HETG

Follow-on Science Instrument

Contract NAS8-01129

 

Monthly Status Report No. 008

October 2002

HETG Science Theme: "Hot" 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

 

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 .

 

2.0 Schedule of Past and Future Events Relevant to HETG

 

 

Date

Past Events

Comment

Oct. 7

Chandra Fellows Symposium , Philips Aud., SAO

(M.F.Gu and J.Lee)

Oct. 10-12

34th COSPAR, Houston TX:

E1.2 …clusters of galaxies and black holes

E1.4 …supernova remnants and neutron stars

S.Gallagher talk;

J. Migliazzo on N103B

M. Stage on NSs

Oct. 20-25

Coevolution of Black Holes and Galaxies, Carnegie Obs.s, Pasadena, CA.

S.Gallagher poster

Oct. 24,25

High Resolution X-Ray Spectroscopy with XMM-Newton and Chandra, UK

D.Dewey talk

Nov. 1

Updated HETG section of Proposers’ Observatory Guide to CXC

HETG provided input

 

 

Date

Future Events

Comment

Nov. 3-8

Galactic Center Workshop 2002, Kailua-Kona HI

(S. Markoff)

Nov. 4-5

First US XMM-Newton SAS Workshop, Goddard

A. Juett

Nov. 6,7

Chandra Calibration Workshop at CXC, Cambridge MA

D.Dewey support

Nov. 14,15

X-ray Binaries in the Chandra and XMM-Newton Era, Camb. MA

A. Juett; M.Jimenez-Garate

Dec. 3

Chandra Quarterly Review

HETG attend

Dec. 5-8

SIRTF Observation Planning Workshop

S. Gallagher attend

Dec. 9-13

XXI "Texas" Symposium on Relativistic Astrophysics , Florence, Italy

J.Lee, AGN

Dec. 15

Chandra AO-5 out

 

Jan. 5-9

American Astronomical Society 201st Meeting , Seattle, WA

S. Gallagher, NGC 5506;

A. Fredericks, E0102;

M. Jimenez-Garate;

R. Gibson, MR2251;

Mar. 23-26

HEAD meeting, Mt. Tremblant, Canada

M.Jimenez-Garate

May 4-7

Constellation X Spectroscopy Workshop, Columbia Univ., NY

 

 

 

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 3 targets observed in 3 observation intervals by the HETG in October 2002.

 

3.2 Science Support to CXC, SWG, etc.

 

An update to the POG HETG section was provided to CXC; of note are updates to the LSF section involving the new LSFPARM products and resulting RMFs as created by CXC/MIT Ishibashi.

 

 

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. A single Cycle-3 HETG GTO target remains to be observed in December and nominal observation dates have been set for the AO-4 observations with SNR E0102 first-up on Dec.18.

 

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 “Hot Stars” theme are presented with help from Norbert Schulz.

 

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

nss,dph,psw,bi

October, 2002.

Norbert Schulz

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

"Hot" Stars Research Progress

 

Introduction to “Hot” Stars

Last month we desribed “Cool stars” which include stellar coronae, active binaries, and low-mass pre-main sequence stars all of which produce X-rays through coronal emission powered by the stars magnetic dynamo. In contrast “Hot stars”, consisting of early type stars (O,B), are thought not to have the convective dynamo action but instead X-rays are produced by shock instabilities in a radiatively driven wind. Some of the detailed mechanisms of this process are not yet understood. Specifically emission mechanisms in young massive stars are notoriously under-studied.

The HETGS high-resolution spectra provide new and more powerful possibilities to diagnose the emission from the hot star plasmas and understand the underlying mechanisms. In addition because young stars are generally found in dense stellar cluster cores, the spatial resolving power of Chandra is essential. These diagnostics include: line identifications, line ratios with their dependence on physical parameters such as temperature and density, line shapes and shifts, and global fitting of plasma models.

In particular the canonical wind model produces blue-shifted, broadened (P-Cygni) profile lines with emission at moderate X-ray temperatures, say up to 10 million degrees K. In some stars even higher temperatures are seen and one possible mechanism is magnetically confined wind shocks. If the magnetic field is high enough and the wind mass loss rate low enough then the outflow gets dominated by magnetic field effects and dense high-temperature regions can form. The diagram below (from http://www.bartol.udel.edu/~owocki/ ) shows the confinement effect on hot plasma as the magnetic confinement parameter increases from left to right. Note the increase of dense (red) regions.

