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Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 20071
1.1. ACIS Calibration: Recent Updates, ACIS Calibration: Recent Updates, Planned Updates, & Future IssuesPlanned Updates, & Future Issues
2.2. E0102: Joint Fits with ACIS S3, E0102: Joint Fits with ACIS S3, MOS1/2 & pnMOS1/2 & pn
Paul Plucinsky, Joseph DePasquale, & Paul Plucinsky, Joseph DePasquale, & Steve SnowdenSteve Snowden
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 20072
1. Recent Updates to the ACIS Calibration 1. Recent Updates to the ACIS Calibration
• BI CCD CTI correction for -120 C (S3 & S1), 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 keV• 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
CALDB 3.3.0 released on 15 December 2006
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 20073
Planned Update: CTI Correction for Graded Mode for FI CCDsPlanned Update: CTI Correction for Graded Mode for FI CCDs • Faint mode CTI correction adjusts the PH of each pixel in the 3x3 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 S2Bottom 256 rows Top 256 rows
Vikhlinin (SAO)
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 20074
Map of Good and Bad Grades Map of Good and Bad Grades
Vikhlinin (SAO)
33 of 256 flightgrades are included in the ASCAG02346 grades
Create average images for each of these 33 grades for multiple energies
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 20075
Comparison of Graded Mode and Faint Mode CTI CorrectionComparison of Graded Mode and Faint Mode CTI Correction
Posson-Brown
(SAO)
Graded modeCTI correctionprovides mostof the benefitof the Faintmode correction
For FI CCDs only !
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 20076
Continuous Clocking Mode Calibration Continuous Clocking Mode Calibration
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
External Calibration Source: No CTI correction applied
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 20077
Update on Contaminant BuildupUpdate on Contaminant Buildup
Data:Grant (MIT)
Model:O’Dell &Tennant(MSFC)
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 20078
Optical Depth ComparisonOptical Depth Comparison
C-K Marshall (MIT)inferred optical depth at 700 eV
ECS Grant (MIT)Mn L
E0102 DePasquale (SAO) OVIII Ly-a
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 20079
Future Issues: Focal Plane Operating TemperatureFuture 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
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 200710
2. E0102: Gratuitous Pretty Pictures of E0102 2. E0102: Gratuitous Pretty Pictures of E0102
S3 Summed Data ~100 ksS3 Summed Data ~100 ks RGS Spectrum (Pollock 2006)RGS Spectrum (Pollock 2006)
Objective:Objective: develop a spectral model which can be used by RGS, HETG, EPIC & ACIS, etc.
Chandra X-Ray Observatory CXC
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Application of RGS Spectral ModelApplication of RGS Spectral Model Dewey (MIT)
Use RGS spectral model
Construct a spatial model
Compare simulation to data
Bright lines agree well
Chandra X-Ray Observatory CXC
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MEG minus 1st order
Simulation
Comparison
KS test
OVIII OVIINeIXNeXMgXI
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 200713
MEG plus1st order
Simulation
Comparison
KS test
MgXI NeX NeIX OVIII OVII
Chandra X-Ray Observatory CXC
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Joint Fit with Pollock Model to ACIS S3, MOS1/2 & pnJoint Fit with Pollock Model to ACIS S3, MOS1/2 & pn
SAS 7.0, latest CCFMany thanksSteve !!No fit, adopt Pollock RGS modelBrems kT = 0.36 keVCCD spectra prefera harder continuumNH=5.36e20Line Es and widths frozen,Norms free
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 200715
Joint Fit with Pollock Model to ACIS S3, MOS1/2 & pnJoint Fit with Pollock Model to ACIS S3, MOS1/2 & pn
Fit, Brems kT =0.60 keVNH=5.36e20Line Es & widths frozen, norms free
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 200716
Individual Fit with Pollock Model to ACIS S3Individual Fit with Pollock Model to ACIS S3
Fit, Brems kT =0.60 keVNH=5.36e20Line Es & widths frozen, norms free
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 200717
Individual Fit with Pollock Model to MOS1Individual Fit with Pollock Model to MOS1
Fit, Brems kT =0.60 keVNH=5.36e20Line Es & widths frozen, norms free
Chandra X-Ray Observatory CXC
Paul Plucinsky EPIC Cal April 200718
Individual Fit with Pollock Model to MOS1: Ne lines freeIndividual Fit with Pollock Model to MOS1: Ne lines free
Fit, Brems kT =0.65 keVNH=5.36e20Ne Line Es free, widths frozen, norms free
Chandra X-Ray Observatory CXC
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Individual Fit with Pollock Model to pnIndividual Fit with Pollock Model to pn
Fit, Brems kT =0.40 keVNH=5.36e20Line Es frozen, widths frozen, norms free
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Let’s Agree on a Model !!!!!!!Let’s Agree on a Model !!!!!!!Purpose: to improve the low-energy response model of ACIS, MOS and pn CCD instruments
1) RGS and HETG agree on flux of bright lines2) RGS and HETG compromise on existence of weak lines3) RGS and HETG agree on widths for the lines4) Select a continuum model and absorption5) HETG team must analyze second epoch observations of E01026) Fit ACIS, MOS, and pn with the same model