HETG

Follow-on Science Instrument

Contract NAS8-01129

 

Monthly Status Report No. 010

December 2002

HETG Science Theme: X-Ray Binaries

 

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:

                                                Deborah Gage             dgage@space.mit.edu

                                                Gail Monahan              gmonahan@mit.edu

 

MIT-Internal Hardcopy:

                                                Claude Canizares         Room 3-234 (via Gail Monahan)

                                                Deepto Chakrabarty     Room 37-501 (via Deborah Gage)

                                                Kathryn Flanagan        Room NE80-6103 (via Deborah Gage)

 

 

 

 

 

 

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
Dec. 3	Chandra Quarterly Review	HETG attend
Dec. 5-8	SIRTF Observation Planning Workshop	S. Gallagher attend
Dec. 9-13	XXI "Texas" Symposium on Relativistic Astrophysics , Florence, Italy	J.Lee, AGN
Dec. 13	Chandra AO-5 out

 

 

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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. There were 2 GO and 2 GTO observations carried out with the HETG in December 2002. Both GTO observations are HETG GTO observations and the data look good.

 

3.2 Science Support to CXC, SWG, etc.

 

No science support of note in December 2002.

 

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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. In December the final HETG Cycle 3 GTO observation was completed, the AGN NGC 7469, as well as the first HETG GTO observation of Cycle 4, the SNR E0102. Both data sets look good.

 

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 X-Ray Binaries theme are presented with help from Norbert Schulz and Mike Nowak.

 

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	Not yet reported [Jan.’03]
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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X-Ray Binaries Research Progress

 

Introduction to X-Ray Binaries

         X-ray binaries, as the name implies, consist of two objects: a compact object – a neutron star (NS) or black hole (BH) - and a companion star. Mass is transferred from the companion and falls toward the compact object often creating an accretion disk (AD) around it. X-ray heating and emission occur in the accretion disk and as mass leaves the accretion disk and lands on (NS) or falls into (BH) the compact object. One of the main classifications of the systems is based on the mass of the companion: for HMXBs the companion is a massive star (> 2 M_solar), and for LMXBs the companion has a mass less than or about 1 M_solar. The Figure at right shows a scientist-artist's image of a binary (taken from:

http://www.astro.soton.ac.uk/~rih/binsim.html .)

 

A variety of parameters determine the behavior of this generic system: primary mass and type (NS or BH); companion's mass and evolutionary status; orbital period; mass transfer rate and mechanism (Roche lobe in LMXB or stellar winds in HMXB); size and composition of the AD and any AD streams; brightness of continuum emission from the central region; the

existence of hotspots in the AD; a photo-ionized AD corona and/or atmosphere; jets from the AD/compact object; the strength and orientation of any magnetic field (NS); compact object rotation rate; the viewing angle of the system - to name a few!

 

However, in spite of this variation, there are some general categories for these objects that help to organize them besides the companion mass (LMXB or HMXB.) “Atoll sources” are thought to have a NS with a weak magnetic field; “z-sources” likely have a NS with a strong magnetic field. An x-ray pulsar has a high-rate rotating magnetic NS.

 

The Figure at left shows a close-up of an X-ray pulsar with its rotation axis offset from the magnetic field poles. Matter falling on the NS is funneled to the magnetic poles and may produce local “hot spots” there. Instabilities in the in-falling stream may be the source of quasi-periodic oscillations (QPOs; high-frequency modulations of the flux.)

 

 

 

These sources are too small to be resolved with current X-ray telescopes so they appear as point sources. Some extra information can be extracted from systems which we observe at high inclination, that is approaching edge-on. The orbital motion then causes our line of sight to vary as if we were walking around the system and seeing it from different angles. By studying the source spectra at these different orbital phases, including eclipses for some systems, we are better able to tease out and test the system geometry.

 

 

 

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The Figure above is from: http://imagine.gsfc.nasa.gov/docs/science/know_l2/binary_flash.html .

 

A useful, extensive reference is “Flourescent iron lines as a probe of astrophysical black hole systems”, by C.S. Reynolds and M.A. Nowak, to be published in “Physics Reports”, 2003 (astro-ph/0212065).

