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Max-Planck-Institut Für Extraterrestrische The X-ray Universe 2011, Berlin Max-Planck-Institut für extraterrestrische Physik Download this poster here: http://www.xray.mpe.mpg.de/~hbrunner/Berlin2011Poster.pdf eROSITA: all-sky survey data reduction, source characterization, and X-ray catalogue creation Hermann Brunner1, Thomas Boller1, Marcella Brusa1, Fabrizia Guglielmetti1, Georg Lamer2, Jan Robrade3, Christian Schmid4, Nico Cappelluti5, Francesco Pace6, Mauro Roncarelli7 1Max-Planck-Institut für extraterrestrische Physik, Garching, 2Leibniz-Institut für Astrophysik, Potsdam, 3Hamburger Sternwarte, 4Dr. Karl Remeis-Sternwarte und ECAP, 5INAF-Osservatorio Astronomico di Bologna, 6Zentrum für Astronomie der Universität Heidelberg, 7Dipartimento di Astronomico, Università di Bologna eROSITA on SRG All-sky survey sensitivity eROSITA (extended Roentgen Survey with an Imaging Telescope Array) is the primary instrument on the Russian Spektrum-Roentgen-Gamma (SRG) mission, scheduled for launch in 2013. eROSITA consists of Effective area on axis 15´Background off-axis 30´off-axis seven Wolter-I telescope modules, each of which is equipped with 54 mirror shells with an outer diameter of 36 cm and a fast frame-store pn-CCD, resulting in a field-of-view (1o diameter) averaged PSF of 25´´-30´´ 1 keV HEW (on-axis: 15´´ HEW) and an effective area of 1500 cm2 at 1.5 keV. eROSITA/SRG will perform a four year long all-sky survey, to be followed be several years of pointed observations (Predehl et al. 2010). More info on eROSITA: http://www.mpe.mpg.de/erosita/ 4 keV eROSITA orbit and scanning strategy 7 keV Orbit: eROSITA/SRG will be placed in an Averaged all-sky survey PSF (examples) L2 orbit with a semi-major axis of about 1 million km and an orbital period of about 6 months. sun pointing sun pointing Survey scanning law: during the four year all-sky survey, the eROSITA tele- w w 1 keV Ray-tracing PSF scopes will scan the sky in great circles with one full circle being completed every four hours. The scan axis is either offset pointing offset pointing pointed directly towards the sun or 4 keV alternatively up to several degrees away from it. As the satellite moves around w w the Sun, the plane of the scan is ad- 7 keV vanced by about 1o per day, resulting in 0´ 15´ 30´ a full coverage of the sky every half year. offset pointing offset pointing Exposure time [s] scan axis pointed at sun t Point source detection sensitivity All-sky survey exposure: After four years (eight full scans of the offset-angles 0.2o 0.7o 1.2o 1.7o t sky), a minimum exposure of 1.3 ks (at the ecliptic equator) and a offset-angles 1.0o 2.8o 4.8o 7.0o t mean exposure of 2.0 ks is achieved (assuming 80% observing Comparison XMM-Newton - eROSITA efficiency) . The exposure close to the ecliptic poles can be opti- The scan axis will be pointed at each offset-angle for one full year, causing the scan poles to rotate Field-of-view averaged effective area at 1.5 keV is ~1500 cm2 for XMM-Newton and eROSITA. mized by appropriately choosing the offset-angles of the scan around the ecliptic poles at these offsets. Field-of-view of eROSITA is four times XMM-Newton. a Grasp is four times XMM-Newton. axis from the sun direction (details tbd). Examples: 100 deg2 On-axis PSF has 15´´ HEW for XMM-Newton and eROSITA. But field-averaged eROSITA PSF around each pole, covered with an exposure of at least 15 ks (red (25´´-30´´ HEW) is twice XMM-Newton. symbols on the right ), or alternatively 250 deg2 with an exposure To achieve same soft band sensitivity, 10 ks of XMM-Newton above 10 ks (blue symbols). exposure time corresponds to about 15 ks of eROSITA time. Data reduction and catalogue creation Simulating the eROSITA sky eROSITA data analysis pipeline Software derived from ROSAT, 3.6o x 3.6o eROSITA max. survey exposure: 20 ks (80% observing efficiency) Ingres Abrixas, XMM-Newton + newly developed code all-sky survey field Compiler: F90/GFortran (for compatibility with exiting code) CFITSIO for file i/o CALDB calibration interface PIL (FTOOLS) command line interface Same programs for pipeline processing and interactive analysis average survey exposure: 2 ks (80% observing efficiency) 15 FTE forseen for software development - 50% done X-ray flux light-cones from hydrodynamical Sky is devided into 5839 equal area fields of ~3ox3o N-body simulations Roncarelli et al. 2006 source content of four year After event-calibration, incoming data stream is split sky map Pace et al. 2008 and accumulated in same number of overlapping all-sky survey: ~3 Mill. AGN 3.6ox3.6o all-sky survey maps, centred on these fields. 50-100 thousand 30-100 z>6 AGN Source detection and further souce-level analysis is clusters, hundreds with z>1 performed on these maps. overlap unique area area (sky map 60) Source detection and characterization K. Dennerl + point sources from Survey II Concept extragal. logN–logS Performed simultaneously in five energy bands (baseline: E -0.5, 0.5-1, 1-2, 2-4, 4-8 keV - details tbd) min box detection with Several different detection algorithms – ongoing local background simulations to determine specific setup of detection pipeline (see example on the right) Bayesian backgr.- spline fit of Wavelet Cappelluti et al. 2009 source separation source free area detection ? ? simulated images + particle + instrumental Guglielmetti et al. 2009 box detection with + soft X-ray background References: + separate poster spline background detection folded with eROSITA PSF N. Cappelluti et al., 2009, A&A, 497, 635 pipeline F. Guglielmetti et al., 2009, MNRAS, 396, 165-190 Max. Likelihood PSF & extent fits F. Pace et al., 2008, A&A, 483, 389 ? ? P. Predehl et al., 2010, SPIE, 7732, 77320U simulation input catalogues ? catalogue of (clusters, AGN) detected sources validation, source matching, catalogue insertion M. Roncarelli et al., 2006, MNRAS, 348. 1078 For further information, please contact: [email protected].
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