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Erosita Extended Roentgen Survey with an Imaging Telescope Array eROSITA extended ROentgen Survey with an Imaging Telescope Array Vadim Burwitz for the eROSITA Team: PI: Peter Predehl Co-Is: Hans Böhringer, Ulrich Briel, Hermann Brunner, Evgeniy Churazov, Michael Freyberg, Peter Friedrich, Günther Hasinger, Eckhard Kendziorra, Dieter Lutz, Norbert Meidinger, Mikhail Pavlinsky, Andrea Santangelo, Jürgen Schmitt, Axel Schwope, Matthias Steinmetz, Lothar Strüder, Rashid Sunyaev, Jörn Wilms System Engineer: Josef Eder Product Assurance: H. Bräuninger, M. Hengmith Electronics Engineering: W. Bornemann, O. Hälker, S. Hermann, W. Kink, S. Müller, O. Hans Mechanical Engineering: H. Huber, Chr. Rohé, L. Tiedemann, R. Schreib, B. Mican, K. Lehmann, H. Eibl, F. Huber, R. Sandmair, P. Straube, H. Kestler, F. Soller, J. Liebhart Mirror System, PANTER: P. Friedrich, W. Burkert, M. Freyberg, B. Budau, E. Pfeffermann, V. Burwitz + students CliThlEiiCooling, Thermal Engineering: MFüM. Fürmetz + stu dents CCD-Camera: N. Meidinger, R. Hartmann, G. Schächner, J. Elbs, S. Ebermayer Attitude: A. Schwope Calibration, Analysis: G. Hartner, U. Briel, K. Dennerl, R. Andritschke, Chr. Tenzer Laboratory, PUMA, Tests: M. Vongehr, R. Gaida, K. Dittrich, F. Schrey Ground Software, Simulation: H. Brunner,,pp, N. Cappelluti, G. Lamer, M. Mühlegg gg,,yer, J. Wilms, I. Kreykenbohm , Chr. Schmid Mission Planning: J. Schmitt, J. Robrade Institutes: Industry: Max-Planck-Institut für extraterrestrische Physik, Garching/D Media Lario/I Mirrors, Mandrels Space Research Institute IKI, Moscow/Ru Kayser-Threde/D Mirror Mechanics Univ. Tübingen/D Carl Zeiss/D Mirror Mandrels Univ. Hamburg/D Invent/D Telescope Structure Univ. Erlangen-Nürnberg/D pnSensor/D CCDs Astroppyhysikalisches Institut Potsdam/D EHP/B Cooling Max-Planck-Institut für Astrophysik/D RUAG/A Mechanisms, MLI ... Historical Development ROSAT 1990-1998 Spectrum-XG First X-ray all-sky survey Jet-X, SODART, etc. with an imaging telescope ABRIXAS Negotiations between Roskosmos and ESA Bundle of 7 small telescopes on a "new" Spectrum-XG mission (2005) To extend the all-sky survey towards higggher energies MoU between Roskosmos and DLR (2007) 1999 Spektr-RG Launch: 2012 ABRIXAS science on the International Space Station ROSITA eROSITA 2002 DUO 2004 Dark Energy 105 Clusters of Galaxies Design Driving Science ABRIXAS eROSITA • obscured AGN in the local universe (~106 AGN , 10 @ z=9) • 6000 clusters (DUO) ~105 clusters, z<1.5, BAOs • "secondary science" • 7 mirror modules, f = 1600mm • Ø = 17cm, 27 shells Ø = 36cm, 54 shells eff. area ~ 80cm2 eff. area ~ 350 cm2 • 30 arcsec HEW 15 arcsec HEW • pnCCD, 2cm × 2cm, 41 arcmin 3cm × 3cm, 61 arcmin DesigneeROSITAROS Driving ITA SeSensitivityn Science sitivity Grasp F/ 4yr eROSITA poles Expectation: 100.000 clusters (DE!) ~100 clusters @ z>1.5 7 telescopes, 350 cm2 each 3 Million AGN [450,120, 36, 10] @ z > lfildfi(61ilarge field of view (61 arcmin Ø) [ 6, 7, 8, 9] ~ 2 × XMM-Newton (MOS+PN) eROSITA Instrument • sunshield • 7 mirror modules + baffles • 2 (redundant) startrackers • CFRP-telescope structure • hexapod mounting for stability • radiator for cooling cameras • 7 pn-CCD cameras • passive cooling system compr. loop-heatpipes, latent cold storage • S/C truss Programmatic Status • June 2006 Proposal to DLR • Mar. 2007 