The massive black hole and central star cluster in the Milky Way Center
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- Jayson Myron Gibbs
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1 The massive black hole and central star cluster in the Milky Way Center R.Genzel SgrA* paradox of MPE youth & UC Berkeley testing the BH paradigm with stellar orbits emission and properties of SgrA* F.Eisenhauer, T.Paumard, R.Schödel, T.Ott, A.Eckart, T.Alexander, S.Trippe, R.Abuter, S.Gillessen, F.Martins
2 Massive Black Holes Reinhard Genzel MPE Garching & UC Berkeley
3 New Results in the Galactic Center R.Genzel MPE Garching & UC Berkeley R.Schödel, T.Ott, A.Eckart, T.Alexander, F.Eisenhauer, R.Abuter, T.Paumard a paradox of youth testing the BH paradigm with stellar orbits accretion, flares & BH spin
4 Quasars: stars or black holes? E <.5 Mc 2 HST WFPC 2 mass distribution radio source 3C 273 Schmidt, Lynden-Bell, Rees E.4 Mc 2 variable X- und γ - radiation relativistic radio jets
5 The Galactic Center as Laboratory: Expectations (Morris 1993, Genzel, Hollenbach & Townes 1994, Melia & Falcke 21, Alexander 22) t ~ 15Myr, 2Myr rt t ms tcoll m m tfor ms tr r 1" mms-ms 1.3M for R 2.5" ms-g tidal disruption of stars ms R 15 light minutes 1/t 1 yr disruption v c α 1 2 σ = + ρgas ρroche 1 R cm " R acc M acc 1" Lacc 1 L 1 LEdd observed : L 1 SgrA* M yr 3 L stellar cusp : ρ( R) ( ) R α =
6 The Galactic Center as Laboratory: Expectations (Morris 1993, Genzel, Hollenbach & Townes 1994, Melia & Falcke 21, Alexander 22) ~ 15Myr, 2Myr tr t ms tcoll m m tfor ms R t r 1" mms-ms 1.3M for R 2.5" ms-g R acc M acc 1" Lacc 1 L 1 LEdd observed : L 1 ms tidal disruption of stars R 15 light minutes low abundance rapid in-spiral of binaries of because σ 1/t cluster >v escape 1 yr dynamical friction (<a few Myr) dense star cluster 5-1 by disruption SgrA* M yr 3 L ρgas ρroche 1 R cm star-stellar BH scattering stellar cusp : ρ( R) " ( ) R α =
7 The MPE G.C.experiments proper motion experiment at the 3.5m ESO NTT (near-ir speckle camera SHARP): since 1991 adaptive optics-assisted (AO) integral field spectroscopy on ESO 2.2m (3D): since 1994 AO camera/spectrometer NAOS/CONICA on 8m ESO VLT: since 22 AO integral field spectroscopy on VLT (SINFONI/SPIFFI): since Feb 23 key people: A.Eckart, F.Eisenhauer, T.Ott, R.Schödel
8 stars (NIR) Ionized gas (radio) 1 ( 8 ly) The center of the Milky Way Hot gas (X-rays) diameter 1 light minutes SgrA* * (synchrotron)
9 Ionized gas (radio) The Center of stars (NIR) diameter 1 light minutes the Milky Way SgrA* * (synchrotron) The center of the Milky Way 6 ( 5 light years) Hot gas (X-rays) 3 light years
10 NAOS/CONICA and SINFONI at the VLT NAOS-CONICA: Co-PIs: G.Rousset (ONERA), R.Lenzen (MPIA), R.Hofmann(MPE) SPIFFI/SINFONI: PIs: F.Eisenhauer & N.Thatte (MPE)
11 Adaptive NACO H/K s /L 15NE E N optics 7 1EE 3 1W SgrA* IRS ( 1 light years) ) 12N ALFA Calar Alto (MPIA/MPE) (Eckart Eckart,, Genzel, 1 (.39 Ghez pc) et al.)
