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All Sky X-‐Ray Survey PLANCK B&E workshop, SPEKTR - RG Caltech eRosita July 22, 2016 SPEKTR-RENTGEN-GAMMA (eRosita and ART-XC) all sky X-Ray survey ART-XC Rashid Sunyaev Max-Planck Instut fuer Astrophysik Space Research Instute (IKI), Moscow SRG Spektr-Roentgen-Gamma (SRG) eROSITA ART-XC Navigator plaorm Lavochkin industry ROSKOSMOS Fregat-SB Booster Space Research InsMtute (IKI), Moscow 2 SRG September 25, 2017 (TBC) L2 Parking orbit Injection into parking orbit with Zenit LV ΔV2 ΔV1 st Fregat 2nd Fregat 1 burn burn M.N. Pavlinsky SRG Ground control stations 4 SRG Radio-visibility 64 m 70 m M.N. Pavlinsky SRG No. Description Value S/C 1 Launch date 2017 2 Launch site Baikonur “Zenit-2SB” 3 Launch vehicles - “Fregat-SB” 4 Operational orbit L2 point 5 Active lifetime 7,5 years 6 S/C dry mass 2267 kg 7 Payload 1228 kg 8 S/C wet mass 2647 kg Radio line frequency 9 X range Data Transmission 512 Кbit/ 10 Rate sec Payload power 11 680 W consumption M.N. Pavlinsky SRG -Launch: Q4 2017 from Baykonour, Kazakhstan (Zenit+Fregat) - eROSITA delivery to Russia: October 25, 2016 - ART-XC delivery to Lavochkin industry: October 5, 2016 1. Three months – flight to L2, perfomance verificaon and calibraon of payload. 2. 4 years – 8 all sky surveys, (scanning mode: 6 rotations/day). 3. 3 years – follow-up pointed observaMons of a selecMon of the most interesng galaxy clusters, AGNs and other objects discovered by SRG. 7 SRG The S/C rotaon axis is always pointed between the Sun and the Earth to ensure that the Earth is always within the beam paern of the spacecra medium gain antenna. Movement of the S/C around the L2 point combined with the movement of the Earth around the Sun leads to nonuniform sky coverage. Two deep fields in the North and South Eciipc Poles Lavochkin industry, IKI eRosita is an instrument designed to perform all sky 0.5 – 10 KeV surveys: Large Field of View, large effecQve area eROSITA good resoluon 15-25” Focal length - 1.6 m Telescope Front Cover Weight ~ 800 kg 2 Star Sensors 7 X-ray Baffles 7 Mirror Modules 2 Sun Sensors 7 Electron Deflectors 2 Camera Cooling Radiators Hexapod = I/F with S/C 7 Filter-Wheels 7 CCD-Cameras 2 E-Box Cooling Radiators 7 Camera Electronics 2 Control Electronics 7 idenQcal Mirror Modules Field of View 1° Ø 54 nested Mirror Shells each Angular ResoluQon 15 arcsec on-axis 7 idenQcal pnCCD Cameras Energy Range ~0,3 - 10 keV eRosita Mirror System MPE MPE 7+1 Framestore pnCCD Meidinger et al, 9144E..1WM A. Merloni - Ringberg, 4/2016 FM Camera Calibration • Spectral resolution at all measured energies within specification (R~20 @1.5keV) • Extremely good uniformity F F F F • Only weak dependence on CCD and electronics temperature (unlike XMM) M M M M 1 2 3 4 C-K 4 5 5 5 (0.2 9 8 8 8 ΔE=49eV @0.28keV 8ke V) O-K 5 6 6 6 (0.5 6 5 4 4 3keV ) Cu-L 6 7 7 7 (0.9 8 4 0 0 =77eV @1.5keV 3keV ) Al-K 7 8 7 7 (1,49 7 2 7 7 keV) Ti-K 1 1 1 1 (4,51 1 2 1 1 =136eV @6.4keV keV) 7 5 8 8 A. Merloni - Ringberg, 4/2016 Fe-K 1 1 1 1 (6,4 3 4 3 3 keV) 6 5 8 8 Cu-K 1 1 1 1 (8.0 5 6 5 5 keV) 6 7 8 9 Ge-K 1 2 1 1 (9.9 7 0 7 7 keV) 5 4 8 3 Effective Area and Grasp - Effective area at 1keV comparable with XMM/Newton @ 1 keV - Factor ~7-8 larger surveying speed - 4 years dedicated to all sky survey (with estimated 70-80% efficiency) A. Merloni - Ringberg, 4/2016 A fast survey machine 100 kpc [0.5” HEW] [26.5” HEW (FoV avg)] Please verify that (1) all pages are present, (2) all figures are correct, (3) all fonts and special characters are correct, and (4) all text and figures fit within the red margin lines shown on this review document. Complete formatting information is available at http://SPIE.org/manuscripts Return to the Manage Active Submissions page at http://spie.org/submissions/tasks.aspx and approve or disapprove this submission. Your manuscript will not be published without this approval. Please contact [email protected] with any questions or concerns. ART-XC PI: M. Pavlinsky (IKI) - Energy range: 5-30 keV - FOV: 34 - On-axis resolution 1 - Energy resol. 