HETG

Follow-on Science Instrument

Contract NAS8-01129

 

Monthly Status Report No. 005

July 2002

HETG Science Theme: The Inter-Galactic Medium (IGM)

 

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 37-582G (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

July 6-13

Making Light of Gravity Conference, Cambridge, UK

C.R. Canizares invited talk

 

 

Date

Future Events

Comment

Aug. 8-10

The IGM/Galaxy Connection: The Distribution of Baryons at z=0 , Boulder CO

T. Fang

Aug. 18-22

X-ray Astronomy School, Berkeley Springs, WV

A. Fredericks

Aug. 25-28

SPIE conference, Hawaii

K. Flanagan invited talk

Sept.4,5

Chandra Quarterly and IAR, Cambridge, MA

HETG participate

Sept. 4-6

Workshop on X-ray surveys, Santander, Spain

Cluster analysis

Sept. 9-13

Wind, Bubbles, and Explosions, Patzcuaro, Mexico

 

Oct. 10-12

34th COSPAR, Houston TX:

E1.2 …clusters of galaxies and black holes

E1.4 …supernova remnants and neutron stars

J. Migliazzo on N103B

Oct. 24,25

High Resolution X-Ray Spectroscopy with

XMM-Newton and Chandra, UK

D.Dewey attending

Nov.1

Updated HETG section of Proposers’ Observatory Guide to CXC

HETG provide input

Nov. 6,7

Chandra Calibration Workshop at CXC, Cambridge MA

HETG/dd support

Dec. 9-13

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

 

July ‘03

IAU Symposium 218, "Young Neutron Stars and Their Environment", Sydney,

Australia

 

 



 

 

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 7 targets observed in 13 observation intervals by the HETG in July 2002. None of these were in the HETG GTO program.

 

The target IM Peg is being observed about once a week with the HETGS for 8 total observations; guest observer Dave Huenemoerder CXC/MIT has preliminarily analyzed the data and the instrument is performing fine.

 

3.2 Science Support to CXC, SWG, etc.

 

Created an ‘N0003 version of the MEG sector files as requested by Ishibashi/CXC to improve the MEG wings in MARX simulations – a very small effect for most observer’s uses.

 

 



 

 

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.

 

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 “Inter-Galactic Medium (IGM)” theme is presented.

 

GTO Science Theme

Abbreviation

(for App’ix A)

Researchers

(HETG in caps)

Date of last [next] reporting

Assembler of theme material

Stars

Star(s)

dph,nss

Not yet reported

X-ray Binaries & Accretion Disks

XRB

MJ-G,AJ,nss

Not yet reported

Supernova Remnants

SNR

KAF,DD,JMM,

AF,jh,gea,tp

May, 2002.

Dan Dewey

Isolated Neutron Stars

iNS

MDS,hlm

Not yet reported

Galaxies & Clusters of Galaxies

Gal., Clust.

TJ,mw,jh

Not yet reported [Aug.’02]

Active Galactic Nuclei and Jets

AGN, Jet

JL,TF,RG,hlm,

pmo

June, 2002.

Herman Marshall

Inter-Stellar Medium

ISM

AJ,nss

Not yet reported

Inter-Galactic Medium

IGM

TF,JL,RG,hlm,

pmo

July, 2002.

Taotao Fang

 



 

 

Inter-Galactic Medium Research Progress

 

Introduction

Image generated by Aladdin Ghostscript 
(device=ppmraw)

CREATOR: XV Version 3.10a  Rev: 12/29/94 
(PNG patch 1.2)  Quality = 100, Smoothing = 20
The standard cosmological theory (these days!) predicts that huge amounts of hot gas should exist in the vast space between galaxies in our local universe. This hot gas has been hidden from view since the time galaxies formed because at its high temperature it does not emit substantial visible light. It is thought that this gas forms part of a gigantic system, or web, of hot gas and dark matter that defines the cosmic landscape. The hot gas part of this system could contain more material than all the stars in the universe. Cosmological hydrodynamic simulations have been carried out to model the formation of structure in the universe as predicted by this theory.

 

 

At left is the image from such a simulation which shows the cosmic web of warm/hot gas as the light-blue filamentary structures. The denser regions in yellow and red are where clusters and groups of galaxies are located and are the only regions we’d see in optical light.

