
operates. Many of these stars are likely in the stellar analog of the Maunder
minimum - a period when the normal cyclic dynamo of the sun was in quiescence. We
propose to study the brightest of these stars with Chandra. The stars present a
unique opportunity to 1) study the properties of the weakest dwarf star coronae,
2) to investigate the coronal product of a predominantly turbulent dynamo in a
high mass star, exploring its dependence on rotation and mass, and 3) to
potentially study (indirectly) the properties of the solar corona during magnetic
minima.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:44:03.88 -15:56:13.45 TAU CETI ACIS-S NONE 50.00
===================================================================================
Proposal Number: 02200607
Proposal Title: TIME-RESOLVED CORONAL SPECTROSCOPY OF THE SHORT-PERIOD ACTIVE
BINARY ER VUL (G0 V + G5 V)
PI: ALEXANDER BROWN
Subject Category: NORMAL STARS AND WD
Abstract: We propose HETGS observations of ER Vul lasting two orbital periods (P
= 60 ksec) to obtain time-resolved coronal emission line spectra. ER Vul is the
brightest short-period RS CVn binary in X-rays. Despite showing a partial optical
eclipse, no X-ray eclipses are evident. Instead continuous small-scale flaring is
seen. We shall investigate the temporal variability of the coronal temperature
and EM distributions, estimate density and abundance variations, and model the
changing coronal plasma conditions. Contemporaneous radio and optical monitoring
will be used to study the nonthermal electron population and starspot
distribution. Study of extreme activity on Sun-like stars extends our ability to
understand the causes of solar activity with its direct effects on the Earth.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:02:25.90 +27:48:26.40 ER_VUL ACIS-S HETG 120.00
===================================================================================
Proposal Number: 02200620
Proposal Title: HIGH RESOLUTION SPECTROSCOPY AND VARIABILITY OF THE
TRAPEZIUM-LIKE SYSTEM HD 206267 IN IC 1396
PI: NORBERT SCHULZ
Subject Category: NORMAL STARS AND WD
Abstract: Trumpler 37 is with 3 Myr one of the youngest open clusters in our
galaxy. The core of the cluster hosts the Trapezium-like complex HD 206267. Its
main component is a young and hot O-star triplet. Twice as distant, this system
strongly resembles the Orion Trapezium Cluster. In AO1 we observed Orion twice
with the HETGS and found that the high resolution spectrum of the central O-star
showed a large number of emission lines which indicated a wide range of
temperatures in the wind of up to 11 keV. Furthermore we found a large number of
transient X-ray sources in the vicinity, which resemble deeply embedded
protostars. In Trumpler 37 we face a similar situation. Two 40 ks exposure with
the HETGS allows us to study a similar star formation scenario in IC 1396.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:38:57.50 +57:29:11.00 HD 206267 ACIS-S HETG 40.00
21:38:57.50 +57:29:11.00 HD 206267 ACIS-S HETG 40.00
===================================================================================
Proposal Number: 02200644
Proposal Title: TORTURED CORONAE IN THE RAPID BRAKING ZONE
PI: THOMAS AYRES
Subject Category: NORMAL STARS AND WD
Abstract: Deep HETGS exposures of four key G0-G5 giants will address fundamental
questions concerning their hot magnetized coronae by determining temperatures and
densities, probing chemical fractionation processes, and exploring plasma
dynamics. The giants lie in or near the "Rapid Braking Zone" where moderate mass
stars undergo a radical transformation of their outer atmospheres, perhaps as a
relic magnetosphere is disrupted by the onset of a solar-like dynamo. ACIS-I CCD
spectra of five G/K supergiants will explore the even more extreme extension of
the RBZ to higher masses: where hot coronae mix freely with cool stellar winds.
These are ideal targets to exploit the experience gained in the Emission Line
Project studies of the active binaries Capella and HR 1099.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:46:46.10 -49:25:12.00 HD 93497 ACIS-S HETG 20.00
10:46:46.10 -49:25:12.00 HD 93497 ACIS-S HETG 60.00
10:46:46.10 -49:25:12.00 HD 93497 ACIS-S HETG 60.00
12:51:41.80 +27:32:26.00 HD 111812 ACIS-S HETG 140.00
23:49:40.80 +36:25:31.00 HD 223460 ACIS-S HETG 100.00
===================================================================================
Proposal Number: 02200908
Proposal Title: X-RAY PROBING OF THE BIRTH OF THE STAR
PI: YOSHITOMO MAEDA
Subject Category: NORMAL STARS AND WD
Abstract: We propose a challenging 50~ksec observation of the youngest protostar
S106 FIR. The scientific goal is to know if a protostar at $1\times10^{2}$ yrs
old emits X-rays or not. The results are crucial to test if X-rays probe the
birth of star or not. The only probe of the young protostars is currently radio
observation of jets. However, jets are indirect probes of the central core
object, i.e., protostar. Hence, our observations may give a new and unique way to
directly test existence of protostars at the beginning of birth.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:27:25.50 +37:22:48.70 S106 FIR ACIS-I NONE 50.00
===================================================================================
Proposal Number: 02200912
Proposal Title: HIGH RESOLUTION SPATIALLY RESOLVED SPECTRA OF THE X-RAY
BRIGHTEST INTERMEDIATE ACTIVITY SYSTEM XI UMA AB
PI: JEREMY DRAKE
Subject Category: NORMAL STARS AND WD
Abstract: The aim of this proposal is to find the missing link between solar-like
coronal activity and the coronal activity of ``active'' stars---stars that can
have X-ray luminosities 10,000 times that of the active Sun. The xi UMa AB system
is the brightest intermediate activity object in X-rays and the optically
identical AB components---one a rapid rotator the other not--are separated by 2
arcsec and can be spatially resolved in Chandra HETG spectra. An 80ks HETG
observation will provide the first and only opportunity to spatially and
spectrally resolve the system and will allow us to perform a comparitive study of
identical stars at different activity levels.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:18:10.90 +31:31:44.00 XI UMA ACIS-S HETG 80.00
===================================================================================
Proposal Number: 02200688
Proposal Title: HIGH RESOLUTION X-RAY SPECTROSCOPY OF GAMMA CASSIOPEIA
PI: MYRON SMITH
Subject Category: NORMAL STARS AND WD
Abstract: Gamma Cas is a unique Be X-ray source with erratic "shots," a hard
spectrum, and a high flux level between that of single Be stars and the Be/X-ray
binaries. Previous low resoluution data have shown both slow, correlated X-ray
and UV variability and fast variability reminiscent to that attributed to
magnetic flaring activity in cool stars. We propose to use the HETG to study the
properties of the temperature, density, composition, bulk motions and ionization
processes in the circumstellar environment of this unusual hot star. This will
serve to shed light on the nature of the energetic processes occuring on this
star.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:56:42.50 +60:43:00.30 GAMMA CAS ACIS-S HETG 54.00
===================================================================================
Proposal Number: 01208024
Proposal Title: CAPTURING WR140 AT PERIASTRON WITH THE CHANDRA HETG
PI: ANDREW POLLOCK
Subject Category: NORMAL STARS AND WD
Abstract: This is a resubmission of our AO2 proposal number 02200508 which was
rejected, despite high scores, because it was mistakenly thought that XMM would
be making similar observations near periastron. In fact, according to its
official WWW visibility tool, XMM is not able to observe any nearer than two
months either side of periastron passage and possibly not at all. The compelling
scientific justification was given in our original proposal and endorsed by the
Peer Review. We are responding to the Review Panel's recommendation to apply for
Director's Discretionary Time.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:20:28.00 +43:51:16.30 WR140 ACIS-S HETG 25.00
20:20:28.00 +43:51:16.30 WR140 ACIS-S HETG 50.00
***********************************************************************************
WD BINARIES AND CV
--------------------------------------------------
===================================================================================
Proposal Number: 02300040
Proposal Title: NEAR-EDDINGTON ACCRETION IN THE BINARY SUPERSOFT X-RAY SOURCE RX
J0513.3-6951
PI: PETER PREDEHL
Subject Category: WD BINARIES AND CV
Abstract: Study of the X-ray properties of the binary supersoft X-ray source RX
J0513.3-6951
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:13:50.80 -69:51:47.00 RX J0513.9-6951 HRC-S LETG 50.00
===================================================================================
Proposal Number: 02300096
Proposal Title: CV AND QLMXB LUMINOSITY FUNCTION IN THE EXTREME GLOBULAR M80
PI: STEPHEN MURRAY
Subject Category: WD BINARIES AND CV
Abstract: We propose to carry out a deep search for cataclysmic variables (CVs)
and quiescent low mass X-ray binaries (qLMXBs) in the galactic globular cluster
M80. Ferraro et al. (1999) have recently used HST-WFPC2 imaging to detect a
remarkably dense population of blue stragglers there. This suggests that the core
of this cluster is the site of vigorous single and binary star interactions,
since the blue stragglers are expected to be collisionally formed. A cluster core
in such a dynamical state is also likely to produce significant numbers of CVs
through similar collisional channels. Thus a deep observation of this cluster is
an ideal extension of our (impending) GTO1 studies of two differing but
contrasting globulars for their CV content: NGC 6397 and 47 Tuc.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:17:02.30 -22:58:32.60 NGC6093 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 02300183
Proposal Title: X-RAY SPECTROSCOPY OF THE BRIGHT SUPERSOFT SOURCES CAL 83 AND
CAL 87
PI: JOCHEN GREINER
Subject Category: WD BINARIES AND CV
Abstract: The AXAF LETG is sensitive to the range of energy of supersoft X-ray
sources (SSS), some of the most puzzling low-mass X-ray binaries ever discovered.
