HETG

Follow-on Science Instrument

Contract NAS8-01129

Monthly Status Report Numbers 020 & 021

October & November 2003

Science Theme: "Hot" and "Cool" Stars, Part II

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

Prepared for

National Aeronautics and Space Administration

Marshall Space Flight Center, Alabama 35812

 

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

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1.0 Distribution List for Monthly Status Report

 

 

MIT-External Electronic:

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

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

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

 

MIT-External Hardcopy:

                                    None specified.

 

 

            MIT-Internal Electronic:

                                                Elaine Tirrell                egt@mit.edu

                                                Gail Monahan              gmonahan@mit.edu

 

MIT-Internal Hardcopy:

                                                Claude Canizares         Room 3-234 (via Gail Monahan)

                                                Deepto Chakrabarty     Room 37-501 (via Elaine Tirrell)

                                                Kathryn Flanagan        Room NE80-6103 (via Elaine Tirrell)

                                                File                              (via Elaine Tirrell)

 

 

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

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2.0 Schedule of Past and Future Events Relevant to HETG

 

 

 

 

 

Date	Future Events	Comment
Dec. 8-12	Multiwavelength AGN Surveys, Cozumel, Mexico	M. Jimenez-Garate, J. Gelbord
Dec.15	Chandra Cycle 6 Call for Proposals issued
Jan. 4-8	203rd AAS meeting, Atlanta GA.	Flanagan, Ishibashi, Marshall, Gelbord, Porro, Jimenez-Garate, Wise, Lopez, Wojdowski, Jeltema, Juett
Jan. 12	Chandra User Committee meeting
Jan. 15-16	Studies of Dark Energy & Cosmology with X-ray Surveys, Greenbelt, MD.
Feb. 3-6	“X-ray and Radio Connection”, Sante Fe, NM.	J. Houck
Feb. 8-12	Polarimetry meeting, Stanford U., CA.	H. Marshall
Feb. 15	Abstracts due for 35th COSPAR meeting: , Paris, France. (in July)
Late Feb.	Chandra Quarterly at MSFC	D. Dewey
May	Wyoming meeting	B. Ishibashi
May 12-14	Conference: "Beyond Einstein: From the Big Bang to Black Holes", Kavli Institute, Stanford U., CA..	K. Flanagan
May 18-24	5th Microquasar Workshop, Beijing, China	H. Marshall(jets; SS433)
May 30-6/3	AAS Meeting, Denver, CO.
June 21-25	Astronomical Telescopes and Inst., SPIE Meeting, Scotland.	K. Flanagan
June 20-25	Growing Black Holes: Accretion in a Cosmological Context, Garching, Germany.	H. Marshall
July 18-24	35th COSPAR meeting, Paris France. E1.2 Clusters of Galaxies: … XMM-Newton, Chandra,… INTEGRAL E1.3 High-Energy Radiation from Black Holes: … Supermassive …Galactic… E1.4 Young Neutron Stars and Supernova Remnants E1.9 … X-ray and EUV Spectroscopy … Solar Physics and Astrophysics	H. Marshall, K. Flanagan

 

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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.

In October and November 2003 there were 6 and 1 observation intervals using the HETG to observer 5 GO targets. The quicklook data look nominal.

 

3.2 Science Support to CXC, SWG, etc.

 

HETG group members attended the Chandra Cal Workshop II and executuve session.

Prodded by E0102 flux ratios from our GTO observations, a “two-level(thickness)” or “Fluffy” contamination model was proposed and investigated as a way to reconcile the ECS and “edge” measurements of the contamination level. For further details see the FAQs on:

http://space.mit.edu/HETG/technotes/contam/twolevel.html

 

The HETG POG section was discussed with Project Scientist Marty Weisskopf and CXC’s Andrea Prestwich towards revisions to support cycle 6 call for proposals.

 

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4.0 GTO Science Program

4.1 Observations and Data status

No new GTO data were received in October and November. Progress in on-going analysis is given in the GTO observation list of Appendix A.

