HETG

Follow-on Science Instrument

Contract NAS8-01129

 

Monthly Status Report No. 005

July 2002

HETG Science Theme: The Inter-Galactic Medium (IGM)

 

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 37-582G (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
July 6-13	Making Light of Gravity Conference, Cambridge, UK	C.R. Canizares invited talk

 

 

 

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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 7 targets observed in 13 observation intervals by the HETG in July 2002. None of these were in the HETG GTO program.

 

The target IM Peg is being observed about once a week with the HETGS for 8 total observations; guest observer Dave Huenemoerder CXC/MIT has preliminarily analyzed the data and the instrument is performing fine.

 

3.2 Science Support to CXC, SWG, etc.

 

Created an ‘N0003 version of the MEG sector files as requested by Ishibashi/CXC to improve the MEG wings in MARX simulations – a very small effect for most observer’s uses.

 

 

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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.

 

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 “Inter-Galactic Medium (IGM)” theme is presented.

 

GTO Science Theme	Abbreviation (for App’ix A)	Researchers (HETG in caps)	Date of last [next] reporting Assembler of theme material
Stars	Star(s)	dph,nss	Not yet reported
X-ray Binaries & Accretion Disks	XRB	MJ-G,AJ,nss	Not yet reported
Supernova Remnants	SNR	KAF,DD,JMM, AF,jh,gea,tp	May, 2002. Dan Dewey
Isolated Neutron Stars	iNS	MDS,hlm	Not yet reported
Galaxies & Clusters of Galaxies	Gal., Clust.	TJ,mw,jh	Not yet reported [Aug.’02]
Active Galactic Nuclei and Jets	AGN, Jet	JL,TF,RG,hlm, pmo	June, 2002. Herman Marshall
Inter-Stellar Medium	ISM	AJ,nss	Not yet reported
Inter-Galactic Medium	IGM	TF,JL,RG,hlm, pmo	July, 2002. Taotao Fang

 

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Inter-Galactic Medium Research Progress

 

Introduction

The standard cosmological theory (these days!) predicts that huge amounts of hot gas should exist in the vast space between galaxies in our local universe. This hot gas has been hidden from view since the time galaxies formed because at its high temperature it does not emit substantial visible light. It is thought that this gas forms part of a gigantic system, or web, of hot gas and dark matter that defines the cosmic landscape. The hot gas part of this system could contain more material than all the stars in the universe. Cosmological hydrodynamic simulations have been carried out to model the formation of structure in the universe as predicted by this theory.

 

 

At left is the image from such a simulation which shows the cosmic web of warm/hot gas as the light-blue filamentary structures. The denser regions in yellow and red are where clusters and groups of galaxies are located and are the only regions we’d see in optical light.

 

The image represents about 60 million light years along each side which is equivalent to a red shift of z ~ 0.004. Objects observed with Chandra for our IGM studies are much further away than this with z generally greater than 0.1 and as high as 2.

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Basically, to detect and measure this warm/hot (0.1 to 10 million degrees) intergalactic medium (WHIM), we select X-ray bright background sources such as distant galaxies/AGN that can be detected by Chandra. When photons pass through places where this hot gas is located, they are absorbed by the highly ionized, "heavy metals" (C, N, O, Si, Fe) in the hot gas and an X-ray absorption feature or “dip” will be produced in the spectrum of the background source. Based on the detected absorption signatures, we can derive the physical properties of the absorbing gas. A key parameter to measure is the Doppler shift of the absorption dips which measures the location of the gas along the line-of-sight.

In this illustrative diagram an X-ray source is shown emitting three different wavelengths of X-rays, coded by the red, yellow, and blue waves. In going through the filament of IGM gas the yellow wavelengths are absorbed and do not reach Chandra. The spectrum in the inset shows actual data where absorption “dips” are visible due to Oxygen in the IGM.