 

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Summary of X-Ray Binaries GTO Observations and Activities

Ten XRBs are included in cycles 1-4 of the HETG GTO program. These XRBs cover a range of types as indicated in the Table below; all of them are in the Galaxy. (Extra-galactic XRBs are too dim for detailed study but note that the near-by LMC X-1 and LMC X-3 were observed in Cycle 1 of the ACIS GTO program.)

The accretion disk is a key component of XRB line emission and so we also have on-going efforts to model accretion disk emission in our science program as described further below. Other investigations include radiative transfer in stellar winds (HMXBs) and BH binary population synthesis from stellar evolution models.

Finally, because many XRBs are bright continuum sources they can be used to probe the absorption details of the interstellar medium (ISM) – this is an extensive topic itself and will be treated in detail in a future report.

 

Obs cycle	Obsid(s)	Name	ISM?	Type*	Period	Comments
4, 1	3504, 104	4U 1626-67	---	LMXB: PS	42 m	Magnetic NS; ultra-compact
4	3505	Sco X-1	Yes	LMXB: NS,Z	18.9 h	Bright! Fe XXV, ADC, ISM (XAFS?)
3	3354	GX 349+2	Yes	LMXB: NS,Z	14.9 d?	ISM Fe-L and O edges
2	1016	Cyg X-2	Yes	LMXB: NS,Z	9.8 d	Bursts, super-orbital P, 0.5 Crab
2	1017	EXO 0748-676	---	LMXB: NS	3.8 h	Bursts, eclipses, dips
1, 2	1020, 1019, 106	SS 433	---	HMXB?: ?	13 d	Precessing jets, super-orbital P
1	103	GX 301-2	---	HMXB: PS	41.5 d	Eccentric orbit, wind accretion
1	102	Vela X-1	---	HMXB: PS	9 d	Winds
1	105	4U 1636-53	Yes	LMXB: NS,A	3.8 h	Bursts
1	107, 1511	Cyg X-1	Yes	HMXB: BH	5.6 d	Fe-line structure, wind

* Key: Z = Z source, A = Atoll source, PS = X-ray pulsar, NS = neutron star, BH = black hole

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Cyg X-1: Black hole candidate – stellar wind absorption

From the papers: “The First High-Resolution X-ray Spectrum of Cygnus X-1: Soft X-ray Ionization and Absorption”, ApJ, 565, 1141 and “Highly Ionized Absorption in the X-ray Spectrum of Cyg X-1”, H.L. Marshall et al., astro-ph/0111464.

In Cyg X-1 we observe ionized absorption of the (suspected) black hole’s continuum X-ray by the gravitationally focused wind from the massive companion; the amount and character of the absorption depends on the orbital phase at which we observe it.

For our continuous clocking observation obsid 1511, we see ionized absorption from a large range of elements, e.g, Ne, Mg, and Fe in the figure below. This figure also shows that many of these lines at this particular phase are red shifted – appearing slightly to the right of the rest wavelengths indicated by the dashed lines. At this phase we expect the wind to be moving away from us towards the accreting black hole, hence the red-shift.

 

 

 

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4U 1626: An ultra-compact system – accretion disk emission

         From the paper: “Double-Peaked X-ray Lines from the Oxygen/Neon-Rich Accretion Disk in 4U 1626-67”, N.S. Schulz et al., ApJ, 563, 941.

The figures below show portions of the spectrum from 4U 1626 for the Neon and Oxygen Lyman alpha lines. Here they show a distinct doubling as well as a broadening indicating velocities of thousands of km/s. The lines and their velocities are consistent with their origin in the accretion disk surrounding the compact object.

In addition to these accretion disk signatures we also see evidence for enhanced neutral absorption by cold, local material. Under the assumption that this is condensed material previously expelled from the system (post-accretion) we can put constraints on the nature and size of the donor star. Based on the inferred abundance ratios we argue that the mass donor is a 0.02 M_solar C-O-Ne or O-Ne-Mg white dwarf with a chemically fractionated core which has previously crystallized.

