HETG

Follow-on Science Instrument

Contract NAS8-01129

 

Monthly Status Report No. 011

January 2003

HETG Science Theme: Isolated Neutron Stars

 

Prepared in accordance with DR 972MA-002; DPD #972

Prepared for

National Aeronautics and Space Administration

Marshall Space Flight Center, Alabama 35812

 

Center for Space Research; Massachusetts Institute of Technology; Cambridge, MA 02139

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1.0 Distribution List for Monthly Status Report

 

 

MIT-External Electronic:

FD03/Mike Smith, MSFC                   Carl.M.Smith@msfc.nasa.gov

PS41/Steve Morris, MSFC                 Steven.D.Morris@msfc.nasa.gov

SD50/Martin Weisskopf, MSFC            martin.weisskopf@msfc.nasa.gov

 

MIT-External Hardcopy:

                                    None specified.

 

 

            MIT-Internal Electronic:

                                                Elaine Tirrell                egt@mit.edu

                                                Gail Monahan              gmonahan@mit.edu

 

MIT-Internal Hardcopy:

                                                Claude Canizares         Room 3-234 (via Gail Monahan)

                                                Deepto Chakrabarty     Room 37-501 (via Elaine Tirrell)

                                                Kathryn Flanagan        Room NE80-6103 (via Elaine Tirrell)

 

Please send distribution requests and other comments on this document to dd@mit.edu .

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2.0 Schedule of Past and Future Events Relevant to HETG

 

 

Date	Past Events	Comment
Jan. 5-9	American Astronomical Society 201st Meeting , Seattle, WA	S. Gallagher,; A. Fredericks; M. Jimenez-Garate; M. Stage; R. Gibson.
Jan. 26-31	Clusters of Galaxies: Probes of Cosmological Structure and Galaxy Evolution. Carnegie Observatories Centennial Symposium III.	T. Jeltema

 

 

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3.0 Instrument Status and Science Support

 

 

3.1 Flight Events and HETG Instrument Status

 

The HETG continues to function with no outstanding issues. This was a quiet month for HETG observations – only three observations using the HETG: they were of the moon Titan as it passed in front of the Crab nebula and the HETG’s purpose was to act as a filter to reduce the Crab’s intensity.

 

3.2 Science Support to CXC, SWG, etc.

 

Helped to test CXC/MIT produced contamination correction data and s/w to make accurate arfs for data analysis taking the ACIS contamination build up into account – congrats to Dave H, Herman M, etc on getting this out.

Contributed an HETG article to the Chandra newsletter – coming out soon.

 

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4.0 GTO Science Program

4.1 Observations and Data status

Progress in the GTO program observations and data analyses are noted in the Table of Appendix A. Presentations at the AAS meeting in Seattle were a major activity in January and planning for GTO Cycle 5 began.

 

4.2 Science theme progress

The HETG GTO science efforts span a range of “science themes” given in the list below. This month progress and plans in the Isolated Neutron Star theme are presented with help from Mike Stage and Herman Marshall.

 

GTO Science Theme	Abbreviation (for App’ix A)	Researchers (HETG in caps)	Date of last [next] reporting Assembler of theme material
“Cool” Stars	Cool Star	dph,nss,psw,bb	September, 2002. Dave Huenemoerder
“Hot” Stars	Hot Star	nss,dph,psw,bi	October, 2002. Norbert Schulz
X-ray Binaries & Accretion Disks	XRB	MJ-G,AJ,nss,hlm, man, jmm, psw	December, 2002. Norbert Schulz, Mike Nowak
Supernova Remnants	SNR	KAF,DD,JMM, AF,jh,gea,tp	May, 2002. Dan Dewey
Isolated Neutron Stars	iNS	MDS,hlm, nss	January, 2003. Mike Stage, Herman Marshall
Galaxies & Clusters of Galaxies	Gal., Clust.	TJ,mw,jh	August, 2002. Michael Wise, Tesla Jeltema
Active Galactic Nuclei and Jets	AGN, Jet	SG,RG,MJ-G,hlm, man,jl,sm,jg	June, 2002. Herman Marshall
Inter-Stellar Medium	ISM	AJ,nss	Not yet reported [Feb.’03]
Inter-Galactic Medium	IGM	SG,RG,hlm	July, 2002. Taotao Fang