MoU between Roskosmos & DLR • April 2007 eROSITA approved and funded by DLR • Summer 2008: Nothing but problems... Mirrors, Payload, Costs • September 2008 Roskosmos decision on payload, orbit & launch ART-XC, L2-orbit, 2012 with Soyuz-Fregat from Baikonur • May 2009 Mirror-FM contract Media Lario Technologies, (Kayser-Threde, Zeiss) • June 2009 Additional Funding by MPG • July 2009 Additional Funding by DLR • August 2009 Contract between Roskosmos and DLR • Now FlliFully in Ph ase C CD, D Flight hardware beeing Manufactured and tested Detailed Agreement eROSITA on MAKS Signature of the "Detailed Agreement" (Reichle, Wörner, Perminov) Mr. Putin gets informed abtDkEbout Dark Energy... Mirror-Module Engineering Model Mirror-EM a t MLT Mirror-EM on shaker at MPE Hardware Development Electron Deflector Filter Wheel on shaker at MPE in preparation for qualification tests Telescope Support Structure Test eROSITA wrapped in MLI Mirror Manipulator at MLT Measuring the Mirror Module Laboratories Precision- metltrology PANTER X-ray Test Facility Profile Errors X-ray measurements Raytracing - Analysis Laboratories electron deflector test at PUMA cryogenics X-ray baffle metrology glue shrinkage tests mirror shell screening device Camera + Electronics CCD - Camera pn-CCDs on wafer in test front-end ceramics camera housing 1.4 105 1.2 105 1.0 105 8.0 104 ounts cc 6.0 104 4.0 104 2.0 104 150 200 250 300 350 400 energy [eV] performance (flat field, E-resolution) Mission Scenario Angle between sun and Earth max. 13° Scan-Axis always pointing towards Earth (antenna!) Scanspeed less than in LEO, ~ 4h/revolution eROSITA Exposure 3ksec 5ksec 30ksec After 4 years Point Spread Function (PSF) 80 ideal 70 15'' on- axis 60 50 ds] nn 40 61’ 30 HEW [arcHEW seco 20 10 0 0 5 10 15 20 25 30 35 40 45 from ABRIXAS test off-axis angle [arc minutes] Point Spread Function (PSF) Angular Resolution Error Budget Summary ••OnOn--AxisAxis PSF: 15’’ HEW mirror system • Average PSF over the 61’ FOV: 26’’ HEW 15’’ → de tec tor, st ruct ure, attit ud e • Angular resolution of the survey: 30’’ HEW eROSITA Simulations by Chr. Schmid Pointing Survey Off-axis blurring of a Wolter-I telescope PSF has to be average d over the Fo V 50:50 Data Share between Ru/D CAELUM EROSITAE CUM RETICULO AEQUATORIALI HERCULES URSA DRACO BOOTES URSA MAIOR MINOR LE CEPHEUS VIRGO O CASSIOPEIA CYGNUS AURIGA AQUILA GEMINI PERSEUS ANDROMEDA SCORPIUS PEGASUS SAGITTARIUS CENTAURUS TAURUS ORION VELA CRUX CANIS MAIOR AQUARIUS CARINA HEMISPHAERA ORIENTALIS HEMISPHAERA OCCIDENTALIS INVESTIGATIO RADIORUM CAELIS ROENTGENIENSIS AB ANNO MMXII Actual definition depends on mission planning Data policy & release (PIs very personal view, only D-part) Maximum science return from the mission • Survey: • reprocessing every half year (8 times corr. to 4 years) • proprietary phase 1 year (after calibration etc., as usual) • analysis by "Working Groups" acc. to topics • solar system objects, stars, .... AGN, BKGR • invitation to all scientists to join the groups / institutes • hope, that Russian partners join that scheme • neccessary for topics requiring whole sky • PitiPointing: • AOs every year (as usual) • proprietary phase 1 year (as usual) • no guaranteed time for hardware institutes, but Deep Survey Phase • TOOs, discretionary time, also interruption of survey.
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