eROSITA: Follow-up for Clusters and AGN Surveys Andrea Merloni (MPE) eROSITA Project Scientist eROSITA on SRG: the Mission -  Launch: November 2013 -  3 Months: flight to L2, verification and calibration phase -  4 years: All sky surveys (8 scans), 4-6 scans per day -  ~3.5 years: pointed observation phase, including ~20% of GTO (gaps, cluster follow-up, etc.). 1 AO per year -  Proprietary data rights shared 50/50 between MPE (Germany) and IKI (Russia): two hemispheres -  German (MPE) half: proprietary period 2 yrs -  German (MPE) half: Public Release of all-sky scan data ~ every year Launcher: Zenith-Fregat Key feature needed: wide AREA eROSITA is an instrument designed to perform all sky 0.5-10 keV surveys: LARGE FOV (0.81 deg2), large effective area, good resolution (28-30”), long life (7.5 years) 1.5 5.0 25 300 ksec Area covered at ~20 ks is ~140 deg2 (M. Fürmetz, MPE) eROSITA and ART: eff. area and grasp On-Axis Effective Area! Grasp 1000! 1000! 100! 100! 2000 (coutesy of M. Pavlinsky, IKI, P.Friedrich MPE) eROSITA sensitivity estimates Point sources (AGN) Extended sources (Clusters) D D e e e p e p a a r e r a e a 6 6 m m o o 4 n 4 n t t y h y h r s r s s s eROSITA sensitivity estimates, surveys in context Point sources (AGN) Extended sources (Clusters) All sky: 10-14 (0.5-2 keV) 2×10-13 (2-10 keV) [erg/cm2/s] Dark Energy studies with 100k Clusters eROSITA Clusters detection simulations M. Mühlegger, PhD thesis 2010 1 1 0 2 , i n a i c r o P , h c i r p i e R , h c i p >70.000 Clusters with log M>14 e l l i P ~2M eROSITA AGN •  First 2-10 keV all-sky survey after HEAO-1 (F ~ 10-13 cgs full survey) lim •  AGN in Large-Scale Structure (clustering vs. z, L) •  AGN ACF, AGN/Clusters CCF, AGN/Gal CCF •  Obscured vs. Unobscured AGN at z~2 •  High-z (z>4) AGN •  Tidal disruption events •  AGN variability over >4 years •  Binary SMBH? Source density: 15-250/sqdeg