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Isolated Neutron Stars Research Progress

 

Introduction to Isolated Neutron Stars

         In the case of X-ray binaries we see a Neutron Star (NS) in a binary system with a companion and mass transferf rom the companion can lead to a bright source of X-rays. But what if the neutron star (presumably created in a core-collapse supernova event) does not have a companion? In this case we have an “isolated neutron star” (iNS). The iNS can be hot and radiate a smooth, featureless black body spectrum. The size, radius, of the neutron star defines the radiating surface area and radii are expected to be of order 10 km (for reference the Schwarzchild radius, R_Schw=2GM/c^2, for M=1.4 solar mass is ~4.2 km - this would appear to be a lower limit to actual NS radii.)

       Departures from a simple blackbody can arise if the neutron star has an atmosphere – due to the high gravity on the NS surface the height of this atmosphere is of order 0.01 to 1 cm – a very thin shell. The temperature of the surface, T*, the surface gravity, g, and the composition of the atmosphere (H, He, Fe, Si, etc.) then determine the spectrum and directionality of emitted radiation. Because of the high surface gravity, the emitted radiation, when seen by a distant observer, is red shifted with the apparent T_obs given by T_eff/(1+z); (1+z) is 1.31 for M=1.4, and R*=10.

If the neutron star has a substantial magnetic field and is spinning, it can interact with surrounding material to generate pulses of synchrotron radiation and be detected as a Pulsar from radio to X-ray.

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[ Figure above is available in various formats: .png , .ps , .fig . -dd ]

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Summary of Isolated Neutron Star GTO Observations and Activities

Three isolated Neutron Stars have been selected for inclusion in our HETG GTO observations to date and are listed in the Table below. Two other iNS are tabulated here as well: the Chandra-discovered point source in Cas A – which is also in our HETG GTO observation of Cas A (though that was not the main focus of the observation) and the LETG GTO (and later DDT) target RX J1856.5-3754 which obtained notoriety when the possibility of its being a “quark star” was suggested.

We have also worked on applying realistic atmosphere models to iNS specifically for the case of the Cas A point source in which context these models are discussed further below.

 

Obs cycle	Obsid	Name	Period	B field (G)	T_bb T* (MK)	R_bb R* (km)	Comments
2	1018	4U 0142+61	8.7 s	1.3x10^14	4.85 --	2 --	Anomalous x-ray pulsar, BB+PL. Young NS ? EW/E < 0.02
1	130 LETG- HRC-S	PSR B0656+14	384 ms	4.7x10^12	0.8 and 1.6 0.23	22 and 1.7 ~410	Two BB model. Spin age 100 k yr. H atmosphere model
1	131 CC-mode	PSR B0833-45, Vela pulsar	89 ms	3.0x10^12	1.49 0.68	2.1 10	Spin age 11 k yr. Magnetic H atmosphere model
2 1(GTO) 2(GO)	1046 114 1952	Cas A X-ray Point Source	None? 13 ms?	Weak, ~ 10^10 ?	5.4   3.8	0.55   7.6	Inside Cas A remnant: BB w/edges   ATM H model fit, R_g.
1(LETG) 2(DDT)	113, 3380+	RX J1856.5-3754 “A quark star?”	None	?	0.71   0.94	3.8 - 8.2   12.5	Drake et al., 2002.   Rot. blurred Si ATM model, R_g.

 

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Neutron Star Atmosphere models and the Cas A Point Source

         Paper: M. Stage, “Recent results fitting ATM atmophere models to Chandra spectra of thermally radiating neutron stars” (COSPAR 2002)and thesis in preparation, 2003.

         The X-ray Point Source, XPS, in the Cas A supernova remnant (below left) was discovered by Chandra in its first scientific image as a small central point if emission in the remnant. It is likely a neutron star from the collapsed core of the progenitor star. Two absorption effects are seen and modelled in the ACIS spectrum of the XPS: the usual (but large) interstellar galactic absorption which cuts off low-energy photons (below right) and local absorption by Si and S in the remnant surrounding the XPS – this absorption is responsible for the extra notches created in the spectrum a little below and a little above 2 keV. With these absorption terms the spectrum can be fit with a simple blackbody of order T_obs = 5 MK and R_obs ~ 0.6 km. This radius is thought to be too small for NS models and so suggests a partial area of emission or NS atmosphere effects are involved.