 

The image represents about 60 million light years along each side which is equivalent to a red shift of z ~ 0.004. Objects observed with Chandra for our IGM studies are much further away than this with z generally greater than 0.1 and as high as 2.



Basically, to detect and measure this warm/hot (0.1 to 10 million degrees) intergalactic medium (WHIM), we select X-ray bright background sources such as distant galaxies/AGN that can be detected by Chandra. When photons pass through places where this hot gas is located, they are absorbed by the highly ionized, "heavy metals" (C, N, O, Si, Fe) in the hot gas and an X-ray absorption feature or “dip” will be produced in the spectrum of the background source. Based on the detected absorption signatures, we can derive the physical properties of the absorbing gas. A key parameter to measure is the Doppler shift of the absorption dips which measures the location of the gas along the line-of-sight.

In this illustrative diagram an X-ray source is shown emitting three different wavelengths of X-rays, coded by the red, yellow, and blue waves. In going through the filament of IGM gas the yellow wavelengths are absorbed and do not reach Chandra. The spectrum in the inset shows actual data where absorption “dips” are visible due to Oxygen in the IGM.

This image is taken from the Chandra Press release at:

http://chandra.harvard.edu/press/02_releases/press_073102.html



 

Summary of IGM GTO Observations and Activities

In the HETG GTO program we've specifically included some bright distant AGN sources to probe for warm/hot gas in the intergalactic medium, in addition some AGN used as calibration targets are also useful in IGM studies. Relevant targets are tabulated here:

 

AO-

Target

z

Lines seen?

1

Q0836+7104

2.17

No line, set upper limit

1/Cal

PKS 2155-304

0.12

OVII, OVIII at z=0; OVIII at z=0.055

Cal

Mkn 421

0.03

In progress

1

PKS 2149-306

2.34

No line, set upper limit

Cal

3C 273

0.16

OVII at z=0

2

H 1821+643

0.30

Fe emission lines at E=6.4 and 6.9 keV

 

 

 

 

3

3C 279

0.64

In progress

3

1ES 1028+511

0.36

In progress

3

1H 0414+009

0.28

recently observed, data will arrive soon

 

 

 

 

4

1H 1426+428

0.13

to be observed in Cycle 4 (starting about Dec ’02)

 

HETGS data have been (or will be) taken on all of these targets and in addition for the "Cal" targets LETG data are often available as well, using the LETG improves sensitivity to redshifted Oxygen lines (O VII, OVIII.)

 

Our science activities to study the IGM are not limited to Chandra observations. We are also making use of the capabilities of the XMM-Newton observatory, working on AO1 data received from two targets: PG 1407+265 and PKS 2135-14, Guest Investigators: T. Fang and C.R. Canizares. We have also talked with the PI of the NASA SMEX mission SPIDR (Spectroscopy and Photometry of the IGM's Diffuse Radiation) and are working on creating an OVI emission map relevant to SPIDR from our simulations. (The SPIDR website is: http://www.bu.edu/spidr/noflash/overview.html .)



 

 

 

High Redshift Quasars: Q[S5]0836+710 and PKS 2149-306

(Published by T. Fang, H.L. Marshall, G.L. Bryan, and C.R. Canizares, ApJ, 555, 356)

We obtained the first high-resolution X-ray spectra of two high-redshift quasars, Q0836+710 and PKS 2149-306, obtained with the Chandra High Energy Transmission Grating Spectrometer (HETGS). The primary goal of this observation is to use the high spectral resolving power of the HETGS to detect X-ray absorption produced by a hot intergalactic medium. The continuum of both quasars can be fit by absorbed power laws. Excess continuum absorption above the Galactic value is found in Q0836+710, as evidenced in ASCA and ROSAT observations. No significant emission or absorption features are detected in either source at a +/-3 sigma level. Based on the detection limits we constrain the properties of possible emitters and absorbers. Absorbers with a column density higher than 8e16 /cm^2 for OVIII or 5e16 /cm^2 for SiXIV would have been detected. We propose a method to constrain the cosmological parameters (namely Omega_0 and Omega_b) via the X-ray forest theory, but current data do not give significant constraints. We also find that combined with the constraints from the distortion of the CMB spectrum, the X-ray Gunn-Peterson test can marginally constrain a uniform, enriched IGM.