 

4.2 Science theme progress

The HETG GTO science efforts span a range of “science themes” given in the list below. For this report we present in the following pages an update on the status of the “Hot” and “Cool” Stars GTO observations.

 

GTO Science Theme	Abbreviation (for App’ix A)	Researchers (HETG in caps)	Date of recent [previous] reporting Contributor of theme material
“Cool” Stars	Cool Star	dph,nss,psw	Oct.&Nov., 2003. [Sept.2002] Dave Huenemoerder
“Hot” Stars	Hot Star	nss,dph,psw,bi	Oct.&Nov., 2003. [Oct. 2002] N. Schulz, P. Wojdowski
X-ray Binaries & Accretion Disks	XRB	MJ-G,AY,AJ,nss,hlm, man, jmm, psw	December, 2002. Norbert Schulz, Mike Nowak
Supernova Remnants	SNR	KAF,DD, AF,jh,gea,mds	August, 2003. [May, 2003] Dan Dewey
Isolated Neutron Stars	iNS	hlm, nss	January, 2003. Mike Stage, Herman Marshall
Galaxies & Clusters of Galaxies	Gal., Clust.	TJ,AY,mw,jh	August, 2002. Michael Wise, Tesla Jeltema
Active Galactic Nuclei and Jets	AGN, Jet	RG,MJ-G,AY,hlm, man,jcl,sm,jg,scg	September, 2003. [June, 2002] Andy Young and Rob Gibson
Inter-Stellar Medium	ISM	AJ,nss	February, 2003. Adrienne Juett, Norbert Schulz
Inter-Galactic Medium	IGM	RG,hlm,tf	July, 2002. Taotao Fang

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“Hot” and “Cool” Stars Progress, Part II (October’02 – November’03)

 

 

 

Summary of ”Cool” Stars Observations and Activities

 

In the past year on the “Cool” star front the analysis of AR Lac was completed and a paper published on it in the ApJ. Also the Cycle 4 GTO observation of TV Crit was carried out and the data have been initially analyzed. Both of these are detailed below.

 

Table of HETG GTO “Cool” star observations.

Obs cycle	obsid	Type	Target	Binary? (period)	Flare(s) seen?	Age (M yrs)	Comment
1	1451	Cool	II Peg	7 d	yes	---	RS CVn binary; “two-ribbon” flare
1	5	Cool	TW Hydra	isolated	yes	~ 5	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
4	3728	Cool	TV Crit.	Pair of binaries,0.8” sep.	yes	~ %	weak-lined T Tauri star; solar-mass “Vega-type'' (dust-disk) system; in TW Hydra assoc.

 

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AR Lac paper published --- Ap.J. 595 (2003) 1131-1147, and at astro-ph/0306380.

 

We observed the coronally active eclipsing binary AR Lac with the HETGS for a total of 97 ks, spaced over five orbits Significant variability in both X-ray and EUV fluxes was observed, dominated by at least one X-ray flare and one EUV flare (see Sept. 02 report.)

Based on line fluxes obtained from total integrated spectra, Figure at right, we have modeled the emission measure and abundance distributions. A strong maximum was found in the differential emission measure, characterized by two apparent peaks near 10 MK and 30 MK, together with a weak but significant cooler maximum just below 2 MK, and a moderately strong hot tail from 40 MK to almost 200 MK.

The resulting model spectra generally agree very well with the observed spectra, see the enlarged region from 12.3 to 13.6 A in the Figure at right: the black lines are the MEG & HEG data and the red lines are the model. There are, however, some significant discrepancies, especially among the many Fe-L-lines.

Both the emission measure and abundance distributions are qualitatively similar to previous observations indicating some long-term stability in the overall coronal structure.

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Our observations include different phases of the binary system, specifically at quadratures and conjunc-tions. Analysis of spectral line widths at these two phases of the system, Figure at left, can be interpreted in terms of Doppler broadening and suggests that both binary stellar components are active.