 

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         The ATM atmosphere models have been used to create modelled surface spectra for NS for different atmosphere compositions, temperatures and surface gravity values. The Figure here shows three such models (solid black lines) corresponding, left-to-right, to i) a Si-ash model at T*=1.01 MK, ii) a Hydrogen-only model at T*=1.5 MK, and iii) an iron (Fe) atmosphere model at T* = 4.0 MK. Note the abundance of spectral features in the Si and Fe atmosphere models (the fluxes have been scaled and do not correspond to a specific physical system.) The effect of surface gravity, g, is also shown here: the solid-line models are for log(g) = 14.0 and for each a dotted-lined version is plotted corresponding to log(g) = 15.2; for reference log(g) is 14.4 for M=1.4, R*=10. The higher surface gravity moves the spectra to slightly higher energies (not unlike a small amount of pileup in ACIS!?…) With high precision data it maybe possible to constrain the g value and have a measure of the actual NS radius assuming a mass value.

 

The promise of observing such detailed structure as these Fe and Si models suggest has lead to observations of iNS with the HETG and LETG. As will be seen in the following, actual observations have yet to reveal any clear atmosphere signature in the spectra.

 

Papers:

J. Madej, “Model atmospheres and X-ray spectra of bursting neutron stars”, ApJ, 376:161 (1991)

V.E. Zavlin et al., “Model neutron star atmospheres with low magnetic fields”, A&A, 315:141 (1996)

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[ Figure created with the IDL routines: ins_plots.pro and ins_spectra.pro . -dd ]

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B0656+14: Atmosphere on isolated Radio Pulsar?

Paper: H.L. Marshall and N.S. Schulz, “Using the High-resolution X-ray spectrum of PSR B0656+14 to constrain the chemical composition of the neutron star atmosphere”, ApJ, 574:377, 2002.

We observed PSR B0656+14 with GTO time using the LETG and HRC-S. The observed spectrum, below, is well modelled by the sum of two black bodies, the dominant one has T_obs = 0.8 MK and R_obs = 22 km. “No significant absorption features are found in the spectrum that might be expected from ionization edges of H or He or bound-bound transitions of Fe in magnetized atmopheres. … we conclude that the atmosphere is not dominated by Fe or other heavy elements that would be partially ionized at a temperature of 10^6 K.”

 

 

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Vela Pulsar: Using everything Chandra’s got!

Paper: G.G. Pavlov et al., “The X-ray spectrum of the Vela pulsar resolved with the Chandra X-ray Observatory”, ApJ, 552:L129, 2001. (These authors are at PSU and MPI Garching.)

 

The Vela pulsar was observed during Cycle 1 using three instrument combinations of Chandra: HETG/ACIS in CC mode (HETG GTO), ACIS-S no grating (ACIS GTO), and LETG/HRC-S (ACIS GTO). The image at right is from the ACIS-only observation and below it is the zeroth-order histogram from the HETG/ACIS CC observation. Note that although the pulsar itself is very bright, the surrounding pulsar wind nebula has a large total flux – this plus background events reduced the usefulness of the HETGS CC mode dispersed data.

 

The neutron star spectrum was modelled by a black body, T_obs = 1.49 MK and R_obs = 2.1 km, and a power-law relevant at high energies.

 

The featureless spectrum seen in the LETGS observation is consistant with a hydrogen NS atmosphere having an effective temperature at the surface of 0.9 MK and emission from the whole NS surface with R* ~ 10 to 13 km.

 

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4U 0142+61: Anomalous X-ray Pulsar

Paper: A.M. Juett et al., “Chandra High-resolution spectrum of the anomanous X-ray pulsar 4U 0142+61”, ApJ, 568:L31, 2002.

The anomalous X-ray pulsar 4U 0142+61 was observed with the HETGS in the Cycle 2 GTO porgram. The continuum spectrum, shown below along with residuals to the fit, is well fit by an absorbed power law plus blackbody with a photon index Tau = 3.3 and T = 4.8 MK.

