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Chandra proposals are divided into the following categories:
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SOLAR SYSTEM
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Proposal Number: 03100101
Proposal Title: SEARCH FOR X-RAYS FROM URANUS ALTERNATE TARGET
PI: GORDON GARMIRE
Subject Category: SOLAR SYSTEM
Abstract: The detection of X-rays from Uranus would help constrain the mechanism
for generating X-rays in planetary magnetospheres. X-rays have been detected from
Jupiter and are likely from saturn. IUE and Voyager 2 found evidence for auroral
acitvity from Uranus, particularly from the south pole. A 30 ks observation by
Chandra should either support (if X-rays are detected) or refute the analog with
Jupiter.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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21:59:07.16 -13:08:15.30 URANUS ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03100308
Proposal Title: X-RAY OBSERVATIONS OF JUPITER
PI: J WAITE
Subject Category: SOLAR SYSTEM
Abstract: Jupiter is an interesting source of x-rays within the solar system.
ACIS and HRI observations are being analyzed at this time that will redefine the
Jovian x-ray source. Spectral observations appear to verify the charge exchange
source of energetic ions, but HRC observations indicate a source location and
oscillatory light curve that are totally unexpected. Many new questions arise. We
propose to use a combination of HRC, ACIS, and HST-STIS to investigate these
exciting new possibilities.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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08:51:29.61 +18:32:18.71 JUPITER HRC-I NONE 72.00
===================================================================================
Proposal Number: 03100792
Proposal Title: ACIS-S LOW ENERGY SPECTROSCOPY AND PHOTOMETRIC IMAGING OF CHARGE
EXCHANGE X-RAY EMISSION FROM COMET C/LINEAR WM1 (2000)
PI: CAREY LISSE
Subject Category: SOLAR SYSTEM
Abstract: Using ACIS-S observations of comet C/LINEAR 1999 S4 with Chandra in
Cycle 1, we conclusively demonstrated the presence of x-ray line emission driven
by charge exchange between highly ionized solar wind minor ions and gases emitted
from the cometary nucleus. A number of important uncertainties remain, however,
that can be answered with ACIS-S observations of the brighter, closer comet
C/LINEAR WM1 (2000) in December 2001: How many CXE lines are ultimately
detectable with Chandra in the 250 - 900 eV energy range? Can we detect spatial
hardness variations due to progressive solar wind charging from the cometary
neutrals? What is the temporal history of the emission? We request a small amount
of ACIS-S time, 35 ksec in Cycle 3, to answer these important questions.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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22:13:00.91 -51:55:03.14 C/LINEAR WM1 (2000) ACIS-S LETG 8.75
22:13:32.79 -51:51:41.80 C/LINEAR WM1 (2000) ACIS-S LETG 8.75
22:14:04.18 -51:48:16.45 C/LINEAR WM1 (2000) ACIS-S LETG 8.75
22:14:37.02 -51:44:33.07 C/LINEAR WM1 (2000) ACIS-S LETG 8.75
===================================================================================
Proposal Number: 03108065
Proposal Title: X-RAY OBSERVATIONS OF THE FIRST COUNTERPART TO A FAST X-RAY
TRANSIENT, XRF010930
PI: FIONA HARRISON
Subject Category: SOLAR SYSTEM
Abstract: Thanks to BeppoSAX we are now aware of a new type of transient -- X-ray
flashes (XRFs, also called Fast X-ray Transients). About one third of the events
seen by the WFC are XRFs. Until today, NOT A SINGLE member of this class has been
localized to arcsecond accuracy. Only gradually has the community come to
appreciate that XRFs have a rate comparable to GRBs. There are two possibilities:
1. XRFs are highly redshifted GRBs (e.g. Heise, Lloyd) 2) XRFs are explosive
events producing Lorentz factors intermediate between GRBs and SNe and thus peak
in the X-ray. On 30.25 October 2001 (UT) the BeppoSAX Wide Field Camera (WFC)
detected a XRF, hereafter XRF011030, unaccompanied by any increased rate in the
Gamma Ray Burst Monitor (GRBM) on SAX, HETE-2 or Ulysses.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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20:43:32.30 +77:17:18.90 FXRT011030 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03108067
Proposal Title: X-RAY OBSERVATIONS OF THE FIRST COUNTERPART TO A FAST X-RAY
TRANSIENT, XRF010930
PI: FIONA HARRISON
Subject Category: SOLAR SYSTEM
Abstract: Thanks to BeppoSAX we are now aware of a new type of transient -- X-ray
flashes (XRFs, also called Fast X-ray Transients). About one third of the events
seen by the WFC are XRFs. Until today, NOT A SINGLE member of this class has been
localized to arcsecond accuracy. Only gradually has the community come to
appreciate that XRFs have a rate comparable to GRBs. There are two possibilities:
1. XRFs are highly redshifted GRBs (e.g. Heise, Lloyd) 2) XRFs are explosive
events producing Lorentz factors intermediate between GRBs and SNe and thus peak
in the X-ray. On 30.25 October 2001 (UT) the BeppoSAX Wide Field Camera (WFC)
detected a XRF, XRF011030, and a Chandra DDF has found an X-ray source coincident
with a radio transient (see below).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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20:43:32.30 +77:17:18.90 FXRT011030 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03108076
Proposal Title: SPECTROSCOPIC IMAGING OF CHARGE EXCHANGE X-RAY EMISSION FROM
COMET C/2002 C1
PI: KONRAD DENNERL
Subject Category: SOLAR SYSTEM
Abstract: Comet C/2002 C1, discovered on February 1, 2002, is predicted to be as
bright as 4 - 5 mag when it will become observable with Chandra from April 10,
2002. We propose to utilize this opportunity for direct spectroscopic imaging
with ACIS-S. This has never been done for such a bright comet. Thanks to a
favorable observing geometry, we can apply a novel observing technique: as the
comet will slowly move along the comet-Sun line, an automatic scan of the x-ray
emission properties will be provided along this direction, where the charge
exchange model predicts a characteristic spectral evolution, which could,
however, not be tested so far. While previous Chandra images and spectra of
comets suffer from low photon statistics, we expect to get about 40 times more
photons than from C/LINEAR S4. This will allow us to utilize the full spectral
and spatial resolution of Chandra. A detailed Scientific Justification is
provided in the attached Postscript file.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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C/2002 C1 ACIS-S NONE 8.00
23:20:00.22 +55:46:43.93 C/2002 C1 ACIS-S NONE 12.00
23:30:26.68 +54:54:45.40 C/2002 C1 ACIS-S NONE 12.00
===================================================================================
Proposal Number: 03108123
Proposal Title: A SEARCH FOR SOFT X-RAY AURORAS ON EARTH
PI: G. GLADSTONE
Subject Category: SOLAR SYSTEM
Abstract: Chandra HRC-I observations of Jupiter made in Dec. 2000 in support of
the Cassini flyby have revealed the surprising result that jovian auroral x-ray
emissions are concentrated in a small `hot spot' which pulsates with a ~45-m
period. The location of the hot spot near the magnetic pole implies a particle
source region near Jupiter's magnetopause, and high-latitude reconnection of
heavy solar wind ions is now a viable explanation for these soft x-ray emissions.
The identical process should operate at Earth as well. Hard x-ray emissions from
electron bremsstrahlung are well known in the terrestrial aurora. Surprisingly,
however, there have been no searches of Earth's aurora for emissions at <2keV. We
propose here a simple slew observation by HRC-I across the auroral region to look
for Earth's soft x-ray aurora. The detection of a Jupiter-like hot spot at Earth
would imply that heavy ion solar wind charge exchange is important for producing
x-rays at planets as well as comets.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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05:26:24.00 -32:51:00.00 EARTH HRC-I NONE 1.00
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NORMAL STARS AND WD
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===================================================================================
Proposal Number: 03200012
Proposal Title: A YSO-LIKE PULSED ASTROPHYSICAL JET AND BIPOLAR NEBULA IN A
DYING STAR: WFPC2/STIS STUDY OF HE2-90
PI: RAGHVENDRA SAHAI
Subject Category: NORMAL STARS AND WD
Abstract: We have discovered an extended, highly-collimated, bipolar jet in
He2-90, an object long classified as a planetary nebula (PN). The discovery
images (obtained with WFPC2/HST) show that the morphology of He2-90 does not look
like that of any known PN, but resembles that of a classical young stellar object
(YSO). This appears to be a unique object. We propose to map the jet near the
central source using the long-slit, medium resolution mode of STIS. We also
propose Chandra X-ray observations (with ACIS-I) to check the association of an
EGRET >~mma-ray source which lies in the direction of He2-90.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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13:09:36.40 -61:19:36.30 HEN2-90 ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03200024
Proposal Title: ORIGIN OF THE X-RAY EMISSION OF THE PREMAIN SEQUENCE STAR V 410
TAU
PI: PETER PREDEHL
Subject Category: NORMAL STARS AND WD
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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04:18:31.10 +28:27:16.00 V 410 TAU ACIS-S NONE 11.20
04:18:31.10 +28:27:16.00 V 410 TAU ACIS-S NONE 15.00
04:18:31.10 +28:27:16.00 V 410 TAU ACIS-S NONE 18.80
===================================================================================
Proposal Number: 03200038
Proposal Title: PROBING THE GAS IN THE V471 TAU SYSTEM WITH ABSORPTION
SPECTROSCOPY
PI: FREDERICK WALTER
Subject Category: NORMAL STARS AND WD
Abstract: The eclipsing dA+K2V binary V471 Tau affords an opportunity to use
X-ray absorption to probe the spatial extent of the chromosphere/corona of an
active dwarf star. HST observations have shown chromospheric and transition
region species (O I through N V) in absorption at radial extents of up to 2 K
star radii on one side of the star, but not on the other. X-ray observations have
revealed large absorption dips, primarily but not exclusively from gas near the
inner Lagrangian points of the system. CHANDRA can probe the neutral gas, by
observing the time-variability of the neutral Hydrogen absorption column, and by
oberving the variations of the depths of absorption edges. The white dwarf
photosphere provides a bright, soft continuous spectrum against which to observe
these changes.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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03:50:25.00 +17:14:47.40 V471 TAU HRC-S LETG 90.00
===================================================================================
Proposal Number: 03200050
Proposal Title: VIOLENT MASSIVE STAR FORMATION IN THE GALAXY: W51 ALTERNATE
TARGET
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Abstract: The proposed observation of W51 will provide a valuable springboard to
understanding starbursts in galaxies other than our own.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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19:23:40.00 +14:31:06.00 W51 ACIS-I NONE 21.00
19:23:40.00 +14:31:06.00 W51 ACIS-I NONE 59.00
===================================================================================
Proposal Number: 03200056
Proposal Title: HIGH RESOLUTION SPECTROSCOPY OF THE YOUNG STELLAR CLUSTER NGC
2362
PI: CLAUDE CANIZARES
Subject Category: NORMAL STARS AND WD
Abstract: We propose a deep HETGS observation of the young stellar cluster NGC
2362. Only 5-7 Myrs old, NGC 2362 is one of the youngest clusters in our Galaxy.
Unlike in most other star forming regions, this cluster is almost completely
devoid of residual gas and it is somewhat deficient in low-mass stars. It main
star, tau CMa, is actaully at least a double star with quite equal massive
constituents and is believed that it already eveloved away from the zero-age main
sequence (ZAMS). As part of our program to perform high resolution spectroscopy
on very young early type O stars we observe tau CMa for 95 ks in order to search
for X-ray emission from dense and hot plasmas. This cluster also enables us to
study high resolution X-ray spectra of ZAMS B-type stars. stars and will provide
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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07:18:43.00 -24:56:59.90 NGC2362 ACIS-S HETG 47.00
07:18:43.00 -24:56:59.90 NGC2362 ACIS-S HETG 48.00
===================================================================================
Proposal Number: 03200079
Proposal Title: HETGS SPECTROSCOPY OF THE LONG-PERIOD ACTIVE BINARY, IM PEGASI.