 

 

 

 

 

 

The data before and during the observed flare were analyzed separately to understand the flaring phenomena. The amount of change or modulation in fluxes from detected ion species is shown in the Figure at left plotted as a function of the temperature of peak emission for the ion. The X-ray flux modulation was largest at high temperature - at and above 10 MK. This indicates a mechanism of flare heating of coronal plasma rather than simply changes in emitting volume or overall electron/ion densities.

 

 

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TV Crit initial results

 

During the past year out Cycle 4 target TV Crt was observed and initial analyses have been carried out. Chandra’s zeroth-order image, Figure below left, clearly resolves the principle binary components: A (red circle) and B (green circle), separated by 0.8 arc seconds. (Sub-pixel event position corrections were applied as described in Li et al., ApJ, 590, 586.) The plot in the Figure at right shows the count rate over the observation for the four circular regions indicated: total counts (black), central component (red), component B (green) and a southern region (blue.) A clear flare is seen in the light curve of the central source.

 

 

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The HETG spectrum from the combined components was formed and is dominated by highly ionized Ne, O, and Fe at wavelengths longward of 12 Å. Weaker lines of Mg, Si, and Ar are present shortward of this value.

Line ratios R = f/i and G = (f + i)/r are measured for the Ne IX triplet, and are plotted in the Figure at left for TV Crt (lower contours) and for the classical T Tauri star TW Hya (upper contours). The fish-net-like grid overlaid on the plot (with “axes” log n vs. log T) illustrates how the ratio R serves as a diagnostic of the density of the gas at the temperature indicated by G. Taken at face value the model densities implied for the post-accretion-phase TV Crt are almost a factor of 10 below those of still-accreting TW Hya.

The red (central), green (middle), and blue (outer) contours represent 99%, 90%, and 68% confidence levels in the measured values of R and G.

 

One goal of the observation was to look for differences in the spectra of the two components. As an example of the data available, the Figure at right shows the MEG minus and plus first-order dispersed events as a function of wavelength and cross-dispersion location, dy. The curve in green at right shows the projection of the zeroth-order image and the centers of the two components are indicated with horizontal lines. Analysis of differences between the two components in on-going.

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Summary of “Hot” Stars Observations and Activities

 

On the “Hot” stars front, another paper on the Trapezium hot stars was published and a DEM survey of hot stars, including the GTO targets iota Ori and tau Cma, is in draft form – these topics are detailed below. A further observation of hot massive stars in the Orion Trapezium area has been added to our cycle 5 GTO program.

 

Table of HETG GTO and related “Hot” star observations

Obs cycle	obsid	Type	Target	Line shape	T range (MK)	Age (M yrs)	Comment
1, 3	3,4, 2567, 2568	Hot	Trapezium	---	---		Many hot (and cool) stars. [2567,’8 are now-public GO HETG observations, PI=Gagne.]
“	“	Hot	Theta-1 Ori C In the Trapezium HD 37022	Narrow, Symmetric	8-74	0.3	Magnetically confined wind shocks?! 25 solar mass star.
2	599, 2420	Hot	Iota Orionis	Broad, Symmetric, Most flat-topped	1-10	< 12	Two O-stars; colliding winds?
3	2525, 2526	Hot	NGC 2362, Tau Cma	Broad, Symmetric, Flat-topped	3-22	> 3	Young (3-7 Myrs ) star cluster in the Galaxy; w/ massive stars.
5	4473, 4474	Hot	Orion Nebula Cluster, Theta-1 Ori	---	---	---	To be observed near end of 2004.

 

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Trapezium hot stars progress --- ApJ 595 (2003) 365-383, and astro-ph/0306008

 

Detailed analysis has continued on the hot stars in the Orion Trapezium, in particular components C, E, and A shown in the image at right.

The brightest component, theta-1 Ori C, has been extensively modeled and shows generally narrow lines agreeing with model fits, Figure below right, with the exception of two low-energy lines, O VIII and Fe XVII, which show clear broadening over the model response, Figure below left.

