HETG

Follow-on Science Instrument

Contract NAS8-01129

Monthly Status Report Numbers 018

August 2003

Science Theme: Supernova Remnants 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

 

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 .

 

2.0 Schedule of Past and Future Events Relevant to HETG

 

 

Date

Past Events

Comment

Aug. 11

Abstracts due for Four Years w/Chandra , Huntsville, AL

Aug. 19

Chandra Quarterly Review

 

Aug. 23

SIRTF Launch

 

 

Date

Future Events

Comment

Sept. 15

EPO Cycle 5 proposals due

 

Sept. 16-18

Four Years with Chandra, Huntsville AL

D. Dewey, J. Houck, A. Juett, M. Wise, Andy Young

Oct. 8

Chandra Fellows Symposium, CfA

T. Fang, S. Heinz, J. Lee

Oct. 12-15

ADASS 2003, Strasbourg France

M. Noble

Oct. 13-19

5th Microquasar Workshop , Tsinghua, Beijing

 

Oct. 27-28

Chandra Calibration Workshop II, Cambridge MA

many

Oct. 27-31

APS Div of Plasma Physics, Albuquerque NM

D. Huenemoerder

Oct. 28-31

Stellar-Mass, Intermediate-Mass, and Supermassive Black Holes , Kyoto, Japan

 

Oct. 29-31

CIAO wokshop (5th) at CfA

 

Nov.1-ish?

POG updated for AO6

 

Nov.2-5

X-Ray Timing 2003: Rossi and Beyond , CfA

M. Nowak

Nov. 6

Chadra Fellows proposals due

 

Nov. 18-19

Chandra: IAR and Quarterly Review

 

Nov. 17-22

Young Compact Binaries in the Galaxy and Beyond, La Paz, Mexico

 

Nov. ??-??

Con-X Facility Science Team meeting

K. Flanagan

Dec. 8-12

Multiwavelength AGN Surveys, Cozumel, Mexico

 

Jan. 4-8

203rd AAS meeting, Atlanta GA.

 

 

 

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 August there were 6 HETG observation intervals for 6 targets. These were all GO observations and included 3 with MIT-based PI-s: VW Cep (Dave Huenemoerder), Her X-1 (Mario Jimenez-Garate) and 4U 1822 (Prof. Chakrabarty). The data from these 3 indicate the instrument is performing nominally.

 

3.2 Science Support to CXC, SWG, etc.

 

Submitted abstract for “Four Years of Chandra Observations” symposium.

 

 

4.0 GTO Science Program

4.1 Observations and Data status

Progress in our GTO program is summarized 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 we present an update on the status of the Supernova Remnant GTO observations in the following pages.

 

GTO Science Theme

Abbreviation

(for App’ix A)

Researchers

(HETG in caps)

Date of recent [previous] reporting

Assembler of theme material

“Cool” Stars

Cool Star

dph,nss,psw,bb

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,

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,mw,jh

August, 2002.

Michael Wise, Tesla Jeltema

Active Galactic Nuclei and Jets

AGN, Jet

RG,MJ-G,hlm,

man,jcl,sm,jg

June, 2002.

Herman Marshall

Inter-Stellar Medium

ISM

AJ,nss

February, 2003.

Adrienne Juett, Norbert Schulz

Inter-Galactic Medium

IGM

RG,hlm

July, 2002.

Taotao Fang

Supernova Remnant Progress, Part II (June’02 – August’03)

 

Summary of Supernova Remnant Observations and Activities

In the last 14 months progress has continued in the analysis and understanding of our GTO observations of Supernova Remnants. A major accomplishment was the recent submittal to Astrophysical Journal of a comprehensive paper on E0102: “Chandra High-Resolution X-Ray Spectrum of Supernova Remnant 1E0102.2-7219” by Flanagan et al. A contribution to the High Resolution Spectroscopy workshop, “Extended Source Analysis for Grating Spectrometers” by D. Dewey (available online), summarized some techniques and results for HETG SNR analysis. The determination of masses and abundances was a focus this period and has lead to an understanding of the importance of spectral model assumptions and geometry assumptions in these calculations. The Table below lists our SNR GTO observations and for reference the other 5 known “Oxygen-rich” remnants as well; these 5 have all been observed with ACIS and no grating. Specific progress is described in the following pages.

Obs

Cycle

HETGS

Obsid(s)

Exp.

Time

(ks)

SNR

Name

Loc.,

Dist.

(kpc)

Ang.

Dia.

Dia.

(pc)

Age

(y)

Comments

2

1045, 2410,

2416

117

N103B

LMC, 50

31”

7.5

1,500

Strong Si and Fe lines.

Type 1a or Core collapse?

 

 

 

 

 

 

 

 

Oxygen-rich SNRs w/HETGS:

2

1046

70

Cas A

Gal., 3.4

340”

5.6

320

 

1

121, 1828

100

N132D

LMC, 50

115”

27.9

1,350

Bright Filaments, “O blob”

1,

4

120, 968

3828

137

138

E0102

SMC, 60

44”

12.8

1,000

Weak Fe lines

90 deg roll from Cycle 1 obs.