 

HEG spectra of Q[S5]0836+710 (top panel) and PKS 2149-306 (bottom panel). The solid line and dotted line in each panel are the observed and fitted spectrum, respectively. The spectral model is an absorbed power-law.



H 1821+643: Setting Limits on IGM Temperature

(Published by T. Fang, D.S. Davis, J.C. Lee, H.L. Marshall, G.L. Bryan, and C.R. Canizares, ApJ, 565, 86)

H 1821+643 is one of the most luminous quasars (m_v = 14.1) at low redshift (z = 0.297). It was discovered as a serendipitous X-ray source detected with the Einstein Observatory and has been studied extensively. At a moderate redshift, the sight line toward H 1821+643 traverses a distance of nearly 1.5 Gpc. Numerous absorption systems (such as H, C, N, O, Si, etc.) have been discovered in this sight line in optical and UV bands. Especially in recent observations, the Hubble Space Telescope and the Far Ultraviolet Spectroscopic Explorer have detected a number of OVI absorption lines which are not clearly associated with any galactic system.

 

We searched for absorption features from a warm/hot component of the IGM along the line of sight to this quasar and no absorption features were detected at or above the 3-sigma level. Based on the lack of OVII/OVIII absorption lines and by assuming collisional ionization equilibrium, we constrain the gas temperature of a typical OVI absorber to be between 0.1 to 1 million K, which is consistent with the results from hydrodynamic simulations of the intergalactic medium.

 

 

 

At left the zeroth-order image of H~1821+643, with North to the top and East to the left. The star K1-16 is indicated. From the contours it appears that there is extended (cluster) emission around the central source.



 

An iron emission line attributed to H1821+643 is clearly resolved at 6.43 keV (rest frame), with an equivalent width of 100 eV. Although we cannot rule out contributions to the line from a putative torus, the diskline model provides an acceptable fit to this iron line. We also detect a weak emission feature at 6.9 keV (rest frame). We suggest that both lines could originate in an accretion disk comprised of a highly ionized optically thin atmosphere sitting atop a mostly neutral disk.

 

 

The simultaneous fit to MEG (red) and HEG (black) spectra between 2 and 7 keV. Two Gaussian components are added to fit the emission features around 5 and 5.3 keV.

 

 

As revealed in the zeroth order image there is also extended emission from the cluster of galaxies which surrounds H1821+643. We have been able to separate the moderate CCD X-ray spectrum of the surrounding cluster from the central quasar and find that this is a hot cluster with a temperature of ~ 10 keV and a metal abundance of 0.3 Z_sun. We also independently obtain the redshift of the cluster, which is consistent with the optical results. We estimate that the cluster makes negligible contributions to the 6.9 keV iron K line flux identified above.



 

PKS 2155-304 : Clear detection!

(Published by T. Fang, H.L. Marshall, J.C. Lee, D.S. Davis, and C.R. Canizares, ApJ Letters, 572, 127)

We report the first detection of an OVIII Ly-alpha absorption line associated with an over-dense region in the intergalactic medium (IGM) along the line of sight towards PKS 2155-304 with the Chandra LETG-ACIS. The absorption line is detected at a 4.5-sigma level with cz ~ 16,600 km/s. At the same velocity Shull et al. detected a small group of spiral galaxies (with an overdensity of 100 and low metalicity HI Ly-alpha clouds. We constrain the intragroup gas that gives rise to the OVIII Ly-alpha line to a baryon density in the range 1e-5 < n_b < 7.5e-5 cm^-3 and a temperature of 4 to 5 million K, assuming 0.1 solar abundance. These estimates are in accordance with those of the warm/hot intergalactic medium (WHIM) that is predicted from hydrodynamic simulations. Extrapolating from this single detection implies a large fraction of the ``missing baryons'' are probed by the OVIII absorber.

 

The Chandra LETG-ACIS spectrum of PKS~2155-304 between 18 and 22 A, the red solid line is the fitted continuum plus three Gaussian absorption dips, the ion species are labeled in blue. The absorption feature at 20.02 A has been identified as OVIII Ly-alpha absorption from the IGM.

 


 

 

 

 

 

 

Our detection and upper limits can be compared with theory on a plot of cumulative probability of OVIII absorption per unit redshift vs. column density. Three data points are: PKS 2155, H1821, Q[S5]0836. We find that the detection is consistent with predictions from cosmological simulations (soild curve).

