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EPIC BGWG

XMM-Newton EPIC B ack G round W orking G roup founded (~1.5 years ago). S teering and supervising committee to provide the user with clear information on the EPIC Background and (SAS)-Tools to treat the EPIC Background correctly for various scenarios (ESAC, Goddard, Leicester, MPE)

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EPIC BGWG

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  1. XMM-Newton EPIC BackGround Working Groupfounded (~1.5 years ago).Steering and supervising committee to provide the user with clear information on the EPIC Background and (SAS)-Tools to treat the EPIC Background correctly for various scenarios (ESAC, Goddard, Leicester, MPE) Regular meetings (4th on 25/10/06) and telecons + presentations etc. Major Releases: BG analysis web page with recommended information, papers, summary tables etc: http://xmm.esac.esa.int/external/xmm_sw_cal/background/index.shtml XMM-ESAS XMM-Newton Extended Source Analysis Software package model the quiescent particle background both spectrally and spatially for the EPIC MOS detectors XMM-Newton blank sky event files used when the user has difficulty in extracting a suitable background region from their observation (clusters, SNRs, filled FOV etc…) Links to sets of filter wheel closed (FWC) EPIC event files (instrumental BG) Other BG analysis scripts/tools EPIC BGWG

  2. Pre-release/under development: SAS tool to perform professional flare screening for EPIC-MOS and EPIC-pn (soon in SASdevel) – Plan to include e.g. pn CCD11 col.63 avoidance… XMM-ESAS for pn Improvements/updates to Blank Sky files Various other BG analysis tools Long-term timeline of instrumental BG + soft proton flare spatial and spectral analysis EPIC BGWG

  3. SS/KK XMM-ESAS Abell 1795 (0.35-1.25 keV) • soft proton flare screening • modeling the quiescent particle background both spectrally and spatially for the EPIC MOS detectors • producing background spectra for user-defined regions of the detectors and background images (FITS standard) • XMM-ESAS is based on the software used for the background modeling described in Snowden, Collier & Kuntz (2004, ApJ, 610, 1182). Proton flare screening • Released early ’06 – User feedback and on-going improvements • Planned extension to EPIC-pn

  4. Superposition of many pointed observations of pipeline product data from 2XMM – flare-cleaned, filtered, source-removed… Background events files and exposure maps - MOS1, MOS2, pn Mode (eFF, FF) Filter (thin, medium, thick) Type (filled, unfilled) Vignetting (with, without [Exp. Maps]) S/W Select BG events from a certain area of the sky Cast event files onto sky Re-project and rebin exposure maps onto sky All to match user’s own data and analysis Available from ESAC BG page Released May ’06 – User feedback – many improvements made Re-released August ’06 (GTI improvements) Plans to increase file sizes, improve BG selection functions (sky position [web-based], count rate, Gal.column etc.) Event ghosting as stand-alone task JAC/AMR Blank Sky Analysis

  5. - Only S-‘Standard’ datasets released so far, i.e. ‘good’ datasets – no anomalous corner (instrumental BG) effects - Plans for XMM-ESAS to access relevant anomalous instrumental FWC event files when/if required

  6. Not all chips are well behaved… (See also MSt’spresentation) Detector Phenomenology (KK) ? ? ? ? ?

  7. -Not all chips are well behaved… MOS1-4, MOS1-5, MOS2-2, MOS2-5 anomalous states occur at different times always characterized by high rates and low hardness Detector Phenomenology

  8. Summary of States S: “standard state” V: “verification” : 1-4, 2-2, 2-5 for Rev<41.5 H: “high”:1-4, 1-5, 2-5, detectable in corner pixels A: “anonymous”: 1-4, not detectable in corner pix. No other chip has yet been detected in A state But since A state can only be detected in FWC data… Need to understand what causes these states Are there detector parameters that can be used to detect these states independently? – Appears not so… Particularly important for the A states! Detector Phenomenology (KK)

  9. Summary of States S: “standard state” V: “verification” : 1-4, 2-2, 2-5 for Rev<41.5 H: “high”:1-4, 1-5, 2-5, detectable in corner pixels A: “anonymous”: 1-4, not detectable in corner pix. No other chip has yet been detected in A state But since A state can only be detected in FWC data… Need to understand what causes these states Are there detector parameters that can be used to detect these states independently? – Appears not so… Particularly important for the A states! Detector Phenomenology (KK)

  10. RGS background count rate - sensitive to both soft protons (few 100s keV) plus higher energy radiation (MeVs),

  11. Summer (Aug 2003) Winter (Dec 2004 – Jan 2005) ‘Acceptable level’ ~ 1 ct/s @ E>10 keV V.Fioretti & L.Foschini

  12. Folded on Orbit Period (48 hours) Summer (Aug 2003) Winter (Dec 2004 – Jan 2005) Evidence for Seasonal Effect! ‘Acceptable level’ ~ 1 ct/s @ E>10 keV V.Fioretti & L.Foschini

  13. Flare-Free Fraction Total Observation Time (max~80 ks) Flare-Free Fraction as a function of orbital position (using ~entire EPIC dataset) GSE-X points towards the sun. GSE-X-GSE-Y plane is the plane of the ecliptic. GSE-Z is towards the north pole. Red indicates higher values. to Sun K.Kuntz The best observations are made: • When the spacecraft is as far from the earth as possible • and at 180 degrees from the sun. • Towards the sun seems to be better than 90 degrees from the sun. • Given the orbit, the best observations will be done in Winter.

  14. EPIC Background Working Group: For updates on: knowledge, understanding, software (ESAS), files (blank sky, closed) etc. … http://xmm.vilspa.esa.es/external/xmm_sw_cal/background/index.shtml

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