We propose to exploit the unique spectral capabilities of the LETG to study in
detail two of the most intriguing SSS, Cal 83 (50 ksec) and Cal 87 (100 ksec).
SSSs probably involve very hot white dwarfs within a binary system, burning
accreted hydrogen in a shell on their surface. We propose to get detailed high
spectral-resolution, high signal-to-noise spectra which will allow to distinguish
between white dwarf (due to characteristic absorption edges) and neutron star
models (smooth black body spectrum), and to search for clues for the differences
between these two objects.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:46:46.52 -71:08:54.00 CAL 87 ACIS-S LETG 100.00
===================================================================================
Proposal Number: 02300236
Proposal Title: CHANDRA SOFT X-RAY SPECTROSCOPY AND TIMING OF THE DWARF NOVA SS
CYGNI IN OUTBURST
PI: CHRISTOPHER MAUCHE
Subject Category: WD BINARIES AND CV
Abstract: We propose to perform Chandra LETGS observations of SS Cygni in
outburst to measure the spectrum of the EUV/soft X-ray component---the ``big blue
bump''--of its boundary layer radiation. These data will be used to determine or
constrain the physical conditions (temperature, density, velocity field) of the
boundary layer plasma; the role, if any, of radiation transport (e.g., scattering
in the system's accretion disk wind) in determining the observed spectrum; and
the characteristics (period, coherence, harmonic content, spectrum) of the
quasi-coherent EUV oscillations, thereby constraining their cause.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:42:42.70 +43:35:09.50 SS CYG HRC-S LETG 50.00
===================================================================================
Proposal Number: 02300245
Proposal Title: IRON LINE BROADENING IN THE INTERMEDIATE POLAR AO PSC
PI: COEL HELLIER
Subject Category: WD BINARIES AND CV
Abstract: ASCA observations of the Fe Kalpha line complex of magnetic cataclysmic
variables revealed a puzzle -- half have narrow lines and half have broad lines.
Further, the broadening is too large to be explained by Doppler shifts and,
simulations show, is too small to be explained by Compton scattering in the
accretion columns. To obtain data better by a factor ~3, and so resolve the
puzzle, we request a HETG observation of AO Psc, the system showing broadening
most securely. We will compare this to our AO-1 observation of V1223 Sgr, which
has narrow lines, to enable us to investigate broadening mechanisms in accretion
columns and use them as a probe of accretion-column physics.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
22:55:18.00 -03:10:40.40 AO PSC ACIS-S HETG 100.00
===================================================================================
Proposal Number: 02300482
Proposal Title: THE ORIGIN OF SOFT X-RAYS IN DQ HERCULIS
PI: KOJI MUKAI
Subject Category: WD BINARIES AND CV
Abstract: DQ Herculis (Nova Her 1934) has been found to be a weak soft X-ray
source, even though the accretion disk is thought to block our line of sight to
the white dwarf primary at all orbital phases. The observed luminosity is an
order of magnitude higher than that expected of the secondary. What, then, is the
origin of these X-rays? One possibility is resonant scattering of a hidden X-ray
source by the accretion disk wind. Another is that the nova shell around DQ Her
has now become an X-ray source, as the ejecta plough into the surrouding
interstellar medium. We propose Chandra imaging to distinguish between these
possibilities, and use timing and spectral information to constrain the model
further.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:07:30.20 +45:51:32.00 DQ HERCULIS ACIS-S NONE 22.00
18:07:30.20 +45:51:32.00 DQ HERCULIS ACIS-S NONE 48.00
===================================================================================
Proposal Number: 02300495
Proposal Title: A HIGH RESOLUTION SPECTROSCOPIC OBSERVATION OF CAL 83
PI: FREDERIK PAERELS
Subject Category: WD BINARIES AND CV
Abstract: We propose a deep observation of the bright supersoft X-ray source
CAL83 with the LETGS. Combined with the high-sensitivity XMM-Newton/RGS spectrum
of this source, the observation will yield a superbly detailed photospheric
spectrum, covering the full range between the Wien cutoff and the cutoff imposed
by interstellar absorption. We will determine the fundamental stellar parameters
and search the spectrum for signatures of exotic effects in the atmosphere of the
object.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:43:34.10 -68:22:22.60 CAL 83 HRC-S LETG 35.00
05:43:34.10 -68:22:22.60 CAL 83 HRC-S LETG 65.00
===================================================================================
Proposal Number: 02300532
Proposal Title: CHANDRA HETG OBSERVATION OF V603 AQUILAE, A HIGH ACCRETION RATE,
NON-MAGNETIC CATACLYSMIC VARIABLE
PI: KOJI MUKAI
Subject Category: WD BINARIES AND CV
Abstract: We propose a 70 ksec HETG observation of V603 Aql, which is the hard
X-ray brightest example of the high accretion rate, non-magnetic cataclysmic
variables. Its ASCA spectrum is dominated by Fe K and L features. We will resolve
the Fe K region into three separate components, enabling us to estimate the shock
temperature and the nature and the covering factor of the reflector. The data
will also allow a simultaneous analysis of Fe K and L features in unprecedented
details. We will also search for K lines of abundant elements from O to Ar, and
constrain the emission measure distribution in the 0.5 to 10 keV range. Finally,
we will search for absorption signatures of the accretion disk wind.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:48:54.50 +00:35:03.00 V603 AQUILAE ACIS-S HETG 70.00
===================================================================================
Proposal Number: 02300588
Proposal Title: STUDYING THE OLD CLASSICAL NOVA SHELLS IN X-RAYS II : THE SHELL
OF CLASSICAL NOVA PICTORIS 1925 (RR PIC)
PI: SOLEN BALMAN
Subject Category: WD BINARIES AND CV
Abstract: We propose a 100 ksec CHANDRA ACIS-S observation to resolve and detect
the shell of old classical nova Pictoris 1925 thereby establishing a second
member, after GK Per, of a possible new class of X-ray emitters, Clasical Nova
Remnants. An archieval ROSAT PSPC data show extended emission from the source. We
plan to exploit the unique spatial and spectral capabilities of the ACIS-S
detector in order to study the morphology and spectrum of the nova shell
simultaneously. We expect that this observation will have great implications on
our understanding of the classical nova evolution, nature of TNRs, outburst
mechanisms together with the interaction of the nova shells with their
environments of interstellar or circumstellar origin and physics of shocks.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
06:35:36.10 -62:38:24.30 RR PIC ACIS-S NONE 25.00
===================================================================================
Proposal Number: 02300626
Proposal Title: THE X-RAY SOURCE POPULATION IN THE CORE OF M15
PI: PHIL CHARLES
Subject Category: WD BINARIES AND CV
Abstract: We are proposing a definitive search for cataclysmic variables and low
luminosity LMXBs in the prototypical post-core collapse cluster M15. This will
provide detailed constraints on the X-ray source population, which could even
contain a second LMXB within the central cusp. Previous searches have been
restricted to nearby clusters, but those which contain the most favorable
environments (mass and compactness) for forming compact binaries are more
distant, and these are now within the reach of Chandra. Furthermore, only the
high spatial resolution of Chandra allows such a search in the ideal cluster
(M15) because of the presence of a bright LMXB in the core.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:29:58.30 +12:10:00.50 M15 HRC-I NONE 10.00
21:29:58.30 +12:10:00.50 M15 HRC-I NONE 10.00
21:29:58.30 +12:10:00.50 M15 HRC-I NONE 10.00
===================================================================================
Proposal Number: 02300734
Proposal Title: HIGH-RESOLUTION X-RAY SPECTROSCOPY OF THE SYMBIOTIC STAR CH CYG:
\ ANY NEED FOR COLLIDING WINDS IN SYMBIOTICS?
