HETG

Follow-on Science Instrument

Contract NAS8-01129

 

Monthly Status Report No. 007

September 2002

HETG Science Theme: "Cool" 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

ES84/Martin Weisskopf, MSFC            martin@smoker.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
Sept.4,5	Chandra Quarterly and IAR, Cambridge, MA	HETG participated
Sept. 4-6	Workshop on X-ray surveys, Santander, Spain	(N. Schulz)
Sept. 9-13	Wind, Bubbles, and Explosions, Patzcuaro, Mexico	(N. Schulz)
Sept. 23-27	The Physics of Relativistic Jets in the Chandra and XMM Era, Bologna, Italy	(S. Markoff)

 

 

 

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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 6 targets observed in 9 observation intervals by the HETG in September 2002. The target MRC 2251-178 (obsid 2977) is an HETG GTO target in cycle 3 and its data are in-house and being examined.

 

3.2 Science Support to CXC, SWG, etc.

 

There were no major support activities besides supporting the IAR in early September. We are on track to provide POG input by the end of October.

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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. This month data from the recent Cycle 3 GTO observation of the AGN MRC 2251-178 were received and processed.

 

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 “Cool Stars” theme are presented.

 

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	September, 2002. Dave Huenemoerder
“Hot” Stars	Hot Star		Not yet reported [Oct.’02]
X-ray Binaries & Accretion Disks	XRB	MJ-G,AJ,nss,hlm	Not yet reported [Nov.’02]
Supernova Remnants	SNR	KAF,DD,JMM, AF,jh,gea,tp	May, 2002. Dan Dewey
Isolated Neutron Stars	iNS	MDS,hlm, nss	Not yet reported
Galaxies & Clusters of Galaxies	Gal., Clust.	TJ,mw,jh	August, 2002. Michael Wise, Tesla Jeltema
Active Galactic Nuclei and Jets	AGN, Jet	SG,RG,hlm	June, 2002. Herman Marshall
Inter-Stellar Medium	ISM	AJ,nss	Not yet reported [Dec.’02]
Inter-Galactic Medium	IGM	SG,RG,hlm	July, 2002. Taotao Fang

 

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“Cool” Stars Research Progress

Introduction to Stars

Stars are the main actors in creating variety in the universe. Their fusion “burning” of primordial H and He creates the elements we are made of and illuminates the universe.

In studying stars we consider two general categories: “Cool stars” which include stellar coronae, active binaries, and low-mass pre-main sequence stars; and “Hot” stars which consist of massive stars, associated winds and shocks, and stars in young star clusters.

 

Cool stars, those of spectral type later than F0, are frequently X-ray sources with band-limited luminosities (0.1-10 keV) on the order of 10^31 ergs/s. They are particularly active if they are rapidly rotating, as the tidally-locked RS CVn (spotted stars) binaries are. The activity is hypothesized to be due to a magnetic dynamo resulting from differential rotation, as seen in the Sun. The dynamo is presumed to be active only in cool stars because they have a convection zone needed to drive the dynamo. Young, low-mass stars are also strong X-ray sources, presumably because they have not yet lost their natal angular momentum. Stars hotter that spectral type F are fully radiative with no convection dynamo; for example, A-stars are well known to be X-ray dark.

 

Although the surface temperature of “Cool” stars is less than 10,000 degrees, the magnetic dynamo can create tempertures in the millions of degrees in the star’s cornoa. This coronal X-ray emission is a small fraction of the total stellar luminosity (10^-6 in the case of the Sun, 10^-3 in the case of the most active stars), but this energy is the primary radiative manifestation of the atmospheric heating by the magnetic dynamo; it represents the generation and rearrangement of magnetic fields from the star, and is an important source of interaction of the star with the surrounding medium.

 

With HETGS X-ray spectra, we can now clearly resolve the coronal X-ray emission into line and continuum components. As the comparison with an ASCA (CCD) spectrum at right demonstrates -- we can now “see the forest-floor between the trees”. From these measurements we can determine the plasma temperature structure, density, elemental abundances, and time variability. If we can detect any eclipses or rotational modulation, then we may also be able to constrain the geometry of the emitting structures.

