HETG

Follow-on Science Instrument

Contract NAS8-01129

 

Monthly Status Report No. 006

August 2002

HETG Science Theme: Galaxies and Clusters

 

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
Aug. 8-10	The IGM/Galaxy Connection: The Distribution of Baryons at z=0 , Boulder	T. Fang
Aug. 18-22	X-ray Astronomy School, Berkeley Springs, WV	A. Fredericks
Aug. 25-28	SPIE conference, Hawaii	K. Flanagan invited talk
Sept.4,5	Chandra Quarterly and IAR, Cambridge, MA	HETG participated
Sept. 4-6	Workshop on X-ray surveys, Santander, Spain

 

 

 

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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 5 targets observed in 8 observation intervals by the HETG in August 2002. The target 1H 0414+009 (obsids 2969, 4284) is an HETG GTO target in cycle 3 and its data are already in-house.

 

We continue to monitor the “streak width” of bright point sources in HETG observations as a check on the continued good focus of the HRMA. The plot on the next page shows the addition of data points in May and July showing the HRMA has remained in stable focus for just about 3 years.

 

3.2 Science Support to CXC, SWG, etc.

 

The yearly editing of the Proposers’ Observatory guide (POG) has started and HETG will support the process working with CXC as in the past. A list of changes to be made by HETG to the HETG section was submitted to CXC.

Dr. Flanagan assisted with preparations for the gratings talk at the GSFC X-Ray Astronomy School.

 

Dr. Flanagan has been charged with drafting a portion of the SEU Roadmap, which has been in preparation for over a year and is due in November. This Roadmap spells out the science priorities for the Structure and Evolution of the Universe (SEU) theme, as well as the future missions which will address these priorities. The SEU Roadmap is one of the necessary inputs to the Space Science Enterprise Strategic Plan, which is updated and revised every three years. Her direct responsibility is for the Research and Analysis (R&A) portion of the SEU Roadmap; she is a member of the SEUS and deputy chair of the Astronomy and Physics Working Group. The SEU draft Roadmap has been submitted and is undergoing final editing and printing. Dr. Flanagan has also been asked to participate in a community Strategic Planning Workshop on November 6-8. The purpose of the workshop is to discuss the inputs to the Strategic Plan and work toward an integrated 5-10 year program.

The HRMA PSF core width is monitored by measuring the FWHM of the ACIS

frame-transfer streak. Just about 3 years of data here shows a very stable FWHM.

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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 cycle 3 GTO observation of AGN 1H0414+009 were received.

 

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 “Galaxies and Clusters of Galaxies” theme are 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,psw	Not yet reported [Sept.’02]
X-ray Binaries & Accretion Disks	XRB	MJ-G,AJ,nss	Not yet reported [Oct.’02]
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	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
Inter-Galactic Medium	IGM	SG,RG,hlm	July, 2002. Taotao Fang

 

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Galaxies and Clusters Research Progress

 

Introduction to Clusters

X-ray observations of clusters provide unique and important insights into a wide range of astronomical topics. As the largest gravitationally bound objects in the universe, clusters of galaxies are important tracers of the large scale distribution of matter. Cluster mass estimates based on X-ray observations provide strong constraints on various cosmological models and independent checks on masses determined from optical velocity dispersions and gravitational lense studies. In addition, X-ray images and spectra allow determination of the physical state of the intracluster medium(ICM) itself. The temperature and abundance structure of the ICM represents a fossil record of the origin and evolution of the gas in the cluster over its lifetime. While the presence of shocks, cold fronts, mergers, AGN interactions, and other phenomena provide clues to various ongoing physical mechanisms which drive the state of the ICM.

 

Galaxy clusters frequently have high X-ray surface brightness cores due to thermal emission from dense gas. Absent a substantial and persistent heat source, this high density, relatively low temperature gas should cool on a timescale that is much less than the age of clusters, leading to a so-called ``cooling flow''. The cooling rates reported from the low resolution X-ray observatories that operated throughout the previous two decades were often extraordinally large, and frequently exceeded several hundred to over two thousand solar masses per year. Such large cooling rates posed a dilemma. They imply the presence of enormous sinks of cold gaseous and stellar matter in the cD galaxies found at the centers of cooling flows. Although substantial amounts of cold gas and vigorous star formation are routinely found in cD galaxies centered in cooling flows, they are found in quantities that are much smaller than the cooling rates would imply.