PI: DAVID HUENEMOERDER
Subject Category: NORMAL STARS AND WD
Abstract: RS CVn binary systems are well known for their activity, interpreted as
large-scale versions of Solar phenomena: spots, prominences, coronae, all with
dynamic behavior. Stellar X-ray luminosity is well known to correlate with
rotation and RS CVn stars are among the most luminous of late-type sources; they
are prime candidates for X-ray spectroscopy. IM Peg is a long-period system
(25d), and relatively X-ray luminous. We propose to obtain 8 HETGS spectra
sampled several times during 2-3 rotations. Each exposure will well expose strong
lines and also provide an integrated flux. Summed spectra will be used for
deriviation of emission measure and abundances. Both long and short-term
variability will be examined and correlated with activity diagnostics.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
22:53:02.30 +16:50:28.30 IM PEG ACIS-S HETG 25.00
===================================================================================
Proposal Number: 03200093
Proposal Title: X-RAYS FROM STARS AT THE FAR END OF THE MAIN SEQUENCE
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Abstract: ACIS observations and detection of HH2 has shown that these outflows
can generate X-rays when they strike the ISM. To increase the sample, we propose
to search for HH80/81 which should be more luminous but farther away..
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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18:19:06.06 -20:51:55.22 HH80/81 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03200086
Proposal Title: HIGH-RESOLUTION SPECTRA OF T TAURI STARS
PI: STEPHEN MURRAY
Subject Category: NORMAL STARS AND WD
Abstract: We request a 35 (to 100) ksec observation (depending upon actual target
approved) with the HETGS to characterize the corona of a young pre-main sequence
star by measuring density sensitive x-ray lines and estimating the mean coronal
density of the (presumed) emitting loop structures. In the cases of the fast
rotator targets (Speedy Mic or HD 283572), we also expect to be able to estimate
the radial extent of the coronal structure by the detecting possible broadening
of the emitted lines. (Our simulation for HD 283572 suggests we may see this
effect for it and, even more likely, for Speedy Mic). By combining density and
the radial extent estimates, we can gain a better picture of the corona of young
fast rotator stars. GTO Priority "B"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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20:47:45.00 -36:35:40.80 SPEEDY MIC ACIS-S HETG 35.00
20:47:45.00 -36:35:40.80 SPEEDY MIC ACIS-S HETG 35.00
===================================================================================
Proposal Number: 03200049
Proposal Title: AN X-RAY STUDY OF X-RAYS FROM THE BETA PIC SYSTEM
PI: GORDON GARMIRE
Subject Category: NORMAL STARS AND WD
Abstract: Search for X-rays from possible planets around Beta Pic displaced from
Beta Pic itself.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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05:47:17.00 -51:03:59.40 BETA PIC ACIS-S NONE 10.00
===================================================================================
Proposal Number: 03200161
Proposal Title: A HIGH-RESOLUTION STUDY OF THE ACTIVE BINARY SYSTEM V824 ARA
PI: STEPHEN DRAKE
Subject Category: NORMAL STARS AND WD
Abstract: We propose to observe the active G5+K0 dwarf binary system V824 Ara (HD
155555), a very young (zero-age main-sequence or pre-main sequence) system with a
1.68 day orbital period, using the Chandra ACIS-S/HETG instrument. V824 Ara is a
synchronized binary similar in age to the prototype young single K dwarf AB Dor.
We will study the X-ray spectrum, both integrated over the whole exposure and as
a function of orbital/rotational phase and overall emission level. We will use
these spectra to infer the coronal temperature structure or DEM, and elemental
abundances. We will compare these coronal properties to those of evolved active
binaries (e.g., AR Lac), and also to those of AB Dor and similar young stars, to
see if there are discernible differences due to binarity and evolutionary stage.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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17:17:25.50 -66:57:03.00 V824 ARA ACIS-S HETG 100.00
===================================================================================
Proposal Number: 03200170
Proposal Title: HARD X-RAY EMISSION FROM THE CLASS I AND CLASS 0 OUTFLOW SOURCES
IN L1630
PI: THEODORE SIMON
Subject Category: NORMAL STARS AND WD
Abstract: The L1630 dark cloud contains three very rare Class 0 and at least six
Class I protostars. Several of them are tightly clustered around HH 24-26, a site
of molecular jets and a luminous but unresolved ASCA X-ray source. We propose to
image this region for 70 ks with the ACIS-S in order to (a) search for the onset
of X-ray emission in the Class 0 stars, (b) perform precise astrometry of the
X-ray emission of the Class I stars, and (c) from spectrometry of the Class I
sources, derive spectral parameters of their associated X-ray sources. Our goal
is to establish an evolutionary progression in X-ray properties within a single
cloud and thus explore the relationship between protostellar X rays, accretion
disks, magnetically collimated jets, and large-scale molecular outflows.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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05:46:08.40 -00:11:52.00 HH 24-26 ACIS-S NONE 70.00
===================================================================================
Proposal Number: 03200178
Proposal Title: THE LOW-MASS POPULATION OF NGC2264 AND ITS CORONAL PROPERTIES.
PI: SALVATORE SCIORTINO
Subject Category: NORMAL STARS AND WD
Abstract: We propose to perform a Chandra ACIS-I 100 ks observation of the star
forming region NGC 2264 (in Monoceros), achieving an unprecedent sensitivity of
fx ~ 5e-16 erg cm-2 s-1 (0.1-4 kev), or Lx ~ 4e28 erg s-1 (for the commonly
assumed distance of 760 pc). This will allow us to detect more than 85% of NGC
2264 low-mass members at least down to 0.1 Msun and a sizable fraction of even
lower mass members making possible: 1) to derive a reliable Initial Mass Function
(IMF) at the very low-mass end, 2) to investigate the role of magnetic fields in
the formation process and resulting IMF, 3) to test the coronal emission level of
young brown dwarfs, 4) to study the relation between coronal emission level and
PMS evolution during the first 3-10 millon year of stellar lifetime.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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06:40:58.10 +09:34:00.40 NGC 2264 ACIS-I NONE 100.00
===================================================================================
Proposal Number: 03200188
Proposal Title: ON THE ORIGIN OF THE X-RAY EMISSION IN LATE B-TYPE STARS
PI: NURIA HUELAMO
Subject Category: NORMAL STARS AND WD
Abstract: We propose for Chandra observations of X-ray emitting late B-type
stars. Because they are (theoretically) not expected to emit X-rays, their X-ray
detections have been attributed to unresolved late-type, magnetically active
stars. The aim of this study is to resolve close binary systems comprised of late
B-type stars and visual late-type companions, in order to identify the X-ray
emitter. The binary separations are between (1-8)'', i.e. well resolvable by
Chandra but not with previous instruments. If we found that X-rays are always
emitted by the late-type companions, it can be taken as evidence against
intrinsic X-ray emission from late B-type stars. If not, it would indicate that
these stars could be intrinsic X-ray emitters and stellar theories may have to be
revised.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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00:20:39.00 -69:37:29.70 HD1685 ACIS-I NONE 2.40
14:08:51.90 -43:28:14.80 HD123445 ACIS-I NONE 2.30
15:08:12.10 -40:35:02.10 HD133880 ACIS-I NONE 2.40
18:31:22.40 -62:16:41.90 HD169978 ACIS-I NONE 2.40
===================================================================================
Proposal Number: 03200237
Proposal Title: UNDERSTANDING THE ENGINE OF GROWTH IN PLANETARY NEBULAE
PI: JOEL KASTNER
Subject Category: NORMAL STARS AND WD
Abstract: We propose a survey of X-ray emission from planetary nebulae (PNs) that
builds on our previous Chandra discoveries of extended X-ray emission from PNs.
The proposed program, consisting of Chandra/ACIS observations of a sample of
well-studied, representative objects, has the potential to firmly establish
extended X-ray emission as a defining characteristic of the class of young,
molecule-rich PNs. By enabling the investigation of the morphology and evolution
of X-ray emission in PNs and the determination of physical conditions that are
otherwise inaccessible to study in these nebulae, these observations will provide
stringent tests of contemporary theories of PN formation and evolution.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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07:37:18.60 -09:38:48.00 M 1-16 ACIS-S NONE 50.00
16:17:12.60 -51:59:08.00 MZ 3 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03200240
Proposal Title: CORONAL EVOLUTION IN SINGLE GIANTS WITH CHANDRA LETGS X-RAY
SPECTROSCOPY
PI: JURGEN SCHMITT
Subject Category: NORMAL STARS AND WD
Abstract: We propose to obtain high resolution Chandra LETGS spectra of the three
single giants 24 UMa, $\beta$ Cet and 39 Cet. These stars are located at
strategic places in the HR-diagram covering the mass range between 1.6 - 3 solar
masses. The data will be sensitive enough to carry out detailed plasma
diagnostics of the coronae of evolved stars. Density diagnostics, differential
emission measure construction and abundance analysis will be carried out. A
comparison to photospheric abundances will be performed since $beta$ Cet has
solar abundances, while the other target stars do not. The three target stars are
the only single giants within practical reach of the Chandra LETGS and will allow
us to study the influence of stellar mass on activity among giant stars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:43:35.30 -17:59:12.00 BETA CETI HRC-S LETG 110.00
===================================================================================
Proposal Number: 03200289
Proposal Title: THE AGE-ROTATION-ACTIVITY RELATION IN LATE-TYPE STARS BETWEEN
~1-10 MYR
PI: JOHN STAUFFER
Subject Category: NORMAL STARS AND WD
Abstract: We propose to conduct a fundamental census of X-ray emission from stars
in Orion and NGC 2264 for which we have a wealth of supporting multi-wavelength
data. This will allow us to investigate a wide variety of scientific questions.
The most important scientific goal of this study is investigating the
relationship between age, rotation, and X-ray activity for late-type stars
ranging in age from ~1-10 Myr. Understanding the X-ray environment of young stars
and how rotation is related to X-ray flux has direct implications for the
chemical and dynamical evolution of protoplanetary disks, and, consequently, for
planet formation.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:35:05.60 -05:41:04.70 ONC FLANKING FIELD S ACIS-I NONE 50.00
05:35:19.10 -04:48:31.40 ONC FLANKING FIELD N ACIS-I NONE 50.00
06:40:48.00 +09:50:60.00 NGC 2264 ACIS-I NONE 50.00
===================================================================================
Proposal Number: 03200359
Proposal Title: STELLAR CORONAE AT THE BOTTOM OF THE MAIN SEQUENCE: A
MULTI-WAVELENGTH STUDY
PI: ROBERT RUTLEDGE
Subject Category: NORMAL STARS AND WD
Abstract: It is well established that coronal activity dramatically decreases at
the bottom of the main sequence. This was expected: the transition near type M2.5
to fully convective interiors gave impetus for the search for a decline in
coronal activity. However, most of the decline occurs later than this transition.