 

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Vela X-1: Wind accreting source seen in eclipse

         From the paper: “The Ionized Stellar Wind in Vela X-1 During Eclipse”, N.S. Schulz et al., ApJ, 564, L21.

We observed the photoionized plasma from the wind of Vela X-1 in eclipse – blocking out the bright continuum. The spectrum below shows several features. One component comes from the photoionized plasma and we observe many lines from various ionization states (blue in the figure.) We also see in the spectrum a few radiative recombination continua which allow us to determine the temperature of the optically thin ionized plasma to be about 120,000 K. In contrast, there is evidence for a much cooler component in the wind that has high column densities and appears to be clumped. At this orbital phase we observe a variety of fluorescence lines from Si, S, Ar, Ca, and Fe (green curves) originating in the wind. In the case of Si and S we are also able to separate various low ionization stages for the first time.

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SS 433: Jets from an accreting system

         From the paper: “The High-Resolution X-ray Spectrum of SS 433 Using the Chandra HETGS”, H.L. Marshall et al., ApJ, 564, 941.

         In this object many emission lines of highly ionized elements are detected with relativistic blue and red Doppler shifts, e.g., the Fe lines in the spectrum below. The emission is consistent with a thermal origin along a conical jet as diagramed here. The inferred velocity is 0.27c which is somewhat larger than the velocity seen in optical emission suggesting the X-rays originate closer-in to the jet source. Modeling the thermal emission gives electron densities dropping from 2x10^15 to 4x10^13 per cm^3 at distances of 2 to 20 x 10^10 cm.

         Surprisingly all of the X-ray emission can be accounted for by this jet emission and there is no indication of continuum emission from an accretion disk!

 

 

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Accretion disk modeling and EXO 0748

         From the paper: “The Structure and X-ray Recombination Emission of a Centrally Illuminated Accretion Disk Atmosphere and Corona”, M.A. Jimenez-Garate, ApJ, 581, 1297.

         The bright continuum radiation from the central object heats and creates an atmosphere above the denser accretion disk. We have carried out extensive modeling of this process to understand the structure of the atmosphere and the expected emission from it, e.g., the model spectrum below.

This modeling is relevant to EXO 0748, an edge-on low inclination source that shows dips, eclipses, and bursts. It has a short orbital period allowing many orbits to be observed. In order to study the photo-ionized layer on top of its accretion disk we observe the “dips”: when the bright central object is obscured by parts of the disk. XMM-Newton saw a warm absorber from O; we see warm absorption from Mg as well.

 

 

 

 

 

 

 

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X-Ray Binaries Plans and Further Work

 

• Compile a catalogue of sectra from bright X-ray binaries correct using our pileup model.

• Continue to investigate the precessional dependance of the lines in SS 433.

• Study the effect of resonance scattering in ionized stellar winds.

• Study models of photoionization in illuminated accretion disks.

• Study the X-ray spectra of black hole candidates with respect to their binary orbit.

• Look for absorption lines in X-ray burst spectra.

 

 

 

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

 

Analysis Software

Pileup correction software is used for the dispersed grating spectra for many XRB sources because they are so bright. Likewise, Continuous Clocking (CC) mode is often used for these observations and so CC software improvements have been driven by XRB observations. The brightest of all, Sco X-1, will allow/require light curve and timing software that works on dispersed data. The use of diffraction orders higher than the first is possible and necessary for these sources and so analysis s/w and calibration values for high-orders are put to use.

 

Modeling Software

In-house resonance scattering code is being developed for stellar wind systems. As mentioned above, we are carrying out photoionization modeling of accretion disk atmospheres. We are also modeling the electric and di-electric recombination in photoionized plasmas.

 

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4.4 Presentations (November and December)

 

A. Juett, “High Resolution Spectroscopy of Ultracompact Binaries”, X-ray Binaries in the Chandra and XMM-Newton Era, Cambridge, MA.

M.A. Jimenez-Garate, “X-ray Spectroscopy and Modeling of Low-Mass X-ray Binaries”, X-ray Binaries in the Chandra and XMM-Newton Era, Cambridge, MA.