 

 

 

 

“No evidence was found for emission or absorption lines. … If the source is a magnetar, then the absence of a proton cyclotron line strongly constrains magnetar atmosphere models and hence the magnetic field strength of the neutron star.” B fields in the 2 to 10 times 10^14 G range are excluded and this is consistant with a dipole field of B = 1.3 x 10^14 G at the polar cap estimated from pulsar spin-down.

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4.3 HETG-related Software: Development, Evaluation, and Support

 

ATM atmosphere model tables were made available for use in XSPEC/ISIS. Interpolation schemes and a distributed computing method of creating the tables were developed as well.

 

 

4.4 Presentations (January)

 

S.C. Gallagher, “Chandra Spectroscopy and Imaging of the Seyfert Galaxy NGC 5506” (poster), AAS, Seattle, Jan. 2003.

A. Fredericks, “Spatially Resolved Plasma Diagnostics with X-ray Emission Lines of 1E0102.2-7219” (poster), AAS, Seattle, Jan. 2003.

M. Jimenez-Garate, “Observation of an Orbiting Photoionized Plasma in EXO 0748-676 with the Chandra HETG” (talk), AAS, Seattle, Jan. 2003.

R.R. Gibson, “The High Resolution X-ray Spectrum of MR 2251-178 Obtained with the Chandra HETGS” (poster), AAS, Seattle, Jan. 2003.

M.D. Stage, “Fitting Chandra Spectra of Thermally Emitting Neutron Stars with the ATM Model” (poster), AAS, Seattle, Jan. 2003.

N.S. Schulz, “Magnetically confined Plasmas in Very Young Massive Stars” (talk), AAS, Seattle, Jan. 2003.

T. Jeltema, “The Evolution of Cluster Substructure” (talk), Carnegie Observatories Centennial Symposium III: Clusters of Galaxies, Pasadena, Jan. 2003.

A. Juett, “Neon-Rich Degenerate Donors in Ultracompact LMXBs” (talk), Ultracompact Binary Workshop at KITP Santa Barbara, Feb.1-2 2003.

 

 

 

4.5 Publications (January), see also: http://space.mit.edu/csr_pubs.html

 

Not aware of any HETG-group publications in January.

 

 

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5.0 Systems and Engineering Support

 

 

5.1 Documentation and “Design Knowledge Capture” and 5.3 Anomalies, Insert/retract, etc. Support

 

No activities in these areas in January.

 

5.2 Spares Retest and Test Instrumentation

 

X-GEF was up and running at the end of January after repairs – vacuum storage retests to take place in February.

 

 

 

6.0 Management

 

6.1 Program Office & NASA Support

 

No direct MSFC-related actions in January.

 

6.2 MIT-internal management activities

 

MIT responded to RFP from SAO for ’05-and-beyond funding on time.

For HETG postdoc hiring: organized the received applications; reviewed all applications; made initial ordering of applicants and starting inviting them for interview visits.

Evaluation and selection of candidates for Administrative Assistant position carried out.

 

 

7.0 Open Issues, Problems, etc.

 

There are no known critical open issues or problems regarding the HETG.

 

Appendix A. GTO Observation Status Tables

 

Notes:

1.    Entries indicating progress during this period are shown in this font.

2.    For CSR Publication references (CSR-YY-NN) see http://space.mit.edu/csr_pubs.html

3.    Up-to-date observation information can be obtained from http://cxc.harvard.edu/cda/ using WebChaSeR .

 