 

 

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From top to bottom the Figures here show the extracted spectra from the three brightest Theta-1 Ori components: C, E, and A respectively.

 

These three show similarlly narrow lines suggesting they all involve magnetic wind confinement.

 

 

 

 

 

 

 

 

 

 

 

 

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DEM survey of hot stars

 

In order to extract information from the spectra of hot stars (and other objects as well), we have developed a technique to measure the effective emmission measure distribution of the object using multi-component fits to the spectra (Wojdowski et al., 2004, in prep.). Each component is the spectrum due to a single ion, e.g. O VII or Fe XVII.

The result of these fits is shown by the emission measure vs temperature plot, Figure above right, where each ion species measured provides a generally diamond-shaped plot symbol indicating in width the temperature range covered by the ion and in height the averaged emission measure for the ion. The Figure at right above shows the MEG spectral data for theta-1 Ori C in black and the resulting multi-ion-components model spectrum in red.

This technique has the advantage of using all of the data and being less sensitive to line blend effects that a line-by-line measurement approach. Work on this technique and its application to model interpretation and determination for hot stars and other systems is on-going.

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“Cool” Stars Plans and Further Work

 

·      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: This star is a visual double, with 1 arcsec separation, and presents a spatial-spectral data analysis challenge – work to see if differences in the two sources can be discerned.

 

·      Compare and contrast more ensembles from many observations, both GO and GTO, like the Ne/Fe comparison plot shown in the September 2002 report (and included in the Jan. 2003 Chandra Newsletter.)

 

·      Design code and software for feature fitting database including lines, continua, absorption lines, edges, etc..

 

“Hot” Stars Plans and Further Work

 

·      Focus on the low mass population of young T-Tauri stars when extracting more spectra from the Trapezium observations including the Gagne GO observations.

 

·      Finish DEM survey of “Hot stars” including iota Ori and tau Cma.

 

·      For Cycle 6 continue with ~ 100 ks exposures around the Trapezium.

 

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

The protoytpe IDL DEM software from a year ago has been ported/rewritten in ISIS. A Monte Carlo wrapper helps to create accurate error estimates for the resulting DEM.

The ion-based DEM technique is coded in ISIS and automates much of the parameter fitting and confidence determination for the technique.

 

4.4 Presentations, etc. (October and November)

D. Huenemoerder, “Chandra X-ray Observatory High-Resolution X-ray Spectroscopy of Stars: Modeling and Interpretation”, an invited talk at the APS/DPP meeting, Albuquerque, Oct., 2003.

K. Flanagan, “A High-Resolution X-Ray Spectrum of SNR E0102-72: X-Ray Astronomy from Your armchair”, at the Joint Steward Observatory/NOAO/NRAO Colloquium Series, October (2003.)

D. Dewey et al., “SNR E0102: Building a Supernova Remnant”, at the SNORE talk series at Center for Astrophysics, Cambridge MA, 12/1/03. (Available: http://space.mit.edu/~dd/Pubs/snore03dd.ppt )

 

 

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

 

T.E. Jeltema et al., “The Evolution of Cluster Substructure with Redshift”, to appear in the proceeding of Multiwavelength Cosmology, ed. M. Plionis. Available at astro-ph/0310124.

A.M. Juett, et al., “High-Resolution X-ray Spectroscopy of the Interstellar Medium: Structure at the Oxygen Absorption Edge”, submitted to the Astrophysical Journal. Available at astro-ph/0312205.

 

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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

5.2 Spares Retest and Test Instrumentation

 

No activities in these areas in October and November.

 

6.0 Management

 

6.1 Program Office & NASA Support

 

Participated in the Chandra IIR on Nov. 18 in Cambridge giving presentation on the HETG and LETG instruments.

 

6.2 MIT-internal management activities

 

In October and November: submitted job description to AAS job register for HETG Post Doc position opening starting September 2004.

 

 

7.0 Open Issues, Problems, etc.

 

There are no open issues or problems regarding the HETG.