 

The high spatial resolution imaging provided by Chandra has dramatically changed our view of cooling flow clusters. Images of the cooling flow regions of clusters now show a great deal of structure, including the large cavities or bubbles in the X-ray emission associated with the radio sources harbored by the central cluster galaxies. The strong interactions between the radio sources generated in the nuclei of cD galaxies and the surrounding X-ray emitting gas may reduce the cooling rates and bring them more in line with the star formation rates. Chandra's superb spatial resolution provides the first opportunity to actually map the temperature structure of the keV gas on fine spatial scales, which permits a direct comparison between the sites of star formation seen at optical and ultraviolet wavelengths, and sites of rapid cooling. In essence, we can now reevaluate the proposition that cooling flows are fueling star formation by comparing the cooling and star formation rates on the same spatial scales. In addition, the newly revealed complexity of the gas in cluster cores has sparked a revaluation of several possible heating mechanisms, such as AGN heating, heat conduction from the hoter outer layers of clusters, and supernovae.

 

Spectroscopically, Chandra and XMM observations of cluster cores are yielding surprising results as well. Naively, one expects that once rapid cooling begins, the gas should rapidly cool below X-ray emitting temperatures as long as no comparable heating source is present. Given this assumption of ``full cooling'', one expects to see X-ray emission lines from gas over the full range of temperatures from that of the hot, ambient medium down to very low temperatures. One can show that the strength of these emission lines is directly proportional to the total cooling rate. Recent XMM RGS observations and the Chandra HETG observations discussed here seem to contradict this simple picture. Neither observatory has yet detected emission lines from cooling cores corresponding to gas temperatures less than about 3 keV. In a way, this eases the earlier dilemma: if the gas is *not* cooling to very low temperatures, the reason why we don't see sufficient cool material in other wavebands becomes clear. Unfortunately, this result raises a deeper problem: why doesn't the gas cool below 3 keV?

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Other Introductory material on Galaxies and Clusters is available at:

1) The web page for the course “Astronomy 1120” from the University of Colorado at Boulder:

http://cosmos.colorado.edu/astr1120/lesson10.html .

2) A Power Point presentation from GSFC’s X-Ray Astronomy School:

http://heasarc.gsfc.nasa.gov/docs/xrayschool/Clusters_files/Clusters.ppt .

 

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Summary of Galaxy/Cluster GTO Observations and Activities

There have been 3 galaxies and 3 clusters of galaxies in the HETG GTO program to date as given in the table below. The targets have sufficiently small sizes to give better-than-ACIS resolution with the HETG. However, spatial-spectral complexity, background subtraction, and low signal-to-noise make analysis of these data difficult. To date, these observations have yielded only upper limits which do not place restrictive constraints on the presence of soft X-ray emission lines from cool gas (e.g. OVII and FeXVII).

In parallel, we are doing scientific work on clusters, for example studying cluster evolution in the universe by making use of non-grating imaging observations of clusters that are in the Chandra archive and by making temperature maps of clusters, both described below.

 

Obs cycle	obsid	Type	Target	red-shift z	Image size 1-D, FWHM	Spectral Resolution (Å, MEG)	Comment
2	1560	Gal.	NGC 4696	0.0100	~ 15”	0.33	Substructure; cD in Centaurus cluster
1	241	Gal.	NGC 4486 = M87	0.0043	~ 45”	1.00	AGN/Jet; cD in Virgo cluster
1	240	Gal.	NGC 1399	0.0049	~ 16”	0.35	Underexposed; cD in Fornax cluster
2	1651	Clust.	ZW 3146	0.2906	~ 11”	0.24	Substructure
1	511	Clust.	Abell 1835	0.2532	~ 15”	0.33	Bi-modal core
1	510	Clust.	PKS 0745-191	0.1028	~ 35”	0.40	---
1	492	Gal	NGC 720	0.0058	~ 60”	---	Archival galaxy data (Garmire GTO.) Shows discrete sources.
1	512	Clust	EMSS 1054.5- 0321	0.83	~ 45”	---	Archival cluster data (Garmire GTO.) High-Z cluster.

 

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HETG Observations of the Clusters ZW 3146, Abell 1835, and PKS 0745-191

The goal of the grating cluster observations is to detect or put upper limits on the strength of low-energy X-ray emission lines from the clusters. Although these objects are extended, the HETG should be able to clearly resolve emission lines of Fe XVII at 15Å and 17Å and O VIII at 19 Å and lines of Ne, Mg, and Si at shorter wavelengths --- if they are present and strong.

 

The flat-fielded, flux image of the 0th order region for PKS 0745-191 is shown at left. The solid circle indicates a radius of 0.5 Mpc; used to estimate the total cluster mass, Hicks et al. (2002). The HEG and MEG extraction regions are shown by the green dashed lines --- dispersed events can be seen extending to the top and bottom of the image.

 

At right, events in the extraction region are plotted in a “banana plot” which shows the ACIS-measured energy plotted against the dispersion distance. The distinct curved bands are the different diffraction orders.

(Data here are from ZW 3146.)