PI: PETER WHEATLEY
Subject Category: WD BINARIES AND CV
Abstract: I have suggested a new interpretation of the X-ray spectra of symbiotic
stars: that they are dominated by absorption by the partially-ionised wind of the
red giant, and that there is no need for emission from colliding winds. \\ I
propose to observe the bright symbiotic star CH Cyg with the Chandra
HETGS/ACIS-S. The high-resolution spectrum will immediately resolve the
emission/absorption ambiguity because individual absorption edges and emission
lines will be directly observable. The detailed analysis of these features will
provide a powerful probe of the wind of the red giant, and of wind accretion onto
a white dwarf.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:24:33.10 +50:14:29.00 CH CYG ACIS-S HETG 50.00
===================================================================================
Proposal Number: 02308048
Proposal Title: THE RECURRENT NOVA CI AQL
PI: JOCHEN GREINER
Subject Category: WD BINARIES AND CV
Abstract: Recurrent novae (RN) are expected to emit soft x-rays during a short
interval after the ejected shell has become optically thin and before the
hydrogen shell-burning ceases. Observations of the soft x-rays will test
theoretical models and will also test the conjecture that RN are SN Ia
progenitors. Unfortunatley, no RN occurred during the ROSAT years, and in fact
only one has been detected as a soft X-ray emitter (Kahabka etal 1999). CI Aql
went into outburst in Apr. 2000. Hachisu & Kato (2001; astro-ph/0104461) predict
that CI Aql should have recently become active at soft X-ray wavelengths and is
potentially detectable until Aug. 2001. We propose (1) a 2 ksec ACIS-S
observation to verify the existence of soft X-rays, and (2) if soft X-rays are
discovered, a 20 ksec LETG-HRC observation to determine crucial parameters (white
dwarf mass, effective temperature, composition, luminosity, wind properties).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:52:03.60 -01:28:39.00 CI AQL ACIS-S NONE 0.00
18:52:03.60 -01:28:39.00 CI AQL ACIS-S NONE 2.00
===================================================================================
Proposal Number: 02308052
Proposal Title: THE RECURRENT NOVA CI AQL
PI: JOCHEN GREINER
Subject Category: WD BINARIES AND CV
Abstract: We propose a 20 ksec ACIS-S observation of the recurrent nova (RN) CI
Aql. RNe are expected to emit soft x-rays during an interval after the ejected
shell has become optically thin and before the hydrogen shell-burning ceases and
the white dwarf cools. A 2 ksec Chandra ACIS-S observation on June 1, 2001
discovered that CI Aql was a soft X-ray source 380 days after outburst. The flux
was much smaller than expected. It is possible that the shell is dense and/or
expanding slowly; i.e. we may still be near the beginning of the soft X-ray
phase. If obscuration is still important, the proposed observation will detect a
distinctive spectral signature and will measure the ejected mass, testing whether
CI Aql is a possible SNIa progenitor. If obscuration is not important, we will
determine the temperature and luminosity of the white dwarf. Making these
measurements and adding a second point to the X-ray light curve, will
significantly add to the evolving understanding of the properties of RNe.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:52:03.60 -01:28:39.00 CI AQL ACIS-S NONE 20.00
===================================================================================
Proposal Number: 02308054
Proposal Title: WZ SGE IN OUTBURST TEN YEARS EARLY: I THE EUV EMISSION
PI: PETER WHEATLEY
Subject Category: WD BINARIES AND CV
Abstract: WZ Sge is the most extreme dwarf nova. While most dwarf novae exhibit
outbursts every few weeks with optical amplitudes of 2-3 magnitudes, WZ Sge waits
thirty years between outbursts which then have amplitudes of 7 mag. These have
never been studied in X-rays. WZ Sge is in outburst right now (began around July
23.5 UT) presenting a unique opportunity to observe it in outburst with Chandra.
We are extremely lucky because the outburst was not expected for another ten
years, and may not repeat for another 30 years. In general dwarf novae are weak
hard X-ray sources in quiescence and strong EUV sources in outburst. We may
expect the same behaviour from WZ Sge though we must also be prepared for
unexpected behaviour from such an extreme system. Count rates are highly
uncertain, but we may expect WZ Sge to be the brightest EUV source in the sky. We
propose LETG spectroscopy to study the EUV component and ACIS-S spectrscopy of
the (probably weaker) hard emission.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:07:36.20 +17:42:15.00 WZ SGE HRC-S LETG 20.00
20:07:36.20 +17:42:15.00 WZ SGE HRC-S LETG 20.00
20:07:36.20 +17:42:15.00 WZ SGE HRC-S LETG 20.00
===================================================================================
Proposal Number: 02308055
Proposal Title: WZ SGE IN OUTBURST TEN YEARS EARLY: II THE X-RAY EMISSION
PI: PETER WHEATLEY
Subject Category: WD BINARIES AND CV
Abstract: This is the second half of the WZ Sge DDT proposal. In the first we
requested HRC-S/LETG spectrscopy of the EUV emission. Here we request ACIS-S
observations of the (probably weak) X-ray emission. The X-ray emission is likely
to be supressed below its usual quiescent level during the outburst, as the
emission is thought to switch to the EUV. However, WZ Sge has never been observed
in X-rays during outburst.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:07:36.20 +17:42:15.00 WZ SGE ACIS-S NONE 5.00
20:07:36.20 +17:42:15.00 WZ SGE ACIS-S NONE 10.00
20:07:36.20 +17:42:15.00 WZ SGE ACIS-S NONE 10.00
20:07:36.20 +17:42:15.00 WZ SGE ACIS-S NONE 10.00
===================================================================================
Proposal Number: 02308056
Proposal Title: FIRST X-RAY OBSERVATIONS DURING AN EXTREMELY RARE OUTBURST OF WZ
SGE
PI: ERIK KUULKERS
Subject Category: WD BINARIES AND CV
Abstract: The cataclysmic variable (CV) WZ Sge has unexpectedly gone into
outburst on 2001 Jul 23 (IAU Circ 7669). Outbursts were seen in 1913, 1946 and
1978 (e.g. ApJ 248, 1067), suggesting a recurrence time of ~33 years. These
extremely rare outbursts, and their decline to quiescence have NEVER been covered
in X-rays. With Chandra we have the unique opportunity to study WZ Sge for the
first time through these phases. In quiescence the accretion disk is truncated by
the white dwarf magnetic field and X-ray oscillations (PASP 110, 403) at 27.9s
were observed. In outburst the disk reaches the white dwarf surface (e.g. MNRAS
305, 473) and possibly the oscillations cease to exist. By taking 10 ksec
snapshots of WZ Sge 3 times in the next 2-3 months, we will catch WZ Sge in its
various states, and get information on accretion rate onto the white dwarf,
abundances, and temperatures, etc. (e.g. MNRAS 288, 649). We have requested a DDT
on HST as well (PI: E. Sion).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:07:36.20 +17:42:15.00 WZ SGE ACIS-S NONE 5.00
20:07:36.20 +17:42:15.00 WZ SGE ACIS-S NONE 10.00
20:07:36.20 +17:42:15.00 WZ SGE ACIS-S NONE 10.00
***********************************************************************************
BH AND NS BINARIES
--------------------------------------------------
===================================================================================
Proposal Number: 02400041
Proposal Title: PHOTOIONIZED X-RAY EMISSION IN CYG X-2
PI: CLAUDE CANIZARES
Subject Category: BH AND NS BINARIES
Abstract: This highly luminous X-ray binary was observed with the Chandra HETGS
during the verification and checkout. The source showed an X-ray flux of nearly
0.5 Crab causing severe depletion of photons in the MEG and HEG 1st order spectra
due to pile up effects. Nevertheless the spectrum showed various remarkable
features at high energies and in the higher orders, which can be identified as
photoionized emission from Mg-, Si-, S-, Ca-, and Fe. However the detections
