Effective Areas. Herman L. Marshall Nov. 17, 2014
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1 Effective Areas Herman L. Marshall Nov. 17,
2 Effective Area Overview Geometric Area (entrance annuli - strut area = Ag) Two mirror bounces (RIr 2 ) Grating Dispersion Efficiency (TTG) ACIS/HRC Optical Blocking Filter (TAl * Tlexan) ACIS detector quantum efficiency (TcontamQACIS) Absorption by SiO2 dead layer, gate structure (FI) Interaction probability in 1 micron thick Si HRC detector quantum efficiency (QHRC) Result: Aeff = Ag RIr 2 [TTG ]TAl Tlexan [QACIS ][QHRC] Also: HRMA overlayer, PSF, OSIP, chip gaps, bad pixels HLM EA & Contamination 2 /29 Chandra ciao/cal Workshop
3 Mirror Reflectivity (CXRO) HLM EA & Contamination 3 /29 Chandra ciao/cal Workshop
4 Mirror Reflectivity (CXRO) HLM EA & Contamination 3 /29 Chandra ciao/cal Workshop
5 HRMA Calibration Measured at MSFC Calibrated SSD and Prop. counters used Emission line source with various materials Empirical correction needed, still not understood See POG for details HLM EA & Contamination 4 /29 Chandra ciao/cal Workshop
6 ACIS EA (with contamination) HLM EA & Contamination 5 /29 Chandra ciao/cal Workshop
7 ACIS EA (with contamination) C-K O-K F-K Si-K Ir-M Al-K HLM EA & Contamination 5 /29 Chandra ciao/cal Workshop
8 HETG Schematic Two types of gratings on HETGS Au bars stand on plating base, on polyimide HLM EA & Contamination 6 /29 Chandra ciao/cal Workshop
9 HETGS Effective Area HLM EA & Contamination 7 /29 Chandra ciao/cal Workshop
10 HETGS Effective Area O-K F-K Chip Gap Ir-M Si-K Au-M HLM EA & Contamination 7 /29 Chandra ciao/cal Workshop
11 Internal Cross-cal of HETGS HLM EA & Contamination 8 /29 Chandra ciao/cal Workshop
12 HRC Effective Area HLM EA & Contamination 9 /29 Chandra ciao/cal Workshop
13 HRC Effective Area N-K O-K I-L C-K Cs-L I-L Ir-M Al-K Cs-L HLM EA & Contamination 9 /29 Chandra ciao/cal Workshop
14 Cross-Cal with XMM HLM EA & Contamination 10/29 Chandra ciao/cal Workshop
15 IACHEC: International Astronomical Consortium for High Energy Calibration Defining High Energy Calibration Standards and Procedures HLM EA & Contamination 11/29 Chandra ciao/cal Workshop
16 IACHEC Annual international meetings Started by 2 largest X-ray groups (Chandra & XMM) First meeting in Iceland in 2006 Support comes from projects (XMM, Suzaku, etc.) Next meeting: Beijing, PRC Meetings involve reports and working groups All major X- & gamma-ray missions represented attendees/meeting, 70% give talks 9 papers published ( ), several in progress URL: with Wiki HLM EA & Contamination 12/29 Chandra ciao/cal Workshop
17 What IACHEC Does Reviews ground calibration plans for new missions Previous meetings: NuSTAR, Swift, This year: Astro-H, erosita Reviews flight calibration plans and results Investigate optics and detector physics Examine methods, systematic errors Define new calibration standards Characterize sources physically Compare & publish results from different missions Arrange coordinated observations Consider infrastructure: statistics, archives HLM EA & Contamination 13/29 Chandra ciao/cal Workshop
18 Cross-Cal with 1E0102 HLM EA & Contamination 14/29 Chandra ciao/cal Workshop
19 Contamination Herman L. Marshall Nov. 17,
20 Contamination Overview 1999: Chandra Launch! 2000: Anomalous C-K edge LETG only?! 2001: Contaminant thickens! 2002: Composition determined (COF), edge NEXAFS indicates C-C single bonding! 2003: Spatial variation found: thin at FoV center! 2004: Fluffium invented as LETG/ACIS and cal source disagree; new model released! 2010: Deposition accelerates, Gaussium replaces fluffium HLM EA & Contamination 16/29 Chandra ciao/cal Workshop
21 The Anomalous C-K Edge 3/00 HLM EA & Contamination 17/29 Chandra ciao/cal Workshop
22 ACIS External Cal Source 700eV / 5.9keV HLM EA & Contamination 18/29 Chandra ciao/cal Workshop
23 The Model NC/NO = 12 NC/NF = 14 HLM EA & Contamination 19/29 Chandra ciao/cal Workshop
24 The Model NC/NO = 12 NC/NF = 14 HLM EA & Contamination 19/29 Chandra ciao/cal Workshop
25 HLM EA & Contamination 20/29 Chandra ciao/cal Workshop
26 As it is now m = +1 HLM EA & Contamination 21/29 Chandra ciao/cal Workshop
27 As it is now m = +1-1 HLM EA & Contamination 21/29 Chandra ciao/cal Workshop
28 Cluster Measurements HLM EA & Contamination 22/29 Chandra ciao/cal Workshop
29 Spatial Variation Bottom half Top half Optical Depth at 700 ev Row HLM EA & Contamination 23/29 Chandra ciao/cal Workshop
30 Composition Changes HLM EA & Contamination 24/29 Chandra ciao/cal Workshop
31 Constant Fluorine/Carbon HLM EA & Contamination 25/29 Chandra ciao/cal Workshop
32 ACIS Fits to 1E0102 O VII O VIII Ne IX Ne X HLM EA & Contamination 26/29 Chandra ciao/cal Workshop
33 ACIS Fits to 1E0102 O VII O VIII Ne IX Ne X HLM EA & Contamination 26/29 Chandra ciao/cal Workshop
34 1E0102 Line Fluxes HLM EA & Contamination 27/29 Chandra ciao/cal Workshop
35 1E0102 Line Fluxes HLM EA & Contamination 27/29 Chandra ciao/cal Workshop
36 Possible Edge Residuals Overcorrected Edges HLM EA & Contamination 28/29 Chandra ciao/cal Workshop
37 Contamination Summary It is mostly made of C, smattering of F & O Origin is unknown, composition doesn t match any on-board substance About the same on ACIS-I and ACIS-S Thicker at detector edges Optical depth at 700 ev is now about 1.5 and climbing Effect at 1 kev is noticeable Time dependence is not predictable Model is not completely physical Uncertainties in exact shape of correction remain HLM EA & Contamination 29/29 Chandra ciao/cal Workshop
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