 

 

Summary of “Hot Star” GTO Observations and Activities

 

Three HETGS “Hot star” targets have been observed to date as listed in the table below. The Orion Trapezium contains a huge number of X-ray point sources (e.g., see next page) and in particular the X-ray-brightest member, Theta-1 Ori C, is young and massive with very high temperature emission. The other two objects, iota Ori and tau Cma, have spectra more similar to the prototype wind shock object zeta Puppis.

 

 

Obs

cycle

obsid

Type

Target

Line

shape

T range

(MK)

Age

(M yrs)

Comment

1

3,4

Hot

Trapezium

---

---

 

Many hot (and cool) stars

“

“

Hot

Theta-1 Ori C

In the Trapezium

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.

 

 

 

The Orion Trapezium – A Stellar Nursery (Schulz et al., ApJ 549, 441S, 2001)

 


The Orion Trapezium Cluster, only a few hundred thousand years old, offers a prime view into a stellar nursery. Its X-ray sources detected by Chandra include several externally illuminated protoplanetary disks ("proplyds") and several very massive stars, which burn so fast that they will die before the low mass stars even fully mature.

The time variability of many of the sources in the field is shown by the two Chandra views above taken a few weeks apart as some objects brighten and fade between the exposures.

 

HETGS Observation of the Orion Trapezium

(Schulz et al., ApJ 545L, 135S, 2000; Schulz et al. 2003, in preparation)

 

The HETGS observation of the Trapezium shows spectra (the linear streaks) from the bright objects in the field. The brightest source in X-rays is the source Theta-1 Orionis C whose spectra are indicated in blue above and is the dominant central source in the blowup of the central region at right.

 

Spectra from ‘C and the other bright sources in the field were extracted in the standard way sometimes using a narrowed cross-dispersion selection range and correcting the fluxes appropriate for the width reduction. Each spectra was also cleaned of contributions from interfering field sources. Some crossing of the spectra is seen and ACIS energy discrimination was able to eliminate spectral contamination.

 

 

 

 

 

Analysis of Theta-1 Ori C

High resolution spectra from Theta-1 Ori C were obtained at two phases of its approximately 15 day (assumed to be) rotational period. Using the measured lines in the spectra emission measure distributions (“DEM”) were created using the same algorithms employed for “Cool star” analysis.

The DEM results for the two phases are shown at right by the red and green curves – the curves for a given color define the upper and lower confidence range for the emission measure. These curves show a relatively phase-independent emission peak at just below 10 million degrees K (peaking ~6.95 in the plot) and more dramatic variations between phases in the 25 to 60 million degree temperature range (7.4 to 7.8 in LogT.)

Combining this phase modulation with the narrowness of the emission lines observed is strongly indicative of a magnetic confinement mechanism for the high-temperature emission.

 

Contrasting Theta-1 Ori C with tau Cma and iota Ori

 

The counts spectra for theta-1 Ori C, tau Cma and iota Ori, are shown respectively above. The temperature of the sources decreases from left to right. Even at a glance it is clear that theta-1 Ori C is a “different beast” from the two other “Hot stars”: it has proportionally far more short-wavelength continuum and its lines are narrow. In addition Theta-1 Ori A and E, the next brightest X-ray emitters in the Trapezium, also show similar “magnetic” characteristics in their HETGS spectra. This raises the question if young massive stars enter the main sequence with significant magnetic fields at moderate outflow rates.

 

"Hot" Stars Plans and Further Work

 

·      Finish current Trapezium paper (paper “3”.)

·      Extract more spectra of massive stars from the Trapezium observations including a newly available AO-2 observation of 100 ks more than doubling the current exposure.

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

·      Select and propose the next best candidate for magnetic confinement in “Hot stars” for AO-5.

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

 

Software described last month is used for both “hot” and “cool” stars.

 

 

4.4 Presentations (October)

 

S.C. Gallagher et al., “Probing Broad Absorption Line Quasar Outflows: X-ray Insights”, 34th COSPAR meeting on “New Results from Clusters of Galaxies and Black Holes”, Houston TX.