 

Another feature of an active corona is flaring activity. Injection of energy through high-energy electrons causes heated plasma to expand while at the same time being confined to loop structures by the local coronal magnetic fields. Such loops are imaged on the Sun by TRACE and Yohkoh satellites and provide models we can apply to other stars.

 

For more fantastic images and an overview of the Solar corona, see

http://vestige.lmsal.com/TRACE/POD/NAS2002v2.html and

http://isass1.solar.isas.ac.jp/ .

For more basic information on the Sun, Stars, and Stellar Evolution see

Lessons 3, 4, and 5 at http://cosmos.colorado.edu/astr1120/hypertext.html

 

"The dynamo is at the core of the activity problem. As argued in here, stellar activity, and therefore the stellar dynamo, is key to understanding life in the Universe and Earth's habitability. There is, however, no comprehensive model of solar and stellar magnetic activity.” K. Schijver (http://canopy.lmsal.com/schryver/ .)

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Summary of “Cool Star” GTO Observations and Activities

The stars in the HETGS GTO program are listed in the table below. There are five “cool” stars among them and some highlights of the observations are presented in the following pages. II Peg is a classical, highly active, single-lined RS CVn binary. AR Lac is a 1.98 day period RS CVn binary comprised of a K0 subgiant and a G dwarf. TW Hydra a pre-main-sequence star which is nearby, isolated, and a classical T Tauri object (artist’s impression at right): it's X-ray spectrum is unlike any of the other cools stars, possibly due to an accretion stream. A related object, TV Crt, has been accepted for AO-4. Finally, TY Pyx is a 3-day period near-totally eclipsing RS CVn system which showed eclipse modulation and a short flare.

 

 

Obs cycle	obsid	Type	Target	Binary? (period)	Flare(s) seen?	Comment
1	1451	Cool	II Peg	7 d	yes	RS CVn binary; “two-ribbon” flare
1	3,4	Hot	Trapezium	---	---	Many hot (and cool) stars
1	5	Cool	TW Hydra	isolated	yes	extremely cool, very low iron abundance, high neon abundance.
1	6-11	Cool	AR Lac.	1.98 d	yes	RS CVn binary;
2	601	Cool	TY Pyx.	3 d	yes	near-totally eclipsing RS CVn
2	599, 2420	Hot	Iota Orionis	---	---	Two O-stars; colliding winds?
3	2525, 2526	Hot	NGC 2362	---	---	Young (5-7 Myrs ) star cluster in the Galaxy; w/ massive stars
4	3728	Cool	TV Crit.	Pair of binaries,1” sep.	Not yet observed	weak-lined T Tauri star; solar-mass “Vega-type'' (dust-disk) system; in TW Hydra assoc.

 

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HETG Observation of II Peg

 

II Peg (AO-1; Obsid 1451) is a classical, highly active, single-lined RS CVn binary with a period of 7 days. It is heavily spotted – the optical light curve amplitude has been as large as 0.5 magnitude. As shown at right, the HETGS spectrum clearly resolves a large number of emission lines peaking above the background continuum level. The brightest lines are from Ne and Oxygen and Fe lines are about 0.1 of Solar values.

 

 

The HETGS observation showed a steady flux for about 25 ks, then an increase by about a factor of 3 in a classic Solar "two-ribbon flare" profile, then began a decay as the observation ended. This is shown in the plot at left by the behavior of the continuum level (dense black vertical lines) which is well fit by a flare model (green line.) The fluxes of discrete lines are shown as well.

 

 

A wide range of temperatures exist in II Peg’s corona with different temperatures giving rise to different patterns of emission lines. For a given set of measured lines and continuum it is possible to create a distribution of temperatures causing the emission. This “DEM” analysis has been carried for both the “quiet” pre-flare time and the flaring period of the observation. The plot below shows a broad range of temperatures between 3 million [LogT=6.5] and 100 million [8.0] degrees in the pre-flare state (green.) During the flare the high temperatures are increased with a peak around 45 million [7.65] degrees (grey).

