HETG

Follow-on Science Instrument

Contract NAS8-01129

Monthly Status Report Numbers 023 & 024

January & February 2004

Science Theme: Source Models

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                   Mike.C.Smith@nasa.gov

PS41/Wayne Harmon, MSFC             Wayne.T.Harmon@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@space.mit.edu .

 

2.0 Schedule of Past and Future Events Relevant to HETG

 

Date

Past Events

Comment

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, G. Allen

Feb. 8-12

Polarimetry meeting, Stanford U., CA.

H. Marshall

March 1

GTO target selections due to CXC

many

March 3-4

Chandra Quarterly at MSFC

D. Dewey

 

Date

Future Events

Comment

May 12-15

"Beyond Einstein: From the Big Bang to Black Holes", Kavli Institute, Stanford U., CA..

K. Flanagan

May 23-28

“The Fate of the Most Massive Stars”, Jackson Hole, Wyoming

Ishibashi, Houck

May 30-6/3

AAS Meeting, Denver, CO.

N. Schulz, H. Marshall

June 7-13

5th Microquasar Workshop, Beijing, China

H. Marshall, S. Heinz

June 15-17

Chandra Peer Review, Cycle 6, Logan Airport Hilton, Boston MA

many

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, S. Heinz

June 28-29

Chicago 2004: A Workshop to Foster Broader Participation in NASA Space Science Missions and Research Programs , Chicago

 

July 5-9

13th Cambridge Workshop on Cool Stars, Hamburg Germany

N. Schulz, D. Huenemoerder

July 7-9

Galaxies viewed with Chandra Workshop 2004, Cambridge MA

 

July 12-16

Cores, Disks, Jets & Outflows in ... Star Forming … , Banff, Canada

N. Schulz

July 18-24

35th COSPAR meeting, Paris France.

 

Canizares,, Flanagan, Marshall, Wise, Wojdowski,Jeltema, Houck, Stage, Allen

 

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 no HETG observations in January 2004.

In February 2004 there were two targets observed in three obsids. These included a 300ks GO observation of IRAS 13349+2438, PI is J. Lee, Chandra Fellow at MIT; the data look OK.

 

3.2 Science Support to CXC, SWG, etc.

 

Contributed HETG article to Chandra Newsletter.

Worked with CXC to get HETG proposal planning thread available on the web.

Supported getting improved ACIS OBF contamination model into the Feb.2 CALDB release.

Working with CXC on reprocessed Capella observations for calibration purposes.

Contributed to Martin Weisskopf’s Chandra paper for Experimental Astronomy.

 

 

 

 

4.0 GTO Science Program

4.1 Observations and Data status

GTO targets for Cycle 6 were submitted to CXC by March 1 as requested. No new GTO data were received in January or February. 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 make a theme diversion and present in the following pages a summary of source models created in our research.

 

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, 2003 [Dec. 2002]

Many contributors.

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

Source Models Created and Used with HETG GTO Research

 

Summary of Source Model Activities

 

One way of demonstrating our understanding of the physics involved in an astronomical source is through the creation of a model of the source that reproduces the essential spatial, spectral, and temporal features that we observe. With Chandra there have been large improvements in the spatial resolution and spectral resolution (and the combined ability to have spatial-spectral resolution) of our data. (I leave temporal-spectral, etc. considerations out of this brief summary.) Consequently the amount of detail needed in our source models has increased as well. A rough summary of the details seen at low and high spatial and spectral resolution is given here:

 

 

Spatial resolution

Low: Just a single or perhaps a few resolution elements per main source feature. Requires simple basic and generally symmetric shapes to model, e.g., "beta-model" for galaxy cluster or a ring+shell model of a supernova remnant.

High: Many resolution elements per feature. Complexity in spatial structure is seen, e.g., knots, wisps, filaments, "holes", "bubbles", non-uniformities, proper motions, small faint features, etc.

Note: that the "spatial resolution" here, "Low" or "High", depends on the source angular size as compared to the telescope resolution; thus there have been "High" spatial resolution observations pre-Chandra and there still remain "Low" spatial resolution data even with Chandra!

 

 

Spectral resolution

Low, Medium: Of order CCD resolution. Allows the overall spectral shape, identification of the brightest emission lines/regions from different elements and some ions, detection of absorption edges, detection of line broadening/distortion effects and bulk Doppler shifts at the thousands of km/s level for high S/N cases.

High: Of order Chandra and XMM-Newton gratings resolution. Can clearly separate emission lines from different ionic species, separate He-like triplets, resolve RRCs, show structure in absorption edges, see weak lines, measure Doppler widths and velocities of hundreds of km/s.