 

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         Creating a histogram of the dispersion distance of the diffracted events and correcting for the HETGS effective area gives the fluxed spectrum of ZW 3146, below. The location of some of the low-energy emission lines expected from a cool X-ray gas are shown and labeled (green) at what would be their observed wavelength; that is, at a redshift of 0.29. Given the size of the error bars (blue) and some residual background we have no clear detection of lines here but can place upper limits on the emission.

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HETG Observation of the Elliptical Galaxy NGC 4696 (in the Centaurus cluster)

The X-ray emission from a galaxy comes from the discrete sources in it (stars, X-ray binaries, supernova remnants), from any central source (like a super-massive blackhole), and from the hot gas which fills the galaxy. The spectrum of a galaxy can therefore be crudely modeled as the sum of a power law component (X-ray binaries, AGN) and a thermal plasma component (stars, supernova remnants.)

The MEG m=-1 order data from the NGC 4696 observation are shown below with a superposed model in purple and slightly (z=0.01) redshifted emission line locations are indicated. Although in crude agreement including a hint of an O VIII line at 19Å, it’s clear that more modeling effort is needed for these data.

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Temperature Map Analysis of Clusters

The combination of Chandra's spectral and spatial resolution allows one to actually map the gas temperature in extended objects whose resolution is limited only by the signal to noise of the data. We have developed a custom module within the ISIS spectral analysis package which automates the process of extracting spectra, generating appropriate ARFs and RMFs, and then fitting a given spectral model. This routine is fully general and can be used to map not only quantities such as the gas temperature in a thermal emission model, but any fit parameter, i.e. abundance, absorption column, or spectral index in a non-thermal, power-law model.

 

Maps are generated using a grid of adaptively sized extraction regions selected to contain a given minimum number of counts. For clusters, the drop off in surface brightness with increasing radius results in an increase in the size of the extraction regions with radius. Consequently, sharp spatial features are not well resolved in the outer parts of the maps. In the cores, however, the extraction regions range in size and can approach the size of the PSF for long exposures with high signal to noise.

 

The temperature map for the cluster ZW 3146 is shown at left with contours of X-ray flux superposed. Note the small near-central region with temperatures as low as 2 keV --- could gas at even lower temperatures of 0.5 to 1 keV be present? These CCD data are unable to tell hence our use of the HETG to look for low-T gas emission (above.)

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Archival Research on Cluster Morphology

Using Chandra archival data, we are starting to quantify the evolution of cluster morphology with redshift. Recent ROSAT surveys have discovered tens of clusters with z>0.8 which are now being followed up with Chandra. At right is an image from the Chandra observation of the cluster MS 1054 at z=0.83 showing a complex internal structure.

With this sample the dynamical "age" of clusters at high-z can be compared to those at low-z. Clusters’ formation and evolution are highly sensitive to the mean matter density of the universe. We are quantifing cluster morphology and dynamical state using the power ratio method of Buote and Tsai (1996). These ratios are constructed from moments of the 2D potential and are capable of distinguishing a large range of cluster morphologies. We will also compare our results to simulated X-ray clusters (with help from Greg Bryan.)

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Analysis Issues for HETG data of Clusters and Galaxies

Analysis of HETG spectra for significantly extended sources presents a number of unique problems. The current analysis is founded on a number of assumptions specific to point sources. These assumptions begin to break down for sources much larger than the PSF. We list some of the key issues here:

Wavelength Scale --- The mapping between dispersion angle relative to the 0^th order position and photon energy assumes a single 0th order location can be defined. For a cluster, we cannot simply define a single 0th order position. Even in the absence of significant substructure in the object, photons from various position in the cluster (different radii for example) will each have a wavelength scale different from neighboring regions in the object. Using the current extraction region paradigm tied to a single 0th position guarantees that photons from positions in the cluster far from the center will have incorrect energies. Clusters represent the extreme case of overlapping spectra from multiple sources.

 

Contrast or Background Definition --- For point sources, the background is essentially negligible and is typically ignored during analysis. For extended objects, the definition of "background" is somewhat different. In the case of clusters, where we are interested in detecting soft emission lines from cool gas at the cores, the "background" is not the usual detector background but rather the spectrum of the hotter surrounding cluster gas. This conceptual issue is exacerbated by the fact that the CIAO software does not currently scale the extracted background spectrum according to area correctly for non-standard (non-point source) size extraction regions.

 

We note that cooling flow clusters are optimal targets for making this separation between source and extended background due to the large temperature difference between the two gas components. In the cores, gas is seen down to temperatures of ~2 keV while the more extended cluster gas typically has temperatures of 5-9 keV. The greater the contrast between the two components, the better.