Even there, X-ray, H-alpha, and radio flaring continues to at least as late as
the brown dwarf LP 944-20 (M9.5), and perhaps is the only means of releasing
magnetic energy from an apparently still active dynamo. This leaves us with the
question: what is supressing the persistent coronal emission, even as the
magnetic flares continue? We will address this question by observing low-mass
stars from M6 to L6 in X-ray, H-alpha, and radio wavelengths.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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00:36:16.00 +18:21:10.00 2MASSW0036+18 ACIS-S NONE 22.00
15:07:48.00 -16:27:38.00 2MASSW1507-16 ACIS-S NONE 28.00
===================================================================================
Proposal Number: 03200381
Proposal Title: STAR FORMATION IN QUIESCENT GIANT MOLECULAR CLOUDS
PI: ERIC FEIGELSON
Subject Category: NORMAL STARS AND WD
Abstract: Most stars are formed in rich stellar clusters within giant molecular
clouds (GMCs). A wide range in GMC star formation efficiencies exists -- half of
GMCs do not have even a single O star. The reason for GMC quiescence is poorly
understood. We propose a Chandra ACIS observation of the prototype quiescent GMC,
G 216-2.5 or Maddalena's Cloud, which will have extraordinary sensitivity to its
present and past star formation rate. This is achieved because pre-main sequence
stars of all masses and a wide range of ages have greatly enhanced X-ray
emission. Possible outcomes are a episodic star formation, a truncated IMF, or
true quiescence. Any of these results will have significant implications for star
formation in the Galaxy.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
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06:49:05.50 -04:33:50.00 MADDALENA'S CLOUD ACIS-I NONE 30.00
===================================================================================
Proposal Number: 03200497
Proposal Title: BURIED ALIVE IN THE CORONAL GRAVEYARD?!
PI: THOMAS AYRES
Subject Category: NORMAL STARS AND WD
Abstract: We propose 20 ks pointings with Chandra HRC-I to obtain detections of 3
red giants in the depths of the "coronal graveyard." Stellar coronal activity is
important to the Sun-Earth connection, to the fate of primitive planetary
atmospheres, and to a broad reaching set of magnetic phenomena in many cosmic
environments. Understanding the activity, and its evolution, therefore is a key
objective in astrophysics. The birth of magnetic activity in young stars is
well-studied; the death of coronae in highly evolved stars is not. Our program
ultimately will test the hypothesis that significant coronal activity persists on
the red giants, but smothered beneath a "cool absorber" in the chromospheric
envelope. Such activity might be the long-sought initiator of red giant winds.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:35:55.20 +16:30:33.00 ALPHA TAURI HRC-I NONE 20.00
14:15:39.60 +19:10:57.00 ALPHA BOOTIS HRC-I NONE 20.00
===================================================================================
Proposal Number: 03200546
Proposal Title: HIGH ENERGY EMISSION FROM THE YOUNG MASSIVE CLUSTER RCW 38
PI: SCOTT WOLK
Subject Category: NORMAL STARS AND WD
Abstract: Taking advantage of Chandra's unique capabilities, we propose to study
the youngest, most embedded, massive cluster studied to date in X-rays - RCW 38.
The immediate goals of this project are the identification of the embedded PMS
stellar population, the investigation of the X-ray properties of the individual
class 0-III sources (~10 class 0 & I protostars) and the derivation of a XLF for
an extremely young (~0.5 Myr) massive cluster. We will derive the gas-to-dust
ratio and its variations towards hundreds of lines of sight across the cluster.
Complementary NIR data already taken with the VLT, which probe approximately the
same cloud depths, allow an unique multi-wavelength description of a massive star
formation episode and its consequences to the surrounding interstellar medium.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:59:19.20 -47:30:22.00 RCW 38 ACIS-I NONE 100.00
===================================================================================
Proposal Number: 03200558
Proposal Title: DENSITY STRATIFICATION OF THE VERY HOT CORONA OF YY MENSAE
PI: MANUEL GUEDEL
Subject Category: NORMAL STARS AND WD
Abstract: Chandra HETGS observations give access to a number of He-like line
triplets that are sensitive to the density of hot coronal plasma. The present
proposal requests observing time on an outstanding single star that has revealed
an extremely hot and luminous corona. We aim at measuring the density structure
of its corona together with its anomalous abundances. The target, YY Mensae,
reveals a corona in which 90 percent of the emission measure resides at 30-40 MK.
It has been suggested that such coronae are heated by statistical flares. A
thorough spectroscopic study of this object could decide on whether its corona is
indeed composed of numerous high-density compact flaring loops. The emission
measure distribution will be studied to investigate whether it is generated by
frequent flaring.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:58:17.90 -75:16:38.00 YY MEN, HD 32918 ACIS-S HETG 90.00
===================================================================================
Proposal Number: 03200561
Proposal Title: HEAVY ION TRANSPORT: MULTI-TEMPERATURE ABUNDANCE STUDIES OF THE
ACTIVE RS CVN LAMBDA AND
PI: NANCY BRICKHOUSE
Subject Category: NORMAL STARS AND WD
Abstract: We propose a 100 ks observation with Chandra LETG to conduct a
comprehensive study of the coronal abundances of the active binary Lambda And.
Chandra HETG observations of Lambda And indicate that the Ne/Fe abundance at high
temperature (10 million K) is about four times larger than the abundance at lower
coronal temperature (1 million) K. LETG offers unique coverage of intermediate
ionization states of many elements, as well as high resolution to isolate weaker
lines from ions previously unresolved by EUVE. Determining the abundance patterns
under different physical conditions in the same system will constrain models of
acceleration, heating, diffusion, and gravitational settling. We will measure
abundances for C, N, O, Ne, Mg, Si, S, and Fe across a broad temperature range.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
23:37:33.80 +46:27:29.30 LAMBDA AND HRC-S LETG 50.00
23:37:33.80 +46:27:29.30 LAMBDA AND HRC-S LETG 50.00
===================================================================================
Proposal Number: 03200569
Proposal Title: X-RAY DOPPLER IMAGING OF CONTACT BINARIES: THE PARTIALLY
ECLIPSING VW CEP
PI: NANCY BRICKHOUSE
Subject Category: NORMAL STARS AND WD
Abstract: Chandra LETG observations of the X-ray bright contact binary VW Cep
will provide diagnostics of coronal structures under the extreme conditions of
rapid rotation. Optical Doppler images of VW Cep have recently provided the first
evidence for large polar spots on a contact binary, similar to polar spots
observed on the less rapidly rotating RS CVn systems. We propose to exploit the
unique spectral resolution of the LETG at long wavelengths to search for Doppler
line shifts from the orbiting poles. Phase-resolved emission line intensity
diagnostics for temperature, density, and abundances will complement the velocity
measurements. This test for localized activity could definitively establish a new
coronal phenomenon in fast rotators.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:37:21.50 +75:36:01.50 VW CEP HRC-S LETG 100.00
===================================================================================
Proposal Number: 03200598
Proposal Title: X-RAYS FROM BROWN DWARFS IN THE SIGMA ORIONIS CLUSTER
PI: SCOTT WOLK
Subject Category: NORMAL STARS AND WD
Abstract: We propose a deep HRC-I observation of the young star forming region
around Sigma Orionis to detect X--ray emission from young brown dwarfs (BDs)
which have been discovered there. We will also measure of the X--ray luminosity
of a well understood sample of hundreds of PMS stars. Detections of BDs by
Chandra have been sparse, this is, in part, because the detector of choice for
clusters, ACIS-I, has very low effective area where BDs are bright, below 400 eV.
The Sigma Ori cluster is uniquely suited to this study; it spans different
stellar interior conditions, almost 3 orders of magnitude in mass, it is
relatively close, almost dust free (5% of the ONC), the proper age to have a good
mix of stars with and without disks and we have measured its mass function well
below the BD limit.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:38:44.80 -02:36:00.20 SIGMA ORIONIS HRC-I NONE 100.00
===================================================================================
Proposal Number: 03200602
Proposal Title: STELLAR WINDS FROM DME STARS
PI: BRADFORD WARGELIN
Subject Category: NORMAL STARS AND WD
Abstract: Despite the fact that the most stars have low mass and lie on the main
sequence, we know virtually nothing about their stellar winds. Existing
measurements of stellar winds extend down only to a few times 1e-10 M_solar/yr
and only apply to high-mass stars and red giants and supergiants. With Chandra's
unparalleled imaging resolution, high sensitivity, and energy resolution, winds
from nearby dwarf stars are now detectable via their X-ray emission from the
charge exchange of stellar wind ions with neutral gas in the ISM. Our proposed
observations of dwarf M flare stars will be capable of imaging stellar winds
comparable to those of the Sun (mass loss rate 2e-14 M_solar/yr), and will
provide information on wind and magnetosphere geometry, ion composition, and mass
loss rates.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:49:49.49 -23:50:11.00 ROSS 154 ACIS-S NONE 60.00
===================================================================================
Proposal Number: 03200661
Proposal Title: X-RAY EVOLUTION OF ACCRETING PROTOSTARS
PI: PHILIPPE ANDRE'
Subject Category: NORMAL STARS AND WD
Abstract: Recent developments have shown that the environment of protostars plays
an important role for their structure and evolution: in dense clusters like
Ophiuchus they have relatively compact envelopes and a rapidly decreasing
accretion rate; in dispersed regions like Taurus they have the extended envelopes
and constant accretion rates considered by the standard model of star formation.
We want to investigate for the first time the corresponding evolution of the
X-ray emission (over time scales ~10^4-10^5 yrs) in Taurus, and search whether
protostellar structure, evolution, and X-ray emission are related. Such a
relation could be the result of feedback effects of X-rays on accretion and
outflow acceleration.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
04:21:56.90 +15:29:46.00 IRAM04191 ACIS-I NONE 20.00
04:39:53.90 +26:03:10.00 L1527 ACIS-I NONE 13.00
04:39:53.90 +26:03:10.00 L1527 ACIS-I NONE 20.00
===================================================================================
Proposal Number: 03200663
Proposal Title: A TALE OF TWO G STARS
PI: THOMAS AYRES
Subject Category: NORMAL STARS AND WD
Abstract: High-quality HETGS exposures of key coronal stars are presenting a
unique, novel view of some of the most ubiquitous high-energy phenomena in the
galaxy; and taking crucial steps toward making X-ray spectroscopy an
indispensable remote-sensing tool for Astronomy. We will focus on the influence
of stellar surface gravity by adding to our ongoing program the active G dwarf
Chi1 Orionis (G0V) and the active G giant 24 Ursae Majoris (G4III). Chandra
transmission grating spectroscopy offers a new way to determine temperatures and
densities in the hot outer atmospheres of cool stars, probe chemical
fractionation processes, and explore plasma dynamics. Our program will add to the
Chandra Emission Line Project and help interpret lower-res XMM-Newton/RGS spectra
of fainter stars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:34:28.80 +69:49:49.00 24 URSAE MAJORIS ACIS-S HETG 33.52
09:34:28.80 +69:49:49.00 24 URSAE MAJORIS ACIS-S HETG 50.00
09:34:28.80 +69:49:49.00 24 URSAE MAJORIS ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03200659
Proposal Title: A CHANDRA STUDY OF THE PLANETARY NEBULA NGC 246
PI: ANDREW SZENTGYORGYI
Subject Category: NORMAL STARS AND WD
Abstract: We propose ACIS observations of the planetary nebula NCG 246 to search
for nebular emission from thermal gas at temperatures between 300,000 and 1
million K. In models of wind-blown bubbles, the fast wind from the central star
(3500 km/s for NGC 246) shocks when it encounters the high pressure imposed by
the external shell. New images of NGC 246 in [Ne V] show an exceptionally bright
structure surrounding a faint central region, possibly a tracer of the boundary
of the wind-blown bubble. Since the central star has Wolf-Rayet abundances, the
CNO-processed gas is expected to have an enormous cooling rate. ACIS images and
spectra will constrain the temperature, composition, and density of the X-ray
emitting gas inside [Ne V] boundary.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:47:03.00 -11:52:20.00 NGC 246 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03200672
Proposal Title: STAR FORMATION AND MYSTERIOUS HARD X-RAY EMISSION IN THE VERY
YOUNG HII REGION, TRIFID NEBULA
PI: JEONGHEE RHO
Subject Category: NORMAL STARS AND WD
Abstract: The Trifid Nebula (M~20) is one of the best-known HII regions, ionized
by a single O7.5 star, HD 164492. The Trifid was rediscovered as a dynamic,
"pre-Orion" star forming region containing young stars undergoing violent mass
ejections. The ROSAT image revealed strong emission from HD 164492 and a dozen
X-ray sources. ASCA spectra of the O star show an unexpectedly hot (3 keV)
component in addition to a cooler component from the O star atmosphere. We
propose an ACIS-S observation of the Trifid Nebula for 60 ks. The sub arcsec
image will resolve the O star from its immediate environment, and likely detect
hundreds of low mass objects. We will examine the high-energy interaction between
the wind from the O star and the dense ISM.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:02:30.31 -23:01:29.40 TRIFID NEBULA ACIS-I NONE 60.00
===================================================================================
Proposal Number: 03200677
Proposal Title: PHASE-RESOLVED SPECTROSCOPY OF THETA-1 ORIONIS C (O7 V)
PI: MARC GAGNE
Subject Category: NORMAL STARS AND WD
Abstract: We propose to obtain phase-constrained HETG spectra of the candidate
magnetic O star theta-1 Orionis C, the ionizing source of the Orion Nebula.
