Major Releases: BG analysis web page with recommended information, papers, summary tables etc:

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1 BGWG -Newton BackGround Working Group founded (~1.5 years ago). Steering and supervising committee to provide the user with clear information on the Background and (SAS)-Tools to treat the Background correctly for various scenarios (ESAC, Goddard, Leicester, MPE) Regular meetings (4 th on 25/10/06) and telecons + presentations etc. Major Releases: BG analysis web page with recommended information, papers, summary tables etc: -ESAS -Newton Extended Source Analysis Software package model the quiescent particle background both spectrally and spatially for the detectors -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) event files (instrumental BG) Other BG analysis scripts/tools

2 BGWG Pre-release/under development: SAS tool to perform professional flare screening for - and -pn (soon in SASdevel) Plan to include e.g. pn CCD11 col.63 avoidance -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

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

4 Blank Sky Analysis Superposition of many pointed observations of pipeline product data from 2 flare-cleaned, filtered, sourceremoved Background events files and exposure maps - 1, 2, 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

5 Blank Sky Analysis Instrument Mode Filter 1 FF Thick 1 FF Medium 1 FF Thin 2 FF Thick 2 FF Medium 2 FF Thin PN FF Thick PN FF Medium PN FF Thin PN FFext Thick PN FFext Medium PN FFext Thin NOBS Exp.time (s) e e e e e e e e e e e5

6 Blank Sky Analysis Galactic centre Galactic anticentre North Galactic pole South Galactic pole

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

13 Detector Phenomenology (KK) ❿Not all chips are well behaved (See also MSt s presentation)?????

14 Detector Phenomenology -Not all chips are well behaved 1-4, 1-5, 2-2, 2-5 anomalous states occur at different times always characterized by high rates and low hardness

15 Detector Phenomenology (KK) 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!

16 Detector Phenomenology (KK) 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!

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

18 Summer (Aug 2003) Winter (Dec 2004 Jan 2005) Acceptable level ~ 1 E>10 kev V.Fioretti & L.Foschini

19 Folded on Orbit Period (48 hours) Summer (Aug 2003) Winter (Dec 2004 Jan 2005) Evidence for Seasonal Effect! Acceptable level ~ 1 E>10 kev V.Fioretti & L.Foschini

20 Flare-Free Fraction as a function of orbital position (using ~entire 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. Flare-Free Fraction Total Observation Time (max~80 ks) 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 CAL/OPS the sun. Meeting Given the orbit, the best observations will be done Mallorca, in Winter. Spain 26-27/10/06

21 Background Working Group: For updates on: knowledge, understanding, software (ESAS), files (blank sky, closed) etc.

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23 L.Foschini