M. Wise, “High Resolution HETG Spectroscopy of Cooling Flow Clusters”, High Resolution X-Ray Spectroscopy with XMM-Newton and Chandra, UK, October, 2002.

D. Dewey, “Extended Source Analysis for Grating Spectrometers”, High Resolution X-Ray Spectroscopy with XMM-Newton and Chandra, UK, October, 2002.

D. Huenemoerder, “Stellar Coronal Spectroscopy with the Chandra HETGS”, High Resolution X-Ray Spectroscopy with XMM-Newton and Chandra, UK, October, 2002.

 

 

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

 

M. Jimenez-Garate, “The Thermal Forming of Glass Micro-sheets for X-ray Telescope Mirror Segments”, accepted by Applied Optics.

 

 

5.0 Systems and Engineering Support

 

5.1 Documentation and “Design Knowledge Capture”

 

Mike McGuirk supported Keith Patrick’s visit on Knowledge Capture / Failure modes in October.

 

5.2 Spares Retest and Test Instrumentation

 

The X-ray Grating Evaluation Facility (X-GEF) was brought back on line in October, carrying out successful test runs which will be analyzed to qualify the system for vacuum storage grating re-testing.

A surplus Sparc 20 computer “rico” operating on Solaris was installed in the X-GEF setup as a backup/replacement for “caliber” which operates on no-longer-supported Sun OS-4.

 

5.3 Anomalies, Insert/retract, etc. Support

 

No action on this front.


 

6.0 Management

6.1 Program Office & NASA Support

 

We received the letter from the Chandra Program Office, FD03 (02-29), with its “heads-up” for planning purposes; we look forward to working with MSFC and CXC on transition planning for FY05 and beyond.

 

6.2 MIT-internal management activities

 

No internal management issues or activities of note this month. Still looking into “RAID” disk storage system for use in backing up large but valuable data analysis files.

 

7.0 Open Issues, Problems, etc.

 

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

 

Thanks for the approval for foreign travel for Dr. Lee to 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.

 

Appendix A. GTO Observation Status Tables

 

Notes:

1.    Entries indicating progress during this period are shown in this font.

2.    For CSR Publication references (CSR-YY-NN) see http://space.mit.edu/csr_pubs.html

3.    Up-to-date observation information can be obtained from http://cxc.harvard.edu/cda/ using the WebChaSeR link.

 

Cycle 4

Object

Science Theme

AO

Obs ID

Seq. No.

Expos.

(ks)

Observer /

Analyst

Start Date

Comments & Analysis

Talks and

Publications

4U 1626-67

XRB

4

3504

400257

[100.0]

N. Schulz

[6/3/03]

Prop. No.: 04400027

(Cycle 1 obs. also)

 

Sco X-1

XRB

4

3505

400258

[15.0]

N. Schulz

[5/9/03]

Reviewed parameters.[9/02]

Prop. No.: 04400046

 

 

H1426+428

IGM

4

3568

700630

[102.0]

T. Fang

[9/11/03]

Prop. No.: 04700987

 

Mrk 290

AGN

4

3567

4399

700629

[165.0]

[ 85.0]

J. Lee

[10/8/03]

[10/6/03]

Prop. No.: 04700988

 

TV Crit

“Cool” Stars

4

3728

200198

[100.0]

D. Huenemoerder

[3/5/03]

Prop. No.: 04200007,

Selected in peer review![6/02]

 

E0102

SNR

4

3828

500307

[140.0]

K. Flanagan,

D.Dewey

[12/18/02]

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

A few line Ids at 3-sigma; ISIS scripts. Data obtained, prelim analysis and line finding carried out.[9/02]

 

NGC 7469

AGN

3

3147

(+2956)

700586

[70.0]

[+80.0]

J. Lee/

H. Marshall

[12/12/02]

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.[9/02] 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,’02

AAS00, AAS01

NGC 2362

Tau CMa

“Hot” Stars

3

2525,

2526

200133,

200134

44.5,

43.8

N. Schulz,

P. Wojdowski,

J. Kastner/RIT

3/28/02,

4/23/02

Analysis continues.[6,9/02]

Previewed the data.[5/02]

Observed 4/23 [4/02]

Patzcuaro, ‘02

1ES 1028+511

 

IGM, AGN

3

2970,

3472

700409

21.8,

69.6

T. Fang,

S. Gallagher

3/27/02,

3/28/02

Shows lovely power law.[9/02] First pass through data.[8/02]

 

3C 279

 

IGM, AGN, Jet

3

2971

700410

108.2

T. Fang,

H. Marshall

3/21/02

Overlay radio contours on jet.[8/02] Data reduced; jet seen in zo image.[5/02] Data are in-house [3/02].