remained spurious and at higher wavelengths very much affected by pile up. We
want to re-observe Cyg X-2 for 15 ks, in order to obtain pile up free 1st order
spectra, enhance and confirm the findings in the higher order spectra as well as
study variability in the line emission.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:44:41.70 +38:19:10.60 CYG X-2 ACIS-S HETG 15.00
===================================================================================
Proposal Number: 02400042
Proposal Title: HIGH RESOLUTION X-RAY SPECTROSCOPY OF X-RAY SPECTRA FROM THE
TRANSIENT X-RAY BURST SOURCE EXO 0748-676
PI: CLAUDE CANIZARES
Subject Category: BH AND NS BINARIES
Abstract: EXO 0748-676 is a transient X-ray burst source that shows X-ray
eclipses as well as broad intensity dips that last for about 1/3 of the orbital
period (3.82 hrs). Recent analysis of the persistent emission revealed a
previously unseen soft X-ray excess. It was indicated that during the dips the
central X-ray source is obscured by dipping material in the accretion disk. We
want to use these event in order to investigate line emission from either an
accretion disk corona or photoionized layers on the disk, which is usually
overpowered by the intense continuum emission of the central source. The source
is also a quite frequent X-ray burster leaving the opportunity to search for
narrow absorption features in the spectra of burst tails.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
07:48:33.30 -67:45:00.00 EXO 0748-676 ACIS-S HETG 50.00
===================================================================================
Proposal Number: 02400051
Proposal Title: THE ANOMALOUS X-RAY PULSAR 4U 0142+61
PI: CLAUDE CANIZARES
Subject Category: BH AND NS BINARIES
Abstract: The properties of 4U 0142+61 are similar to those of a small group of
"anomalous" X-ray pulsars (AXPs) with spin periods in the range 6-12 sec.
BeppoSAX as well as ASCA observed a blackbody spectral component in the soft
X-ray spectrum. The X-ray flux is quite strong and amounts to about 1.1xE^-10
erg/cm2/sec. Although highly absorbed (1E^22 cm2) its high soft flux allows to
search for possible cyclotron line emission features. From RXTE observations as
well as optical photometric studies a white dwarf companion seems to be possible,
although a scenario of an isolated neutron star accreting from a residual disk is
proposed as well. Due to the possibility for quite similar evolutionary
scenarios, we also search for line emission as observed in 4U 1626-67.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:46:22.00 +61:45:12.00 4U 0142+61 ACIS-S HETG 25.00
===================================================================================
Proposal Number: 02400069
Proposal Title: HIGH RESOLUTION X-RAY SPECTROSCOPY OF THE PRECESSING JET IN SS
433 (PART III)
PI: CLAUDE CANIZARES
Subject Category: BH AND NS BINARIES
Abstract: SS 433 is quite a unique galactic X-ray binary. The X-ray emission from
emerging jets are of thermal origin. The cooling hydrodynamical outflow in form
of a jet has dimensions of the binary separation. SS 433 has been observed during
AO1 for 30 ks revealing a variety of redshifted and blue shifted lines from Si
and higher elements. The line ratios of various H/He-like ions as well as deduced
temperatures differed considerably from what has been observed with ASCA during
approximately the same phase. We intend to observe SS 433 at several more
precession phases (part III: eclipse) in order to monitor the plasmas conditions
at the base of the jet as well as measure the X-ray Doppler shifts of the lines
from the precessing jet.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:11:49.50 +04:58:58.00 SS 433 ACIS-S HETG 25.00
===================================================================================
Proposal Number: 02400070
Proposal Title: HIGH RESOLUTION X-RAY SPECTROSCOPY OF THE PRECESSING JET IN SS
433 (PART II)
PI: CLAUDE CANIZARES
Subject Category: BH AND NS BINARIES
Abstract: SS 433 is quite a unique galactic X-ray binary. The X-ray emission from
emerging jets are of thermal origin. The cooling hydrodynamical outflow in form
of a jet has dimensions of the binary separation. SS 433 has been observed during
AO1 for 30 ks revealing a variety of redshifted and blue shifted lines from Si
and higher elements. The line ratios of various H/He-like ions as well as deduced
temperatures differed considerably from what has been observed with ASCA during
approximately the same phase. We intend to observe SS 433 at several more
precession phases (part II: 0.65) in order to monitor the plasmas conditions at
the base of the jet as well as measure the X-ray Doppler shifts of the lines from
the precessing jet.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:11:49.50 +04:58:58.00 SS 433 ACIS-S HETG 25.00
===================================================================================
Proposal Number: 02400090
Proposal Title: ACCRETION DISK LINES AND CONTINUUM IN 4U 1820-30
PI: STEPHEN MURRAY
Subject Category: BH AND NS BINARIES
Abstract: We propose to use the ACIS-HETG to study the spectral evolution of 4U
1820-30. We seek to accurately measure the 6.4 keV Fe line and look for narrow
line components superimposed that may likely arise from re-processing on the
companion (white dwarf) star. We can measure the equivalent width and the
velocities as a function of accretion rate and orbital phase to constrain the
orgin of the emission. Also, by measuring changes in line EW and width between a
low vs. high state, we can test Comptonization models for an accretion disk
corona at differing optical depths.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:23:40.50 -30:21:40.00 NGC6624 ACIS-S HETG 10.00
18:23:40.50 -30:21:40.00 NGC6624 ACIS-S HETG 10.00
===================================================================================
Proposal Number: 02400133
Proposal Title: HIGH RESOLUTION UV/X-RAY SPECTROSCOPY OF SMC X-1
PI: SAEQA VRTILEK
Subject Category: BH AND NS BINARIES
Abstract: We propose simultaneous observations of the X-ray pulsar system SMC
X-1/SK160 with HST/STIS, Chandra, and ground-based optical telescopes. We will
search for correlation between orbital phase and ``bleaching'' of important P
Cygni lines by X-ray photoionization. We will model the X-ray, UV, and optical
continuum emission at different phases of the superorbital period. Using the
Chandra ACIS-S in CC mode we will conduct pulse-phased spectroscopy of the X-ray
emission. Our multiwavelength observations will enable us to analyze the density
structure and composition of the wind; set limits on the size, shape, rotation,
and precession of the disk; and determine the effects of X-ray illumination on
the disk, the star, and the stellar wind.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
01:17:05.20 -73:26:34.60 SMC X-1 ACIS-S NONE 6.00
01:17:05.20 -73:26:34.60 SMC X-1 ACIS-S NONE 6.00
01:17:05.20 -73:26:34.60 SMC X-1 ACIS-S NONE 6.00
01:17:05.20 -73:26:34.60 SMC X-1 ACIS-S NONE 6.00
01:17:05.20 -73:26:34.60 SMC X-1 ACIS-S NONE 6.00
01:17:05.20 -73:26:34.60 SMC X-1 ACIS-S NONE 6.00
01:17:05.20 -73:26:34.60 SMC X-1 ACIS-S NONE 6.00
01:17:05.20 -73:26:34.60 SMC X-1 ACIS-S NONE 6.00
===================================================================================
Proposal Number: 02400153
Proposal Title: PHASE RESOLVED SPECTROSCOPY OF THE X-RAY P-CYGNI PROFILES FROM
CIRCINUS X-1
PI: WILLIAM BRANDT
Subject Category: BH AND NS BINARIES
Abstract: In a Cycle 1 HETGS observation of the extremely luminous and violent
X-ray binary Cir X-1, we have discovered many new X-ray emission lines showing
broad P-Cygni profiles; these are from H-like and He-like ions of Ne, Mg, Si, S,
Ar and Fe. The lines originate in a high-velocity (up to 2000 km/s) outflow,
probably an accretion disk wind that is shielded by the outer disk bulge. The
P-Cygni profiles are also likely related to the unusually broad, asymmetric