 

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Appendix A. HETG GTO Observation Status Tables

 

Notes:

1. Entries indicating progress during this period are shown in this font.
2. For CSR Publication references (CSR-YY-NN) see http://space.mit.edu/csr_pubs.html
3. Up-to-date observation information can be obtained from http://cxc.harvard.edu/cda/ using WebChaSeR ; this archive page also has a link to the ADS which allows searching for papers by Chandra obsid.

 

Cycle 5

Object Science Theme	AO	Obs ID	Seq. No.	Expos. (ks)	Observer / Analyst	Start Date	Comments & Analysis	Talks and Publications
4U 1957+11 XRB	5	4552	400335	[67]	M. Nowak	[8/2/04]	Target accepted in peer review. Prop. 05400034
MCG—6-30-15 AGN	5	4759, 4760, 4761, 4762	700845	[170, 170, 170. 30]	J. Lee	[5/26/04, 5/19/04, 5/19/04, 5/29/04]	Prop. 05700032
Orion Nebula Cluster “Hot” Stars	5	4473, 4474	200242, 200243	[50.0, 50.0]	N. Schulz	[11/6/04, 12/.3/04]	Prop. 05200040

 

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 and 1	3504	400257	97.1	N. Schulz	6/5/03	XMM obs on 8/20. Spectra analyzed[7,8/03]. Data in-house, spectra good[6/03].
Sco X-1 XRB	4	3505	400258	16.1	N. Schulz	7/21/03	CC Data being processed [7/03]. Multi-wavelength obs organized[1/03].	Example spectra at CCW II 10/03.
H1426+428 IGM	4	3568	700630	101.0	T. Fang	9/8/03	Prop. No.: 04700987
Mrk 290 AGN	4	3567 4399 4441 4442	700629	55 85 61 50	J. Lee	6/29/03 7/15/03 7/15/03 7/17/03	Fe lines searched.[10/03] Mg, Ne lines; Began data reduction…[9/03] Replanning FUSE obs.[8/03] Data in-house [6,7/03].
TV Crit “Cool” Stars	4	3728	200198	100.2	D. Huenemoerder	3/7/03	Data in-house – looks good[4/03]. Selected in peer review![6/02]
E0102 SNR	4	3828	500307	137.7	K. Flanagan, D.Dewey	12/20/02	Measure shelf, arc, correct for contam.[10/03] Extracted counts and flux ratios.[9/03] Measure counts in lines. S-S analysis of Ne X line; arfs made. Quick look images[1/03].

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	UV flux insufficient to pump forbidden to intercomb.[10/03] ISIS and IDL EW s/w…[9/03] Re-analyzed, hlm IDL scripts used; import to ISIS[12/02]. A few line Ids at 3-sigma; ISIS scripts.[10/02]	First draft finished.[7/03].AAS03.
NGC 7469 AGN	3	3147 (+2956 Kriss)	700586	69.8, 79.8	J. Lee/ H. Marshall	12/13/02	Analyzed data, id absorp lines.[1/03] Data in-house, look good.[12/02] w/HST.
1H 0414+009   IGM, AGN	3	2969, 4284	700408	50.8, 36.9	T. Fang, S. Gallagher	8/1/02	Shows lovely power law.[9/02] First pass through data. Data in-house.[8/02]
GX 349+2 XRB, ISM	3	3354	900193	35.2	N. Schulz, A. Juett	4/9/02	For ISM study; Observed on 4/9; data available 5/2 [4/02]	Santander,’02 AAS00, ‘01
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
IRAS 18325-5926 AGN	3	3148, 3452	700587	56.9, 51.1	J. Lee, S. Gallagher	3/19/02, 3/23/02	Work ongoing[8/03]. XTE and SAX obs analyzed.[12/02] Multi obs. Collab.[7/02]	Paper draft w/ Iwasawa[12/02]