Cycle 4

Object Science Theme	AO	Obs ID	Seq. No.	Expos. (ks)	Observer / Analyst	Start Date	Comments & Analysis	Talks and Publications
4U 1626-67 XRB	4	3504	400257	[100.0]	N. Schulz	[6/3/03]	Prop. No.: 04400027 (Cycle 1 obs. also)
Sco X-1 XRB	4	3505	400258	[15.0]	N. Schulz	[5/9/03]	Multi-wavelength obs organized. Parameters finalized[12/02]. Prop. No.: 04400046
H1426+428 IGM	4	3568	700630	[102.0]	T. Fang	[9/11/03]	Prop. No.: 04700987
Mrk 290 AGN	4	3567 4399	700629	[165.0] [ 85.0]	J. Lee	[10/8/03] [10/6/03]	FUSE proposal submitted for coord. Obs. Prop. No.: 04700988
TV Crit “Cool” Stars	4	3728	200198	[100.0]	D. Huenemoerder	[3/5/03]	Prop. No.: 04200007, Selected in peer review![6/02]
E0102 SNR	4	3828	500307	[140.0]	K. Flanagan, D.Dewey	12/20/02	Measure counts in lines. S-S analysis of Ne X line; arfs made. Quick look images. Data in-house and look good. Parameters OK.[12/02]

Cycle 3

Object Science Theme	AO	Obs ID	Seq. No.	Expos. (ks)	Observer / Analyst	Start Date	Comments & Analysis	Talks and Publications
MRC 2251-178   AGN	3	2977	700416	148.5	J. Lee/ H. Marshall, R. Gibson	9/11/02	Re-analyzed, hlm IDL scripts used; import to ISIS[12/02]. A few line Ids at 3-sigma; ISIS scripts.[10/02]	AAS03
NGC 7469 AGN	3	3147 (+2956 Kriss GO)	700586	69.8, 79.8	J. Lee/ H. Marshall	12/13/02	Analyzed data, id absorp lines. Data in-house, look good.[12/02] w/HST.
1H 0414+009   IGM, AGN	3	2969, 4284	700408	50.8, 36.9	T. Fang, S. Gallagher	8/1/02	Shows lovely power law.[9/02] First pass through data. Data in-house.[8/02]
GX 349+2   XRB, ISM	3	3354	900193	35.2	N. Schulz, A. Juett	4/9/02	For ISM study; Observed on 4/9; data available 5/2 [4/02]	Santander,’02 AAS00, AAS01
NGC 2362 Tau CMa “Hot” Stars	3	2525, 2526	200133, 200134	44.5, 43.8	N. Schulz, P. Wojdowski, J. Kastner/RIT	3/28/02, 4/23/02	Analysis continues.[6,9/02] Previewed the data.[5/02] Observed 4/23 [4/02]	Patzcuaro, ‘02
1ES 1028+511   IGM, AGN	3	2970, 3472	700409	21.8, 69.6	T. Fang, S. Gallagher	3/27/02, 3/28/02	Shows lovely power law.[9/02] First pass through data.[8/02]
3C 279   IGM, AGN, Jet	3	2971	700410	108.2	T. Fang, H. Marshall	3/21/02	Overlay radio contours on jet.[8/02] Data reduced; jet seen in zo image.[5/02] Data are in-house [3/02].
IRAS 18325-5926 AGN	3	3148, 3452	700587	56.9, 51.1	J. Lee, S. Gallagher	3/19/02, 3/23/02	XTE and SAX obs analyzed.[12/02] Multi obs.y collaboration…[7/02]	Paper draft w/ Iwasawa[12/02]