N. Schulz, “Highly Resolved X-ray Spectra from Galactic Objects with Chandra”, X-ray Binaries in the Chandra and XMM-Newton Era, Cambridge, MA.

P. Wojdowski, "A Sobolev Monte Carlo Scattering Method from HMXB Winds", X-ray Binaries in the Chandra and XMM-Newton Era, Cambridge, MA.

M. Stage, “Recent results fitting ATM atmosphere models to Chandra spectra of thermally radiating neutron stars”, 34^th COSPAR, Houston TX. [poster]

J. Migliazzo, “N103B: Chandra HETG Spectrometer Observations and Results”, 34^th COSPAR, Houston TX. [poster]

J. Lee, “High Resolution X-ray Spectra of Galactic and Extragalactic Black Hole Systems”, XXI Texas Symposium on Relativistic Astrophysics, Florence, Italy. [poster]

 

 

 

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

 

M.A. Jimenez-Garate, N.S. Schulz, and H.L. Marshall, “Discrete X-ray Signatures of a Photoionized Plasma Above the Accretion Disk of the Neutron Star EXO 0748-676”, ApJ submitted.

S. Gallagher et al., “Probing Quasar Outflows: X-ray Insights”, Advances in Space Research, submitted; available at http://www.ociw.edu/ociw/symposia/series/symposium1/proceedings.html .

T. Jeltema et al., “X-ray Source Population in the Elliptical Galaxy NGC 720 with Chandra”, ApJ accepted; astro-ph/0211192.

N. Schulz et al., “X-ray Modelling of Very Young Early Type Stars in the Orion Trapezium: Signatures of Magnetically Confined Plasmaas and Evolutionary Implications”, submitted.

D. Dewey, “Extended Source Analysis for Grating Spectrometers”, High Resolution X-ray Spectroscopy with XMM-Newton and Chandra, Proceedings of the international workshop held at the Mullard Space Science Laboratory of University College London, Holmbury St Mary, Dorking, Surrey, UK, 2002; available at: http://www.mssl.ucl.ac.uk/~gbr/rgs_workshop/workshop_ADS_index.html .

 

 

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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

 

A new activity was initiated: to support evaluation of the effects of radiation on the ACIS optical blocking filters (windows) by testing the radiation-exposed grating samples at MIT – samples were identified.

 

5.2 Spares Retest and Test Instrumentation

 

Last month we reported new cables were ordered for the PSPC detector ; these arrived and worked fine. Continued PSPC problems lead us to send the PSPC preamps and AIM206 processing electronics back to Ordella for repair at the end of December.

We now plan to run qualification tests and then grating re-tests in the Jan.-Feb.’03 time frame.

 

 

6.0 Management

6.1 Program Office & NASA Support

 

Supported the Quarterly Review on 12/3.

 

6.2 MIT-internal management activities

 

Supported internal work to respond to RFP from SAO for ’05-and-beyond funding. Supported internal hiring activity for an administrative assistant.

 

 

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 the WebChaSeR link.

 

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]	Parameters finalized. Reviewed parameters.[9/02] 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]	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	Data in-house and look good. Parameters OK.

 

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. A few line Ids at 3-sigma; ISIS scripts.[10/02]	AAS03 abstract
NGC 7469 AGN	3	3147 (+2956)	700586	69.8, 79.8	J. Lee/ H. Marshall	12/13/02	Data in-house, look good. w/HST Supplement w/Kriss GO.
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. Multi obs.y collaboration…[7/02]	Paper draft w/ Iwasawa

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]	Submitted Paper. AAS03 abstract. 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. ISIS scripts for fluxes and energies.[10/02]	AAS’03 abstract.[10/02] 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. Analysis complete.	Revised manuscript. Co-authors comments received.[9/02] 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] Examination begun.[6/02]
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 analysis. XSTAR modeling w/Kallman; Fe UTAs (Ming); LLB edges.[7/02]	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	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 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	Plasma diag.s section work; fluxes.html. Sasaki models compared.[10/02] Allowed plasma region, abundances; shelf and arc fluxes.[9/02]	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.