H-alpha line observed from Cir X-1. We propose three 8 ks observations designed
to measure the X-ray P-Cygni profiles at key phases of the 16.5-day orbital cycle
and critically test our model for the origin of these remarkable lines. We expect
line strength and profile variability due to changes in mass accretion rate and
disk shielding.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:20:41.00 -57:10:00.00 CIR X-1 ACIS-S HETG 8.00
15:20:41.00 -57:10:00.00 CIR X-1 ACIS-S HETG 8.00
15:20:41.00 -57:10:00.00 CIR X-1 ACIS-S HETG 8.00
===================================================================================
Proposal Number: 02400161
Proposal Title: XTE J1739-302 IN QUIESCENCE
PI: DAVID SMITH
Subject Category: BH AND NS BINARIES
Abstract: This unusual x-ray transient was seen once in outburst with RXTE in
1997. It has the spectrum typical of an x-ray pulsar, making it likely to be a
Be/NS binary, and therefore to have significant quiescent emission. Its outburst
luminosity was near the highest ever seen from one of these systems. We propose a
series of two Chandra pointings to find its precise location (for counterpart
identification), luminosity, quiescent spectrum, and pulse period. If it is not
seen by Chandra, or has a flux much lower than predicted, then it would be the
only known transient with an x-ray pulsar spectrum and a very high
outburst/quiescence ratio (the latter being typical of soft x-ray transients).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:38:57.60 -30:18:36.00 XTE J1739-302 ACIS-I NONE 5.00
===================================================================================
Proposal Number: 02400179
Proposal Title: HIGH RESOLUTION SPECTROSCOPY OF THE ADC SOURCE 2S0921-630
PI: TIMOTHY KALLMAN
Subject Category: BH AND NS BINARIES
Abstract: We propose to observe the high inclination low mass X-ray binary
2S0921-630 in order to test the hypothesis that the residual X-rays seen during
eclipse are due to reprocessing and scatttering in an accretion disk corona. By
observing the iron K line and lines from medium-Z elements at high resolution
using the HETG, we can determine the ionization state and emission measure, and
thereby infer the density and size of the corona. Using the ACIS detector we can
test for variability in the spectrum during the eclipse, and constrain the
geometrical extent of the corona. This source is ideal for such a study owing to
its demonstrated strong line emission and its long eclipse.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:22:34.70 -63:17:42.00 2S0921-630 ACIS-S HETG 80.00
===================================================================================
Proposal Number: 02400252
Proposal Title: DOPPLER-SHIFTED EMISSION LINES FROM THE JETS OF 1E1740.7-2942?
PI: WEI CUI
Subject Category: BH AND NS BINARIES
Abstract: During Cycle 1 we observed 1E1740.7-2942 with the HETGS for 10 ks (but
with an effective exposure only 7 ks). The dispersed grating spectrum shows
marginal detection of weak, narrow emission lines. Nearly all of the lines could
be identified with highly ionized species such as H-like and He-like Fe, Ca, S,
and Ar, if some of the line pairs (which are otherwise difficult to interpret)
are attributed to the Doppler red- and blue-shifted lines from the jets which are
known to be always present in the system. To verify this exciting scenario, we
propose to observe the source again for 70 ks with a more appropriate set of data
modes. The observation would increase the significance of any physical lines from
about 2 sigma to 5 sigma, which would place the interpretation on a much firmer
ground.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:43:54.80 -29:44:42.60 1E1740.7-2942 ACIS-S HETG 70.00
17:43:54.80 -29:44:42.60 1E1740.7-2942 ACIS-S HETG 70.00
===================================================================================
Proposal Number: 02400316
Proposal Title: THE X-RAY EMISSION ASSOCIATED WITH THE BLACK WIDOW PULSAR
B1957+20
PI: BENJAMIN STAPPERS
Subject Category: BH AND NS BINARIES
Abstract: The wind is the primary mechanism for carrying away a pulsar's
spin-down energy, hence determining its nature is of central importance. The
eclipsing binary PSR B1957+20 is presently the only system where we can study the
wind of a weakly magnetized pulsar. Its wind ablates and heats its companion and
powers a bow-shock nebula. ROSAT detections show that the wind produces X-rays,
but can't confirm their origin. We propose Chandra observations where the spatial
resolution will for the first time allow us to distinguish bow-shock and
intra-binary emission, and if the latter, they will be sensitive to orbital
modulations distinguishing between the companion and the pulsar as the origin.
With this we will better determine the energy and particle composition of a
low-magnetic field pulsar wind
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:59:36.80 +20:48:15.10 PSR B1957+20 ACIS-S NONE 43.00
===================================================================================
Proposal Number: 02400382
Proposal Title: SEARCHING FOR X-RAY PULSARS IN M31
PI: PHILIP KAARET
Subject Category: BH AND NS BINARIES
Abstract: Study of x-ray sources in external galaxies (other than the LMC and
SMC) has been limited to flux and spectral measurements. Classification of the
sources based on such observations is often ambiguous. We propose to use the high
resolution and large collecting area of Chandra to search for pulsations from
x-ray sources in M31. These observations should lead to unambiguous
identification of luminous accreting x-ray pulsars and may permit discovery of
very young rotation powered pulsars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:42:42.30 +41:16:08.40 M31 HRC-I NONE 50.00
===================================================================================
Proposal Number: 02400455
Proposal Title: X-RAY BURSTERS WITH LOW PERSISTENT X-RAY LUMINOSITIES
PI: FRANK VERBUNT
Subject Category: BH AND NS BINARIES
Abstract: We propose to make snap-shot observations of new X-ray sources detected
only during type I bursts, with persistent X-ray luminosities <10^36 erg/s. We
expect to detect the systems easily, and will obtain accurate positions for
optical/infrared followup and estimates of the luminosity level. We thus can
study that part of the population of low-mass X-ray binaries which has persistent
X-ray luminosities below 10^36 erg/s, and test theory of thermonuclear bursts in
the low accretion regime.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:24:27.00 -63:13:26.00 SAX J1324.5-6313 ACIS-S NONE 5.00
17:52:24.00 -31:37:42.00 SAX J1752.3-3138 ACIS-S NONE 5.00
17:53:34.00 -23:49:24.00 SAX J1753.5-2349 ACIS-S NONE 5.00
18:06:34.00 -22:15:06.00 SAX J1806.5-2215 ACIS-S NONE 5.00
18:18:44.00 +14:24:12.00 SAX J1818.7+1424 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 02400398
Proposal Title: A SEARCH FOR X-RAY JETS IN TWO MICRO-QUASARS
PI: WILLIAM HEINDL
Subject Category: BH AND NS BINARIES
Abstract: We propose to make detailed images with the HRC-I of the two Galactic
"micro-quasars" GRS 1758-258 and 1E 1740.7-2942 in order to search for X-ray
jets. Both sources have spectral and timing properties which are quite similar to
the canonical black hole candidate Cyg X-1. They are also, however, associated
with the time variable cores of double-lobed radio sources. This morphology is
quite reminiscent of the extra-galactic radio sources, but on parsec length
scales. In analogy with the radio loud AGN, we plan to search for X-ray jets
which may feed the radio lobes. Because the jets may be less than an arcsecond in
length, we will use the high resolution imaging capabilities of the HRC-I.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:01:13.20 -25:44:29.00 GRS 1758-258 HRC-I NONE 10.00
===================================================================================
Proposal Number: 02400492
Proposal Title: DO QUIESCENT BLACK HOLE ACCRETION DISKS ACCRETE?
