Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Update on ACIS Calibration 1) Update to the ACIS contamination model 2) Temperature-dependent CTI correction for FI and BI CCDs 3) Cross-calibration with G

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Why Update the ACIS Calibration Model ? The growth of the contaminant with time has been diverging from the model Optical depth at 660eV (Vikhlinin SAO)Optical depth at C-K (Marshall MIT)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal E0102 Flux vs. Time with Previous Contaminant Model DePasquale (SAO) Blue (full frame) Red (subarray)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal E0102 Flux vs. Time with New Contaminant Model DePasquale (SAO) Blue (full frame) Red (subarray)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal E0102 OVIII Flux vs. Time with Previous Contaminant Model DePasquale (SAO) Blue (full frame) Red (subarray)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal E0102 Flux vs. Time with New Contaminant Model DePasquale (SAO) Blue (full frame) Red (subarray)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Change in Effective Area DePasquale (SAO)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Comparison to MOS and pn and other instruments O VII black O VIII red Ne IX green Ne X blue DePasquale(SAO) )

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Comparison to MOS and pn and other instruments O VII black O VIII red Ne IX green Ne X blue DePasquale(SAO) )

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Temperature-Dependent CTI Correction many observations were affected by a warm FP temperature before April 2008 FI and BI CCDs have different T dependence of CTI, FI CTI gets worse with increasing T, BI CTI gets slightly better simply scaling the CTI correction with temperature recovers the mean PH well but the FWHM is significantly larger Grant (MIT)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Temperature-Dependent CTI Correction Grant (MIT)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Temperature-Dependent CTI Correction for I3 Posson- Brown (SAO)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Temperature-Dependent CTI Correction for S3 Posson- Brown (SAO)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Temperature-Dependent CTI Correction Posson- Brown (SAO)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Cross-Calibration with G Posson- Brown (SAO) much simpler spectrum than E0102, but extraction region is an issue flux measurements in the keV bandpass should be consistent with the cluster analysis

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal G Spectral Fit Results and 1  CLs InstrumentNH(10 22 cm 2 )IndexFlux( ) (2-8 keV) ergs cm -2 s -1 Red Chi DOF MOS12.90[2.87,2.94]1.80[1.79,1.82]5.46[5.43,5.49] MOS22.91[2.88,2.95]1.85[1.83,1.87]5.28[5.26,5.31] pn2.76[2.74,2.79]1.79[1.78,1.80]5.61[5.59,5.63] ACIS S33.07[3.05,3.09]1.84[1.83,1.85]6.06[6.04,6.08] Suzaku3.20[ ]1.91[ ]6.38[ ] Swift [ ]1.77[ ]5.61[ ] Swift [ ]1.91[ ]5.46[ ] Preliminary results from non-thermal SNR IACHEC working group The 2-8 keV flux should be consistent with what has been found in the cluster analysis, namely ACIS is the highest, MOS1/2 are 5% lower than ACIS and pn is 5% lower than MOS we need to explore why this might be different than the cluster analysis, we should fit MOS, pn, and ACIS with the same NH and power-law index and then compare fluxes Tsujimoto et al.

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Backup Material

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal IACHEC Thermal SNR Working Group XMM-Newton RGS Andy Pollock (ESAC) Chandra HETG Dan Dewey (MIT) XMM-Newton MOS Steve Sembay (Leicester) XMM-Newton pn Frank Haberl, Victoria Grinberg (MPE) Chandra ACIS Joe DePasquale, Paul Plucinsky (SAO) Suzaku XIS Eric Miller (MIT) Swift XRT Andrew Beardmore, Olivier Godet (Leicester) Models Randall Smith (SAO/GSFC) One of the “Standard candle” working groups.: Plucinsky et al., 2008 SPIE, Vol. 7011, arXiv:

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Chandra Images of E0102: S3 Summed Data ~248 ks Three Color Image Red: keV, Green: keV, Blue: keV o Young (~1,000-2,000 yr) SNR in the SMC (D~61 kpc), classified as “O-rich” SNR o Relatively simple morphology, but significant spectral variations DePasquale (SAO) 45 arcseconds 1E

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal XMM-Newton RGS Spectrum of E0102: Spectrum dominated by O & Ne, little or no Fe emission O VIII O VII C VI O VIII Ne IX Ne X Haberl Grinberg (MPE)

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal O VII black O VIII red Ne IX green Ne X blue Comparison of OVII, OVIII, NeIX, & NeX Normalizations: 28 of 32 normalizations agree to within +/- 10% appears to be a 4% difference between RGS1 & RGS2 which is mostly independent of energy uncertainties are the statistical uncertainties and underestimate the true uncertainty MOS QE was adjusted in 2007 with the intent of improving agreement with the RGS ACIS, XIS, & XRT show similar trend with energy max differences are 23% at O VII, 24% at O VIII, 13% at Ne IX, and 19% at Ne X RGS, HETG, ACIS, MOS, XIS0 agree to within +/- 5% at Ne IX and Ne X DePasquale(SAO) )

Chandra X-Ray Observatory CXC Paul Plucinsky EPIC Cal Census of ACIS Modes and CTI Correction ModeCorrections/Calibrations% & number of Observations TE FaintCTI correction for all 10 CCDs46.4% (3205) TE Very Faint CTI correction for all 10 CCDs48.9% (3377) TE Graded Prototype CTI correction for 8 FI CCDs BI CCDs use spatial gain correction 1.4% (94) CC FaintPrototype CTI correction for 10 CCDs2.2% (153) CC Graded ?? Hybrid approach of Vikhlinin graded mode correction and Edgar CC CTI ?? 1.1% (73) Clocking Modes: “Timed Exposure” (TE) and “Continuous Clocking (CC) Telemetry Formats: “Faint” (F) reports 9 PHs in 3X3 event island “Very Faint” (VF) reports 25 PHs in 5X5 event island “Graded” (G) reports a summed PH all modes report frame #, position, grade, & summed PH