 

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Observations of AR Lac

AR Lac a 1.98 day period RS CVn binary comprised of a K0 subgiant and a G dwarf. Observations were made at 6 times to sample 3 phases twice each, covering quadratures and eclipses as shown in the count-rate plot at right.

There was much intrinsic variation, including one moderate flare (blue, peak at phase 0.47). No observations at repeated phases showed repeatable flux, though the quadrature observations (phase 0.2-0.3) largely overlap in flux. Eclipses were not detected. Both simultaneous and contemporaneous EUVE data were obtained in collaboration with J.Drake/CfA.

Using the “DEM” method mentioned previously (II Peg’s flare temperatures above), a DEM plot for AR Lac’s emission has been created and is shown at left. The solid line is the estmated DEM; the dashed lines give an estimate of the confidence range of the DEM. Features of the DEM are a low temperature (1.6 million [6.2] deg.s) and two high temperature (8 and 23 million [6.9,7.37] deg.s) peaks as well as a high-temp plateau region extending to above 100 million degrees [8.].

 

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Ne and Fe variation in a set of Cool Stars

 

The Sun “is only one example of a large class of stars; a single example provides insufficient constraints to outline a path for dynamo theorists. In order to understand the solar dynamo, we need a population study: look at stars like the Sun, at young stars, old stars, binary stars, exotic stars, ... " K. Schijver (http://canopy.lmsal.com/schryver/ .)

 

The Chandra archive has a growing collection of high-resolution stellar X-ray spectra. Here are assembled HETG spectra of TW Hya and the active, late-type stars AB Dor (a rapidly rotating K dwarf, obsid 16), Capella (obsid 1318), HR 1099 (obsid 62538), AR Lac (6,9), TY Pyx, UX Ari (605), Lambda And (obsid 609), and II Peg in the spectral region encompassing the 13.56 A He-like Ne IX triplet and the 15.01 A Fe XVII line (see also Drake et al. 2001, Canizares et al. 2000, and Huenemoerder et al. 2001).

Spectra are shown as raw counts in the summed MEG +/-1^st orders, in 0.005 A bins, and have been smoothed slightly. They are arranged from top to bottom roughly in order of the Ne IX 13.56 A to Fe XVII 15.01 A ratio, which is more sensitive to abundance than to temperature. Lines labeled are of Ne IX , Fe XVII-XVIII , and O VII.

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“Cool” Stars Plans and Further Work

 

·      AR Lac: finish paper with final revisions of co-author comments.

 

·      TY Pyx: finish detailed analyses

o      Measure line strengths

o      fit the emission measure distribution and abundances

o      extract light curves in continuua and lines

o      examine differences in spectra for different count rates

 

·      TV Crt observations (AO-4) have not been scheduled. This star is a visual double, with 1 arcsec separation, and will present a spatial-spectral data analysis challenge. Continue exploring spatial-spectral analysis methods in preparation for these data.

 

·      Improve the modeling of the density sensitive He-like triplets of Ne IX and Mg XI, which are blended with. Current results on these ratios should be considered preliminary and subject to revision.

 

·      Compare and contrast more ensembles from many observations, both GO and GTO, like the Ne/Fe comparison plot shown above.

 

·      A common feature of most observations to date is that flares are frequent. It may not be possible to detect uncompromised rotational modulation or eclipse signatures, which are crucial to density/volume estimates and magnetic loop models. Consider observations of less active, though fainter, stars for this purpose.

 

 

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

 

Software was created in IDL and in ISIS to support the complex and computationally intense process of creating “emission measure distributions” or DEMs from measurements of the line and continuum fluxes in a stellar spectrum. Various monte carlo techniques and tests were investigated to get accurate error bars on the DEM values.

Modeling techniques are being enhanced. Plasma models have been improved in ISIS with support of J.Houck, P.Wodjowski, and D.Huenemoerder. Efforts are under way or planned to incorporate tabulation of flux measurements and differential emission measure modeling.

 

 

4.4 Presentations (September)

 

N.S. Schulz, “X-Rays from Very Young Massive Stars”, Sept.11, 2002, Winds, Bubbles and Explosions, Patzcuaro, Mexico.

 

 

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

 

No publications this month.