Cycle 2

Object	AO	Obs ID	Seq. No.	Expos. (ks)	Observer / Analyst	Start Date	Comments & Analysis	Talks and Publications
Cyg X-2   XRB, ISM	2	1016	400094	15.1	N. Schulz, A. Juett	8/12/01	Fit O, Fe, Ne edges.[7/02] ISM study: cold absorption edges[5/02]	Santander,’02 AAS00, AAS01
Cas A   SNR	2	1046	500112	69.9	K. Flanagan, D.Dewey, M. Stage	5/25/01	Began NEI fits to Si knot image for continuum.[8/02] Si knot analysis started [3/02].	High-Res UK talk.[10/02] CRC Royal Soc.’02
4U 0142+61   iNS, AXPs	2	1018	400096	25.4	N. Schulz, A. Juett	5/23/01	Finishing additional analysis [3/02]	ApJ, 2002, 568, pp. L31, HEAD-2002[4/02] CSR-02-16[3/02]
Mrk 766   AGN	2	1597	700213	90.5	P. Ogle, J. Lee	5/7/01	XTE data simultaneous w/obs.[10/02] Paper in preparation [4/02]
NGC 4696 Gal.	2	1560	600117	85.8	M. Wise	4/18/01	To be analyzed.
EXO 0748-676   XRB	2	1017	400095	49.0	N. Schulz, H. Marshall, M. Jimenez-Garate	4/14/01	Photo-excitation rates.[10/02] Performed abundance measurements.[8/02]	Revise/reply to ref. report.[1/03] AAS03. HEAD02
SS 433   XRB, Jet	2 2 1	1019, 1020, 106	400097, 400098, 400019	23.7, 23.0, 28.9	H. Marshall, N. Schulz, L. Lopez	3/16/01, 11/28/00, 9/23/99	Jet model: expected density and cooling time.[11/03]	Lopez draft[8/03]. 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	Re-analysis using light/phase curve s/w…[9/03] 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	Investigating models by Badenes et al, ApJ 593:358.[11/03] 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	Draft complete, internal review[7,8/03]. O VII and RRC[6/03] Paper progress.[4/03] XTE simult obs reduced; spectral and image analysis progress.[12/02]	AAS’03 Paper in prep.[4/02]
ZW 3146   Clust.	2	1651	800119	167.8	M. Wise	12/25/00	MEG +/-1 spectrum.[10/02] Include background subtraction.[7/02] Re-analysis continued w/ ISIS[6/02]; started[5/02]	High-Res UK talk.[10/02] Cluster paper in draft[5/02]

Cycle 2, above.

 