 

 

 

 

 

 

 



Inter-Galactic Medium Plans and Further Work

 

 

- Complete analysis of the three sources from AO3: 3C 279, 1H0414, 1ES1028; publish detections or limits to lines from O VII and O VIII.

 

- Analyze new Chandra cycle 3 and cycle 4 GTO observations.

- Continue analyzing data from 3C 273 and Mkn 421 to search for weak absorption features from the IGM.

 

- Continue analysis of XMM-Newton GO data on PG 1407+265 and PKS 2135-14.

 

- Collaborate with F. Nicastro on Chandra/XMM TOO observations of Seyfert I Galaxies and blazers in outburst.

 

- Perform cosmological simulations on the non-equilibrium evolution of IGM ionization structure.



 

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

 

In connection with IGM research, we are developing new software programs to systemically analyze weak absorption/emission features in X-ray spectra of extragalactic sources. These programs involve accurate measuring of the small-scale continuum level, fitting features with a set of Gaussian lines in emission and/or absorption, and identification of bulk Doppler shifts of lines from individual ions. The software is written as a suite of S-Lang scripts that can be run in ISIS.

 

 

4.4 Presentations (July)

 

C.R. Canizares, “Results from Chandra”, Making Light of Gravity, Cambridge UK, 7/9/02.

 

 

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

 

A.K. Hicks, M.W. Wise, J.C. Houck, and C.R. Canizares, “Chandra X-Ray Spectroscopy and Imaging of the Galaxy Cluster PKS 0745-191”, ApJ accepted, 2002.

 

J.C. Lee, “The Chandra and RXTE view of GRS 1915+105”, Proceedings of the 4th Microquasar Workshop, 2002, astro-ph/0208187.


5.0 Systems and Engineering Support

 

5.1 Documentation and “Design Knowledge Capture”

 

Received Chandra knowledge capture import file format from Eric Martin for our evaluation and use; will provide requested input for 8/20 and 8/30 deadlines.

 

5.2 Spares Retest and Test Instrumentation

 

Continued getting X-GEF system working…

 

5.3 Anomalies, Insert/retract, etc. Support

 

Noted that when inserted, telemetry usually indicates an angle of 6.34 degrees for the HETG and occasionally shows a value of 5.96 degrees. Brought this to SOT attention and Bill Podgorski noted that these are only one bit different from each other and not a cause for concern – a slow drift in the pot angle readout may cause this bit flip-flopping and it may be more common in future. In any case, the HETG is being inserted in the same repeatable location.


 

6.0 Management

6.1 Program Office & NASA Support

 

The final report for the previous HETG “Phase C/D” contract was submitted to MSFC and is available on the web at http://space.mit.edu/HETG/papers/HETG_Final_Report.pdf .

Submitted GFE equipment list in Excel format to MSFC (on 8/6/02.)

 

6.2 MIT-internal management activities

 

Two new computers were received and setup for HETG personnel. Continue working perennial office and disk space issues – with some success.

 

7.0 Open Issues, Problems, etc.

 

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

 


Appendix A. GTO Observation Status Tables

 

Notes:

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

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

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

 

Cycle 4

Object

Science Theme

AO

Obs ID

Seq. No.

Expos.

(ks)

Observer /

Analyst

Start Date

Comments & Analysis

Talks and

Publications

4U 1626-67

XRB

4

---

---

[100.0]

N. Schulz

 

Prop. No.: 04400027

 

Sco X-1

XRB

4

---

---

[15.0]

N. Schulz

 

Prop. No.: 04400046

 

H1426+428

IGM

4

---

---

[102.0]

T. Fang

 

Prop. No.: 04700987

 

Mrk 290

AGN

4

---

---

[250.0]

J. Lee

 

Prop. No.: 04700988

 

TV Crit

Stars

4

---

---

[100.0]

D. Huenemoerder

 

Prop. No.: 04200007,

Selected in peer review![6/02]

 

E0102

SNR

4

---

---

[140.0]

K. Flanagan,

D.Dewey

 

Prop. No.: 04500008,

Selected in peer review![6/02]

 

 


Cycle 3

Object

Science Theme

AO

Obs ID

Seq. No.

Expos.