theta-1 Ori C exhibits remarkable 15.4-day periodic X-ray, UV and optical line
variations thought to arise from the interaction of a radiatively driven O-star
wind with a magnetosphere. New MHD calculations predict that strong X-ray shocks
and rotational modulation occur if the magnetic poles are inclined with respect
to the rotation axis. HEG and MEG spectra obtained at X-ray min (phase 0.5) and
max (phase 0.0) along with archival spectra obtained at phases 0.82 and 0.37 will
be used to measure line ratios, line profiles and phase-dependent temperatures,
abundances, and absorption to test magnetic wind shock emission models.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
05:35:16.50 -05:23:23.10 HD 37022 ACIS-S HETG 50.00
05:35:16.50 -05:23:23.10 HD 37022 ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03200678
Proposal Title: RESOLVING THE MASSIVE OB CORE OF THE YOUNG CLUSTER NGC 6193
PI: STEPHEN SKINNER
Subject Category: NORMAL STARS AND WD
Abstract: Located at the center of the young open cluster NGC 6193 are two nearly
identical O stars HD 150135 (O6V) and HD 150136 (O5 III-V), separated by only 10
arc-secs. This pair was detected as a bright variable X-ray source by ROSAT, but
was not resolved. We propose to use ACIS-S/HETG to resolve the pair and determine
the origin of the X-ray emission. The HETG spectrum will allow us to discriminate
between X-rays from radiative shocks in the winds of one or both O stars and
colliding wind shock emission in HD 150136, which is known to be a O + O
spectroscopic binary. The sensitive ACIS-S image will provide the first accurate
X-ray census of the massive OB concentration at the center of NGC 6193.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:41:20.40 -48:45:46.60 HD 150136 ACIS-S HETG 95.00
===================================================================================
Proposal Number: 03200698
Proposal Title: CORONAL DYNAMICS AND THE COMPLETE FLARE ENERGY BUDGET FOR THE M
DWARF FLARE STAR AD LEO
PI: ALEXANDER BROWN
Subject Category: NORMAL STARS AND WD
Abstract: We propose coordinated Chandra-HETGS (110 ksec), HST-STIS (6 orbits),
and FUSE (50 ksec) observations of the the dMe flare star AD Leo to accurately
measure for the first time the complete energy budget for coronal flares. FUV
observations of the Fe XVIII 975 A and Fe XXI 1354 A coronal forbidden lines are
needed from FUSE and STIS to determine the dynamical energy losses of the flares.
HETGS spectra will be used to measure the temporal changes in the coronal
emission measure, temperature, density, and elemental abundances. AD Leo is one
of the brightest dMe stars in X-rays and flaring rate data suggests that we
should see about 10 moderate (factor of a few) and one large (factor of 10-20
enhancement) flares in a 30 hour observation.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:19:36.22 +19:52:11.60 AD_LEO ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03200704
Proposal Title: CHANDRA HETGS OBSERVATIONS OF THE RAPIDLY ROTATING OE STAR ZETA
OPH
PI: WAYNE WALDRON
Subject Category: NORMAL STARS AND WD
Abstract: We propose a 92 ks Chandra HETG observation of the O 9.5V(e) star Zeta
Oph. Several very interesting results have emerged from HETG observations of O
stars, e.g., not only are the X-rays distributed throughout the stellar wind, we
also find X-ray emission from high ion stages (S XV and Si XIII) at the base of
the wind. These results were determined from O stars with moderately thick winds.
To probe near surface X-ray emission characteristics we need high resolution
spectra of an O star in an optically thin environment. Zeta Oph is the ideal
target. It is a well know X-ray source, relatively bright in X-rays, has an
optically thin windto all HETG X-rays, and is one of the most rapidly rotating O
stars, showing Be characteristics, which by itself makes it a very interesting
target.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:37:09.40 -10:34:02.00 ZETA OPH ACIS-S HETG 40.00
16:37:09.40 -10:34:02.00 ZETA OPH ACIS-S HETG 52.00
===================================================================================
Proposal Number: 03200743
Proposal Title: OBSERVING FAST AND MASSIVE HOT STAR WINDS IN THE CYG OB2
ASSOCIATION
PI: JOSEPH CASSINELLI
Subject Category: NORMAL STARS AND WD
Abstract: We will use HETG spectra of the very luminous star Cyg OB2 8a to
investigate the effects of higher speeds and denser winds on resolved X-ray line
profiles. Higher ion stages and a greater attenuation of line emission from the
far side of the star are expected. These observations could explain the anomalous
broadening of X-ray emission lines in Chandra spectra of other O-stars. We can
simultaneously obtain another HETG spectrum and several ACIS spectra of other
early-type stars in the association.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
20:33:15.10 +41:18:50.50 CYG OB2 8A ACIS-S HETG 70.00
===================================================================================
Proposal Number: 03200765
Proposal Title: TRACING THE CHRONICLE OF MASSIVE YOUNG STARS IN A GIANT
MOLECULAR CLOUD NGC 6334
PI: YU-ICHIRO EZOE
Subject Category: NORMAL STARS AND WD
Abstract: We propose 40 ksec X 2 pointing observations of NGC 6334 with the
Chandra ACIS-I. It is one of the most luminous giant molecular clouds in infrared
and X-rays, and contains many active massive star-forming regions at different
stages of stellar evolution. With ASCA, we found luminous high-temperature X-ray
emission from these regions. With Chandra, we can resolve young stellar objects
at various evolution stages simultaneously, and study the X-ray properties of
young stellar objects as a function of the evolutionary stage.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:20:01.00 -35:56:07.00 NGC 6334 REGION 2 ACIS-I NONE 40.00
17:20:54.00 -35:47:04.00 NGC 6334 REGION 1 ACIS-I NONE 40.00
===================================================================================
Proposal Number: 03200773
Proposal Title: HIGH-RESOLUTION X-RAY SPECTROSCOPY OF BETA CRUCIS: A NEARBY HOT
STAR WITH A HIGH X-RAY COUNT RATE
PI: DAVID COHEN
Subject Category: NORMAL STARS AND WD
Abstract: We propose to use HETG spectroscopy to diagnose the bulk motions and
the temperature and density distributions in the hot plasma on the nearby
early-type star beta Cru. We will use these data to constrain our models of
hot-star X-ray production: the intrinsic wind shock (IWS) model as well as the
magnetically confined wind shock (MCWS) model. Beta Cru is the brightest normal
hot star not already observed with Chandra, and will provide a high
signal-to-noise HETG spectrum. We will make detailed comparisons with the HETG
data from the several other hot stars observed with this instrument. Comparisons
with the anomalous star, tau Sco, which is of a very similar spectral type to
beta Cru will be especially illuminating.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:47:43.30 -59:41:19.50 BETA CRU ACIS-S HETG 90.00
===================================================================================
Proposal Number: 03200776
Proposal Title: INVESTIGATING COLLIDING WINDS AND MAGNETISED STARS IN YOUNG
PLANETARY NEBULAE IMAGED WITH HST
PI: RAGHVENDRA SAHAI
Subject Category: NORMAL STARS AND WD
Abstract: The biggest stumbling blocks to progress in our understanding of the
death of intermediate-mass stars and the accompanying formation of planetary
nebulae (PNs), are the complex stellar-wind episodes and the interactions between
them which occur during the post-AGB phase. We propose ACIS-S observations of 5
young PNs with very fast outflows for which HST emission-line images are
available, in order to directly probe the very hot (10$^{7-8}$K) shocked gas
resulting from the most recent wind-wind interactions in these objects, as well
as compact X-ray emission from the (possibly) magnetised central stars. A
comparative analysis of the CXO and HST data on these PNs, supplemented by
detailed modelling, will be invaluable in solving the mystery of how PNs are
formed and shaped.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
13:39:34.70 -67:22:51.00 MYCN 18 ACIS-S NONE 40.00
14:11:52.20 -51:26:24.00 HEN2-104 ACIS-S NONE 20.00
17:05:37.70 -10:08:32.50 M 2-9 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03200352
Proposal Title: STUDY OF THE X-RAY EMISSION MECHANISM AND ITS EVOLUTION OF BROWN
DWARFS
PI: KATSUJI KOYAMA
Subject Category: NORMAL STARS AND WD
Abstract: We propose ACIS-S observations on two intermediate-age (10-600 Myr)
brown dwarfs, PC 0025+0447 and 296A. We will establish a unified picture of
X-rays from brown dwarfs, together with the recent discoveries of X-rays from
young (~1 Myr) and old (~1 Gyr) brown dwarfs. The scientific objectives of our
Chandra observations are (1) to search for any correlations of X-rays to other
physical parameters; age, H alpha intensity, bolometric luminosity, and
circumstellar disk, and (2) to extend the X-ray detection toward a lower mass
star (M9.5), which is one step to a big challenge of searching for young Jupiter
type planets using X-rays.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:27:42.00 +05:03:41.00 PC 0025+0447 ACIS-S NONE 70.00
===================================================================================
Proposal Number: 03200753
Proposal Title: PROBING WIND-WIND INTERACTIONS AND STELLAR MAGNETIC FIELDS IN
PRE-PLANETARY NEBULAE
PI: RAGHVENDRA SAHAI
Subject Category: NORMAL STARS AND WD
Abstract: Preplanetary nebulae (PPNs) - the progenitors of planetary nebulae
(PNs) - hold the key to our understanding of the very late stages of stellar
evolution. Recent HST studies show that the fast wind-slow wind interaction
process believed to produce diffuse X-ray emission from PNs, must already be
active in PPNs. Sensitive observations for X-ray emission in PPNs, however, do
not exist. We propose ACIS-S observations of 4 well-studied PPNs with very fast
outflows in order to directly probe (a) the very hot (10$^{7-8}$K) shocked gas
which must result from the interaction, and (b) the presence of strong stellar
magnetic fields which may be responsible for collimating the fast outflows. These
data will be invaluable in testing theoretical models of X-ray emission in PPNs
and PNs.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:45:14.20 -17:56:47.00 HEN3-1475 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03200591
Proposal Title: X-RAY INDUCED CHEMISTRY IN PROTOSTARS
PI: THIERRY MONTMERLE
Subject Category: NORMAL STARS AND WD
Abstract: The envelopes of protostars are the subject of intense research in the
mm domain because of their cold temperatures (T ~ 10-30 K). However, for some
moderately luminous protostars (Lbol ~ 10 Lsun) there is evidence for enhanced
heating and ionization in their interiors (T ~ 300 K), from CO+, SO+ and FIR
high-J CO studies. We have developed a model to explain these enhancements in
terms of internal irradiation by a central luminous X-ray source (Lx ~ 10^31 erg
s-1, Tx ~ 3 keV), quite comparable with existing X-ray detections of protostars.
