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A Comparison of Spectral Fit Results of E0102 from the Chandra and XMM CCDs Paul Plucinsky & PowerPoint Presentation
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A Comparison of Spectral Fit Results of E0102 from the Chandra and XMM CCDs Paul Plucinsky & Joseph DePasquale. Other Contributors to this Effort. CXC: R. Edgar , N. Schulz, A. Vikhilin MIT: K. Flanagan, D. Dewey, lots of help from MIT ACIS team.

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slide1

A Comparison of Spectral Fit Results of E0102 from the Chandra and XMM CCDs

Paul Plucinsky &

Joseph DePasquale

slide2

Other Contributors to this Effort

CXC: R. Edgar , N. Schulz, A. Vikhilin

MIT: K. Flanagan, D. Dewey, lots of help from MIT ACIS team

slide3

Why Use E0102 as a Calibration Source for the CCDs?

  • Well-characterized spectrum, both the Chandra HETG and XMM RGS have observed the object
  • The spectrum is relatively simple by astrophysical standards, no or very little Fe, strong lines of O, Ne, and Mg
  • Extended source so pileup effects are minimized
  • Constant source
  • The O and Ne lines sample an energy range in which the on-board calibration source does not have strong lines
  • Low-energy part of the bandpass is always a challenge to calibrate
slide4

Spectral Model: Calibration vs. Astrophysics

  • Primary Objectives are to measure the gain, the spectral redistribution function, and detection efficiency in the 0.5 -2.0 keV range
  • Our immediate concern is to develop a model useful for calibration, not to develop an astrophysically-meaningful model,
  • We use a model consisting of 24 Gaussians for the lines identified by the HETG and RGS, a bremsstrahlung for the continuum, and a two component absorption (Galactic and SMC)
  • Line energies are fixed at the true values and the widths of the Gaussians are fixed at zero, so the only parameter which varies is the normalization
  • Constrain the ratio of the OVII For (561 eV)/O VII Res (574 eV) to 0.58 based on HETG and OVII (665 eV)/ OVIII Ly-alpha (654 eV) to 0.1368 (ratios from Flanagan et al. 2004)
slide5

ACIS-Specific Calibration Issues:

  • CTI Correction for the FI CCDs
  • Time-dependent gain correction for both BI and FI CCDs
  • QE correction for the S3 CCD (summer 2004)
  • Time-dependent and spatial-dependent correction for the contamination (aka ``The Marshall Layer’’)
  • We used CIAO 3.2 and CALDB 3.0.0 (released Dec 2004)

Chandra Data:

  • 44 observations on I3 and 20 observations on S3, roughly once every 6 months
  • Data (spectra, rmfs, & arfs) available at: “http:cxc.harvard.edu/acis/E0102/splash.html” Available for any one to download, please do if you would like the data !!

XMM Data:

  • Provided by Andy Read (16 MOS1/MOS2) and Michael Smith (1 each MOS1/MOS2/PN)
slide6

Gratuitous Pretty Pictures of E0102

S3 Summed Data ~100 ks

True Color Image

slide8

S3(BI)

Ne X Ly-a

Mg XI triplet

OVIII Ly-a

Ne IX triplet

OVII triplet

slide9

I3(FI)

OVIII Ly-a

OVII triplet

Mg XI Ly-a

Ne IX triplet

Ne X Ly-a

slide12

Thick filter

Large Window

MOS 1

MOS 2

slide13

Thick Filter

Large Window

MOS 1

MOS 2

slide14

Thick Filter

Small Window

PN

MOS 1

MOS 2

slide15

PN

Thick Filter

Small

Window

slide17

Mkn 421

Obsid 4148: row 178

Obsid 5332: row 512

Schulz

(MIT)

12.35 A (1004 eV)

15.54 A ( 798 eV)

18.71 A ( 662 eV)

21.12 A ( 587 eV)

23.48 A ( 528 eV)

25.09 A ( 494 eV)

slide18

Schulz

(MIT)

1004 eV

662 eV

587 eV

494 eV

slide19

Conclusions and Future Work

  • ACIS BI and FI CCD results are more consistent than earlier, but discrepancies still exist
  • ACIS results appear to be more consistent with the PN results
  • We need to fit the rest of the XMM data
  • We need to understand and constrain the relative contribution of the lines and the continuum
  • We need to improve the BI spectral redistribution function
  • We need to understand the apparently “discrepant” data sets for ACIS