Cycle 2

Object	AO	Obs ID	Seq. No.	Expos. (ks)	Observer / Analyst	Start Date	Comments & Analysis	Talks and Publications
Cyg X-2   XRB, ISM	2	1016	400094	15.1	N. Schulz, A. Juett	8/12/01	Fit O, Fe, Ne edges.[7/02] ISM study: cold absorption edges[5/02]	Santander,’02 AAS00, AAS01
Cas A   SNR	2	1046	500112	69.9	K. Flanagan, D.Dewey, M. Stage	5/25/01	Began NEI fits to Si knot image for continuum.[8/02] Si knot analysis started [3/02].	High-Res UK talk.[10/02] CRC Royal Soc.’02
4U 0142+61   iNS, AXPs	2	1018	400096	25.4	N. Schulz, A. Juett	5/23/01	Finishing additional analysis [3/02]	ApJ, 2002, 568, pp. L31, HEAD-2002[4/02] CSR-02-16[3/02]
Mrk 766   AGN	2	1597	700213	90.5	P. Ogle, J. Lee	5/7/01	XTE data simultaneous w/obs.[10/02] Paper in preparation [4/02]
NGC 4696 Gal.	2	1560	600117	85.8	M. Wise	4/18/01	To be analyzed.
EXO 0748-676   XRB	2	1017	400095	49.0	N. Schulz, H. Marshall, M. Jimenez-Garate	4/14/01	Photo-excitation rates.[10/02] Performed abundance measurements.[8/02]	Revise/reply to ref. report. AAS03. HEAD02
SS 433   XRB, Jet	2 2 1	1019, 1020, 106	400097, 400098, 400019	23.7, 23.0, 28.9	H. Marshall, N. Schulz	3/16/01, 11/28/00, 9/23/99	Complete analysis of Cycle 2 data	CSR-02-01, CSR-01-78
1H 1821+643   AGN, IGM	2	1599	700215	101.3	P. Ogle, T. Fang	2/9/01		CSR-02-16.5[4/02], CSR-01-69
Iota Orionis   “Hot” Star	2	599, 2420	200075	37.6, 12.9	N. Schulz, P. Wojdowski	2/7/01, 2/8/01	DEM distribution derived.[9/02] Make arfs for one-ion analysis.[8/02] Data reviewed[5/02]	Patzcuaro, ‘02
TY Pyx, HD77137 “Cool” Star	2	601	200076	49.8	D. Huenemoerder	1/3/01	Preliminary analysis done.	(spectrum in CSR-02-02)
N103B   SNR	2	1045, 2410, 2416	500111	74.0, 25.7, 17.6	K. Flanagan, J. Migliazzo, D. Dewey	1/1/01, 1/3/01, 1/2/01	New fits, abundance plots, one-ion fits.[9/02] Fit vpshock w/APED lines…[7/02]	High-Res UK talk.[10/02] Poster: HEAD02[4/02]
NGC 5506   AGN	2	1598	700214	90.0	P. Ogle, J. Lee, S. Gallagher	12/31/00	XTE simult obs reduced; spectral and image analysis progress.[12/02] ISIS scripts for fluxes and energies.[10/02]	AAS’03 Paper in prep.[4/02]
ZW 3146   Clust.	2	1651	800119	167.8	M. Wise	12/25/00	MEG +/-1 spectrum.[10/02] Include background subtraction.[7/02] Re-analysis continued w/ ISIS[6/02]; started[5/02]	High-Res UK talk.[10/02] Cluster paper in draft[5/02]

Cycle 2, above.

 

 

 