12 SINFONI ( = SPIFFI (MPE, PI F.Eisenhauer)+MACAO(ESO,, PI H.Bonnet)) Integral field spectrometer with reflective image slicer 32x64 spatial pixels (.125,.5,.125 ) x 2 spectral pixels (2K Hawaii) spectral resolving power: 2-5 ~4% throughput in J, H and K 6 element, curvature sensor AO system/bimorph mirror with APDs Eisenhauer et al. 23, ESO Messgr. 113, 17, Eisenhauer et al. 23, SPIE 4841, 1548, Bonnet et al. SPIE 4839, 329 Bonnet et al., 24, ESO Messgr 117, 17 anticipated LGS performance (25)
13 4 3 IRS1 EE (K5 Ia/b) stellar cusp and its properties.2 IRS3 (WC 5/6) 2 1 H+K, K s 17 crowding corrected wavelength (µm) wavelength (µm) IRS16SE2 (WN5/6) S2 (O8/9 V) IRS16 SgrA* wavelength (µm) IRS1 EE (M7/8 adaptive III) optics IR instruments on Keck IRS16 SW (Ofpe/LBV) 1 and VLT: 5 mas resolution wavelength (µm) Genzel et al. 23, Ott et al. 24 NACO H/K s /L SINFONI wavelength (µm) Ghez et al. 24, Keck laser guide star AO
14 1 e a r ly K < e a r ly K < 1 2 c lo c k w is e two coeval, rotating discs of stars at R~ pc x(arcsec) J z /J z (max) r a d ia l y (arcsec) c o u n te r c lo c k w is e p SgrA* (arcsec) 4 early type stars type clockwise counterclockwise V z (km/s) LBV/WN1 WN9/Ofpe Genzel et al. 2, 23 Ott et al. 24, Paumard et al. 21, Dec-offset (") WN7/8 WN5/6 WC8/9 WC5-7 OB > >5
15 NACO NACO H/K s /L images 15NE E N 7 1EE 3 1W SgrA* IRS ( 1 light years ) 1 (.39 pc) 12N
16 Integral field spectroscopy 1996:.6 with 3D 24:.7 with SINFONI/VLT +AO 1.5 (22 ld) 3 23:.27 SPIFFI/VLT
17 stars in the central 2 light days: a paradox of youth SINFONI : K(75 mas) 7 S () (λ/2.157) 2 (mjy) 5.5 S S S Dec.-offset from SgrA* (arcsec) light days R.A.-offset from SgrA* (arcsec) S S S S S14 5. S S1 Brγ velocity offset (km/s) Eisenhauer et al. 25
18 ordinary B main sequence-stars stars! HeI (±35) km/s 1.3(±.3) Å HI Brγ (±2) km/s 5.8(±.4) Å HeI: v rot sin(i)~.55 FWHM = 154(±19) km/s. solar neighborhood early B stars <v rot sini>~13 km/s (Gathier, Lamers & Snow 1981) <1Å FWHM= 12(±8) km/s EW=11.7(±2) Å wavelength (µm)
19 parodox of youth: two basic scenarios in situ formation from molecular clouds formation in massive disk collision of less massive stars general problem: tidal field external star formation and migration - mass segregation - spiraling in of star cluster - scattering general problem: timescale and efficiency Morris 1993, Genzel, Hollenbach & Townes 1994, Lee 1994, Sanders 1998, Gerhard 21, Portegies Zwart et al. 22, Levin & Beloborodov 23, Nayakshin et al. 23, 24, Gould & Quillen 23, Genzel et al.23, Hansen & Milosavlevic 23, Kim & Morris 23, Alexander 23, Milosavlevic & Loeb 24
20 NACO/VLT AO images H+K, K s 17 crowding corrected surface density (sources per square arcsecs) ρ * ( R )=3x1 7 (R/arcsec) -1.4 (M pc -3 ) fraction of late type stars radius from SgrA* (arcsecs) 1 (.39 pc) Genzel et al. 23, Ap.J. 594, 812
21 NACO/VLT AO images 1 (.39 pc)
22 radius from SgrA* (arcsecs) surface density (sources per square arcsecs) fraction of late type stars
23 Properties of nuclear star cluster: K-luminosity function surface density (sources per sq.-arcsec per mag) supergiants Galactic center KLF 8 Gyr SSP model Zoccali et al. Bulge KLF AGB O/B V K/M giants p 9" K-mag HB A/F V Best fit: old metal rich component + young burst population, or constant star formation Genzel et al. 23, Zoccali et al.22, Tiede et al. 1995, Figer 22
24 Properties of nuclear star cluster: K-K luminosity function surface density (sources per sq.-arcsec per mag) Galactic center KLF Zoccali et al. Bulge KLF supergiantso/b V AGB HB K/M giants p 9" A/F V NACO Galactic center Zoccali et al. Bulge KLF p 1.5" Genzel et al. 23 K-mag K-mag
