erosita on SRG Andrea Merloni MPE, Garching
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1 erosita on SRG Andrea Merloni MPE, Garching A. Merloni - Ringberg, 4/2016
2 Spectrum- Roentgen- Gamma erosita (MPE) ART- XC (IKI) Navigator (Lavochkin Ass.) Fregat- SB Booster + Launcher + Ground Segment
3 History ROSAT First X- ray all- sky survey with an imaging telescope Bundle of 7 small telescopes To extend the all- sky survey towards higher energies failed shortly after launch ABRIXAS science on the International Space Station ROSITA 2002 ABRIXAS 1999 in phase C/D completely funded Launch in 2017 erosita on Russian SRG Mission 10 5 Clusters of Galaxies 7 bigger mirror modules extended field of view not realised due to Shuttle schedule And ISS contamination problems DUO 2004 Dark Energy 10 4 Clusters of Galaxies SMEX- proposal, lost against NuStar
4 Main science driver: Clusters of galaxies, LSS and Cosmology Rosati, Norman, Borgani 2002 A signature of clusters is the detection of hot (~10 7 K) ICM Clusters of galaxies are the largest gravitational bound structures They are exponentially sensitive tracers of growth of structures Cosmological constraints with (well calibrated) ROSAT samples of <100 obj.
![0 11.0 log(lx) [erg/cm 2 /s/arcmin2 ] Diffuse X- ray emitting gas traces the massive knots of](/docs-images/92/109248810/images/5-1.jpg "the cosmic web (Clusters) Point sources (Quasars) signpost the growth of black holes Detect")
5 Mapping the structure of the hot Universe: Requirements Coma Virgo Hydra Images coutesy of K. Dolag (LMU), M. Mühlegger (MPE), O. Hahn (ETH) Centaurus Perseus log(lx) [erg/cm 2 /s/arcmin2 ] Diffuse X- ray emitting gas traces the massive knots of the cosmic web (Clusters) Point sources (Quasars) signpost the growth of black holes Detect Clusters of Galaxies! All- sky survey sensitivity erg/cm2/s! Deep survey field(s) (~100 deg2) to ! Individual pointed observations! Moderate angular resolution (<30 aver. over FoV)! Large collecting area (> 2000 Large FoV (1 Ø)! Long duration survey: 4 years " # 1/2 year (ROSAT) Simulation of an erosita field A. Merloni - Ringberg, 4/2016
6 erosita Collaboration PI: Peter Predehl; PS: A. Merloni (MPE) Core Institutes (DLR funding): MPE, Garching/D Universität Erlangen- Nürnberg/D IAAT (Universät Tübingen)/D SB (Universität Hamburg)/D Astrophysikalisches Institut Potsdam/D Associated Institutes: MPA, Garching/D IKI, Moscow/Ru USM (Universität München)/D AIA (Universität Bonn)/D Industry: Media Lario/I Mirrors, Mandrels Kayser- Threde/D Mirror Structures Carl Zeiss/D ABRIXAS- Mandrels Invent/D Telescope Structure pnsensor/d CCDs IberEspacio/E Heatpipes RUAG/A Mechanisms HPS/D,P MLI + many small companies MPE: Scientific Lead Institute, Project Managment Instrument Design, Manufacturing, Integration & Test Data Handling & Processing, Archive etc.
7 The erosita telescope Telescope structure Focal length 1.6 m F.o.V. = 0.81 sqdeg Total weight ~800 kg 7 identical telescopes (Wolter- I/ pnccd- cameras) Energy range: kev Energy resolution: ~136 6 kev Effective Area: ~1400 cm 2 (@1keV)
8 7+1 Mirror assemblies FM1 FM2 FM3 FM4 FM5 FM6 C- K (0.28 kev) Al- K (1.49 kev) Cu- K (8.04 kev) nested gold- coated nickel mirror shells - Mirror assemblies (mirror + baffles) integrated & tested in Calibration of all 8 telescopes at PANTER until mid- May! - On- axis Half- Energy width (HEW) ~16
9 Focal Plane Mapping (FM2) Al Kα (1.49 kev) HEW = 16,3 arcsec Cu Kα (8 kev) HEW = 14,7 arcsec
10 7+1 Framestore pnccd Meidinger et al, 9144E..1WM
11 FM Camera Calibration Spectral resolution at all measured energies within specification Extremely good uniformity Only weak dependence on CCD and electronics temperature (unlike XMM) FM1 FM2 FM3 FM4 C- K (0.28keV) O- K (0.53keV) Cu- L (0.93keV) Al- K (1,49keV) Ti- K (4,51keV) Fe- K (6,4keV) Cu- K (8.0keV) Ge- K (9.9keV)
12 Effective Area and Grasp Effective area at 1keV comparable with 1 kev Factor ~7-8 larger surveying speed 4 years dedicated to all sky survey (with estimated 70-80% efficiency)