Cycle 1

Object	AO	Obs ID	Seq. No.	Expos. (ks)	Observer / Analyst	Start Date	Comments & Analysis	Talks and Publications
NGC 1068 AGN	1	332	700004	46.3	H. Marshall, P. Ogle, J. Lee	12/4/00	Examine zeroth-order pileup[5/02]	Paper in submitted[5/02]
4U 1626-67 XRB	1	104	400017	40.0	N. Schulz	9/16/00	Analysis complete.	CSR-01-81
AR Lac     “Cool” Star	1	6,7,8, 9,10,11	20000N: 4,5,6,7,8,9	32.5,7.5, 7.5,32.6, 7.3,7.3	D. Huenemoerder	9/11/00- 9/19/00	Fixed errors.[12/02] Analysis complete.	Submitted to ApJ. Revised manuscript.[12/02] CSR-01-112
Abell 1835     Clust.	1	49896 511	800019	9.8 127.0	M. Wise	8/25/00 8/26/00	MARX simulations (1T, 2T, etc.)[10/02] Include background subtraction.[7/02]	High-Res UK talk.[10/02] Cluster paper in draft[5/02]
N132D   SNR	1	121, 1828	500008	22.3 77.6	K. Flanagan, D. Dewey	7/19/00 7/20/00	Fe and O line ratios from many regions/features	CSR-01-10,26, Y2Chandra01
TW Hydra “Cool” Star	1	5	200003	48.3	D.Huenemoerder, J. Kastner	7/18/00	Analysis complete.	CSR-02-02, CSR-01-29
NGC 4486, M87   Gal., AGN, Jet	1	241	600001	38.5	M. Wise	7/17/00	Absorption and cooling maps.[9/02]
GX 301-2 XRB	1	103	400016	40.0	N. Schulz	6/19/00	Re-analysis initiated [3/02]	Draft paper begun [3/02], AAS00
NGC 1399   Gal.	1	49898, 240, 2389	600214 600000	13.2 44.1 14.8	M. Wise	5/8/01 6/15/00 5/8/01	Examination begun.[6/02]
Vela X-1 XRB	1	102	400015	28.4	N. Schulz	4/13/00		ApJ, 2002, 564, L21
MCG –6-30-15 (w/Fabian)     AGN	1	433	700105	128.2	H. Marshall, J. Lee	4/5/00	Helped with XMM obs [12/02]analysis. XSTAR /Kallman; Fe UTAs (Ming); LLB edges.[7/02]	Draft 1 of XMM paper. Lee et al 2002, CSR-02-15 [3/02], CSR-01-02
NGC 4151 AGN	1	335	700007	48.0	H. Marshall, P. Ogle	3/5/00		CSR-00-87
PSR B0656+ 14 iNS	1	130	500017	38.1	H. Marshall	11/28/99	LETG/HRC	Paper accepted, CSR-02-12[3/02]
PKS 2149-306 IGM, AGN	1	336, 1481	700008	36.0 54.8	H. Marshall	11/18/99 11/20/99		CSR-01-67
Trapezium, Theta Ori   “Hot” Stars	1	3, 4	200001 200002	50.1 31.3	N. Schulz, D. Huenemoerder	10/31/99 11/24/99	Add new archive obs. Theta Ori A and E line fluxes.[10/02]	Draft papers III and IV [9/02]. CSR-01-118, CSR-00-89, CSR-00-75
4U 1636-53 XRB, ISM	1	105	400018	29.8	N. Schulz, A. Juett	10/20/99	Fit O, Fe, Ne edges.[7/02]	Santander, AAS00, AAS01
PKS 2155-304   AGN, IGM	1	337, 1703, 1705	700009 700261 700263	39.1 26.2 25.8	H. Marshall, T. Fang, J. Lee	10/20/99 5/31/00 5/31/00	HETG and LETG w/ACIS-S	ApJ Letter in press.[6/02] Paper accepted.[4/02]
Cyg X-1   XRB	1	107, 1511	400020	2.5 12.6	N. Schulz, H. Marshall, J. Miller	10/19/99 1/12/00	Second paper continuing[5,6/02] Paper…[3/02]	ApJ, 2002, 564, pp. 941 (CSR-01-57), HEAD00
II Peg, HD 224085 “Cool” Star	1	1451	200010	43.3	D. Huenemoerder	10/17/99	Analysis complete.	CSR-01-50
Q0836+7104 IGM, AGN	1	1450, 1802	700006	61.0 14.1	H. Marshall	10/17/99 8/25/00		CSR-01-67
PKS 0745-191 Clust.	1	510, 1509, 1509	800018	45.3, 40.4, 39.9	M. Wise	10/14/99 4/25/00 3/4/00	MEG +/-1 spectrum.[10/02] Include background subtraction.[7/02]	High-Res UK talk.[10/02] CSR-02-32[8/02] Responded to referee report.[6/02] ApJ submitted, Hicks et al. [3/02]
PSR B0833-45, Vela Pulsar iNS	1	131	500018	36.1	H. Marshall	10/12/99		HEAD00
NGC 1275 AGN	1	333, 428	700005 700201	53.2 25.0	H. Marshall, P. Ogle	10/10/99 8/25/00	Determined PL spectral slope	No pubs of note
E0102   SNR	1	120, 968	500007	88.2, 49.0	K. Flanagan, J. Houck, A. Fredericks, D.Dewey	9/28/99 10/8/99	Ejecta masses and errors. Plasma diag.s section work; fluxes.html[12/02]. Sasaki models compared.[10/02]	AAS’03 Poster. High-Res UK talk.[10/02] Final polishing of ApJ paper [3-6/02]; CSR-01-10,11,24,25,26, Y2Chandra01
Object	AO	Obs ID	Seq. No.	Expos. (ks)	Observer / Analyst	Start Date	Comments & Analysis	Talks and Publications

Cycle 1, end.