This image is taken from the Chandra Press release at:

http://chandra.harvard.edu/press/02_releases/press_073102.html

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Summary of IGM GTO Observations and Activities

In the HETG GTO program we've specifically included some bright distant AGN sources to probe for warm/hot gas in the intergalactic medium, in addition some AGN used as calibration targets are also useful in IGM studies. Relevant targets are tabulated here:

 

AO-	Target	z	Lines seen?
1	Q0836+7104	2.17	No line, set upper limit
1/Cal	PKS 2155-304	0.12	OVII, OVIII at z=0; OVIII at z=0.055
Cal	Mkn 421	0.03	In progress
1	PKS 2149-306	2.34	No line, set upper limit
Cal	3C 273	0.16	OVII at z=0
2	H 1821+643	0.30	Fe emission lines at E=6.4 and 6.9 keV
3	3C 279	0.64	In progress
3	1ES 1028+511	0.36	In progress
3	1H 0414+009	0.28	recently observed, data will arrive soon
4	1H 1426+428	0.13	to be observed in Cycle 4 (starting about Dec ’02)

 

HETGS data have been (or will be) taken on all of these targets and in addition for the "Cal" targets LETG data are often available as well, using the LETG improves sensitivity to redshifted Oxygen lines (O VII, OVIII.)

 

Our science activities to study the IGM are not limited to Chandra observations. We are also making use of the capabilities of the XMM-Newton observatory, working on AO1 data received from two targets: PG 1407+265 and PKS 2135-14, Guest Investigators: T. Fang and C.R. Canizares. We have also talked with the PI of the NASA SMEX mission SPIDR (Spectroscopy and Photometry of the IGM's Diffuse Radiation) and are working on creating an OVI emission map relevant to SPIDR from our simulations. (The SPIDR website is: http://www.bu.edu/spidr/noflash/overview.html .)

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High Redshift Quasars: Q[S5]0836+710 and PKS 2149-306

(Published by T. Fang, H.L. Marshall, G.L. Bryan, and C.R. Canizares, ApJ, 555, 356)

We obtained the first high-resolution X-ray spectra of two high-redshift quasars, Q0836+710 and PKS 2149-306, obtained with the Chandra High Energy Transmission Grating Spectrometer (HETGS). The primary goal of this observation is to use the high spectral resolving power of the HETGS to detect X-ray absorption produced by a hot intergalactic medium. The continuum of both quasars can be fit by absorbed power laws. Excess continuum absorption above the Galactic value is found in Q0836+710, as evidenced in ASCA and ROSAT observations. No significant emission or absorption features are detected in either source at a +/-3 sigma level. Based on the detection limits we constrain the properties of possible emitters and absorbers. Absorbers with a column density higher than 8e16 /cm^2 for OVIII or 5e16 /cm^2 for SiXIV would have been detected. We propose a method to constrain the cosmological parameters (namely Omega_0 and Omega_b) via the X-ray forest theory, but current data do not give significant constraints. We also find that combined with the constraints from the distortion of the CMB spectrum, the X-ray Gunn-Peterson test can marginally constrain a uniform, enriched IGM.

 

HEG spectra of Q[S5]0836+710 (top panel) and PKS 2149-306 (bottom panel). The solid line and dotted line in each panel are the observed and fitted spectrum, respectively. The spectral model is an absorbed power-law.

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H 1821+643: Setting Limits on IGM Temperature

(Published by T. Fang, D.S. Davis, J.C. Lee, H.L. Marshall, G.L. Bryan, and C.R. Canizares, ApJ, 565, 86)

H 1821+643 is one of the most luminous quasars (m_v = 14.1) at low redshift (z = 0.297). It was discovered as a serendipitous X-ray source detected with the Einstein Observatory and has been studied extensively. At a moderate redshift, the sight line toward H 1821+643 traverses a distance of nearly 1.5 Gpc. Numerous absorption systems (such as H, C, N, O, Si, etc.) have been discovered in this sight line in optical and UV bands. Especially in recent observations, the Hubble Space Telescope and the Far Ultraviolet Spectroscopic Explorer have detected a number of OVI absorption lines which are not clearly associated with any galactic system.

 

We searched for absorption features from a warm/hot component of the IGM along the line of sight to this quasar and no absorption features were detected at or above the 3-sigma level. Based on the lack of OVII/OVIII absorption lines and by assuming collisional ionization equilibrium, we constrain the gas temperature of a typical OVI absorber to be between 0.1 to 1 million K, which is consistent with the results from hydrodynamic simulations of the intergalactic medium.

 

 

 

At left the zeroth-order image of H~1821+643, with North to the top and East to the left. The star K1-16 is indicated. From the contours it appears that there is extended (cluster) emission around the central source.