We propose for the first time a "live" study of the chemical interactions between
X-rays and circumstellar envelopes, by searching for X-ray emission from three
"chemically active" young protostars.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:32:22.70 -24:28:32.00 IRAS16293 ACIS-I NONE 30.00
===================================================================================
Proposal Number: 04200312
Proposal Title: UNVEILING ETA CAR: CHANDRA OBSERVATIONS DURING THE 2003.5 EVENT
PI: MICHAEL CORCORAN
Subject Category: NORMAL STARS AND WD
Abstract: Understanding the supermassive star Eta Car is important for a variety
of topics: the formation and evolution of extremely massive stars and their
influence on their environments. Eta Car has been a mystery since its giant
eruption in the 1840s. A possible key to the puzzle is the identification of
periodic changes in some near IR emission lines, and the discovery of repeatable
X-ray eclipses. The next X-ray eclipse will occur during AO4, and we propose to
use HETG to observe the variations in the spectral and spatial distribution of
the emission during this event. In conjunction with scheduled HST/STIS, INTEGRAL,
IR and optical spectroscopy, and radio observations, these HETG observation
provide key information which may finally help us solve the riddle of this star.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
10:45:03.60 -59:41:04.30 ETA CARINAE ACIS-S HETG 100.00
***********************************************************************************
WD BINARIES AND CV
--------------------------------------------------
===================================================================================
Proposal Number: 03300018
Proposal Title: FLARES, MAGNETIC RECONNECTIONS AND ACCRETION DISK VISCOSITY
PI: WILLIAM WELSH
Subject Category: WD BINARIES AND CV
Abstract: Accretion disks are invoked to explain a host of astrophysical
phenomena, from protostellar objects to AGN. Yet the mechanism allowing accretion
disks to operate are completely unknown. This proposal seeks to observe the
``smoking gun'' signature of magnetically-driven viscosity in accretion disks.
Magnetically-induced viscosity is a plausible and generally accepted hypothesis,
but it is completely untested. These data will establish the importance of
magnetic fields in accretion disks. Because of its known flaring properites, we
will observe the accretion disk in EM Cyg simulataneously with STIS/FUV-MAMA and
CHANDRA. The simultaneous X-rays are absolutely necessary for the unambiguous
detection of accretion disk magnetic reconnection flares.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:38:40.10 +30:30:28.00 EM CYG ACIS-S NONE 25.00
19:38:40.10 +30:30:28.00 EM CYG ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03300064
Proposal Title: RESOLVING THE COMPACT BINARIES IN NGC 6397
PI: STEPHEN MURRAY
Subject Category: WD BINARIES AND CV
Abstract: We propose to obtain two moderately deep ACIS-S observations (25ksec
each) of the globular cluster NGC 6397 in order to resolve and identify the
population of compact binaries we have discovered in our cycle 1 ACIS-I
observation. Each exposure will approximately match the counts obtained for each
of the 14 sources found within 10arcsec of the cluster center, allowing the
spectral variability to be measured for the bright sources (>500 cts) and total
flux variability for the faintest (3ct) sources. This will enable the population
of millisecond pulsars (MSPs) to be distinguished from the cataclysmic variables
(CVs) and quiescent low mass x-ray binaries (qLMXBs), and will also enable a deep
search for flaring main sequence binaries. GTO Priority "A"
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:40:42.00 -53:40:27.90 NGC6397 ACIS-S NONE 30.00
17:40:42.00 -53:40:27.90 NGC6397 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03300181
Proposal Title: BOUNDARY LAYERS AND HOT FLOWS IN QUIESCENT DWARF NOVAE
PI: JOHN RAYMOND
Subject Category: WD BINARIES AND CV
Abstract: The X-ray emitting boundary layers of quiescent dwarf novae offer a
rare opportunity to probe the thermal and dynamical structure of the flow in the
vicinity of the white dwarf via detailed spectroscopic diagnostics. Using an
extension of the Raymond-Smith code able to compute the detailed continuum and
line emission spectrum expected from a hot flow with arbitrary temperature and
density profiles, we are in a position to carry out such diagnostics. We propose
to observe the promising candidate WX Hyi with the Chandra X-ray Observatory and
test the various theoretical models of boundary layers and hot accretion flows
developed in this context.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
02:09:50.80 -63:18:40.30 WX HYI ACIS-S HETG 50.00
02:09:50.80 -63:18:40.30 WX HYI ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03300197
Proposal Title: ACCRETION IN HIGH DENSITY AND TEMPERATURE CONDITIONS (V426 OPH)
PI: PAULA SZKODY
Subject Category: WD BINARIES AND CV
Abstract: We will use HETG to observe the 0.4-10 keV spectrum of the bright, high
mass transfer rate, disk accreting cataclysmic variable V426 Oph, which is known
from Ginga, ASCA data to have a strong Fe complex as well as other emission lines
in the 0.5-2 keV region. These lines provide information on the correct T and
density, the photoionization/collisional processes and the abundances of the
plasma as it undergoes the transition from a 14-19 keV low density regime to the
atmosphere of an accreting 30,000K white dwarf. The velocity broadening of the
lines will provide insights into the rotation and location of the gas as it
follows its accretion path from the Keplerian disk to the slower rotating white
dwarf, possibly along magnetic field lines.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:07:51.70 +05:51:48.50 V426 OPH ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03300263
Proposal Title: MULTIWAVELENGTH TARGET OF OPPORTUNITY OBSERVATIONS OF A BRIGHT
NOVA IN OUTBURST
PI: SUMNER STARRFIELD
Subject Category: WD BINARIES AND CV
Abstract: We propose to obtain spectrophotometry with CHANDRA, plus ground based
optical and IR spectra of one bright nova in outburst. Our X-ray studies have
shown that X-rays are the best tool for studying the hot phase of the outburst.
In Cycle 1 we obtained spectra of V382 Vel and V1494 Aql. V382 Vel showed only an
emission line spectrum in our data while V1494 Aql evolved from an emission line
spectrum to that of a Super Soft Source (SSS). Observations of these phases
provided an opportunity to study the composition of the underlying white dwarf,
the lifetime of the TNR phase of the outburst, and the energy budget of the
explosion. More data on new novae is needed because the behavior of these two
novae was very different, which is expected from theory.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
IM Nor HRC-S LETG 25.00
IM Nor HRC-S LETG 25.00
15:39:26.50 -52:19:18.20 IM Nor ACIS-S NONE 5.00
===================================================================================
Proposal Number: 03300412
Proposal Title: THE HIGH RESOLUTION X-RAY SPECTRUM OF AM HERCULIS: PROBING THE
ACCRETION PROCESS
PI: ANDREW BEARDMORE
Subject Category: WD BINARIES AND CV
Abstract: We propose a 100ks Chandra HETG observation of the polar AM Herculis.
To ensure data is obtained when the source is in a high state we request a TOO
(or even an `anti-TOO') observation. With the good quality, high energy
resolution data this will provide, we be able to use the HEG to: (i) examine the
nature of the 6.4 keV fluorescence line in order to see if it has its origin in
reflection from the white dwarf surface or absorption in the pre-shock flow. (ii)
Measure the widths of the thermal Fe Kalpha lines in order to constrain the
importance of Compton broadening in this star. Also, using the MEG we will be
able to (iii) measure the line strengths of the lighter elements and estimate the
physical conditions in the post-shock region.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:16:13.33 +49:52:04.20 AM HERCULIS ACIS-S HETG 100.00
===================================================================================
Proposal Number: 03300437
Proposal Title: A UNIFORM STUDY OF GLOBULAR CLUSTER X--RAY SOURCES: THE KEYS TO
CLUSTER DYNAMICAL EVOLUTION
PI: WALTER LEWIN
Subject Category: WD BINARIES AND CV
Abstract: We propose to extend our ongoing studies of the dynamical evolution of
globular clusters by observing their populations of low-luminosity X-ray sources.
Many of these sources are binary systems (or have evolved from them) and hold the
key to the cluster's dynamical evolution. We propose observations of a variety of
clusters with widely different physical properties such as central concentration,
cluster size and mass, which are all key ingredients in the formation and
evolution of binaries. To make this study as uniform as possible, the clusters
will be observed to the same limiting luminosity. Numerical simulations with the
world's fastest computer will assist in the interpretation of our observational
data.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:18:33.80 +02:04:57.70 NGC 5904 ACIS-S NONE 45.00
17:01:12.60 -30:06:44.50 NGC 6266 ACIS-S NONE 63.00
17:27:44.30 -05:04:35.90 NGC 6366 ACIS-S NONE 24.00
===================================================================================
Proposal Number: 03300823
Proposal Title: RESOLVING THE COMPACT BINARY DISTRIBUTION IN THE CENTRAL HALF
ARCMIN OF THE COLLAPSED-CORE GLOBULAR CLUSTER M30
PI: HALDAN COHN
Subject Category: WD BINARIES AND CV
Abstract: The collapsed-core globular cluster M30 is a prime target for the study
of the formation and evolution of compact binaries in one of the densest
environments found in the Galaxy. ROSAT observations have detected X-ray emission
from the vicinity of the cluster core, that probably arises from a population of
low-Lx, compact binaries, including cataclysmic variables. Only Chandra can
resolve this emission into individual sources to study their properties and
spatial distribution. Grindlay et al (2001) have detected over 100 faint Chandra
sources in the dense cluster 47 Tuc. We propose a deep ACIS-S exposure, to be
used with our deep HST imaging of M30, to investigate the expected population of
compact binaries in the central half arcmin.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:40:22.00 -23:10:45.00 NGC 7099 ACIS-S NONE 50.00
===================================================================================
Proposal Number: 03300829
Proposal Title: CHANDRA GRATING SPECTROSCOPY OF DWARF NOVAE
PI: PETER WHEATLEY
Subject Category: WD BINARIES AND CV
Abstract: Dwarf novae are spectacular examples of accreting systems that have
formed the basis of much of our understanding of accretion disks, from AGN to
YSOs. Chandra grating observations have the power to resolve the temperature
structure of the X-ray bright boundary layer for the first time, both in the
optically-thin quiescent state and optically-thick outburst state, however only
two systems have been observed to date. Here we propose to observe SU~UMa and
VW~Hyi, the 2nd and 3rd brightest dwarf novae.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
08:12:28.20 +62:36:23.00 SU UMA ACIS-S HETG 25.00
08:12:28.20 +62:36:23.00 SU UMA ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03300850
Proposal Title: MULTIWAVELENGTH OBSERVATIONS OF V1494 AQL IN OUTBURST
PI: SUMNER STARRFIELD
Subject Category: WD BINARIES AND CV
Abstract: We propose 2 HRC-S+LETG followup observations of V1494 Aql which we
observed with CHANDRA as a TOO in Cycle 1. Our grating data show that it has
become a Super Soft Source (SSS) and an analysis of the light curve shows a 2500s
period. More grating data is necessary both to determine its evolution during the
SSS phase and to measure any changes in period. We also observed a factor of 6
rise in counts during the observation and further data could help to determine if
this were a common phenomenon. It is evolving slowly in the optical and should
still be bright in X-rays in Cycle 3. Analysis of the grating data will allow us
to study the composition of the ejecta, the lifetime of the TNR phase of the
outburst, and the energy budget of the explosion.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:23:05.30 +04:57:21.60 V1494 AQL HRC-S LETG 25.00
19:23:05.30 +04:57:21.60 V1494 AQL HRC-S LETG 25.00
===================================================================================
Proposal Number: 03300300
Proposal Title: MULTIWAVELENGTH STUDY OF THE GLOBULAR CLUSTER M28 (NGC~6626)
PI: WERNER BECKER
Subject Category: WD BINARIES AND CV
Abstract: We propose a 60 ks, ACIS-S observation of the globular cluster M28.