25 KLF of cusp surface density (sources per sq.-arcsec per mag) supergiants NACO Galactic center Zoccali et al. Bulge KLF 8 Gyr SSP model AGB O/B V K/M giants p 1.5" K-mag HB A/F V lack of red clump/hb stars KLF+cusp mass model: either KLF steepens at K>19, or IMF is flatter than Salpeter
26 4 3 2 IRS1 EE (K5 Ia/b) SPIFFI 3D spectroscopy.2.1 IRS3 (WC 5/6) wavelength (µm) wavelength (µm) IRS16SE2 (WN5/6) S2 (O8/9 V) wavelength (µm) 7.5 IRS1 EE (M7/8 III) IRS16 SW (Ofpe/LBV) (.39 pc) wavelength (µm) wavelength (µm) Ott et al. 24, in prep. S2: see Ghez et al. 23
27 la te ty p e s ta r s K < e a r ly K < e a r ly K < c lo c k w is e 1 c lo c k w is e Dynamics of stellar components J z /J z (max) r a d ia l J z /J z (max) r a d ia l -1 c o u n te r c lo c k w is e c o u n te r c lo c k w is e proper motions and radial velocities (Ott et al. 24) p SgrA* (arcsec) p SgrA* (arcsec) 4 late type stars 4 early type stars 2 2 v z ( km/s ) McGinn et al. 1989, Sellgren et al.199, Krabbe et al. 1995, Haller et al. 1996, Genzel et al. 2, 23, Paumard et al. 21, Figer et al. 23 Dec-offset from SgrA* (arcsec) Dec-offset (")
28 v perpendicular (km/s) clockwise J(z)>, i=12 o, φ o =-6 o counter-clockwise χ 2 =3.9 (1.9) red d(sgra*)<7" o J(z)<, i=-4, φo =16 o χ 2 =5.1 (4.8) red d(sgra*)<7" v parallel (km/s) v parallel (km/s) Genzel et al. 23, Ap.J. 594, 812, Levin & Beloborodov, 23, ApJ, 59, L33
29 massive stars in two counter-rotating disks x(arcsec) z (arcsec) 5 x(arcsec) y (arcsec) z (arcsec) type clockwise counterclockwise -2.5 LBV/WN1 4 1 WN9/Ofpe 4 2 WN7/8 1 1 WN5/ y (arcsec) WC8/9 5 5 WC5-7 1
30 NACO 1.6.4: H (4mas).5 (23 light days) Dec.-offset from SgrA* (arcsec) SINFONI : K(75 mas) 26 S S S S5 S S S S9 15. S S S1 S S S S W W S13 S S R.A.-offset from SgrA* (arcsec) -.6
31 S-stars are main sequence B-starsB K= : S5,6, 8, 12, 13, 14 July+Aug K 15: S1,2,4,8,9 July+Aug HeI (±35) km/s 1.3(±.3) Å HI Brγ (±2) km/s 5.8(±.4) Å 1. S ν ν -2 (mjy) HI Br HeI HI Br HI Br S ν ν -2 (normalized) <1Å FWHM= 12(±8) km/s EW=11.7(±2) Å wavelength (µm) wavelength (µm) Eisenhauer et al. 25
32 A Paradox of Youth : how did the massive stars get into the cusp? formation outside and mass-segregation into center: excluded for stars >2 M in situ formation in extremely dense gas (>1 9 cm -3 ): fragmentation of self-gravitating accretion disk, following cloud infall and dissipation, + perhaps cloud-cloud collisions sinking to the center of a young, very massive (1 5 6 M ) and compact (<.2pc) cluster formed at R~1 pc creation of massive stars from collisions and mergers of lower mass stars in the central.5 (but not further out) shuttling in of stars by intermediate mass black hole binary scattering resonant scattering by stellar black holes near SgrA* Morris 1993, Genzel, Hollenbach & Townes 1994, Lee 1994, Sanders 1998, Gerhard 21, Portegies Zwart et al. 22, Levin & Beloborodov 23, Nayakshin et al. 23, Gould & Quillen 23, Genzel et al.23, Hansen & Milosavlevic 23, Kim & Morris 23, Alexander 23, Milosavlevic & Loeb 24
33 S-stars are main sequence B-starsB K= : S5,6, 8, 12, 13, 14 July+Aug K 15: S1,2,4,8,9 July+Aug K 15 K> HeI (±35) km/s 1.3(±.3) Å I HI Brγ (±2) km/s 5.8(±.4) Å 1. S ν ν -2 (mjy) HI Br HeI HI Br HI Br S ν ν -2 (normalized) III.95 V.9.85 <1Å FWHM= 12(±8) km/s EW=11.7(±2) Å wavelength (µm) wavelength (µm) Eisenhauer et al. 25
34 7 1 IRS 13 E IRS 16 NE/C log (L Bol (L o ) ) Sgr A* cluster 15 6 AF 2 M o IRS 7 2 M o AGB M o 2 M o 4 M o 12 M o Najarro et al. 1997, Genzel et al. 1997, 21, Ghez et al. 23, Blum et al. 23, Tanner et al log (T eff (K) )
