Chandra XRay Observatory CXC 1 ACIS Calibration Recent

Chandra X-Ray Observatory CXC 1. ACIS Calibration: Recent Updates, Planned Updates, & Future Issues 2. E 0102: Joint Fits with ACIS S 3, MOS 1/2 & pn Paul Plucinsky, Joseph De. Pasquale, & Steve Snowden Paul Plucinsky 1 EPIC Cal April 2007

Chandra X-Ray Observatory CXC 1. Recent Updates to the ACIS Calibration CALDB 3. 3. 0 released on 15 December 2006 • BI CCD CTI correction for -120 C (S 3 & S 1), need to have CIAO 3. 4 also to apply the correction, BI CTI correction is now part of the standard data processing • Effective area correction around the Si K edge, ~4 % at 1. 8 ke. V • FI CCD ``dead area’’ correction to account for the area lost on average in each frame to cosmic rays, 2. 5 -4. 0% as a function of row Paul Plucinsky 2 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Planned Update: CTI Correction for Graded Mode for FI CCDs • Faint mode CTI correction adjusts the PH of each pixel in the 3 x 3 event island • In Graded mode, only have x, y position of event, grade, and summed PH • Use grade and summed PH to determine the most likely charge distribution based on ``average’’ images • Use this information in an Graded mode CTI correction Mn-K flight grade 8 (left split) for S 2 Bottom 256 rows Top 256 rows Vikhlinin (SAO) Paul Plucinsky 3 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Map of Good and Bad Grades Vikhlinin (SAO) 33 of 256 flight grades are included in the ASCA G 02346 grades Create average images for each of these 33 grades for multiple energies Paul Plucinsky 4 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Comparison of Graded Mode and Faint Mode CTI Correction Posson. Brown (SAO) Graded mode CTI correction provides most of the benefit of the Faint mode correction For FI CCDs only ! Paul Plucinsky 5 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Continuous Clocking Mode Calibration External Calibration Source: No CTI correction applied Edgar (SAO) In CC mode: - row-to-row transfer time is different so the effects of CTI are different -- don’t know the y position of the events, but for some observations you know the y position of the source Paul Plucinsky 6 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Update on Contaminant Buildup Data: Grant (MIT) Model: O’Dell & Tennant (MSFC) Paul Plucinsky 7 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Optical Depth Comparison C-K Marshall (MIT) inferred optical depth at 700 e. V ECS Grant (MIT) Mn L E 0102 De. Pasquale (SAO) OVIII Ly-a Paul Plucinsky 8 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Future Issues: Focal Plane Operating Temperature • current operating temperature is -119. 7 C • as the mission has progressed, the frequency and magnitude of deviations from the desired temperature have increased • it might become necessary to operate at a higher temperature, significant impact for the FI CCDs Paul Plucinsky 9 EPIC Cal April 2007

Chandra X-Ray Observatory CXC 2. E 0102: Gratuitous Pretty Pictures of E 0102 S 3 Summed Data ~100 ks RGS Spectrum (Pollock 2006) Objective: develop a spectral model which can be used by RGS, HETG, EPIC & ACIS, etc. Paul Plucinsky 10 EPIC Cal April 2007

Chandra X-Ray Observatory Application of RGS Spectral Model CXC Dewey (MIT) Use RGS spectral model Construct a spatial model Compare simulation to data Bright lines agree well Paul Plucinsky 11 EPIC Cal April 2007

Chandra X-Ray Observatory CXC MEG minus 1 st order Mg. XI Ne. X Ne. IX OVIII OVII Simulation Comparison KS test Paul Plucinsky 12 EPIC Cal April 2007

Chandra X-Ray Observatory CXC MEG plus 1 st order Mg. XI Ne. X Ne. IX OVIII OVII Simulation Comparison KS test Paul Plucinsky 13 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Joint Fit with Pollock Model to ACIS S 3, MOS 1/2 & pn SAS 7. 0, latest CCF Many thanks Steve !! No fit, adopt Pollock RGS model Brems k. T = 0. 36 ke. V CCD spectra prefer a harder continuum NH=5. 36 e 20 Line Es and widths frozen, Norms free Paul Plucinsky 14 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Joint Fit with Pollock Model to ACIS S 3, MOS 1/2 & pn Fit, Brems k. T =0. 60 ke. V NH=5. 36 e 20 Line Es & widths frozen, norms free Paul Plucinsky 15 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Individual Fit with Pollock Model to ACIS S 3 Fit, Brems k. T =0. 60 ke. V NH=5. 36 e 20 Line Es & widths frozen, norms free Paul Plucinsky 16 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Individual Fit with Pollock Model to MOS 1 Fit, Brems k. T =0. 60 ke. V NH=5. 36 e 20 Line Es & widths frozen, norms free Paul Plucinsky 17 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Individual Fit with Pollock Model to MOS 1: Ne lines free Fit, Brems k. T =0. 65 ke. V NH=5. 36 e 20 Ne Line Es free, widths frozen, norms free Paul Plucinsky 18 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Individual Fit with Pollock Model to pn Fit, Brems k. T =0. 40 ke. V NH=5. 36 e 20 Line Es frozen, widths frozen, norms free Paul Plucinsky 19 EPIC Cal April 2007

Chandra X-Ray Observatory CXC Let’s Agree on a Model !!!!!!! Purpose: to improve the low-energy response model of ACIS, MOS and pn CCD instruments 1) 2) 3) 4) 5) 6) RGS and HETG agree on flux of bright lines RGS and HETG compromise on existence of weak lines RGS and HETG agree on widths for the lines Select a continuum model and absorption HETG team must analyze second epoch observations of E 0102 Fit ACIS, MOS, and pn with the same model Paul Plucinsky 21 EPIC Cal April 2007