 

 

 

 

 

 

 

 

Other Known O-rich SNRs:

 

 

 

Puppis A

Gal., 2.0

 

3300”

32.0

~ 5,000

 

 

 

 

G292.0+1.8

Gal., 4.8

540”

12.5

< 1,600

 

 

 

 

B0540-69

LMC, 50

68”

16.5

~ 1,700

PWN; 8” dia. O III ring.

 

 

 

0103-72.6

SMC, 60

170”

49.4

~20,000

Older version of E0102 ?

Park et al. Astro-ph/0309271

 

 

 

NGC 4449

3900

<0.03”

< 0.6

~ 100

Patnaude and Fesen, ApJ 2003

 

E0102

We have devoted quite a bit of energy to analysing and understanding SNR E0102 during the past year or so. During this time a comprehensive paper was completed and submitted to ApJ and includes a range of our initial results and more recently estimates of the mass of the Oxygen and Neon in the ejecta and a discussion of possible mechanisms to produce an axial/cylinderical symmetry of the remnant. Look for Flanagan et al 2003 in ApJ very soon!

 

Research extending beyond the paper has been on-going and some items are described here below.

 

 

A second E0102 HETGS observation, obsid 3828, was taken in December 2002 at a roll 90 degress from the earlier data; the MEG m=-1 order image is shown above. This 135 ks exposure has equal or greater counts than the earlier obsid 120 data (87 ks) and simultaneous analysis of them is planned especially for the Oxygen lines (red above.)

 

Count rate ratios of these Oxygen lines do show the effect of the ACIS contamination layer and their quantitative values provide support for the External Cal Source measured absorption model – indicating that there is some small additional absorption not currently in the edges-only derived model.

 

A first look spatial-spectral analysis of these new E0102 data give a spatial-velocity image for the Ne X line at right very similar to that derived from obsid 120; this inspite of the 90 degree rotation is a good confirmation of the reality of the result.

 

 

The HETGS data for E0102 can be roughly fit by a single, global vnpshock model, above, which allows relative abundances of the elements to be determined under this model assumption. In the plot at right, these abundances (red) are compared with expectations from SNR models, specifically Core-collapse models (purple) and Type Ia models (green); for reference SMC/ISM abundances are also shown (blue.) As expected E0102 is unambiguously a core-collapse remnant from a progenitor of ~30 solar masses.

 

Using Chandra’s high spatial resolution we have started to study localized regions of the E0102 ejecta ring, specifically the Northern “shelf” and Southeast “arc” bright features. The plots below show contours in temperature-tau model space for Oxygen line ratios from these regions. Although not identical, the similarity of temp and tau for ejecta in these two regions is a little puzzling given other indications of overall temperature and tau differences between north and sourth parts of the remnant, e.g. the intensity of flux above 2keV shown at left. These results therefore add constraints on the overall 3D model of the ejecta-plus-blastwave that we hope to create, see “3D Modeling” section below. (Plots from Fredericks et al., poster at 201st AAS meeting.)

 


N132D

One item of note in N132D analysis is the overplotting of the grid of shock model predictions on the ratio-ratio plot shown above. The ratio of O VIII Lyman alpha to total O VII triplet (r+I+f) flux is plotted on the X-axis. The Y-axis gives the O VII forbidden to resonance ratio. Values of these ratios for a variety of features/filaments in N132D are plotted by red symbols. The overlayed grid shows the region spanned by the model for various T and tau values. The NE-corner region has an unexpectedly high f/r ratio. The raw data for NE-corner are shown at right with the model fit and decomposition into the r, i, and f contributions; the bottom panel shows the nominal feature profile and specific region of interest. (Plots from Fredericks et al., Poster at Con-X meeting, May 2003.)

 

 

N103B

 

We fit the global HETGS spectrum of N103B with a model, shown above left, that is the sum of high-T (green) and low-T (red) “vnpshock”s with variable abundances plus a small synchrotron “srcut” component (blue.) The total spectrum agrees well with our data.

The plot in the upper right shows the contribution of Fe emission (green) to a shock model (other elements’ emission shown in grey.) The “Iron forest” between 7A and 18A is a major contributor to the N103B model in that range making it hard to clearly identify Ne and Mg emission in that range.

Shown at right are the abundances from the 2T model (red) compared with Ia and core-collapse models (green, purple) and the LMC ISM abundance (blue dotted.) Our model abundance ratios are tantalizingly in between the Ia and core-collapse predictions; mass estimates are ongoing. (From M.S. Thesis by J. Migliazzo, 2003.)

 

3D Modeling

 

1:, 2:, 3:, 4:.