(ks)

Observer /

Analyst

Start Date

Comments & Analysis

Talks and

Publications

MRC 2251-178

AGN

3

2977

700416

[150.0]

J. Lee/

H. Marshall

---

Scheduled: Sept. ‘02

 

NGC 7469

AGN

3

3147

(+2956)

700586

[70.0]

[+80.0]

J. Lee/

H. Marshall

---

Scheduled: Oct. ‘02 w/HST

Supplement Kriss GO.

 

1H 0414+009

IGM, AGN

3

2969

700408

[93.0]

T. Fang

---

Scheduled: Aug. ‘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]

 

NGC 2362

 

Stars

3

2525,

2526

200133,

200134

44.5,

43.8

N. Schulz,

P. Wojdowski,

J. Kastner/RIT

3/28/02,

4/23/02

Analysis continues.[6/02]

Previewed the data.[5/02]

Observed 4/23 [4/02]

 

1ES 1028+511

IGM, AGN

3

2970,

3472

700409

21.8,

69.6

T. Fang

3/27/02,

3/28/02

Both data sets are in-house [4/02]

 

3C 279

 

IGM, AGN, Jet

3

2971

700410

108.2

T. Fang,

H. Marshall

3/21/02

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

3/19/02,

3/23/02

Multi observatory collaboration… 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. ISM study: cold absorption edges[5/02]

 

Cas A

SNR

2

1046

500112

69.9

K. Flanagan,

D.Dewey

5/25/01

Si knot analysis started [3/02].

In CRC Royal society talk 2002.

4U 0142+61

 

iNS

2

1018

400096

25.4

N. Schulz,

A. Juett

5/23/01

Finishing

additional analysis [3/02]

ApJ, 2002, 568, pp. L31, HEAD-2002[4/02]

CSR-02-16[3/02]

Mrk 766

AGN

2

1597

700213

90.5

P. Ogle,

J. Lee

5/7/01

Paper in preparation [4/02]

 

NGC 4696

Gal.

2

1560

600117

85.8

M. Wise

4/18/01

To be analyzed.

 

EXO 0748-676

 

XRB

2

1017

400095

49.0

N. Schulz,

H. Marshall,

M. Jimenez-Garate

4/14/01

Performed spectral fits in time cuts. Analyzed burst spectra;

Created spectral lightcurves[5/02]

First draft of paper complete. HEAD02

SS 433

 

XRB, Jet

2

2

1

1019,

1020,

106

400097,

400098,

400019

23.7,

23.0,

28.9

H. Marshall,

N. Schulz

3/16/01,

11/28/00,

9/23/99

Complete analysis of Cycle 2 data

CSR-02-01,

CSR-01-78

1H 1821+643

 

AGN, IGM

2

1599

700215

101.3

P. Ogle,

T. Fang

2/9/01

 

CSR-02-16.5[4/02],

CSR-01-69

Iota Orionis

Stars

2

599,

2420

200075

37.6,

12.9

N. Schulz,

P. Wojdowski

2/7/01,

2/8/01

Data reviewed[5/02]

 

TY Pyx

(HD77137)

Star

2

601

200076

49.8

D. Huenemoerder

1/3/01

Preliminary analysis done.

(spectrum in CSR-02-02)

N103B

 

SNR

2

1045,

2410,

2416

500111

74.0,

25.7,

17.6

K. Flanagan,

J. Migliazzo,

D. Dewey

1/1/01,

1/3/01,

1/2/01

Fit vpshock w/APED lines… NEI, vshock, and Si 2-D analyses.[4/02]

1-D and 2-D analyses started [3/02]

Poster: HEAD-2002[4/02]

NGC 5506

AGN

2

1598

700214

90.0

P. Ogle,

J. Lee

12/31/00

 

Paper in preparation[4/02]

ZW 3146

Clust.

2

1651

800119

167.8

M. Wise

12/25/00

Include background subtraction. Re-analysis continued w/ ISIS[6/02]; started[5/02]

Cluster paper in draft[5/02]

Cycle 2, above.

 

 

Cycle 1

Object

AO

Obs ID

Seq. No.

Expos.