 

Of course improved spatial resolution requires a higher geometric fidelity in the source model. But even for a source seen at "Low" spatial resolution, e.g., the case of an AGN or an XRB observed by Chandra, if it is seen at "High" spectral resolution there may be many signatures of the detailed source geometry imprinted and visible in the observed spectrum. Hence, the actual 3D geometry and dynamics of the source become more important for both higher spatial and higher spectral resolution.

 

Higher spectral resolution of course additionally puts greater demands on the accuracy of the atomic physics used to predict the emission, scattering, and absorption of X-rays. Combined with a more complex geometry, there is also a need to ensure self-consistency between local plasma properties, e.g. electron temperature and ionization state, and the local radiation environment.

 

XSPEC models (as also imported into or recreated in other packages like ISIS, Sherpa, etc.) are an off-the-shelf community set of models. For these, however, the underlying geometry is generally simple (a volume of plasma) or hardwired (a continuum-illuminated cone) and the model output is at "Low" spatial resolution, typically a single spatial bin. Spectrally the APED database of lines and continuum emissivities is used (high-resolution) and Doppler broadening and shifts can be included and multiple components summed; e.g., modeling of the SS 433 jets in partial eclipse was done in this way. But because of the simplicity of the database interface and source geometry assumed, the model spectra do not encode the full complexity of a realistic source, e.g., continuous parameter variation along a jet.

 

"Community" codes of greater spectral and geometric complexity are also growing in use, e.g., XSTAR and PHOTOION and are beginning to address some of these issues.

 

In the course of our HETG GTO research program, driven by high-resolution HETG spectra, we have also worked on advanced X-ray source models to better model the data. In the following pages some of these modeling efforts are briefly described.

Direct APED Database-access Plasma Model

 

Use: Determine temperature distributions and elemental abundances.

 

Geometry: DEM method assumes a sum of regions of different temp.s and a common abundance.

 

Spectral: APED database: lines plus continuum combined with more flexibility than XSPEC models currently allow. Line-based modeling.

 

Output: Synthetic continuua, DEM distribution and abundances

 

Coded in: ISIS, S-Lang.

 

Comments: This modeling is an example of using APED continuum emission models as an iterative baseline for fitting emission line fluxes. This is followed by the use of APED line emissivities to determine temperature distributions and elemental abundances. Finally, generation of synthetic spectra and observed counts using the multi-thermal, variable abundance plasma model (or even a pair for binary components at different radial velocities). Also some direct line-ratio fitting of the He-like triplets for density constraints.

 

Scientist: Dave Huenemoerder


Single-Zone Photoionization Model

Use: Applied to AGN, e.g., MR 2251, data modeling. Study the effect of (the unmeasured) EUV flux.

 

Geometry: Assumes a uniform plasma under illumination.

 

Spectral: Arbitrary ionization continua. Ionization rates, etc. from many sources.

 

Output: Heating rates, cooling rates, temperature, and ionization levels as a function of ionization parameter. Also ranges of ionization parameters and temperatures where a given ion is expected to be abundant.

 

Coded in: C++

 

Comments: A single-zone thin photo-ionized plasma model designed after the fashion of Krolik, McKee, and Tarter (1981). It includes the following heating processes: photo-ionization, Compton scattering, and Auger electrons. And the following cooling processes: recombination (including dielectronic), bremsstrahlung, and collisional line excitation (assumed from ground.) Collisional ionization is also modelled, as a contribution to ionization balances.

 

Scientist: Rob Gibson


Non-thermal Emission from Electron Distribution

 

Use: Model non-thermal emission see in SNe and SNR; SN 1006.

 

Geometry: Assumes a uniform volume of electrons.

 

Spectral: The spectral characteristics are calculated based on a given, arbitrary distribution of non- thermal electrons.

 

Output: Spectrum of non-thermal emission.

 

 

 

 

 

 

Coded in: C (comp. intensive) and S-Lang

 

Scientist: John Houck

Monte Carlo 3D Disk reflection model

 

Use: Accretion disk reflected spectra.

 

Geometry: General: array of grid cells with density, temp., and ionization state. Input from n-D hydro-code; e.g. 2D radiation-MHD calculations by Neal Turner. Input illumination given by position and direction distributions.

 

Spectral: Illuminated by power law. Detailed photon-tracing of through propagation, absorption, scattering, (re-)emission, and ionization effects.

 

Output: Reflected photons and their spectrum.

 

 

 

Coded in: C.

 

Comments: XSTAR pre-computed results are used to map the local ionization parameter to ionization fraction and temp. of each cell. Ultra-rough draft of paper in process...

 

Scientist: Andy Young.

Disk Atmosphere and Corona Emission

Use: Model disk/corona emission in LMXBs containing neutron stars; Model narrow-line Seyfert I galaxies containing, e.g., a super-massive Kerr Blackhole, MCG --6-30-15; NGC 4051; Mkn 766.

