The Discovery of Quasars

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1 Massive Black Holes Reinhard Genzel Max-Planck Institut für extraterrestrische Physik, Garching & Departments of Physics & Astronomy, University of California, Berkeley, USA

2 Radio source 3C 273 The Discovery of Quasars z=0.16, distance 2.4 billion light years! L~10 3 L MW 1973: z~3.5 (t 0 =11.6 Gyr), L~10 5 L MS Marten Schmidt 1963

3 What powers QSOs? R. Sunyaev HST WFPC 2 Fusion: E < Mc 2 E.Salpeter Schwarzschild throat (Schwarzschild-Kerr) E < 0.4 Mc 2 variable X- und - radiation relativistic radio jets D.Lynden-Bell M. Rees

4 How does one prove the existence of a black hole? an unambiguous proof of the existence of a black hole requires the determination of the gravitational field/space time metric to the scale of the event horizon. Kepler orbits of the planets V~1/ R

5 early evidence for a central mass concentration near-infrared image SgrA* C.H.Townes 10 (1 light year) E.Becklin Becklin et al. 1971, Balick & Brown 1974, Lo et al. 1975, Wollman et al. 1977, Lacy et al. 1980, 1982

6 high resolution stellar NIR imaging/spectroscopy adaptive the ESO/VLT and Keck NACO ESO VLT(I) MPE SINFONI Keck UCLA PARSEC Lenzen, Hofmann, Eisenhauer, Bonnet, Rabien, Davies, Matthews, McLean, Larkin, Wizinovich

7 As seen from Zuerich in Geneve in San Francisco Astrometric Precision mas 2mas on the Moon μas year 10μas

8 M.Morris A.Ghez R.Schoedel A.Eckart S.Gillessen F.Eisenhauer Kepler Experiment : motions of stars near SgrA* 2000 km/s R= (1 Lichtmonat) Eckart & Genzel 1996, 1997, Ghez et al. 1998

stellar orbits testing the potential: S2 MPE-VLT UCLA-Keck 1992 2002/ 2018 S2/S02

14) stat ( 0.2) sys x10 6 M R 0 = 8.36 (±0.1) stat (±0.15) sys kpc ρ >10 16..19.

3mas S2-orbit Schödel et al. 2002, 2003, Ghez et al. 2003, 2008, Eisenhauer et al.

9 stellar orbits testing the potential: S2 MPE-VLT UCLA-Keck / 2018 S2/S02 P=15.9 y R peri =1400 R S (17 lh) peri =0.03 SgrA* M = 4.26(±0.14) stat ( 0.2) sys x10 6 M R 0 = 8.36 (±0.1) stat (±0.15) sys kpc ρ > M pc -3 M extended /M < a few 10-2 M & SgrA* coincident <0.3mas S2-orbit Schödel et al. 2002, 2003, Ghez et al. 2003, 2008, Eisenhauer et al. 2003, 2005, Gillessen et al. 2009a,b, Meyer et al. 2012, Chatzopoulos et al. 2015, Fritz et al. 2015, Plewa et al Cluster

10 SgrA* R/R s light months 37 μarcsec 10 1 v pm 2, 20 km/s (50 μarcseconds/yr!) 4 R s Model of 1.3mm Emission from SgrA* Backer & Sramek 1996, Bower et al. 2003, 2005, Reid & Brunthaler 2004, Shen et al. 2005, Doeleman et al. 2008

11 density (M pc -3 sun pc ) -3 ) density (g cm -3 ) density (g cm -3 ) density (M pc -3 ) Is SgrA* a black hole? size (R s (3x10 6 size (pc) M )) x10 6 >10 yrs 10 M BH >10 9 yrs 4x10 6 M sun BH boson star boson star density nuclear star cluster at 0.3 pc density stellar cusp at 0.5" constraints from stellar orbits SgrA* (17 kev) size/motion fermion ball and S-star and motions SgrA* radio properties >10 5 yrs >10 5 yrs dark astrophysical clusters with life times >10 5 years SgrA* size/motion and S-star motions fermion ball (17 kev) >10 9 yrs density stellar cusp at 0.5" > x10 yrs M BH 6 density nuclear star cluster at 0.3 pc size/radius 3x10 of event horizon of BH 6 M BH boson star size (R s (3x10 6 M )) size (R (3x10 M )) size s (pc) Maoz 1998, Schödel et al. 2003, Ghez et al. 2005, Coleman Miller 2006, Tsiklauri & Viollier 1998, Torres et al. 2000, Chapline et al. 2001, 2003, Mazur & Mottola 2004 boson star

Yet another surprise in the Galactic Center : a gas cloud falling straight

2014, Pfuhl et al. 2014, Witzel et al. 2014, Valencia-S et al.

2012, 2015, Murray-Clay & Loeb 2012, Miralda-Escude 2012, Meyer &

12 Yet another surprise in the Galactic Center : a gas cloud falling straight into the hole Gillessen et al. 2012, 2013, 2014, Pipher et al. 2014, Pfuhl et al. 2014, Witzel et al. 2014, Valencia-S et al. 2014, theory: Burkert et al. 2012, Schartmann et al. 2012, 2015, Murray-Clay & Loeb 2012, Miralda-Escude 2012, Meyer & Meyer-Hofmeister 2012, Moscibrodzka et al. 2012, Scoville et al. 2013, Ballone et al. 2014, Guillocjon et al , Mapelli & Ripamonti 2015

offset from SgrA* (arcsec) G2: Text book case of tidal

R p =20 lh e=0.97 P~300 y 2014.7 0.2 0-0.

13 offset from SgrA* (arcsec) G2: Text book case of tidal shearing velocity offset (km/s) R p =20 lh e=0.97 P~300 y Evolution of pv structure of Br -emission in G with SINFONI & AO: Gillessen et al. 2012, 2013a,b, Pfuhl et al. 2014

14 Simulation of tidally disrupting gas cloud Simulation of a purely ballistic evolution of tidally disrupting gas cloud

15 Demographics of massive black holes in nearby galaxies NGC 4258 (VLBA) M =10 8 M M (M sun) M =3.6x10 7 M 10 6 MW M31 (HST) M Bulge (M sun ) M /M bulge ~2-5x10-3 Green, Barth & Ho 2006, Kormendy & Ho 2013, McConnell & Ma 2013

16 The cosmic evolution of galaxies and massive black holes SFR BH accretion (scaled) (major) mergers & starbursts rate ~ 20-30% Soifer et al Madau & Dickinson14 20 semi-continuous accretion from halo (including minor mergers) & disk instabilities rate ~ %

17 The next steps: using the GC-BH to test GR 8m Pulsars? 39 (30) m MICADO Astrometric Camera EELT (TMT) 120m Inter-Continental Submm-VLBI Event Horizon Telescope Black Hole Cam Near-IR Interferometric Astrometry ESO-VLTI

18 GRAVITY dewar in Paranal Integration hall 12 tons of GRAVITY on Paranal July16, 2015 GRAVITY Team July 28 Metrology installation on ATs July 20

19 Inward bound IR & radio instruments residuals of S2 data-newton vs. GR shadow β 2 effects in radial velocities 1 relativistic prograde precession 2 spin from Flares, L-T precession 3 Quadrupole moment of metric, no hair & Strong quantum effects curvature: 5 photon orbit 4 3 RS S2: S ~ 12' 2 1 e a GRAVITY (first years)

The Galactic Center a unique laboratory for studying massive black holes

The Galactic Center a unique laboratory for studying massive black holes Reinhard Genzel MPE on behalf of the ESO Galactic Center community (MPE, MPIA, UCologne, Observatoire de Paris, Granada, MPIfR,