 

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5.0 Systems and Engineering Support

 

5.1 Documentation and “Design Knowledge Capture”

 

No major efforts in this area this month.

 

5.2 Spares Retest and Test Instrumentation

 

Test system software is operational and now the source and detectors’ operation are being check prior to starting retests.

 

5.3 Anomalies, Insert/retract, etc. Support

 

No action on this front.

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6.0 Management

6.1 Program Office & NASA Support

 

Received contract mod for updated GFE equipment list.

 

6.2 MIT-internal management activities

 

Supported drafting of job description for new Administrative Assistant position. Looking into “RAID” disk storage system for use in backing up large but valuable data analysis files.

 

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7.0 Open Issues, Problems, etc.

 

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

 

Thanks for timely approval of Dr. Dewey’s October travel to the UK to participate in the meeting “High Resolution X-ray Spectroscopy with XMM-Newton and Chandra”.

 

A request for foreign travel for Dr. Lee in the amount of $5,900 was sent from MIT dated 9/30/02 and as outlined will support collaboration on a paper on the GTO target MCG—6-30-15 in the UK and presentation of HETG results at the “XXI Texas Symposium on Relativistic Astrophysics” in Italy.

 

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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		Prop. No.: 04400027 (Cycle 1 obs. also)
Sco X-1 XRB	4	3505	400258	[15.0]	N. Schulz		Reviewed parameters. Prop. No.: 04400046
H1426+428 IGM	4	3568	700630	[102.0]	T. Fang		Prop. No.: 04700987
Mrk 290 AGN	4	3567	700629	[250.0]	J. Lee		Prop. No.: 04700988
TV Crit “Cool” Stars	4	3728	200198	[100.0]	D. Huenemoerder		Prop. No.: 04200007, Selected in peer review![6/02]
E0102 SNR	4	3828	500307	[140.0]	K. Flanagan, D.Dewey		Prop. No.: 04500008, (Cycle 1 obs. also) Selected in peer review![6/02]

 

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	Data obtained, prelim analysis and line finding carried out.
NGC 7469 AGN	3	3147 (+2956)	700586	[70.0] [+80.0]	J. Lee/ H. Marshall	---	Scheduled: Oct. ‘02 w/HST Supplement 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. First pass through data. Data in-house.[8/02]
GX 349+2 XRB	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, AAS00, AAS01
NGC 2362   “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.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	Multi observatory collaboration…[7/02] Data are in-house [3/02].

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, 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].	In CRC Royal society talk 2002.
4U 0142+61   iNS	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	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	Performed abundance measurements.[8/02] Performed spectral fits in time cuts.[7/02] Analyzed burst spectra.[5/02]	Work on paper continued. Second draft and new figure created.[8/02] 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. 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. Fit vpshock w/APED lines…[7/02]	Poster: HEAD-2002[4/02]
NGC 5506 AGN	2	1598	700214	90.0	P. Ogle, J. Lee, S. Gallagher	12/31/00	Created radial profile. Literature review; analyze imaging data; get HST data.[8/02]	Paper in preparation[4/02]
ZW 3146 Clust.	2	1651	800119	167.8	M. Wise	12/25/00	Include background subtraction.[7/02] Re-analysis continued w/ ISIS[6/02]; started[5/02]	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	Analysis complete.	Co-authors comments received. Revised and back to co-authors.[8/02] CSR-01-112
Abell 1835 Clust.	1	49896 511	800019	9.8 127.0	M. Wise	8/25/00 8/26/00	Include background subtraction.[7/02] Re-analysis continued w/ ISIS[6/02]; started[5/02]	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. 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       MCG –6-30-15 Cont. AGN	1	433	700105	128.2	H. Marshall, J. Lee	4/5/00	360ks XMM analysis in proc.; 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   “Hot” Stars	1	3, 4	200001 200002	50.1 31.3	N. Schulz, D. Huenemoerder	10/31/99 11/24/99	Draft papers III and IV continued… Emission measure modeling.[8/02]	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	Include background subtraction.[7/02] Re-analysis continued w/ ISIS[6/02]	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	Allowed plasma region, abundances; shelf and arc fluxes. Created “movie” of plasma vs tau for SPIE.[8/02]	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.