 

The red-green spatial-velocity image of derived for the Ne X line in E0102 suggests a cylinderical ejecta distribution, 1 above, viewed nearly on-axis. In order to qualitatively and quantitatively test this and related ideas on E0102’s structure we’ve started to explore the creation of 3D plasma models and their X-ray emission. As an example 2 above, shows the X-ray color-coded intensity image cylinderical ejecta surrounded by a spherical blastwave shell.

We’re also looking at available 3D software and how it could be used in 3D astrophysical modeling. For example, 3 above, shows a view from the modeling window of the Blender software in which a cylinder (green mesh), an observer (pink) and light source (yellow dot) have been defined. When this model is “rendered” the image shown in 4 above is generated. Ideally the same model definition software could be used as input to an “X-ray renderer” for X-ray modeling.

 

Supernova Remnant Plans, Part II

 

Our plans for the next year or so are given here. A general additional topic for all of our SNR research would be to include and understand obseravtions made at other wavelengths like radio, optical and IR.

 

E0102

·      Compare fluxes with models, e.g., power-law shock model values.

·      Investigate 3-D models for their agreement with the Ne X spatial-velocity results and the variation of ionization stage with position.

·      Create s/w to jointly analyze the Cycle 1 and Cycle 4 E0102 observations, especially for O VIII, O VII lines.

 

N132D

·      Try including an Fe "pseudo continuum" to better measure Ne and Mg line fluxes in the various regions.

·      Understand the enhanced O forbidden emission in the NE-corner region.

·      Find the abundance ratios for a global fit to a single vnpshock model, compare w/Ia,II yields.

 

N103B

·      Complete Paper 1 on N013B.

·      Carry out spatial-spectral analysis of Si lines by combining MEG and HEG data sets.

 

Cas A

·      For the Si feature combine grating line flux values with ACIS zeroth-order continuum values to get n_H/n_Si and feature masses.

·      Analyze additional features in Si and S for flux, temp, mass, and doppler velocities.

·      Find the abundance ratios for a global fit to a single vnpshock model, compare w/Ia,II yields.

 

Advanced Analysis

·      Investigate use of 3D s/w and tools for SNR modeling, specifically for E0102 modeling.

·      Work with ISIS s/w team to determine useful spatial-spectral s/w functions to be added to ISIS.

 

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

 

Software created for the SNR analyses described here include: a combined random-search/fitting method was used in ISIS to find good fits of the vnpshock model to E0102 and N103B data sets; the procedure rr_grid.pro was written to overplot model grids on the ratio-ratio plots (N132D); and a set of IDL routines (“v3d_….pro”)were written to do some simple 3D modeling and visualization.

4.4 Presentations, etc. (August)

 

 

A quiet month for talks.

 

 

 

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

 

K.A. Flanagan, C.R. Canizares, D. Dewey, J.C. Houck, A.C. Fredericks, M.L. Schattenburg, T.H. Markert, D.S. Davis, “Chandra High-Resolution X-Ray Spectrum of Supernova Remnant 1E0102.2-7219”, ApJ submitted.

Adrienne M. Juett & Deepto Chakrabarty, “X-ray Spectroscopy of the Low-Mass X-ray Binaries 2S 0918-549 and 4U 1543-624”, ApJ accepted, Vol. 599 (2003.)

Herman L. Marshall, Daniel Dewey, and Kazunori Ishibashi, “In-Flight Calibration of the Chandra High Energy Transmission Grating Spectrometer”, SPIE Volume 5165 (2003.)

 

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 August.

 

6.0 Management

 

6.1 Program Office & NASA Support

 

Supported the Chandra Quarterly Review on 8/19.

 

6.2 MIT-internal management activities

 

Arranged/initiated phone and room changes for September personnel changes.

 

 

7.0 Open Issues, Problems, etc.

 

There are no open issues or problems regarding the HETG.

 

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

TBD

Prop.

05400034

[67]

M. Nowak

[TBD]

Target accepted in peer review.

 

MCG—6-30-15

AGN

5

TBD

Prop.

05700032

[540 ! ]

J. Lee

[TBD]

 

 

Orion Nebula Cluster

“Hot” Stars

5

TBD

Prop.

05200040

[100.0]

N. Schulz

[TBD]

 

 

 

 

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

97.1

N. Schulz

6/5/03

XMM obs on 8/20. Spectra analyzed[7,8/03]. Data in-house, spectra good[6/03].

(Cycle 1 obs. also)

 

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].

 

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

Replanning FUSE obs.[8/03] Data in-house [6,7/03]. FUSE proposal submitted for coord. Obs[1/03].

 

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 counts in lines. S-S analysis of Ne X line; arfs made. Quick look images[1/03]. Data in-house and look good. Parameters OK.[12/02]

 

 

 

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

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 GO)

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] Data reduced; jet seen in zo image.[5/02]

 

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.y collaboration…[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

Complete analysis of Cycle 2 data

L. 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

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.[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] ISIS scripts for fluxes and energies.[10/02]

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]. Sasaki models compared.[10/02]

ApJ submitted[8/03].

AAS’03 Poster. High-Res UK talk.[10/02]

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.