PI: MICHAEL GARCIA
Subject Category: BH AND NS BINARIES
Abstract: There is currently a raging debate within the black hole community
which can be summarized as: Do the black holes in quiescent x-ray nova accrete
(or not)?. The answer to this question is fundamental to black hole research, for
example a positive answer supports the 'proof' of event horizons in black holes,
while a negative answer discredits this proof. XTE J1118+480 is likely the
nearest black hole x-ray nova, and definitely has the lowest A_V. Chandra (and
HST) observations of this system during the mini-outbursts which may occur in AO2
will allow the most complete view of a black hole accretion disk during a time
when the mass transfer in the outer disk is enhanced. Our study should determine
if the mass transfer into the black hole is similarly enhanced.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:18:10.80 +48:02:11.00 XTE J1118+480 ACIS-S LETG 5.00
11:18:10.80 +48:02:11.00 XTE J1118+480 ACIS-S LETG 5.00
11:18:10.80 +48:02:11.00 XTE J1118+480 ACIS-S LETG 5.00
===================================================================================
Proposal Number: 02400498
Proposal Title: CHANDRA OBSERVATIONS OF FAST SPINNING HARD TRANSIENTS IN
QUIESCENCE: PROBING THE SPECTRUM DEEP IN THE PROPELLER REGIME
PI: SERGIO CAMPANA
Subject Category: BH AND NS BINARIES
Abstract: We propose Chandra observations of five HXRTs containing fast spinning
and/or high magnetic field neutron stars to probe their quiescent emission. Due
to their faintness these sources are likely in an accretion regime which does not
allow matter to fall directly onto the neutron star surface (propeller state).
Indeed, we have already carried out BeppoSAX observations onsome of these sources
with promising results as the dramatic increase in the X-ray luminosity by a
factor of 100 in 15 hr in 4U 0115+63, interpreted as the overcome of the
centrifugal barrier. The selected sample allows us to probe the physics of the
propeller in a variaty of conditions (P=69 ms-103 s / B=10^11-10^13 G), and in a
range of luminosities unaccessible to previous X-ray missions.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:34:59.90 +53:10:23.20 V 0332+53 ACIS-S NONE 5.00
===================================================================================
Proposal Number: 02400584
Proposal Title: SPECTROSCOPY OF THE MICROQUASAR GRO J1655-40 DURING OUTBURST
PI: DUANE LIEDAHL
Subject Category: BH AND NS BINARIES
Abstract: We propose a 40 ksec Chandra HETG TOO observation of the microquasar
GRO J1655-40 during outburst. The object shows both radio-loud and radio-quiet
X-ray outbursts, with relativistic jets accompanying the radio outbursts. Clear
evidence for complex absorption in the iron K band has been observed with ASCA.
The HETG can be used to great advantage here, allowing us to extract detailed
line diagnostics and, through precise measurements of redshifts, determine the
location and kinematic properties of the absorber. GRO J1655-40 represents a
unique opportunity to explore (``up close'') transient outburst accretion physics
near a black hole.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:54:00.10 -39:50:44.90 GRO J1655-40 ACIS-S HETG 40.00
===================================================================================
Proposal Number: 02400625
Proposal Title: DETAILED STUDY OF THE IRON LINE AND LOW ENERGY FEATURES IN Z AND
ATOLL SOURCES
PI: NATALE ROBBA
Subject Category: BH AND NS BINARIES
Abstract: We propose Chandra HETGS observations of the atoll source 4U 1705-44
and the Z source GX 340+0 for 30 ks each, to perform a detailed study of the iron
K$\alpha$ line, and the correlation between line parameters and kHz QPOs. These
sources are known to show broad ($\sim 1$ keV FWHM) iron K$\alpha$ lines: several
hypothesis were proposed to explain their width ({\it e.g.} relativistic and
Doppler effects in an accretion disk, Compton scattering, line-blending), and we
expect that the high energy resolution (the highest in the iron line range) of
the Chandra HETGS will be able to resolve the complex line shape and to constrain
the various models proposed.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:45:47.60 -45:36:39.00 GX340+0 ACIS-S HETG 5.00
16:45:47.60 -45:36:39.00 GX340+0 ACIS-S HETG 25.00
17:09:00.40 -44:06:48.00 4U1705-44 ACIS-S HETG 5.00
17:09:00.40 -44:06:48.00 4U1705-44 ACIS-S HETG 25.00
===================================================================================
Proposal Number: 02400631
Proposal Title: 4U 2129+47: FROM ADIOS TO ADAF OR ISOLATED NEUTRON STAR?
PI: MICHAEL NOWAK
Subject Category: BH AND NS BINARIES
Abstract: 4U2129+47 is one of the three original `Accretion Disk Corona' sources.
The partial X-ray eclipses in these near edge-on systems imply that the X-ray
emission must extend over radii a substantial fraction of the binary separation,
possibly related to an outflow, as in models of `Adiabatic Inflow/Outflow'
accretion. Since 1983 4U2129+47 has been in a protracted quiescent state. Two
models exist for this state: `Advection Dominated Accretion' or thermal emission
from the cooling surface of the neutron star. The latter would imply a sharp,
total eclipse in the lightcurve. We propose a 38 ksec (two binary orbits) Chandra
observation of 4U2129+47 which will test thermal emission models of the quiescent
spectrum and determine whether any eclipse in the observed lightcurve is total or
partial.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:31:26.20 +47:17:24.00 4U2129+47 ACIS-S NONE 38.00
===================================================================================
Proposal Number: 02400678
Proposal Title: DYNAMICS OF THE IONIZED STELLAR WIND IN VELA X-1
PI: STEVEN KAHN
Subject Category: BH AND NS BINARIES
Abstract: We propose to observe the archetypal low-luminosity high mass X-ray
binary, Vela X-1 to study the dynamics of the stellar wind in the system. The
high resolving power capabilities of the Chandra HETGS will allow us study the
ionization structure and geometrical distribution of matter in the circumstellar
medium through accurate measurements of emission measures and Doppler shifts of
bright emission lines during several different orbital phases. We will also be
able to simultaneuously constrain some of the key stellar wind parameters
including the mass-loss rate and velocity structure of the stellar wind.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:02:06.90 -40:33:16.90 VELA X-1 ACIS-S HETG 30.00
09:02:06.90 -40:33:16.90 VELA X-1 ACIS-S HETG 35.00
09:02:06.90 -40:33:16.90 VELA X-1 ACIS-S HETG 85.00
===================================================================================
Proposal Number: 02400714
Proposal Title: TEMPORAL EVOLUTION OF TRANSIENT TYPE I BURSTERS IN QUIESCENCE
PI: LARS BILDSTEN
Subject Category: BH AND NS BINARIES
Abstract: In transiently accreting neutron stars (NSs), the NS crusts are heated
during the accretion outbursts. The timescale on which this heat is radiated away
after outburst depends on the depth where this heat is deposited. In deep crustal
heating, the relevant depths have thermal timescales of days -- years, with most
being radiated on a 2 yr timescale. We request observations to observe transient
NSs soon after they return to quiescence, to observe this evolution. This
proposal is a resubmission of a partially granted ToO proposal which was not
triggered during AO1.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:11:16.00 +00:35:06.00 AQL X-1 HRC-S LETG 10.00
19:11:16.00 +00:35:06.40 AQL X-1 ACIS-S NONE 8.00
19:11:16.00 +00:35:06.40 AQL X-1 ACIS-S NONE 8.00
19:11:16.00 +00:35:06.40 AQL X-1 ACIS-S NONE 8.00
19:11:16.00 +00:35:06.40 AQL X-1 ACIS-S NONE 8.00
===================================================================================
Proposal Number: 02400819
Proposal Title: QUIESCENT AND LOW LUMINOSITY X-RAY BINARIES
PI: CRAIG MARKWARDT
Subject Category: BH AND NS BINARIES
Abstract: The galactic bulge contains many old neutron star and black hole
binaries now identified as low luminosity X-ray sources. Observed sources can be
persistent at a level of a few mCrab, or transients which peak at 10-200 mCrab
and then fade to quiescent levels <0.5 mCrab. Theoretical models, including
ADAFs, propeller effects, and thermal surface emission, have been tested on only
a handful of sources. We propose Chandra observations of 4 faint low mass
binaries, XTE J1710-281, XTE J1743-363, SAX J1747.0-2853, and XTE J1723-376, the
first two persistently variable and the second two in apparent quiescence.