This medium deep exposure will clarify the nature of the apparently extended
X-ray emission at its core and establish the X-ray luminosity function of M28's
constituents down to 10^31 erg/s. In addition, the exposure will provide an
accurate, confusion-free spectrum of the millisecond pulsar PSR B1821-24 near the
center of M28, and spectra of various other X-ray sources in the globular cluster
we will detect. Furthermore, by referencing the Chandra-determined positions to
the very accurate radio position of PSR B1821-24 and the X-ray bright star HD
315622, we shall determine the absolute positions of identified sources to better
than 0.25\arcsec, greatly facilitating identifications studies in the optical and
radio band.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:24:32.00 -24:52:10.70 M28 ACIS-S NONE 13.33
18:24:32.00 -24:52:10.70 M28 ACIS-S NONE 13.33
18:24:32.00 -24:52:10.70 M28 ACIS-S NONE 13.33
===================================================================================
Proposal Number: 03308072
Proposal Title: TOO OBSERVATIONS OF THE RECURRENT NOVA IM NORMAE IN OUTBURST
PI: SUMNER STARRFIELD
Subject Category: WD BINARIES AND CV
Abstract: IM Nor is a Recurrent Nova (RN) discovered in outburst on 10 Jan 02. It
rose to V~7.7 on 16 Jan suggesting that it was caught at the beginning of its
outburst. Based on its first outburst in 1920 (near maximum for ~ 100 days), it
is one of only two SLOW RN. While CHANDRA observed another RN with ACIS-S (CI Aql
in 2000), the resulting spectrum was weak. However, CI Aql was fainter at maximum
and the spectrum was taken after it had returned to quiescence. RN may be
progenitors of SN Ia suggesting that we need to obtain as much information as we
can about their properties. We, therefore, propose a 5 ksec ACIS-S observation to
see if it is bright in X-rays followed by a 25 kse c HRC-S+LETG spectrum to study
the ejecta. The ACIS-S spectrum will show either emission lines from a hot gas
(seen in V382 Vul) or a hot continuum from a white dwarf atmosphere (V1494 Aql).
Neither of these resemble the spectrum of a dwarf nova (WZ Sge).
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:39:26.50 -52:19:18.20 IM NORMAE ACIS-S NONE 5.00
15:39:26.50 -52:19:18.20 IM NORMAE ACIS-S NONE 25.00
===================================================================================
Proposal Number: 03308083
Proposal Title: CHANDRA HETG SPECTROSCOPY OF GK PER IN OUTBURST
PI: CHRISTOPHER MAUCHE
Subject Category: WD BINARIES AND CV
Abstract: GK Persei is an extraordinary object: the first nova of the last
century, it contains a magnetic white dwarf, an evolved secondary, and a large
truncated accretion disk. ASCA demonstrated that in outburst the X-ray spectrum
of GK Per contains strong Fe K emission lines and a strong low-energy (0.5-3 keV)
excess. The nature of the low-energy excess is not known, but it is expected to
consist of a mixture of thermal emission lines from the accretion column and
fluorescent emission lines from the white dwarf surface and accretion disk. We
propose to obtain two Chandra HETG observations of GK Per in outburst to
determine the nature of the low-energy emission, measure the Fe K emission line
strengths, and search for other emission lines, thereby constraining the
accretion geometry and the plasma conditions (range of temperatures, abundances,
and density) of the X-ray--emitting plasma.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
03:31:11.80 +43:54:16.80 GK PER ACIS-S HETG 35.00
03:31:11.80 +43:54:16.80 GK PER ACIS-S HETG 35.00
***********************************************************************************
BH AND NS BINARIES
--------------------------------------------------
===================================================================================
Proposal Number: 03400017
Proposal Title: ULTRALUMINOUS X-RAY SOURCES AND INTERMEDIATE MASS BLACK HOLES
PI: JOEL BREGMAN
Subject Category: BH AND NS BINARIES
Abstract: Ultraluminous X-ray sources (ULX) are second only to AGNs in
point-source luminosity yet they have no known optical counterparts. These
extraordinary X-ray objects, which radiate at the Eddington luminosity of a
30-100 Mo object, are non-nuclear sources in normal disk galaxies. One
explanation is that they are binary systems where the accreting black hole has a
mass of 30-100 Mo. Another possibility is that ULXs are intermediate mass black
holes (1E3-1E4 Mo), acting as micro-quasars in galaxy disks and representing the
link between stellar black holes (4-10 Mo) and supermassive black holes (1E6-1E10
Mo). We can distinguish between the models by identifying the optical
counterparts of ULXs and measuring their colors.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:35:50.60 +27:54:47.00 NGC 4559 ACIS-S NONE 3.00
===================================================================================
Proposal Number: 03400284
Proposal Title: UNTWISTING THE TORNADO
PI: BRYAN GAENSLER
Subject Category: BH AND NS BINARIES
Abstract: G357.7-0.1 ("the Tornado") is an unusual radio source whose morphology
defies classification. We have discovered an X-ray source coincident with the
Tornado, which we argue represents either a central pulsar or an exotic accreting
system, both of which could power the surrounding radio emission. High-resolution
X-ray imaging, followed by a search for an infrared counterpart, can distinguish
between these possibilities. We thus propose ACIS observations with which we can
establish the properties of the central source in the Tornado, and so finally
determine the nature of this enigmatic object.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:40:11.70 -30:58:38.20 TORNADO ACIS-I NONE 21.00
===================================================================================
Proposal Number: 03400295
Proposal Title: CHANDRA OBSERVATIONS OF LONG-DURATION TRANSIENTS AND PERSISTENT
LOW-MASS X-RAY BINARIES IN QUIESCENCE
PI: RUDY WIJNANDS
Subject Category: BH AND NS BINARIES
Abstract: We propose to observe a long-duration transient or a persistent
low-mass X-ray binary when it turns-off and transits in to quiescence. This will
give an excellent opportunity to study the effects of prolonged accretion on the
quiescent properties of low-mass X-ray binaries. A follow-up observation taken
about half a year later will provide important information about the time
evolution of the quiescent properties, i.e., the neutron-star cooling time.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:02:06.30 -29:56:45.00 MXB 1659-298 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03400303
Proposal Title: OBSERVATIONS OF THE TRANSIENT X-RAY PULSAR 2S 1845-024
PI: MARK FINGER
Subject Category: BH AND NS BINARIES
Abstract: 2S 1845-024 is a 94 second transient X-ray pulsar which outbursts near
the periastron passage of its highly eccentric, 242 day binary orbit. Its yet
unidentified companion is likely a Be star. The source's outbursts have occurred
regularly each orbit for at least the last 10 years. The source is unique in
showing both evidence for its companion's equator being inclined with respect to
the orbital plane, and in showing evidence for accretion disk formation during
recurrent outbursts. Our proposal is to make Chandra ACIS-S/HETG observations
during the outburst expected in September 2002 to study the spectral evolution
associated with the disk formation. A secondary objective of our proposal is to
obtain an accurate source position so that the optical companion may be
identified.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:48:18.00 -02:25:12.00 2S 1845-024 ACIS-S NONE 5.00
18:48:18.00 -02:25:12.00 2S 1845-024 ACIS-S HETG 15.00
18:48:18.00 -02:25:12.00 2S 1845-024 ACIS-S HETG 15.00
18:48:18.00 -02:25:12.00 2S 1845-024 ACIS-S HETG 15.00
===================================================================================
Proposal Number: 03400316
Proposal Title: LOCATING THE ELUSIVE COUNTERPART OF THE UNUSUAL X-RAY DIPPER
X1624-490
PI: STEFANIE WACHTER
Subject Category: BH AND NS BINARIES
Abstract: X-ray dippers are high inclination low mass X-ray binary systems in
which the central X-ray source is periodically occulted by a thickened region of
the accretion disk rim. X1624-490 is one of the most unusual members of this
class; its persistent X-ray emission is the brightest, its dip profiles the most
erratic, and its 20.9-hour orbital period is the longest. Despite a wealth of
X-ray observations, the optical counterpart of X1624-490 has not yet been
identified. With its high spatial resolution, the Chandra HRC-I is the perfect
instrument for, and the only one capable of, directly pinpointing the optical/IR
counterpart of X1624-490. This project can be achieved with a minimal amount of
observing time (1 ksec) and the result can be applied immediately to already
existing IR data.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:28:03.30 -49:11:30.30 X1624-490 HRC-I NONE 1.00
===================================================================================
Proposal Number: 03400384
Proposal Title: THE FAINTEST 'FIELD' LOW-MASS X-RAY BINARIES
PI: MICHIEL VAN DER KLIS
Subject Category: BH AND NS BINARIES
Abstract: We propose to continue our survey, begun in Cycle 1, of the group of
persistently faint galactic X-ray sources outside globular clusters which are
thought to be LMXBs, but about which very little was known before Chandra. Our
exploratory Cycle 1 work confirmed the low Lx of these objects, and produced some
intriguing new results. Given theoretical as well as empirical arguments for the
detection of spectral lines, in Cycle 3 we propose HETG follow-up observations
for 4 sources, and further exploratory ACIS pointings for 4 others. Our aim is to
extend knowledge about compact-object accretion physics towards lower accretion
levels than previously accessible and to provide a sample against which to
compare the faint globular-cluster LMXBs.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:05:45.80 +25:51:45.00 1603.6+2600 ACIS-S NONE 8.00
17:14:19.20 -34:02:57.60 1711-339 ACIS-S NONE 5.00
17:42:44.00 -30:30:51.50 1739-304 ACIS-S NONE 1.00
17:42:44.00 -30:30:51.50 1739-304 ACIS-S NONE 3.00
17:50:03.90 -32:25:51.00 1746.7-3224 ACIS-S NONE 8.00
===================================================================================
Proposal Number: 03400337
Proposal Title: RESOLVING GALACTIC BLACK HOLE ACCRETION GEOMETRY WITH CHANDRA
PI: WALTER LEWIN
Subject Category: BH AND NS BINARIES
Abstract: Recent results have shown that the X-ray states observed in all black
hole X-ray binary systems cannot be driven solely by the mass accretion rate, but
depend on the accretion flow geometry in a complicated way. Our own results from
AO-1 and AO-2 may reveal a previously unseen geometry. Additionally, correlations
between discrete radio ejections, radio jets, and the X-ray state, have been
noted recently. We propose to probe the accretion flow geometry in a black hole
system in outburst with the HETGS to diagnose the geometry in different X-ray
states; by doing so we will constrain what mechanisms act with the mass accretion
rate to drive the state transitions. Ours is a global, simultaneous,
multi-wavelength effort, which spans the radio, IR, optical, X-ray and gamma-ray
bands.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:50:01.00 -49:57:45.00 BHC TRANSIENT ACIS-S HETG 15.00
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S HETG 30.00
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03400454
Proposal Title: HIGH RESOLUTION SPECTROSCOPY OF HERCULES X-1
PI: DANIEL SCOTT
Subject Category: BH AND NS BINARIES
Abstract: We propose a set of high resolution spectral observations of the
accreting pulsar X-ray binary Her X-1/HZ Her. A strong, pulsed, blackbody
spectral component has been detected with a temperature of about 0.1 keV probably
originating from X-ray reprocessing by the inner edge of the precessing accretion
disk. Chandra LETGS observations can determine if emission lines from this
component are present and if so use them to probe the physical conditions there.
Observations with the HETGS will resolve the strong Fe K line and determine
whether a mysterious large unresolved bump in the spectrum between 0.8 and 1.4
keV is due to a multi-temperature Fe L emission complex or involves other lines.
The Main High state peak and flux decline and a Short High state will be
surveyed.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:57:49.80 +35:20:32.90 HER X-1 SHORT HI ACIS-S HETG 20.00
16:57:49.80 +35:20:32.90 HER X-1 SHORT HI ACIS-S HETG 20.00
16:57:49.80 +35:20:32.90 HER X-1 MAIN HI PEAK HRC-S LETG 10.00
16:57:49.80 +35:20:32.90 HER X-1 MAIN HI LATE ACIS-S HETG 20.00
16:57:49.80 +35:20:32.90 HER X-1 MAIN HI PEAK ACIS-S HETG 10.00
===================================================================================
Proposal Number: 03400510
Proposal Title: AN ULTRALUMINOUS BINARY IN A HORSESHOE NEBULA?