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An iron emission line attributed to H1821+643 is clearly resolved at 6.43 keV (rest frame), with an equivalent width of 100 eV. Although we cannot rule out contributions to the line from a putative torus, the diskline model provides an acceptable fit to this iron line. We also detect a weak emission feature at 6.9 keV (rest frame). We suggest that both lines could originate in an accretion disk comprised of a highly ionized optically thin atmosphere sitting atop a mostly neutral disk.     The simultaneous fit to MEG (red) and HEG (black) spectra between 2 and 7 keV. Two Gaussian components are added to fit the emission features around 5 and 5.3 keV.

 

 

As revealed in the zeroth order image there is also extended emission from the cluster of galaxies which surrounds H1821+643. We have been able to separate the moderate CCD X-ray spectrum of the surrounding cluster from the central quasar and find that this is a hot cluster with a temperature of ~ 10 keV and a metal abundance of 0.3 Z_sun. We also independently obtain the redshift of the cluster, which is consistent with the optical results. We estimate that the cluster makes negligible contributions to the 6.9 keV iron K line flux identified above.

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PKS 2155-304 : Clear detection!

(Published by T. Fang, H.L. Marshall, J.C. Lee, D.S. Davis, and C.R. Canizares, ApJ Letters, 572, 127)

We report the first detection of an OVIII Ly-alpha absorption line associated with an over-dense region in the intergalactic medium (IGM) along the line of sight towards PKS 2155-304 with the Chandra LETG-ACIS. The absorption line is detected at a 4.5-sigma level with cz ~ 16,600 km/s. At the same velocity Shull et al. detected a small group of spiral galaxies (with an overdensity of 100 and low metalicity HI Ly-alpha clouds. We constrain the intragroup gas that gives rise to the OVIII Ly-alpha line to a baryon density in the range 1e-5 < n_b < 7.5e-5 cm^-3 and a temperature of 4 to 5 million K, assuming 0.1 solar abundance. These estimates are in accordance with those of the warm/hot intergalactic medium (WHIM) that is predicted from hydrodynamic simulations. Extrapolating from this single detection implies a large fraction of the ``missing baryons'' are probed by the OVIII absorber.

 

The Chandra LETG-ACIS spectrum of PKS~2155-304 between 18 and 22 A, the red solid line is the fitted continuum plus three Gaussian absorption dips, the ion species are labeled in blue. The absorption feature at 20.02 A has been identified as OVIII Ly-alpha absorption from the IGM.

 

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Our detection and upper limits can be compared with theory on a plot of cumulative probability of OVIII absorption per unit redshift vs. column density. Three data points are: PKS 2155, H1821, Q[S5]0836. We find that the detection is consistent with predictions from cosmological simulations (soild curve).

 

 

 

 

 

 

 

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Inter-Galactic Medium Plans and Further Work

 

 

- Complete analysis of the three sources from AO3: 3C 279, 1H0414, 1ES1028; publish detections or limits to lines from O VII and O VIII.

 

- Analyze new Chandra cycle 3 and cycle 4 GTO observations.

- Continue analyzing data from 3C 273 and Mkn 421 to search for weak absorption features from the IGM.

 

- Continue analysis of XMM-Newton GO data on PG 1407+265 and PKS 2135-14.

 

- Collaborate with F. Nicastro on Chandra/XMM TOO observations of Seyfert I Galaxies and blazers in outburst.

 

- Perform cosmological simulations on the non-equilibrium evolution of IGM ionization structure.

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

 

In connection with IGM research, we are developing new software programs to systemically analyze weak absorption/emission features in X-ray spectra of extragalactic sources. These programs involve accurate measuring of the small-scale continuum level, fitting features with a set of Gaussian lines in emission and/or absorption, and identification of bulk Doppler shifts of lines from individual ions. The software is written as a suite of S-Lang scripts that can be run in ISIS.

 

 

4.4 Presentations (July)

 

C.R. Canizares, “Results from Chandra”, Making Light of Gravity, Cambridge UK, 7/9/02.

 

 

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

 

A.K. Hicks, M.W. Wise, J.C. Houck, and C.R. Canizares, “Chandra X-Ray Spectroscopy and Imaging of the Galaxy Cluster PKS 0745-191”, ApJ accepted, 2002.

 

J.C. Lee, “The Chandra and RXTE view of GRS 1915+105”, Proceedings of the 4^th Microquasar Workshop, 2002, astro-ph/0208187.

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5.0 Systems and Engineering Support

 

5.1 Documentation and “Design Knowledge Capture”

 

Received Chandra knowledge capture import file format from Eric Martin for our evaluation and use; will provide requested input for 8/20 and 8/30 deadlines.