 

Projection effects --- Since clusters are 3D objects, even photons dispersed from the same focal plane position actually sample many different points in the cluster and consequently many potentially different spectral distributions. The spectrum from any point in the cluster actually represents the superposition of a wide range of gas temperatures and densities. This projection effects imaging analysis as well as dispersed spectra and is not treated at all by current analysis software.

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Galaxies and Clusters Plans and Further Work

 

 

-       Clusters PKS 0745-191, A1835, and Zw3146:

§       Improve background subtraction

§       Produce combined +/-1st order spectra

 

-       Galaxies NGC 4696, and '4486 and '1399:

§       Investigate appropriate galaxy models to fit the data.

§       Better background estimation/subtraction is needed for the HETG dispersed data.

 

-       Cluster archival morphology project:

§       Continue modeling the spatial non-uniformity of the background to subtract from cluster images;

§       Create “power ratios” software to evaluate cluster image morphology.

 

-       Algorithms and software:

§       Implement 0th order based RMF profile routine in ISIS.

§       Evaluate/implement Monte-Carlo and other techniques for fitting spatially varying spectral models to HETG data of extended sources.

 

 

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

 

For archival evolution study: created scripts to do initial processing, including acis_process_events, grade and status filtering, source detection, flare fitting, and exposure map creation. Progress made on background subtraction and morphology "power ratios" software.

Extensive s/w in ISIS to do temperature map generation (by J. Houck and M. Wise.)

Created custom ISIS routine to account for projection effects from extended objects in fitting spectral data (by M. Wise and J. Houck.)

 

 

4.4 Presentations (August)

 

K.A. Flanagan, “Probing the Cosmic X-ray Laboratory with the Chandra HETGS”, invited talk at SPIE Astronomy Meeting, Waikaloa HI. (Two of the three targets presented were HETG GTO targets.)

 

 

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

 

K.A. Flanagan, “Probing the Cosmic X-ray Laboratory with the Chandra HETGS”, 2002, submitted for SPIE proceedings.

 

"The Structure and X-Ray Recombination Emission of a Centrally Illuminated Accretion Disk Atmosphere and Corona", M.A. Jimenez-Garate, J.C. Raymond, D.A. Liedahl. It is tentatively scheduled for the v581 n2 ApJ December 20, 2002 issue. CSR-02-33.

 

"XMM-Newton EPIC observations of Her X-1", Gavin Ramsay, Silvia Zane,Mario Jimenez-Garate, Jan-Willem den Herder, C. Hailey, accepted for publication in MNRAS.

 

 

5.0 Systems and Engineering Support

 

5.1 Documentation and “Design Knowledge Capture”

 

Provided input to Eric Martin in support of Knowledge Capture effort.

 

5.2 Spares Retest and Test Instrumentation

 

Progress in making small but tricky modifications to the controlling LabView s/w to allow system to run…

 

5.3 Anomalies, Insert/retract, etc. Support

 

No action on this front.

 

6.0 Management

6.1 Program Office & NASA Support

 

Created HETG presentation to support the September 4th IAR.

 

6.2 MIT-internal management activities

 

Helped settle in the new HETG post-doc, Sara Gallagher; in addition we have an NSF fellow, Sera Markoff, who is hosted by MIT and Prof. Canizares group.

 

7.0 Open Issues, Problems, etc.

 

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

 

As a heads up, HETG will be submitting a travel request for Dr. Dewey for foreign travel to attend and give a talk (“Extended Source Analysis for Grating Spectrometers”) at the “High Resolution X-Ray Spectroscopy with XMM-Newton and Chandra” meeting in the UK, Oct. 24-25.

 

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, R.Gibson	---	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, 4284	700408	50.8, 36.9	T. Fang, S. Gallagher	8/1/02	First pass through data. Data in-house.
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, S. Gallagher	3/27/02, 3/28/02	First pass through data. 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	Overlay radio contours on jet. 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]
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. 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. Performed spectral fits in time cuts.[7/02] Analyzed burst spectra; Created spectral lightcurves[5/02]	Second draft and new figure created. First draft of paper complete.[7/02] 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 Stars	2	599, 2420	200075	37.6, 12.9	N. Schulz, P. Wojdowski	2/7/01, 2/8/01	Make arfs for one-ion analysis. 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…[7/02] 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, S. Gallagher	12/31/00	Literature review; analyze imaging data; get HST data.	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		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.	Revised and back to co-authors. 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.[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 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	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   Stars	1	3, 4	200001 200002	50.1 31.3	N. Schulz, D. Huenemoerder	10/31/99 11/24/99	Emission measure modeling. Draft paper started.[6/02]	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]	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.[7/02] Re-analysis continued w/ ISIS[6/02]	CSR-02-32 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	Created “movie” of plasma vs tau for SPIE. Updated model tables, new ratio contours. Multi-NEI & vnpshock fits.[7/02]	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.