 

Geometry: 2D disk: height(r), to 3D: azimuthally symmetric. Orbital velocities are included. Centrally illuminated (Neutron star.) "Self illuminated": assume non-thermal X-rays are produced uniformly above the disk using the disk's own energy.

Spectral: Semi-Analytic or Monte Carlo spectral model used. Kerr metric relativistic effects and Doppler shifts are included for BH simulation.

 

Output: Continuum spectrum, line spectrum; 3D structure with charge state distribution, Temp., density.

 

Coded in: FORTRAN, IDL, S-Lang.

 

Comments: Using Raymond code for ionization balance, HULLAC recombination rates, and own structure and spectral calculations.

 

Scientist: Mario Jimenez-Garate

Recombination and Resonance Scattering Models

 

Use: Model Seyfert II ionization cone; wind of super-soft source, CAL 87.

 

Geometry: Single or multiple ionization zones; arbitrary fixed covering fraction.

 

Spectral: Illumination by a BB or PL continuum, e.g., white dwarf or Seyfert, respectively.

 

Output: Binned spectra of components: resonance scat., radiation recombination lines, and RRCs.

 

Coded in: IDL.

 

Comments: Uses XSTAR for ionization balance, and HULLAC recombination rates.

 

Scientist: Mario Jimenez-Garate

3D Model Projected to Sky w/Doppler Shifts

 

 

Use: SNR spatial-spectral models especially for E0102.

 

Geometry: General: given by 3D array of "norm". Routines allow easy input of simple shapes.

 

Spectral: Emission is spectrally colored by: i) single line w/Doppler shifts, or ii) a MARX-assigned spectrum.

Output: Events file for input to MARX ray-trace.

 

Coded in: IDL; uses S-Lang user interface to MARX .

 

Comments: Reproduces qualitative E0102 plus/minus order differences in Ne X line. Multiple components can be combined. This is an exploratory prototype...

 

Scientist: Dan Dewey

 

 

4.4 Presentations, etc. (January and February 2004)

 

(None in January & February besides the AAS meeting covered in the December report.)

 

 

 

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

 

D.P. Huenemoerder, “Chandra X-ray Observatory High-resolution X-ray Spectroscopy of Stars: Modeling and Interpretation”, Physics of Plasmas, May 2004; astro-ph/0403085.

J. Kastner et al., “The Coronal X-ray Spectrum of the Multiple Weak-Lined T Tauri Star System HD 98800 [TV Crt]”, ApJ Letters, accepted; astro-ph/0403062.

Jimenez-Garate, “The X-ray Spectra of Accretion Disk Atmospheres in the Kerr Metric”, Proceedings paper for the 10th Marcel Grossman meeting, Brazil, 2003; submitted and to be on astro-ph soon.

 

 

 

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 January and February.

 

6.0 Management

 

6.1 Program Office & NASA Support

 

Prepared input for and attended the Chandra Quarterly Review at MSFC on March 3, ‘04.

 

6.2 MIT-internal management activities

 

Received ~20 very good applications for the HETG Post Doc position by the closing date of January 15th. Interviewed 5 candidates and plan to make decisions and get offer out in March.

 

 

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

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

Prelim analysis [1/04] XMM obs on 8/20.

 

Sco X-1

XRB

4

3505

400258

16.1

N. Schulz

7/21/03

CC Data being processed [7/03]. Multi-wavelength obs

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

Curve of growth [1/04] Identify-ing lines, back-ground [12/03]. Fe lines searched [10/03] Mg, Ne lines.

 

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]

Paper re-submitted[2/04]

E0102

SNR

4

3828

500307

137.7

K. Flanagan,

D.Dewey

12/20/02

Echelle O III data[1-2/04] Measure shelf, arc, 10/03] Extracted counts and flux ratios.[9/03]

 

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

Wind aspect [2/04] Improved photo-ion model[1/04] High-velocity outflow [12/03]. UV flux insufficient to pump forbidden to intercomb.[10/03] ISIS and IDL EW s/w…[9/03]

Improved paper [1/04] First draft finished.[7/03].AAS03.

NGC 7469

AGN

3

3147

(+2956)

700586

69.8,

79.8

J. Lee, (Kriss),

H. Marshall

12/13/02

UROP working [2/04] Analyzed data, id absorp lines.[1/03] 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
Wind aspect [2/04] Work ongoing[8/03]. XTE and SAX obs analyzed.[12/02]

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,

A. Young

5/7/01

Extract, identify lines [2/04] 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]

Press confer-ence, Jan.04. Final draft[12/03] CSR-02-01,‘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].

ApJ Accepted! Astro-ph 0312509 [12/03]

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.