 

5.2 Spares Retest and Test Instrumentation

 

Continued getting X-GEF system working…

 

5.3 Anomalies, Insert/retract, etc. Support

 

Noted that when inserted, telemetry usually indicates an angle of 6.34 degrees for the HETG and occasionally shows a value of 5.96 degrees. Brought this to SOT attention and Bill Podgorski noted that these are only one bit different from each other and not a cause for concern – a slow drift in the pot angle readout may cause this bit flip-flopping and it may be more common in future. In any case, the HETG is being inserted in the same repeatable location.

 

6.0 Management

6.1 Program Office & NASA Support

 

The final report for the previous HETG “Phase C/D” contract was submitted to MSFC and is available on the web at http://space.mit.edu/HETG/papers/HETG_Final_Report.pdf .

Submitted GFE equipment list in Excel format to MSFC (on 8/6/02.)

 

6.2 MIT-internal management activities

 

Two new computers were received and setup for HETG personnel. Continue working perennial office and disk space issues – with some success.

 

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	---	---	[100.0]	N. Schulz		Prop. No.: 04400027
Sco X-1 XRB	4	---	---	[15.0]	N. Schulz		Prop. No.: 04400046
H1426+428 IGM	4	---	---	[102.0]	T. Fang		Prop. No.: 04700987
Mrk 290 AGN	4	---	---	[250.0]	J. Lee		Prop. No.: 04700988
TV Crit Stars	4	---	---	[100.0]	D. Huenemoerder		Prop. No.: 04200007, Selected in peer review![6/02]
E0102 SNR	4	---	---	[140.0]	K. Flanagan, D.Dewey		Prop. No.: 04500008, 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	[150.0]	J. Lee/ H. Marshall	---	Scheduled: Sept. ‘02
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	700408	[93.0]	T. Fang	---	Scheduled: Aug. ‘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]
NGC 2362   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.[6/02] Previewed the data.[5/02] Observed 4/23 [4/02]
1ES 1028+511 IGM, AGN	3	2970, 3472	700409	21.8, 69.6	T. Fang	3/27/02, 3/28/02	Both data sets are in-house [4/02]
3C 279   IGM, AGN, Jet	3	2971	700410	108.2	T. Fang, H. Marshall	3/21/02	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	3/19/02, 3/23/02	Multi observatory collaboration… 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. ISM study: cold absorption edges[5/02]
Cas A SNR	2	1046	500112	69.9	K. Flanagan, D.Dewey	5/25/01	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 spectral fits in time cuts. Analyzed burst spectra; Created spectral lightcurves[5/02]	First draft of paper complete. 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 Stars	2	599, 2420	200075	37.6, 12.9	N. Schulz, P. Wojdowski	2/7/01, 2/8/01	Data reviewed[5/02]
TY Pyx (HD77137) 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	Fit vpshock w/APED lines… NEI, vshock, and Si 2-D analyses.[4/02] 1-D and 2-D analyses started [3/02]	Poster: HEAD-2002[4/02]
NGC 5506 AGN	2	1598	700214	90.0	P. Ogle, J. Lee	12/31/00		Paper in preparation[4/02]
ZW 3146 Clust.	2	1651	800119	167.8	M. Wise	12/25/00	Include background subtraction. 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		CSR-01-81
AR Lac     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 added[6,7/02]; 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. 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 Star	1	5	200003	48.3	D. Huenemoerder, J. Kastner	7/18/00	Analysis complete.	CSR-02-02, CSR-01-29
NGC 4486, M 87 Gal., AGN, Jet	1	241	600001	38.5	M. Wise	7/17/00	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.	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   Stars	1	3, 4	200001 200002	50.1 31.3	N. Schulz, D. Huenemoerder	10/31/99 11/24/99	Draft paper started.[6/02] Detailed modeling work continued[5/02]	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.	AAS00
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 in process [3/02]	ApJ, 2002, 564, pp. 941 (CSR-01-57), HEAD00
II Peg (HD 224085) 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. Re-analysis continued w/ ISIS[6/02]; started[5/02]	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. Fredricks, D.Dewey	9/28/99 10/8/99	Updated model tables, new ratio contours. Multi-NEI & vnpshock fits. “One-ion” fitting and masses.[6/02] Fluxes and ratios in “arc”.[4/02]	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.