12% at 14keV - Time res. 1ms Figure 2. The ART-XC telescope array with seven mirror modules and seven focal-plane detectors. The basic structure of ART- XC is the optical bench – the conical carbon-fiber tube that is equipped with a moveable cover to protect the optics during launch (not shown).The star tracker with its own radiator is installed on the top of this tube. The detector collimators, cooling radiator with cooling pipes and the electronics boxes are visible at the bottom of the tube. 2.2 Qualification model of ART-XC All subsystems of the QM ART-XC instrument successfully passed the qualification tests at the end of October 2014 at IKI. The qualification period for subsystem turned out to be several months more than scheduled as more time was required for further development of the attachment structure forfo the detector’s beryllium window. The beryllium windows rifted in two detectors during the thermo cycling test, as the temperature of the seven detectors was cycled within the range −35°C to +55° C (Figure 3) a few dozen times. Figure. 3. Left: complex of X-ray detectors in climatic chamber during test. Right: one of the detector’s cover with brroken beryllium window. 9603 - 11 V. 10 (p.3 of 12) / Color: No / Format: A4 / Date: 8/7/2015 5:19:20 PM SPIE USE: ____ DB Check, ____ Prod Check, Notes: eROSITA extragalactic sky Image credits: MPE, eRosita_DE consortium, XMM-XXL Wide-area census of galaxy clusters (105) and active galactic nuclei (106) during 4 years long all sky survey Mapping the structure of the hot Universe: Coma Requirements Virgo Centaurus Hydra Perseus Detect 100.000 Clusters of Galaxies (MPE), O. Hahn (ETH) -14 2 23.0 21.0 19.0 17.0 15.0 13.0 11.0 ü 2 2 All-sky survey sensitivity 6×10 erg/cm /s log(Lx) [erg/cm /s/arcmin ] 2 -14 Mühlegger ü Deep survey field(s) (~100 deg ) to 1×10 Diffuse X-ray emitting gas traces ü Individual pointed observations (LMU), M. the massive knots of ü Moderate angular resolution (<30‘‘ aver. Dolag the cosmic web over FoV) of K. (Clusters) ü Large collecting area (> 2000 cm2 @1keV) Point sources coutesy ü (Quasars) signpost the Large FoV (1° Ø) Images growth of black holes ü Long duration survey: 4 years ß à 1/2 year (ROSAT) Simulation of an eROSITA field Clusters of galaxies in X-rays Evoluon of Cluster Mass Funcon court. Churazov/MPA z = 0 z = 0.5 z = 1.4 Number of most massive clusters is extremely sensive to cosmology Will eROSITA detect all Clusters? Churazov/IKI,MPA: Yes! -110k clusters with >50 net counts (“secure” detections) -23k clusters with accurate redshift determination from X-ray alone -~2k clusters with accurate temperature determination from X-ray spectra Prac5cally all rich clusters of galaxies contain bright gravita5onal arcs (strong lensing), easiest way to look for very high redshiQ objects A lot of beau5ful physics: shock waves, bubbles , filled by cosmic rays, plasma physics in extremely low density and hot plasmas, physics of high Z ions Phoenix Cluster discovered by SPT at z=0.596 and observed by CHANDRA, GALEX and Magellan. Cooling flow, star burst ~ 800 Msun/year. AGN in the center, bright filaments. Compe5on with ground based instruments: South Pole and Atacama Cosmology Telescopes (20 000 sq degrees and hundreds of thousands of clusters and groups of galaxies detected in the microwave spectral band due to the thermal SZ-effect) Bleem et al, 2015 In 2016 SPT plans to start 3G phase of observa5ons with 15 000 cryogenic bolometers in the focal plane: goal: 4000 new discovered clusters on 2500 sq degrees. In 2020 – 150 000 bolometers!!! It will be great to overlap eRosita X-Ray map with 100 000 clusters and groups of galaxies onto high quality y-map (SZ-effect) from the future CMB spacecra_ ~ 10 thousand star forming galaxies ~ 10 thousand ellipMcal galaxies, AGN containing low mass X-Ray binaries 3 Mio. AGN • Accreon History: XLF, obscured vs. unobscured • LSS: AGN ACF, AGN/Galaxy CCF, AGN/Cluster CCF • AGN host Galaxies: Morphology, SFR, Obscuraon • Sub-Populaons: • High Redshij (z>6) • Extreme Luminosity • Compton thick AGN • Spectra: Obscuraon, Connuum, So Excess, Iron Lines • Variability: Var. vs. L, L/Ledd, z, Tidal Disrupons • BAOs 10s detecQon, but precise redshis needed. Komossa et al., 2006 Brusa et al. 2009 BAO (eRosita forecast) requirements to optical follow-up 0.5 5 14 6 7 12 ) σ 0.4 4 3 6 5 7 8 10 0.3 9 3 5 4 7 6 8 9 cat 8 f 0.2 10 failures 6 3 7 6 5 4 9 8 10 0.1 11 4 12 CL for BAO detection (in fractionof catastrophic 0 14 13 12 11 10 9 8 7 6 5 4 3 2 0.001 0.01 0.1 σ0 ² 3 mln AGN will be detected redshift error σ0 ² ~15σ BAO detecQon ² opQcal follow-up needed to measure redshijs ² Δz~0.03 or better is required Marat Gilfanov (IKI, MPA) eROSITA surveys in context Point sources sensitivity Extended sources sensitivity -14 All sky: 10 (0.5-2 keV) All sky: 3.4 x 10-14 (0.5-2 keV) 210-13 (2-10 keV) [erg/cm2/s] Merloni et al.
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