 

IRAS 18325-5926

AGN

3

3148,

3452

700587

56.9,

51.1

J. Lee,

S. Gallagher

3/19/02,

3/23/02
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,’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.

CRC Royal Soc.’02

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

XTE data simultaneous w/obs. 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. Performed abundance measurements.[8/02] Performed spectral fits in time cuts.[7/02]

Work on paper continued.[9-10/02] 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.[9/02] Make arfs for one-ion analysis.[8/02] Data reviewed[5/02]

Patzcuaro, ‘02

TY Pyx,

HD77137

“Cool” Star

2

601

200076

49.8

D. Huenemoerder

1/3/01

Preliminary analysis done.

(spectrum in CSR-02-02)

N103B

 

SNR

2

1045,

2410,

2416

500111

74.0,

25.7,

17.6

K. Flanagan,

J. Migliazzo,

D. Dewey

1/1/01,

1/3/01,

1/2/01

New fits, abundance plots, one-ion fits.[9/02] Fit vpshock w/APED lines…[7/02]

High-Res UK talk.

Poster: HEAD02[4/02]

NGC 5506

 

AGN

2

1598

700214

90.0

P. Ogle,

J. Lee,

S. Gallagher

12/31/00

ISIS scripts for fluxes and energies. Created radial profile.[9/02] Literature review; analyze imaging data; get HST data.[8/02]

AAS’03 abstract. Paper in prep.[4/02]

ZW 3146

 

Clust.

2

1651

800119

167.8

M. Wise

12/25/00

MEG +/-1 spectrum. Include background subtraction.[7/02] Re-analysis continued w/ ISIS[6/02]; started[5/02]

High-Res UK talk. 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.[9/02]

CSR-01-112

Abell 1835

 

 

Clust.

1

49896

511

800019

9.8

127.0

M. Wise

8/25/00

8/26/00

MARX simulations (1T, 2T, etc.) Include background subtraction.[7/02]

High-Res UK talk. Cluster paper in draft[5/02]

N132D

 

SNR

1

121,

1828

500008

22.3

77.6

K. Flanagan,

D. Dewey

7/19/00

7/20/00

Fe and O line ratios from many regions/features

CSR-01-10,26,

Y2Chandra01

TW Hydra

“Cool” Star

1

5

200003

48.3

D.Huenemoerder,

J. Kastner

7/18/00

Analysis complete.

CSR-02-02,

CSR-01-29

NGC 4486, M87

 

Gal., AGN, Jet

1

241

600001

38.5

M. Wise

7/17/00

Absorption and cooling maps.[9/02] Examination begun.[6/02]

 

GX 301-2

XRB

1

103

400016

40.0

N. Schulz

6/19/00

Re-analysis initiated [3/02]

Draft paper begun [3/02], AAS00

NGC 1399

 

 

Gal.

1

49898,

240,

2389

600214

600000

13.2

44.1

14.8

M. Wise

5/8/01

6/15/00

5/8/01

Examination begun.[6/02]

 

Vela X-1

XRB

1

102

400015

28.4

N. Schulz

4/13/00

 

ApJ, 2002, 564, L21

MCG –6-30-15

(w/Fabian)

 

 

AGN

1

433

700105

128.2

H. Marshall,

J. Lee

4/5/00

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,

Theta Ori

 

“Hot” Stars

1

3,

4

200001

200002

50.1

31.3

N. Schulz,

D. Huenemoerder

10/31/99

11/24/99

Theta Ori A and E line fluxes. Draft papers III and IV continued…[9/02] 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

MEG +/-1 spectrum. Include background subtraction.[7/02]

High-Res UK talk. 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

Sasaki models compared. Allowed plasma region, abundances; shelf and arc fluxes.[9/02]

High-Res UK talk.

AAS’03 abstract.

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.