PI: PATRICK SLANE
Subject Category: BH AND NS BINARIES
Abstract: We propose a Chandra observation of 1E0953.8+6918 to assess its
relationship to the very strange horseshoe-shaped nebulosity seen in the
direction of the galaxy Ho IX. The position and morphology of the X-ray emission
is currently not well known, and this is crucial for our understanding of the
nebula. If located in Ho IX, Lx is very high, possibly indicating a 100 solar
mass BH binary, and the size of the nebula implies a huge shock-heated structure,
which is difficult to understand. However, a Galactic interpretation is no less
puzzling. The proposed observation will provide an improvement in the source
location, permit a search for multiple emission components, and allow us to
search pulsations from any compact emission region identified in the high
resolution Chandra image.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
09:57:53.00 +69:03:51.00 1E0953.8+6918 HRC-I NONE 7.00
===================================================================================
Proposal Number: 03400562
Proposal Title: THE EXTRAORDINARY GLOBULAR CLUSTER SYSTEM OF M87: THE VIEW FROM
CHANDRA
PI: PATRICK COTE
Subject Category: BH AND NS BINARIES
Abstract: With the launch of Chandra, a new era in the study of globular cluster
(GC) X-ray sources has arrived. It is at last possible to identify bright X-ray
sources belonging to the GCs of giant elliptical galaxies: the natural targets
for such studies by virtue of their rich GC systems. We propose to exploit the
exceptional spatial resolution and sensitivity of Chandra to carry out the
definitive study of LMXBs in GC environments. Our target is M87, the cD galaxy in
the nearby Virgo cluster. Its GC system (the most populous of any galaxy within
20 Mpc) is the focus of a comprehensive optical study we are conducting with HST
and ground-based telescopes. This program will reveal hundreds of LMXBs
associated with M87 GCs, and provide a definitive test of models for their
origin.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:30:49.40 +12:23:28.00 NGC4486 ACIS-S NONE 23.00
12:30:49.40 +12:23:28.00 NGC4486 ACIS-S NONE 105.00
===================================================================================
Proposal Number: 03400564
Proposal Title: RESOLVING IRON K-ABSORPTION LINE FEATURES IN THE X-RAY SPECTRA
OF THE LOW MASS X-RAY BINARY GX 13+1
PI: YOSHIHIRO UEDA
Subject Category: BH AND NS BINARIES
Abstract: We propose to observe the Low Mass X-ray Binary GX 13+1 with Chandra
HETGS, which is the unique neutron-star binary that exhibits iron-K absorption
lines revealed from previous ASCA observations. Moreover, since GX 13+1 is a
relatively bright and persistent radio source, it is of great interest to study
the relation to the transient superluminal sources GRO J1655-40 and GRS 1915+105,
which have shown similar spectral features in the X-ray spectra. The high
resolution spectroscopy of GX 13+1 in the iron-K band will give important clues
for understanding common physics of an accretion disk in neutron star and black
hole binaries.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:14:31.00 -17:09:26.00 GX 13+1 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03400614
Proposal Title: THE HIGH LATITUDE NEUTRON STAR X-RAY TRANSIENT XTE J2123-058
PI: JOHN TOMSICK
Subject Category: BH AND NS BINARIES
Abstract: XTE J2123-058 is a high Galactic latitude neutron star transient. The
high latitude of the source provides the observational advantage of low
extinction, which is critical for soft X-ray and optical observations. From
optical spectroscopy, we find that the source distance is near 8.9 kpc, making it
unusually far from the Galactic plane for an LMXB. We previously obtained an
X-ray luminosity upper limit of 3.6E33 erg/s for this source with BeppoSAX, and
more sensitive observations are required. I propose to observe XTE J2123-058 with
Chandra to measure its luminosity. Although a detection is likely, a
non-detection will provide a luminosity upper limit of 3E31 erg/s, which has
implications for the question of whether quiescent black hole systems are dimmer
than neutron star systems.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
21:23:14.50 -05:47:52.90 XTE J2123-058 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03400623
Proposal Title: OUTFLOWS FROM X-RAY PULSARS IN THE PROPELLER STATE
PI: WEI CUI
Subject Category: BH AND NS BINARIES
Abstract: As an accreting X-ray pulsar enters the propeller state, the accreted
matter encounters a centrifugal barrier and thus cannot follow the field lines to
reach the magnetic poles. Consequently, the X-ray pulsation ceases. It is thought
that in this state the accreted material is actually ejected and thus forms an
outflow. Indirect evidence for such an outflow exists for GX 1+4, based on the
non-thermal nature of its observed X-ray spectrum in the propeller state. Now the
powerful combination of the HETG and ACIS allows, for the first time, an attempt
to studying gas dynamics in X-ray pulsars during this poorly understood state, by
measuring Doppler-shifted iron fluorescent lines. We propose a joint Chandra and
RXTE ToO campaign to observe GX 1+4 in the propeller state.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:32:03.00 -24:44:44.30 GX 1+4 ACIS-S HETG 60.00
===================================================================================
Proposal Number: 03400626
Proposal Title: ACIS-HETG OBSERVATIONS OF MICROQUASAR XTE J1748-288
PI: JULIA LEE
Subject Category: BH AND NS BINARIES
Abstract: The recently discovered microquasar XTE J1748-288 show spectral
differences between the very high, high, and low state. ASCA and RXTE
observations show prominent iron line(s). We propose to observe with HETG for a
140ks total exposure over these 3 phases in order to characterize the X-ray
spectral features and resolve presently unknown lines for these states. We will
also look for emission lines from any X-ray jet, and P-Cygni profiles indicative
of a disk-wind. This will be compared to previous Chandra observations of similar
energetic systems. We were awarded time in the last Chandra cycle for this
proposal but did not trigger on the TOO. The source has remained off.
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 55.00
17:48:08.00 -28:28:48.00 XTE J1748-288 ACIS-S HETG 55.00
===================================================================================
Proposal Number: 03400636
Proposal Title: MONITORING THE MORPHOLOGY OF THE MICRO-QUASARS GRS 1758-258 AND
1E 1740.7-2942
PI: WILLIAM HEINDL
Subject Category: BH AND NS BINARIES
Abstract: We propose to monitor the "micro-quasars" GRS 1758-258 and 1E
1740.7-2942 in order to search for changes in the morphology of their arcsecond
scale extended X-ray emission. In GRS 1758-258, this extended structure changed
shape (as seen by the Chandra/HRC-I) in about a month, indicating a possible
near-luminal outflow. In this investigation, we will use the HRC-I in concert
with our approved RXTE/Proportional Counter Array and VLA monitoring programs to
track changes in the extended X-ray morphology of GRS 1758-258 and see if similar
changes occur in 1E 1740.7-2942. We will correlate these variations with the
radio flux and hard X-ray (3-60 keV) spectral behavior which will allow us to
study the role of the disk/corona with the ejection of material from the binary
system.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:43:54.80 -29:44:42.80 1E 1740.7-2942 HRC-I NONE 7.50
17:43:54.80 -29:44:42.80 1E 1740.7-2942 HRC-I NONE 7.50
17:43:54.80 -29:44:42.80 1E 1740.7-2942 HRC-I NONE 7.50
17:43:54.80 -29:44:42.80 1E 1740.7-2942 HRC-I NONE 30.00
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
18:01:12.40 -25:44:35.90 GRS 1758-258 HRC-I NONE 3.33
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 HRC-I NONE 10.00
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 HRC-I NONE 10.00
===================================================================================
Proposal Number: 03400642
Proposal Title: A CHANDRA STUDY OF NEARBY PERSISTENT MICROQUASAR LS 5039
PI: WALTER LEWIN
Subject Category: BH AND NS BINARIES
Abstract: LS 5039 is a persistent microquasar with many striking similarities to
SS 433. Located only 3 kpc away and suffering minimal extinction, the X-ray
structure of the jets and inner accretion region may be revealed simultaneously
with Chandra. We propose an HETGS observation of this source to resolve the jet
structure and energetics, to constrain the accretion flow geometry in this
system, to place LS 5039 in the context of other microquasars such as SS 433, 1E
1740.7-2942, and GRS 1915+105.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:26:14.90 -14:50:51.00 LS 5039 ACIS-S HETG 10.00
===================================================================================
Proposal Number: 03400646
Proposal Title: BLACK HOLE X-RAY TRANSIENTS DURING OUTBURST DECAY
PI: JOHN TOMSICK
Subject Category: BH AND NS BINARIES
Abstract: Most observations of black hole candidate (BHC) X-ray transients have
been made when the sources are at very high luminosity (>1E36 erg/s) or very low
luminosity (<1E32 erg/s), and not much observing time has been devoted to
intermediate luminosities. Observations in this intermediate regime are critical
since the competing theoretical models predict different emission properties
here. We propose to use Chandra to observe a BHC X-ray transient in this
luminosity regime during outburst decay. These observations will provide
constraints on accretion geometries and emission mechanisms and will provide
definitive tests of existing theoretical models. We have an active RXTE program
for observing these systems during decay, and will use our RXTE observations to
trigger this TOO.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S HETG 10.00
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S HETG 10.00
16:50:01.00 -49:57:45.00 XTE J1650-500 ACIS-S NONE 20.00
===================================================================================
Proposal Number: 03400757
Proposal Title: LOCALIZING THE HIGH LATITUDE X-RAY TRANSIENT 4U 0042+32
PI: JOHN TOMSICK
Subject Category: BH AND NS BINARIES
Abstract: 4U 0042+32 is a very interesting and unusual high Galactic latitude
X-ray transient. This source was detected in X-rays several times during the
1970s, and is probably a black hole X-ray transient, but has not been observed in
outburst for over 20 years. Due to its high latitude, the level of extinction is
low, but 4U 0042+32 has not been optically identified. We propose to use
Chandra's sensitivity and positioning capabilities to localize 4U 0042+32 in
quiescence to facilitate its optical identification. We have already obtained a
deep optical image so that a Chandra detection is likely to lead to a rapid
identification. Follow-up optical observations could then be performed to
determine the source distance, the binary orbital parameters and possibly the
mass of the compact object.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:44:50.30 +33:01:17.00 4U 0042+32 ACIS-S NONE 40.00
===================================================================================
Proposal Number: 03400827
Proposal Title: PROBING THE CIRCUMSTELLAR MATERIAL IN GX 301-2
PI: MASAO SAKO
Subject Category: BH AND NS BINARIES
Abstract: We propose to obtain high-resolution spectroscopic data of the
high-mass X-ray binary GX 301-2/Wray977 to study the geometry of circumstellar
material in the system. The observation consists of two exposures --
pre-periastron (PP) and near-apastron (NA) flares -- during which the source
brightens by as much an order of magnitude compared to the normal quiescent
state. The emission line spectrum, especially in the iron K region, changes
dramatically during these flares, and a detailed spectral analysis will allow us
to probe the distribution of material in the system, as well as the dynamical
properties of the stellar wind. Measurements of the Fe K fluorescent line profile
will also unambiguously distinguish the broadening mechanism, which has been
difficult with low-resolution spectra.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
12:26:37.60 -62:46:13.00 GX 301-2 ACIS-S HETG 40.00
12:26:37.60 -62:46:13.00 GX 301-2 ACIS-S HETG 60.00
12:26:37.60 -62:46:13.00 GX 301-2 ACIS-S HETG 60.00
===================================================================================
Proposal Number: 03400837
Proposal Title: COMPLETE COMPACT OBJECT AND BINARY SURVEY OF 47TUC
PI: JONATHAN GRINDLAY
Subject Category: BH AND NS BINARIES
Abstract: Our cycle 1 observation of 47Tuc has shown its promise as the ultimate
laboratory for study of the production and evolution of compact binaries and