Observations of 30 ks with ACIS I and S would provide for improved positions,
light curves and spectra for the active sources, and at least a flux measurement
for the quiescent ones.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:23:38.10 -37:39:44.60 XTE J1723-376 ACIS-I NONE 30.00
17:47:09.10 -28:53:01.00 SAX J1747.0-2853 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 02400850
Proposal Title: ACIS-HETG OBSERVATIONS OF MICROQUASAR XTE J1748-288
PI: JULIA LEE
Subject Category: BH AND NS BINARIES
Abstract: RXTE observations of the recently discovered microquasar XTE J1748-288
reveal spectral differences between the very high, high, and low state. ASCA \&
RXTE observations show prominent iron line(s). We propose HETG 140ks total
exposure over these 3 phases in order to characterize the X-ray spectral features
and resolve presently unknown lines for these 3 phenomenological states. We will
also look for emission lines from any X-ray jet, and P-Cygni profiles indicative
of a disk-wind. This will allow for a comprehensive study (when compared to our
Cycle 1 Chandra observations of GRS1915+105, SS433, and Cir X-1) of GBC systems,
and in particular of the poorly understood systems termed microquasars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:48:08.00 -28:28:48.00 XTE J1748-288 ACIS-S HETG 30.00
17:48:08.00 -28:28:48.00 XTE J1748-288 ACIS-S HETG 40.00
17:48:08.00 -28:28:48.00 XTE J1748-288 ACIS-S HETG 70.00
===================================================================================
Proposal Number: 02400903
Proposal Title: HIGH RESOLUTION SPECTROSCOPY OF THE X-RAY BURSTER 4U 1636-53
PI: NORBERT SCHULZ
Subject Category: BH AND NS BINARIES
Abstract: The LMXB 4U 1636-53 is a prototype atol source in which a neutron star
accretes matter from a low mass companion star producing moderate to
sub-Eddington X-ray luminosities. The X-ray luminosity, and thus to a large
extent mass-accretion rate, differs by orders of magnitude in different spectral
states. 4U 1636-53 is mostly found in its lower banana state, where it exhibits
type I X-ray bursts on quite regular time scales. It has been observed for 30 ks
in AO1 but was found in a very bright state with no bursts and severe pile-up
defects in the 1st order grating spectra. We propose to re-observe this target
for another 30 ks with significantly reduced CCD frametime.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:40:55.50 -53:45:05.00 4U 1636-53 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 02400911
Proposal Title: MAPPING THE JETS OF SS 433
PI: MASAAKI NAMIKI
Subject Category: BH AND NS BINARIES
Abstract: ASCA revealed Doppler-shifted emission lines in its X-ray spectrum
originating from the two anti-parallel jets. The ASCA data indicated the X-ray
jet is $\sim10^{13}$~cm long \cite{Kotani97a}, ten times longer than the previous
estimations (e.g., \cite{Stewart87}, \cite{Watson86}). The data also suggest the
existence of an absorber, a disk outflow and/or matter distributed in the orbital
plain \cite{Kotani96}. Our proposal is to reveal the violent outflow/inflow of
SS~433, which is the only system ever know to be in a steady super-critical
accretion state, and to explore the nature of it.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:11:49.50 +04:58:58.10 SS 433 ACIS-S HETG 20.00
19:11:49.50 +04:58:58.10 SS 433 ACIS-S HETG 20.00
19:11:49.50 +04:58:58.10 SS 433 ACIS-S HETG 20.00
===================================================================================
Proposal Number: 02400913
Proposal Title: THE WIND AND ACCRETION DISK IN CEN X-3/V779 CEN
PI: PATRICK WOJDOWSKI
Subject Category: BH AND NS BINARIES
Abstract: We propose a 50 ks HETG observation of Cen X-3 out of eclipse in a low
state. We will observe emission lines from the wind and from the accretion disk
and inner accretion structure. From the fluxes of recombination lines we will
measure the density and ionization structure of the wind. From the the line
velocities we will measure the velocity and mass loss rate of the ionized wind.
By measuring the line velocities of fluorescent lines from near the neutron star
we will derive constraints on the location of inner accretion structures. This
observation complements an already executed Chandra observation of Cen X-3 in
eclipse.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:21:15.20 -60:37:24.00 CEN X-3 ACIS-S HETG 50.00
===================================================================================
Proposal Number: 02400917
Proposal Title: ACCRETION DISK STRUCTURE IN VARIOUS SPECTRAL STATES OF GRS
1915+105
PI: RONALD REMILLARD
Subject Category: BH AND NS BINARIES
Abstract: GRS~1915$+$105 displays 9 types of light curves that fall in 3
categories. In the steady-hard states, the Fe line is strongest, and there is a
steady type of jet. In the soft states, the accretion disk dominates the X-ray
spectrum, and we often detect the 67 Hz QPO thought to arise from GR effects in
the inner disk. The remaining states show a variety of instability oscillations,
some producing violent mass ejections. Progress on all fronts requires high
resolution spectra to help interpret the disk structure. We have particular
interest in the profiles of broad Fe emission, intending to gain physical
insights using theoretical models of Nayakshin et al. With monitoring timescales
selected to randomize the 9 states, we request 3 obs likely to sample different
conditions in the disk.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:15:11.60 +10:56:44.90 GRS 1915+105 ACIS-S HETG 30.00
19:15:11.60 +10:56:44.90 GRS 1915+105 ACIS-S HETG 30.00
19:15:11.60 +10:56:44.90 GRS 1915+105 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 02400927
Proposal Title: WHERE IS OAO 1657-415?
PI: DEEPTO CHAKRABARTY
Subject Category: BH AND NS BINARIES
Abstract: The high-mass X-ray binary OAO 1657-415 consists of a 38 s pulsar
accreting from a (still unidentified) OB supergiant. The system is only the 7th
known eclipsing X-ray binary, and the only one which seems to form a transient
accretion disk from the companion's stellar wind. It provides a rare opportunity
to measure a neutron star mass, if the optical companion can be identified.
However, the X-ray position of this highly absorbed source is only known to 30
arcsec. I propose a short ACIS-HETG observation to determine its position
precisely, and probe the stellar wind of the companion using fluorescent X-ray
lines.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:00:47.10 -41:39:14.60 OAO 1657-415 ACIS-S HETG 5.00
===================================================================================
Proposal Number: 02408033
Proposal Title: CHANDRA OBSERVATIONS OF CYGNUS X-1 IN A RARE, SUSTAINED
HIGH/SOFT STATE
PI: JON MILLER
Subject Category: BH AND NS BINARIES
Abstract: The full SJ is contained in an email to the Director. A clear High/Soft
State was observed in Cyg X-1 between 15 Oct. and 15 Nov. 2000 (mean flux: 0.5-1
Crab, 2-12 keV RXTE ASM). Following a short Low/Hard state, the mean rate
returned to ~1 Crab on 7 Dec. 2000. This flux and observed spectral softness
indicate that Cygnus X-1 has entered a second sustained High/Soft state episode.
This outburst profile is similar to the 83-day High/Soft state observed May-Aug.
1996 (see http://xte.mit.edu/~rr/cygx1.ps). A Chandra observation of Cygnus X-1
(PI, Canizares; Cui et al. in prep.) in the Low/Hard state shows evidence for an
Fe K-alpha line, Fe L edges (Cui et al, in prep). The dynamics and geometry of
the L/Hard and H/Soft state are expected to be markedly different. Measurements
of the iron e
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:58:21.70 +35:12:05.80 CYGNUS X-1 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 02408040
Proposal Title: A CHANDRA OBSERVATION OF THE LONG-DURATION TRANSIENT AND NEUTRON
STAR LOW-MASS X-RAY BINARY KS 1731-260 IN QUIESCENCE
PI: RUDY WIJNANDS
Subject Category: BH AND NS BINARIES
Abstract: The full scientific justification is sent in an email to the Director.
