Chandra XRay Observatory CXC A Comparison of Spectral

Chandra X-Ray Observatory CXC A Comparison of Spectral Fit Results of E 0102 from the Chandra and XMM CCDs Paul Plucinsky & Joseph De. Pasquale Paul Plucinsky 1 February 2005

Chandra X-Ray Observatory CXC Other Contributors to this Effort CXC: R. Edgar , N. Schulz, A. Vikhilin MIT: K. Flanagan, D. Dewey, lots of help from MIT ACIS team Paul Plucinsky 2 February 2005

Chandra X-Ray Observatory CXC Why Use E 0102 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 Paul Plucinsky 3 February 2005

Chandra X-Ray Observatory CXC 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 ke. V 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 e. V)/O VII Res (574 e. V) to 0. 58 based on HETG and OVII (665 e. V)/ OVIII Ly-alpha (654 e. V) to 0. 1368 (ratios from Flanagan et al. 2004) Paul Plucinsky 4 February 2005

Chandra X-Ray Observatory CXC ACIS-Specific Calibration Issues: • CTI Correction for the FI CCDs • Time-dependent gain correction for both BI and FI CCDs • QE correction for the S 3 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 I 3 and 20 observations on S 3, roughly once every 6 months • Data (spectra, rmfs, & arfs) available at: “http: cxc. harvard. edu/acis/E 0102/splash. html” Available for any one to download, please do if you would like the data !! XMM Data: • Provided by Andy Read (16 MOS 1/MOS 2) and Michael Smith (1 each MOS 1/MOS 2/PN) Paul Plucinsky 5 February 2005

Chandra X-Ray Observatory CXC Gratuitous Pretty Pictures of E 0102 S 3 Summed Data ~100 ks Paul Plucinsky True Color Image 6 February 2005

Chandra X-Ray Observatory CXC S 3(BI) Paul Plucinsky 7 February 2005

Chandra X-Ray Observatory CXC S 3(BI) Ne X Ly-a Mg XI triplet OVIII Ly-a OVII triplet Paul Plucinsky Ne IX triplet 8 February 2005

Chandra X-Ray Observatory CXC I 3(FI) OVIII Ly-a OVII triplet Mg XI Ly-a Ne IX Ne X Ly-a triplet Paul Plucinsky 9 February 2005

Chandra X-Ray Observatory Paul Plucinsky 10 CXC February 2005

Chandra X-Ray Observatory Paul Plucinsky 11 CXC February 2005

Chandra X-Ray Observatory CXC Thick filter Large Window MOS 1 MOS 2 Paul Plucinsky 12 February 2005

Chandra X-Ray Observatory CXC Thick Filter Large Window MOS 1 MOS 2 Paul Plucinsky 13 February 2005

Chandra X-Ray Observatory CXC Thick Filter Small Window PN MOS 1 MOS 2 Paul Plucinsky 14 February 2005

Chandra X-Ray Observatory CXC PN Thick Filter Small Window Paul Plucinsky 15 February 2005

Chandra X-Ray Observatory CXC Comparison of Fitted Results between XMM and Chandra ACIS S 3 ACIS I 3 MOS 1/ MOS 2 PN Flux(0. 4 -2. 5 2. 41 2. 52 2. 10 2. 49 ke. V) (e-11 ergs [2. 40, 2. 42] [2. 51, 2. 54] [2. 09, 2. 11] [2. 48, 2. 50] cm^2 s) OVIII Ly-a (e-3 photons/ cm^2 s) Ne IX triplet (e-3 photons/ cm^2 s) Paul Plucinsky 6. 51 5. 26 5. 02 6. 63 [6. 14, 16. 9] [4. 95, 5. 70] [4. 93, 5. 16] [6. 60, 7. 28] 3. 19 2. 80 2. 93 2. 60 [2. 58, 3. 80] [2. 48, 3. 11] [2. 51, 2. 69] [2. 78, 3. 08] 16 February 2005

Chandra X-Ray Observatory Mkn 421 CXC Obsid 4148: row 178 Obsid 5332: row 512 Schulz (MIT) 12. 35 A (1004 e. V) 15. 54 A ( 798 e. V) 18. 71 A ( 662 e. V) 21. 12 A ( 587 e. V) 23. 48 A ( 528 e. V) 25. 09 A ( 494 e. V) Paul Plucinsky 17 February 2005

Chandra X-Ray Observatory 1004 e. V 662 e. V 587 e. V 494 e. V Paul Plucinsky 18 CXC Schulz (MIT) February 2005

Chandra X-Ray Observatory CXC 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 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 Paul Plucinsky 19 February 2005