compact objects in globular clusters. We propose a deep (4 x 75ksec) ACIS-S
observation to measure the complete populations of millisecond pulsars (MSPs) and
cataclysmic variables (CVs) by their variability and spectra and to constrain the
main sequence binary population. Coordinated HST (ACS) data would provide unique
identifications of CVs and many MSPs and allow the full population of quiescent
low mass x-ray binaries to be distinguished from CVs. This dataset would provide
fundamental constraints for the origins of neutron stars, millisecond pulsars,
magnetic white dwarfs and compact binaries in globular clusters.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 5.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 5.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 5.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 5.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 69.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 69.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 69.00
00:24:05.80 -72:04:51.20 47 TUCANAE ACIS-S NONE 69.00
===================================================================================
Proposal Number: 03400840
Proposal Title: MEASURING THE ABSOLUTE DISTANCE TO THE BURSTER GS 1826-238
PI: RICHARD ROTHSCHILD
Subject Category: BH AND NS BINARIES
Abstract: We propose to measure the distance to the clocked x-ray burster GS
1826-238 by measuring the burst-induced temporal variability of the x-ray
scattering halo. When combined with the bolometric flux measured simultaneously
with Chandra and RXTE, this will yield the absolute bolometric luminosity from
this object for both the persistent and burst emission. This novel and very
powerful technique for absolute distance determination will provide a measurement
of the neutron star radius as well as the fraction of the neutron star surface
involved in the persistent, steady state hydrogen burning. It is important to
establish this method of distance determination since it could have wide
applications for variable sources.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:29:28.20 -23:47:49.12 GS 1826-238 ACIS-S HETG 70.00
===================================================================================
Proposal Number: 03400841
Proposal Title: PHASE RESOLVED HIGH ENERGY RESOLUTION SPECTROSCOPY OF THE BLACK
HOLE X-RAY BAINARY CYGNUS X-1
PI: SHUANG ZHANG
Subject Category: BH AND NS BINARIES
Abstract: We propose to carry out phase resolved high resolution spectroscopy of
the black hole X-ray binary Cygnus X-1 with ACIS-S HETG. Our observations consist
of four snap-shots of 5-ks each at orbital phases 0.0, 0.25, 0.5 and 0.75. Our
observational goals are to determine the Oxygen abundance, column density and the
continuum spectrum independent of each other. Our scientific objectives include
the study of the properties of the corona and accretion disk around the black
hole and disk formation in wind accretion system. Our feasibility study
demonstrates that our proposed observations serve our objectives well.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
19:58:21.70 +35:12:05.80 CYG X-1 ACIS-S HETG 5.00
19:58:21.70 +35:12:05.80 CYG X-1 ACIS-S HETG 5.00
19:58:21.70 +35:12:05.80 CYG X-1 ACIS-S HETG 5.00
19:58:21.70 +35:12:05.80 CYG X-1 ACIS-S HETG 5.00
===================================================================================
Proposal Number: 03400937
Proposal Title: WIND ACCRETION IN LOW-MASS X-RAY BINARIES
PI: DUNCAN GALLOWAY
Subject Category: BH AND NS BINARIES
Abstract: We have identified a group of neutron-star low-mass X-ray binaries
which are likely accreting from the stellar wind of their companion rather than
via the usual Roche-lobe overflow. If confirmed,this would be a previously
unrecognized mode of mass transfer in LMXBs with significant implications for our
understanding of their evolution and population, since these binaries could be
X-ray active without being in contact. We will test for wind accretion by using
the HETGS to search for fluorescent lines from stellar wind nebulae in these
sources.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:32:02.20 -24:44:43.60 GX 1+4 ACIS-S HETG 20.00
17:47:56.00 -26:33:48.60 GX 3+1 ACIS-S HETG 10.00
===================================================================================
Proposal Number: 03400979
Proposal Title: RESOLVING THE SOFT EXCESS IN 4U 1850-087
PI: DEEPTO CHAKRABARTY
Subject Category: BH AND NS BINARIES
Abstract: A soft excess near 0.7 keV, consistent with unresolved emission lines,
has been previously reported in several LMXBs. Our recent reanalysis of archival
ASCA and BeppoSAX data shows that this excess can also be explained by
photoelectric absorption by material with non-solar abundance, or by a failure to
account for the thermodynamically required turnover of the power law continuum at
low energies. We propose an ACIS-S/LETGS observation of the soft excess source 4U
1850-087 in order to discriminate between these alternatives.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:53:04.80 -08:42:19.80 4U 1850-087 ACIS-S LETG 5.00
18:53:04.80 -08:42:19.80 4U 1850-087 ACIS-S LETG 55.00
===================================================================================
Proposal Number: 03400860
Proposal Title: STUDY OF THE IRON LINE AND LOW ENERGY FEATURES IN 4U 1728-34
WITH CHANDRA/HETGS
PI: TIZIANA DI SALVO
Subject Category: BH AND NS BINARIES
Abstract: We propose a 30 ks Chandra/HETGS observation of 4U 1728-34 to perform a
detailed study of the iron Kalpha line and other low energy features. This source
shows a broad (1 keV FWHM) iron Kalpha line: several hypotheses can be proposed
to explain the width (e.g. relativistic and Doppler effects in an accretion disk,
Compton scattering, line-blending), and we expect that the high energy resolution
of Chandra HETGS will be able to resolve the complex line shape and to constrain
the various models proposed. These kind of sources are also expected to be rich
sources of discrete features at low energy (0.3-3 keV), because of the presence
of a photoionized corona (ADC). These low energy features are an important
diagnostic tool for the physical conditions of the emitting regions.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:31:57.40 -33:50:05.00 4U 1728-34 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03400921
Proposal Title: SPECTRAL SIGNATURES OF A PRECESSING ACCRETION DISK IN HER X-1
PI: CHARLES HAILEY
Subject Category: BH AND NS BINARIES
Abstract: Observations of Her X-1 with the XMM-Newton RGS show the most prominent
line emission in the low-state of its 35-day flux cycle. Chandra HETG can detect
a dozen H-like and He-like ion lines and test our photoionized disk atmosphere
model, which has been successful in predicting the lines of EXO 0748-67 and
4U1822-37. The precessing disk hypothesis for Her X-1 can be tested by observing
changes in velocity dispersion with the 35-day cycle, as the inner disk comes in
and out of view. Her X-1 is one of the brightest low-mass X-ray binaries (LMXB)
at high inclination, making it a prime target to observe line emission.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
16:57:49.80 +35:20:32.60 HER X-1 ACIS-S HETG 50.00
===================================================================================
Proposal Number: 03400987
Proposal Title: A SEARCH FO EMISSION LINES IN THE MICRO-QUASAR GRS 1758-258
PI: WILLIAM HEINDL
Subject Category: BH AND NS BINARIES
Abstract: We propose to obtain a high significance, high resolution spectrum of
the micro-quasar GRS 1758-258 in order to search for emission lines from possible
X-ray jets. As revealed in Chandra/HRC observations, GRS 1758-258 has arcsecond
scale extended X-ray emission associated with a core point source. This extended
structure changed shape in about a month, evidence for a near-light-speed
outflow. In this investigation, we will use the ACIS-S/HETG, supported by
concurrent Rossi X-ray Timing Explorer and VLA observations, to search for red-
and blue-shifted emission lines. If found, these lines will confirm the presence
of relativistic flows in this system and should allow us to constrain the
geometry of the system.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
18:01:12.40 -25:44:35.90 GRS 1758-258 ACIS-S HETG 30.00
===================================================================================
Proposal Number: 03401009
Proposal Title: MULTIWAVELENGTH OBSERVATIONS OF THE BLACK HOLE XTE J1118+480 IN
QUIESCENCE
PI: STEPHEN MURRAY
Subject Category: BH AND NS BINARIES
Abstract: The X-ray nova XTE J1118+480 has minimal interstellar extinction and
therefore represents an outstanding opportunity for multiwavelength studies. In
outburst we conducted a comprehensive study of this object that was extremely
rewarding. Now we propose an analogous campaign to observe the quiescent state
using Chandra, HST and the MMT. Our objectives are to (1) assemble the best
possible optical to X-ray spectrum of a quiescent black hole, (2) constrain the
radius of the inner edge of the accretion disk, (3) determine if the UV/optical
emission is due to the accretion disk or to an advection-dominated flow, (4)
acquire key data on the extreme faintness of black holes relative to neutron
stars, and (5) test models proposed to explain the faintness of quiescent black
holes.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
11:18:10.80 +48:02:12.30 XTE J1118+480 ACIS-S NONE 10.00
11:18:10.80 +48:02:12.30 XTE J1118+480 ACIS-S NONE 42.00
===================================================================================
Proposal Number: 03400483
Proposal Title: ``QPO-FOLDED'' SPECTROSCOPIC STUDY OF 3 LOW-MASS X-RAY BINARIES
AND DIPPING SOURCES
PI: MARIANO MENDEZ
Subject Category: BH AND NS BINARIES
Abstract: We will use Chandra's ACIS-S detector in combination with HETG and LETG
to do phase-resolved spectroscopy of the three low-mass X-ray binaries and
dippers 4U 1746-37, 4U 1323-62, and EXO 0748-676. Using the 1 Hz QPO that we
recently discovered in these sources we will construct ``QPO-folded'' light
curves to study separately spectra from different QPO-phase intervals. We will
correlate the presence/absence of emission and absorption features in the energy
spectrum of Chandra (and XMM-Newton) with timing properties measured both by
Chandra, and simultaneous RXTE observations. This should help us determine how
timing properties depend on mass accretion rate, and whether mass flows onto the
central object through different channels of accretion.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
17:50:12.70 -37:03:08.00 4U 1746-37 ACIS-S HETG 40.00
===================================================================================
Proposal Number: 03408078
Proposal Title: IMAGING THE JET/ISM INTERACTIONS AROUND THE BLACK HOLE
XTEJ1550-564
PI: STEPHANE CORBEL
Subject Category: BH AND NS BINARIES
Abstract: We discovered a new radio source, 22" West of the black hole
XTEJ1550-564 (IAUC 7795; 2002 Jan 19). Subsequent observations show it has a
variable spectrum, is extended toward XTEJ1550 and is located along the axis of
the VLBI jets observed during the Sept 1998 radio flare. Our Chandra images from
Aug-Sept 2000 show an extended X-ray source also along the VLBI jet axis, but
directly opposite the radio source (23" to the East), and with similar flux
during the two Chandra observations (21 days apart). We found a transient radio
source in archival data at this position in Feb 2001, indicating a lifetime of a
few months. It is likely that both components represent superluminal plasmons
ejected during the Sept 1998 major radio flare and interacting with the ISM. The
proposed Chandra observation will allow us to study the physics of jet/ISM
interactions and the total power of relativistic jets, with implications for our
understanding of relativistic jets from AGN.
Grat- Exp.
R.A. Dec. (J2000) Target Name Det. ing Time
-----------------------------------------------------------------------------------
15:50:58.70 -56:28:35.60 XTE J1550-564 ACIS-S NONE 30.00
===================================================================================
Proposal Number: 03408085
Proposal Title: A FAINT NEUTRON STAR SOFT X-RAY TRANSIENT RETURNING TO
QUIESCENCE
PI: PETER JONKER
Subject Category: BH AND NS BINARIES
Abstract: Approx 10 SXTs like SAXJ1808.4-3658 form a class of faint SXTs,
calculations show that the NS magnetic field will not be buried in these systems.
We propose to obtain three observations of a faint SXT as it returns to
quiescence. Monitoring observations will allow us to observe the transition from
a spectrally hard state in outburst to a soft spectral state in quiescence. To
find out which emission mechanism is responsible for the low-level X-ray
emission, it