The long-duration transient KS 1731-260 has been active for over a decade,
however, our recent RXTE/PCA observations show that the source has now gone back
in to quiescence. This opens the oppertunity to study the affects of prolonged
accretion onto the neutron star on the quiescence X-ray properties of a neutron
star X-ray transient. This would be the first time ever that such a study can be
performed. Considerable differences (e.g., a considerable higher luminosity
compared to that of short-duration transients) are expected if the quiescence
properties depend on the time averaged accretion rate in outburst. We will also
obtain an excellent position of the source allowing the identification of its
optical and infrared counter parts.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:34:13.50 -26:05:16.80 KS 1731-260 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 02408042
Proposal Title: HIGH RESOLUTION SPECTROSCOPY OF THE POSSIBLE JETS IN GRS
1758-258
PI: WILLIAM HEINDL
Subject Category: BH AND NS BINARIES
Abstract: As of 28 Feb, the microquasar GRS1758-258 has entered an extremely dim
x-ray state (RXTE- IAUC submitted). This is unlikely to happen again for 10
years. Two HRC observations in 2000 Sept/Oct revealed a variable point source
plus elongated (~1") emission. In one month, the morphology changed showing the
likely formation of an ~arcsecond x-ray jet. At the likely source distance
(8.5kpc), relativistic bulk motion would be required. The current state is ~3x
dimmer in RXTE than typical. We suspect the point source has turned off, and the
residual flux is from ejected material. Cui et al. (ACIS/HETG, astro-ph/0009380)
found extended emission around another microquasar, 1E1740.7-2942, and may have
detected spectral lines, but they could not separate the core and extended
components. We will measure the spectrum of the extended (jet?) emission without
point source contamination. This has the possibility of discovering red and
blue-shifted emission lines a la SS433.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 10.00
18:01:12.40 -25:44:35.90 GRS 1758-258 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 02408061
Proposal Title: LOCALIZATION AND IDENTIFICATION OF THE X-RAY TRANSIENT IN NGC
6440
PI: JEAN IN 'T ZAND
Subject Category: BH AND NS BINARIES
Abstract: X1745-203 in NGC 6440 is one of five X-ray transients in galactic
globular clusters, with recorded outbursts in 1971 and 1998. The last outburst
(In 't Zand et al, 1998, A&A 345, 100) was followed up by us with VLT and NTT
observations which identified two candidate optical counterparts (Verbunt et al,
2000, A&A 359, 960). Both of these have counterparts in a Chandra observation of
NGC 6440 taken during quiescence in July 2000. An accurate position of the X-ray
transient while it is active would secure the identification of the quiescent
X-ray as well as the optical counterpart. With such an identification, we can
study the quiescent X-ray emission and determine what it is due to. One of the
most likely explanations is emission from a cooling neutron star; if so, given
the known distance, we can directly measure the neutron-star radius. ASM/RXTE
observations show that X1745-203 has gone into outburst again, and this presents
the opportunity to determine the position of the transient.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:48:52.60 -20:21:33.80 NGC 6440 ACIS-S NONE 2.50
===================================================================================
Proposal Number: 02408064
Proposal Title: CYGNUS X-1 IN THE HIGH STATE
PI: WEI CUI
Subject Category: BH AND NS BINARIES
Abstract: Cyg X-1 is now in a rare high state, as seen by the ASM and radio
monitoring. Such a state transition occurs only once every few years, and
therefore offers a great opportunity for us to conduct a detailed study of this
important black hole candidate in the high state, making use some of the
unprecedented capabilities offered by Chandra. Previous Chandra observations of
the source have revealed the presence of numerous emission lines and absorption
edges (Schulz et al. 2001). There is already evidence that the line emission
seems to vary depending upon the state of the source (low state vs. flare). It
would, therefore, be very interesting to see how the source behaves in the high
state. The results would almost certainly shed light on the difference in X-ray
production processes and the binary environment between the low and high states,
and, ultimately, on the physical process that is responsible for triggering a
state transiton.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:58:21.60 +35:12:07.20 CYG X-1 ACIS-S HETG 30.00
***********************************************************************************
SN, SNR AND ISOLATED NS
--------------------------------------------------
===================================================================================
Proposal Number: 02500055
Proposal Title: OBSERVATION OF MKR 231
PI: GORDON GARMIRE
Subject Category: SN, SNR AND ISOLATED NS
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:56:14.30 +56:52:25.30 Mrk 231 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 02500067
Proposal Title: NEAREST SNR
PI: GORDON GARMIRE
Subject Category: SN, SNR AND ISOLATED NS
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:52:00.00 -46:21:00.00 RX J0852.0-4622 ACIS-I NONE 1.00
08:52:00.00 -46:21:00.00 RX J0852.0-4622 ACIS-S HETG 16.00
08:52:00.00 -46:20:30.00 RX J0852.0-4622 ACIS-I NONE 3.00
08:52:01.38 -46:17:53.34 RX J0852.0-4622 ACIS-S NONE 31.00
===================================================================================
Proposal Number: 02500074
Proposal Title: G0.9+0.1 AND G74.9+1.2
PI: GORDON GARMIRE
Subject Category: SN, SNR AND ISOLATED NS
Abstract: This observation is search for central objects in G0.9+0.1 and
G74.9_1.2
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:47:23.60 -28:09:35.00 G0.9+0.1 ACIS-S NONE 35.00
20:15:60.00 +37:13:15.00 G74.9+1.2 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 02500086
Proposal Title: EXPANSION OF THE SNR CAS-A
PI: STEPHEN MURRAY
Subject Category: SN, SNR AND ISOLATED NS
Abstract: A second epoch image of Cas-A with the HRC-I to compare with the AO-1
image. A direct measure of the expansion of the outer shock front, and the
various knots, filamnets and floculli will provide information on the kinematics
of this young SNR as it expands into the surrounding ISM. A timing analysis of
the central point-like source will be made to look for pulsations and to compare
with earlier epoch timing studies.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
23:23:27.85 +58:48:42.10 CAS-A HRC-S NONE 50.00
===================================================================================
Proposal Number: 02500117
Proposal Title: ACIS OBSERVATION OF THE LMC SUPERNOVA REMNANT N23
PI: STEPHEN HOLT
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We propose to observe the ISM-dominated remnant N23 in the Large
Magellanic Cloud using ACIS-S3 on Chandra. Our objectives are spatially resolved
spectroscopy and spectral imaging, in particular to distinguish between the
spectrum of the bright western side with the fainter north and east, and to
search for harder emission than was detected with ASCA.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:55:00.00 -68:01:45.00 Mispointing ACIS-S NONE 40.00
===================================================================================
Proposal Number: 02500119
Proposal Title: OBSERVATION OF SNR RCW103
PI: GORDON GARMIRE
Subject Category: SN, SNR AND ISOLATED NS
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:17:36.31 -51:02:24.72 RCW103 ACIS-I NONE 3.50
16:17:36.31 -51:02:24.72 RCW103 ACIS-I NONE 3.50
16:17:36.31 -51:02:24.72 RCW103 ACIS-I NONE 3.50
16:17:36.31 -51:02:24.72 RCW103 ACIS-I NONE 3.50
16:17:36.31 -51:02:24.72 RCW103 ACIS-I NONE 3.50
16:17:36.31 -51:02:24.72 RCW103 ACIS-S NONE 3.50
===================================================================================
Proposal Number: 02500120
Proposal Title: OBSERVATION OF SNR N49B
PI: GORDON GARMIRE
Subject Category: SN, SNR AND ISOLATED NS
Abstract: LMC SNR, a Sedov phase object for study with a large number of
photons.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:25:25.00 -65:59:22.00 N49B ACIS-S NONE 35.00
===================================================================================
Proposal Number: 02500044
Proposal Title: ACIS OBSERVATION OF THE SUPERNOVA REMNANT 3C397
PI: STEPHEN HOLT
Subject Category: SN, SNR AND ISOLATED NS
Abstract: We will use ACIS-S on Chandra to observe the Galactic remnant 3C397.
Previous X-ray imaging observations show a central hot spot and an extended
bright region to the west; the integrated X-ray spectrum is seen to be very
complex, including a strong Fe K blend. We will search for a point source
embedded in the hot spot, and perform spatially resolved spectroscopy.
Grat- Exp.
R.A. Dec. (J2000)