Contamination WG Summary
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1 Contamination WG Summary Eric D. Miller (MIT)
2 Membership Eric Miller (chair, Suzaku, Hitomi) Andy Beardmore (Swift) Akos Bogdan (Chandra) Dave Burrows (Swift) Vadim Burwitz (erosita) Sunil Chandra (Astrosat) Larry David (Chandra) Tadayasu Dotani (Hitomi) Megan Eckart (Hitomi SXS) Michael Freyberg (erosita) Terry Gaetz (Chandra) Catherine Grant (Chandra) Kenji Hamaguchi (Suzaku) Beverly LaMarr (Suzaku, NICER) Maurice Leutenegger (Hitomi SXS) Herman Marshall (Chandra) Kallol Mukerjee (Astrosat) Koji Mori (Suzaku, Hitomi) Steve O'Dell (Chandra) Paul Plucinsky (Chandra) Steve Sembay (XMM-Newton EPIC) Doug Swartz (Chandra) Masahiro Tsujimoto (Suzaku, Hitomi) Cor de Vries (XMM-Newton RGS)
3 Objectives comparison among instruments and missions chemical composition time dependence spatial dependence (micron to cm scales) environmental dependence (orbit) mitigation for current instruments celestial monitoring targets effects on calibration and science results "bake-out" procedures temperature dependence (where is the coldest surface?) mitigation for future instruments design (cold traps, contamination blocking filters) procurement ground procedures ground testing and calibration on-orbit monitoring
4 Contamination WG Plan (2016) legacy/heritage WG white paper lessons learned for design and ground mitigation lessons learned for first light targets, zerocontamination baseline targets and observing strategies to detect and monitor contamination Suzaku vs. Chandra vs. XMM comparison paper Eric & Herman will start this at MIT (A/I Eric due 2016 August 30) 12th IACHEC will be a working session
5 Contamination WG Agenda A. Bogdan "Characterizing the contaminant on Chandra ACIS using Abell 1795 observations H. Marshall "The New Chandra ACIS Contamination Model" K. Mori and E. Miller "Discussion of Hitomi SXI Contamination Measurements S. Sembay, XMM EPIC-MOS Contamination Update
6 Chandra/ACIS with A1795 (Akos) The time evolution of the contaminant can be described with two exponential models The spatial structure is exponential, possibly another contaminant layer that is less sensitive to temperature differences between the center and edge of the detector 2 Apr 2016 Apr 2015 Apr 2014 Τ (E=0.66 kev) Row number
7 Chandra/ACIS Physical Model (Herman) aromatic compound C-K resonance feature v9968 released in caldb as version N0010 Tested against 1E0102, clusters, grating data, SN1987a (Dave) C-K Resonance Feature Typical C-K edges Herman Marshall 22/25 Contamination Model 3/29/17 Herman Marshall 23/25 Contamination Model 3/29/17
8 Hitomi/SXI Contamination Limits (Eric) RXJ1856: 2 observations, 1 week apart Nc cm -2 in both epochs upper limit consistent with t = 0 contamination of Suzaku SXI RXJ 1856 w/ C contamination normalized counts s 1 kev normalized counts s 1 kev Energy (kev) 1 milleric 21 Dec :31
9 XMM-Newton (Steve) NB: No contamination on EPIC-pn, which has a cold trap.
10 Contamination WG Plan (2017) instrument-specific refereed papers (e..g JATIS) Chandra/ACIS monitoring, modeling (Herman et al.) currently: a few SPIE papers Suzaku/XIS observational paper (Eric, XIS team) currently: Koyama+2007, Tech. Description, web pages XMM EPIC-MOS? RGS? currently: CCF documentation first step toward legacy white paper via Optics WG
11 Objectives Contamination WG Optics WG { comparison among instruments and missions chemical composition time dependence spatial dependence (micron to cm scales) environmental dependence (orbit) mitigation for current instruments celestial monitoring targets effects on calibration and science results "bake-out" procedures { procurement ground procedures ground testing and calibration on-orbit monitoring temperature dependence (where is the coldest surface?) mitigation for future instruments design (cold traps, contamination blocking filters)
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