(ks)

Observer /

Analyst

Start Date

Comments & Analysis

Talks and

Publications

NGC 1068

AGN

1

332

700004

46.3

H. Marshall,

P. Ogle, J. Lee

12/4/00

Examine zeroth-order pileup[5/02]

Paper in submitted[5/02]

4U 1626-67

XRB

1

104

400017

40.0

N. Schulz

9/16/00

 

CSR-01-81

AR Lac

 

 

Star

1

6,7,8,

9,10,11

20000N:

4,5,6,7,8,9

32.5,7.5,

7.5,32.6,

7.3,7.3

D. Huenemoerder

9/11/00-

9/19/00

Analysis complete.

Co-authors comments added[6,7/02];

CSR-01-112

Abell 1835

Clust.

1

49896

511

800019

9.8

127.0

M. Wise

8/25/00

8/26/00

Include background subtraction. Re-analysis continued w/ ISIS[6/02]; started[5/02]

Cluster paper in draft[5/02]

N132D

 

SNR

1

121,

1828

500008

22.3

77.6

K. Flanagan,

D. Dewey

7/19/00

7/20/00

Fe and O line ratios from many regions/features

CSR-01-10,26,

Y2Chandra01

TW Hydra

Star

1

5

200003

48.3

D. Huenemoerder,

J. Kastner

7/18/00

Analysis complete.

CSR-02-02,

CSR-01-29

NGC 4486, M 87

Gal., AGN, Jet

1

241

600001

38.5

M. Wise

7/17/00

Examination begun.[6/02]

 

GX 301-2

XRB

1

103

400016

40.0

N. Schulz

6/19/00

Re-analysis initiated [3/02]

Draft paper begun [3/02], AAS00

NGC 1399

 

 

Gal.

1

49898,

240,

2389

600214

600000

13.2

44.1

14.8

M. Wise

5/8/01

6/15/00

5/8/01

Examination begun.[6/02]

 

Vela X-1

XRB

1

102

400015

28.4

N. Schulz

4/13/00

 

ApJ, 2002, 564, L21

MCG –6-30-15

(w/Fabian)

AGN

 

 

 

MCG –6-30-15

Cont.

AGN

1

433

700105

128.2

H. Marshall,

J. Lee

4/5/00

360ks XMM analysis in proc.; XSTAR modeling w/Kallman; Fe UTAs (Ming); LLB edges.

Lee et al 2002, CSR-02-15 [3/02], CSR-01-02

NGC 4151

AGN

1

335

700007

48.0

H. Marshall,

P. Ogle

3/5/00

 

CSR-00-87

PSR B0656+ 14

iNS

1

130

500017

38.1

H. Marshall

11/28/99

LETG/HRC

Paper accepted,

CSR-02-12[3/02]

PKS 2149-306

IGM, AGN

1

336,

1481

700008

36.0

54.8

H. Marshall

11/18/99

11/20/99

 

CSR-01-67

Trapezium

 

Stars

1

3,

4

200001

200002

50.1

31.3

N. Schulz,

D. Huenemoerder

10/31/99

11/24/99

Draft paper started.[6/02]

Detailed modeling work continued[5/02]

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.

AAS00

PKS 2155-304

 

AGN, IGM

1

337,

1703,

1705

700009

700261

700263

39.1

26.2

25.8

H. Marshall,

T. Fang, J. Lee

10/20/99

5/31/00

5/31/00

HETG and LETG w/ACIS-S

ApJ Letter in press.[6/02] Paper accepted.[4/02]

Cyg X-1

 

XRB

1

107,

1511

400020

2.5

12.6

N. Schulz,

H. Marshall,

J. Miller

10/19/99

1/12/00

Second paper continuing[5,6/02] Paper in process [3/02]

 

ApJ, 2002, 564, pp. 941 (CSR-01-57), HEAD00

II Peg (HD 224085)

Star

1

1451

200010

43.3

D. Huenemoerder

10/17/99

Analysis complete.

CSR-01-50

Q0836+7104

IGM, AGN

1

1450,

1802

700006

61.0

14.1

H. Marshall

10/17/99

8/25/00

 

CSR-01-67

PKS 0745-191

Clust.

1

510,

1509,

1509

800018

45.3,

40.4,

39.9

M. Wise

10/14/99

4/25/00

3/4/00

Include background subtraction. Re-analysis continued w/ ISIS[6/02]; started[5/02]

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. Fredricks,

D.Dewey

9/28/99

10/8/99

Updated model tables, new ratio contours. Multi-NEI & vnpshock fits. “One-ion” fitting and masses.[6/02] Fluxes and ratios in “arc”.[4/02]

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.