Cycle 1

Object	AO	Obs ID	Seq. No.	Expos. (ks)	Observer / Analyst	Start Date	Comments & Analysis	Talks and Publications
NGC 1068 AGN	1	332	700004	46.3	H. Marshall, P. Ogle, J. Lee	12/4/00	Examine zeroth-order pileup[5/02]	Paper in submitted[5/02]
4U 1626-67 XRB	1	104	400017	40.0	N. Schulz	9/16/00	Analysis complete.	CSR-01-81
AR Lac     “Cool” Star	1	6,7,8, 9,10,11	20000N: 4,5,6,7,8,9	32.5,7.5, 7.5,32.6, 7.3,7.3	D. Huenemoerder	9/11/00- 9/19/00	Fixed errors.[12/02] Analysis complete.	Submitted to ApJ.[1/03] Revised manuscript.[12/02] CSR-01-112
Abell 1835     Clust.	1	49896 511	800019	9.8 127.0	M. Wise	8/25/00 8/26/00	MARX simulations (1T, 2T, etc.)[10/02] 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	Model grid added.[4/03] Fe and O line ratios from many regions/features	CSR-01-10,26, Y2Chandra01
TW Hydra “Cool” Star	1	5	200003	48.3	D.Huenemoerder, J. Kastner	7/18/00	Analysis complete.	CSR-02-02, CSR-01-29
NGC 4486, M87   Gal., AGN, Jet	1	241	600001	38.5	M. Wise	7/17/00	Absorption and cooling maps.[9/02]
GX 301-2 XRB	1	103	400016	40.0	N. Schulz	6/19/00	Re-analysis initiated [3/02]	Draft paper begun [3/02], AAS00
NGC 1399   Gal.	1	49898, 240, 2389	600214 600000	13.2 44.1 14.8	M. Wise	5/8/01 6/15/00 5/8/01	Examination begun.[6/02]
Vela X-1 XRB	1	102	400015	28.4	N. Schulz	4/13/00		ApJ, 2002, 564, L21
MCG –6-30-15 (w/Fabian)     AGN	1	433	700105	128.2	H. Marshall, J. Lee	4/5/00	XMM obs analysis.[12/02] XSTAR /Kallman; Fe UTAs (Ming); LLB edges.[7/02]	Draft paper 3 progress[8/03]. Lee et al 2002, CSR-02-15 [3/02], CSR-01-02
NGC 4151 AGN	1	335	700007	48.0	H. Marshall, P. Ogle	3/5/00		CSR-00-87
PSR B0656+ 14 iNS	1	130	500017	38.1	H. Marshall	11/28/99	LETG/HRC	Paper accepted, CSR-02-12[3/02]
PKS 2149-306 IGM, AGN	1	336, 1481	700008	36.0 54.8	H. Marshall	11/18/99 11/20/99		CSR-01-67
Trapezium, Theta Ori   “Hot” Stars	1	3, 4	200001 200002	50.1 31.3	N. Schulz, D. Huenemoerder	10/31/99 11/24/99	Add new archive obs.[1/03] Theta Ori A and E line fluxes.[10/02]	Second paper submitted.[4/03] Draft papers III and IV [9/02]. CSR-01-118, CSR-00-89, CSR-00-75
4U 1636-53 XRB, ISM	1	105	400018	29.8	N. Schulz, A. Juett	10/20/99	Fit O, Fe, Ne edges.[7/02]	Santander, AAS00, AAS01
PKS 2155-304   AGN, IGM	1	337, 1703, 1705	700009 700261 700263	39.1 26.2 25.8	H. Marshall, T. Fang, J. Lee	10/20/99 5/31/00 5/31/00	HETG and LETG w/ACIS-S	ApJ Letter in press.[6/02] Paper accepted.[4/02]
Cyg X-1   XRB	1	107, 1511	400020	2.5 12.6	N. Schulz, H. Marshall, J. Miller	10/19/99 1/12/00	Second paper continuing[5,6/02] Paper…[3/02]	ApJ, 2002, 564, pp. 941 (CSR-01-57), HEAD00
II Peg, HD 224085 “Cool” Star	1	1451	200010	43.3	D. Huenemoerder	10/17/99	Analysis complete.	CSR-01-50
Q0836+7104 IGM, AGN	1	1450, 1802	700006	61.0 14.1	H. Marshall	10/17/99 8/25/00		CSR-01-67
PKS 0745-191 Clust.	1	510, 1509, 1509	800018	45.3, 40.4, 39.9	M. Wise	10/14/99 4/25/00 3/4/00	MEG +/-1 spectrum.[10/02] Include background subtraction.[7/02]	High-Res UK talk.[10/02] CSR-02-32[8/02] Responded to referee report.[6/02] ApJ submitted, Hicks et al. [3/02]
PSR B0833-45, Vela Pulsar iNS	1	131	500018	36.1	H. Marshall	10/12/99		HEAD00
NGC 1275 AGN	1	333, 428	700005 700201	53.2 25.0	H. Marshall, P. Ogle	10/10/99 8/25/00	Determined PL spectral slope	No pubs of note
E0102   SNR	1	120, 968	500007	88.2, 49.0	K. Flanagan, J. Houck, A. Fredericks, D.Dewey	9/28/99 10/8/99	Start 3D modeling; Asymetry mechanisms[6/03]. Ejecta masses and errors finalized.[1-4/03] Plasma diag.s[12/02].	Accepted! Astro-ph 0312509 [12/03] ApJ submitted[8/03]. AAS’03 Poster. High-Res UK talk.[10/02] 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.