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EPIC Background Working Group

This summary covers the progress and updates of the XMM-ESAS Background Working Group meeting. It includes discussions on background conditions, image processing, file issues, and ongoing research projects. Relevant topics such as soft proton flaring and quiescent particle background modeling are also covered.

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EPIC Background Working Group

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  1. EPIC Background Working Group Summary: Meeting 11/04/07

  2. BG web pages accessible from main XMM web page

  3. XMM-ESAS : Example (SS/KK) • XMM-ESAS processing of the two observations of Abell 1835 yield the same results. • Temperature radial profiles for A1835 from two separate observations. • Two observations have very different background conditions – one is very low BG – one is very soft proton flare dominated

  4. XMM-ESAS : Background Subtracted andExposure Corrected Images • 2.0-8.0 keV • 0.35-1.25 keV Background subtracted and exposure corrected images of Abell 1795

  5. XMM-ESAS - Mosaicked Images Mosaic of M101 observations.

  6. Blank Sky Analysis JAC/AMR Current status, April 2007 • Files+software being used, comments + suggestions/questions coming in • Paper published: A&A, 464, 1155, 2007 • File issues from several users – dealt with individually – new products released/to be released • RA/Dec Selector tool - trial in java • Event Ghosting tool – available on web already: • http://www.star.le.ac.uk/~jac48/tools/

  7. Papers accepted, submitted, in preparation... A&A, 464, 1155, 2007 A&A, submitted

  8. New MOS FWC files (each ~65MB) created from all of the FWC data for which: • All chips were on in full imaging mode • All chips were in their "normal" state

  9. Can create images, spectra and time-series using XMM-SAS All-CCD pn multi-exposure-stacked FWC data (all modes) are also available

  10. Compares the flux in and out of the FOV for any EPIC event file to estimate the amount of residual Soft Proton flare contamination…

  11. Script to perform image creation + cleaning + exposure correcting + smoothing + … SN2004dj in NGC 2403 (M. Ehle, R. Willatt, W. Pietsch, M. Bauer) • Runs cifbuild, odfingest, epchain, emchain, (omichain) • Performs gti file preparation, gti cleaning, cleans bad pixels and columns, subtracts ooT events (pn) • Makes images, exposure maps, masks, smoothes images, makes combined exposure map and mask • Weighs pn against MOS cameras in each band • Use images, exposure maps, masks and weights to combine images from all cameras

  12. WR25 Carina Nebula

  13. M 83

  14. Soft Proton Flaring (KK/SS) (JAC/AMR looking at pn equivalent) Soft proton flaring is very dependent on the geometry of the observation. Plotted here is the good-time fraction as a function of time of year and position of XMM in its orbit. Plotted here is the good-time fraction as a function of position of XMM in its orbit. The black lines show the position of the magnetosheath. Large values of GSE-X occur during summer.

  15. BG pages accessible from main XMM front page • Talks from all meetings available at EPIC-cal site…

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

  17. Step 1 – Filter the Data and Extract Spectra • Comparing the de Luca and Molendi ratio criteria (8-12 keV band) and the fitted flux for screened observations does aid in the identification of observations affected by residual contamination.

  18. Step 2 – Model the Quiescent Particle Background • Temporal variation of the 0.3-10.0 keV count rate from the CCD corners

  19. Step 2 – Model the Quiescent Particle Background • Temporal variation of the (2.5-5.0)/(0.4-0.8) keV ratio from the CCD corners

  20. MOS1-4 Anonymous State • Images from MOS1-4 in 0.3-1.0 keV an the anonymous anomalous state. Values are the counts ks-1 for one ninth of the CCD • Monthly FWC exposures of 10ks would produce 20 counts for each CCD ninth, enough for some tracking of the state and sufficient to produce 2160 counts/chip/year (enough for spectral analysis) in the standard state

  21. OMC2

  22. 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.

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