13 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 figure margin lines shown on this review document. Complete formatting information is available at ART- XC Return to the Manage Active Submissions page at and approve or disapprove this submission. Your ma be published without this approval. Please contact with any questions or concerns. PI: M. Pavlinsky (IKI) - Energy range: 5-30 kev - FOV: 34ʹ - On- axis resolution 1ʹ - Energy resol. 12% at 14keV - Time res. 1ms Figure 2. Th he ART-XC tellescope array with w seven mirro or modules and d seven focal-plane detectors. T The basic structure of AR XC is the op ptical bench th he conical carbo on-fiber tube th hat is equipped with a moveable cover to prottect the optics during d lau (not shown)..the star trackeer with its own n radiator is installed on the to op of this tube. The detector ccollimators, coo oling radi with cooling g pipes and the electronics e boxees are visible att the bottom of the tube. 2.2 Qu ualification model m of AR RT-XC All subsystem ms of the QM ART-XC insstrument succeessfully passeed the qualificcation tests at the end of Occtober 20 IKI. The quaalification perriod for subsy ystem turned out to be sev veral months more than sccheduled as more m time required for further devellopment of the attachmen nt structure for fo the detecttor s beryllium m window. The T bery windows rifteed in two dettectors during g the thermo cycling c test, as a the temperrature of the sseven detecto ors was c within the ran nge 35 C to +55 C (Figurre 3) a few do ozen times. A. Merloni - Ringberg, 4/2016
14 A fast survey machine 100 kpc [0.5 HEW] [26.5 HEW (FoV avg)]
15 erosita extragalactic sky Image credits: MPE, erosita_de consortium, XMM-XXL Wide- area census of galaxy clusters (105) and active galactic nuclei (106) A. Merloni - Ringberg, 4/2016
16 SRG: Mission timeline ART-XC IKI erosita MPE Navigator NPO Lavochkin - erosita delivery to Russia: Q Launch: September 2017 from Baykonour (Zenit+Fregat); Next launch window in March Months: flight to L2, PV and calibration phase - 4 years: 8 all sky surveys erass:1-8 (scanning mode: 6 rotations/day). Exact exposure map still TBD years: pointed observation phase, including ~20% GTO. 1 AO per year
17 Multi- wavelength synergy, SEP A. Merloni - Ringberg, 4/2016
18 erosita surveys in context Point sources sensitivity Extended sources sensitivity All sky: (0.5-2 kev) (2-10 kev) [erg/cm 2 /s] All sky: 3.4 x (0.5-2 kev) Merloni et al. 2012
19 All massive clusters Log Mass (solar masses) Log redshift 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
20 3 Million AGN: Physics and Cosmology z=1 1. The most luminous AGN, tracers of large scale structure: the quasar mode of AGN feedback 2. Nearby LLAGN: the kineuc (radio) mode of AGN feedback 3. Quiescent Black holes revealed by Udal disrupuon of nearby stars L X =10 44 erg/s - AGN/QSO densities r<22.5 [deg - 2 ]: Reach ~100/deg 2 in 0.8<z<2.5 (BAO) - erass:8 only: 48 (26 in 0<z<0.8; 22 in 0.8<z<2.5) - erass:8+xdqso: 24 (0.8<z<2.2) - XDQSO only: 50 (0.8<z<2.2)
21 erosita sensitivity to variables Expect 1000 s of TDE over 4 years (Khabibullin et al. 2013) Merloni et al. 2012
22 And More Provide a detailed view of the compact objects (NS, BH) population of the Milky Way Survey of 700k active (young, magnetic) stars Map the diffuse X- ray emission and the hot ISM in the Milky Way and in the Solar neighborhood Study nearby star- forming galaxies and galaxy groups Provide a dynamical view of the X- ray sky and identify transients and variable sources Serendipity
23 Working with erosita erosita is a PI instrument Data split 50% MPE and 50% IKI West/East (gal. coord.) German data public after 2 years, 2 releases (~T launch +3.3 and T launch +6.3 TBC); no commitment yet on the Ru side Proprietary access via erosita_de consortium Projects/papers regulated by working groups Working Groups: Science: Clusters/Cosmology, AGN, Normal galaxies, Compact objects, Diffuse emission/snr, Stars, Solar System, Time Domain Astrophysics Infrastructure: Data analysis and catalogues, Multiwavelength follow- up, Calibration, Background Collaboration policy: Individual External Collaborations (proposal to WGs) Group External Collaborations (team- to- team MoUs)
24 Multi- wavelength synergy
25 Welcome to Ringberg! Discuss about science Multiwavelength synergies Planning collaborations Discussion sessions: Tomorrow afternoon 5:40pm- 6:30pm Wedensday morning: 12:00-12:30 Plus many rooms available in the evening A. Merloni - Ringberg, 4/2016
26 Thank you Image courtesy of K. Dolag
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