35 Tidally disrupted dispersion rings R. Sanders 1998
36 Proper Motions and Orbit of S2 H (1.6µm): 4 mas Aug H/K 22 s /L NW 15NE N E E 7 E N N CC 16 C 1EE W 5mas 2 light days 21 IRS16 3 SgrA* 13 S2 S2 S3 S1 SgrA* (±3σ) SgrA* 1 km/s 9 12N SW 1 (.39 pc) 1 (46 light days) 1 (46 light days)
37 stellar proper motions in central 45 light days S km/s 24 5mas 2 light days 2 NACO H 4 mas T~15 years e=.88 R min =17 lh 22 1 (46 ld)
38 probing the central gravitational potential with stellar orbits 2 light days R o =7.9±.5 kpc SgrA* 6 light months Schödel et al. 22, 23, Ghez et al. 23, 24, Eisenhauer et al. 23, 25
39 precision determination of S2 orbit Schödel et al. 22, NATURE 419, 694 Schödel, et al. 23, Ap.J. 596, 115 Eisenhauer et al., 23, Ap.J.Lett 597, L121, 25 in prep Ghez et al. 23, ApJ 586, L127, + astro-ph 3613 S2 parameters Eisenhauer et al ± ± ±.29(.59) ± ± ± ± ± ± ± ±.1 R o (kpc) 7.94±.42 line of sight velocity (km/s) Ghez et al ± ± ± ± ± ± ± ± ±.25 Brγ time 5mas 2 light days R o =7.94±.42 kpc
40
41 3D structure of orbits.6.5 x=+2.5mas y=-2.1 mas M o =3.68±.2x1 6 M(sun).4 (R o = 8 kpc) Dec-offset (arcsec) S17 S8 S14 S12 S13 S8 S2 S1 line of sight velocity (km/s) RA-offset (arcsec) time Schödel et al. 23, Ghez et al. 23, Eisenhauer et al. 25
42 .2 x z.2 3 x y.2 sky plane view (x-y) 1 y y-z view.2 z view in the plane of the clockwise, outer star ring/disk x z 1 x-z view y y -.2 S1 S2 S8 S12 S13 S14 S17 z
43
44 orientation of orbital spin directions Eisenhauer et al. 25
45 3 x x y y S1 S2 S8 S12 S13 S14 S z z 2 4 Orientation of S-orbits relative to outer star disks
46 mass distribution radius (light hours) enclosed mass (solar masses) R o = 8 kpc multiple orbits S2 dark cluster ρ o =1.6x1 18 M(sun) pc -3 α =5 S3 3.35(±.15) x1 6 M(sun) point mass plus visible star cluster (χ 2 =1.2) red G G visible star cluster ρ o =1.5x1 6 M(sun) pc -3 r core =.46 pc, α=1.7 G G radius (parsec) Schödel et al., NATURE 22, 419, 694; 23, Ap.J. 596, 115, Ghez et al. 23, Ap.J. 586, L127, astro-ph 3613, Eisenhauer et al. 23, ApJ 597, L121
47 mass distribution radius (light hours) enclosed mass (solar masses) R o = 8 kpc multiple orbits S2 dark cluster ρ o =1.6x1 18 M(sun) pc -3 α =5 S3 3.35(±.15) x1 6 M(sun) point mass plus visible star cluster (χ 2 =1.2) red G G visible star cluster ρ o =1.5x1 6 M(sun) pc -3 r core =.46 pc, α=1.7 G G radius (parsec) Schödel et al., NATURE 22, 419, 694; 23, Ap.J. 596, 115, Ghez et al. 23, Ap.J. 586, L127, astro-ph 3613, Eisenhauer et al. 23, ApJ 597, L121
48 stars: v> 5 km/s SgrA* * does not move VLBI: v(sgra*)<1 (2) km/s diameter radio source <2 R s (Backer, Reid et al. 1999, 24) M SgrA* > 1 5 M ρ SgrA* > M pc -3 = g cm -3 Reid et al. 1999, 24, Chatterjee et al. 22, Dorband et al. 23
49 limits to the proper motion of SgrA* 4 IR radio Dec-offset from best focus of S2 (mas) RA-offset from best focus of S2 (mas) v IR 1 km/s v rad < 2 (2) km/s proper motion of SgrA* Backer &Sramek 1999, Reid et al. 1999, Genzel et al. 23, Ghez et al. 24, Reid et al. 24
50 X-ray flares 1 light minutes 2 (3 light years) Chandra May 22 campaign: ~.5 flares/day 2 light hours Baganoff et al. 2, 21,23
51 properties of SgrA* radio/mm 4 IR flares radio Dec-offset from best focus of S2 (mas) 2-2 SgrA* (.1 pc) RA-offset from best focus of S2 (mas) v IR 1 km/s v rad < 2 (2) km/s proper motion of SgrA* Lo et al. 1998, Zhao et al. 22, Doeleman et al. 22, Backer & Sramek 1999, Reid et al. 1999, Genzel et al. 23, Ghez et al. 24, Reid et al. 24, Bower et al. 24
52 Black hole or not black hole? 2.8x1 3x1 6 6 M sun BH size (R s (2.8x1 3x1 6 6 M sun )) boson star 23 22/3 1 2 density (M sun pc -3 ) >1 5 yrs >1 9 yrs SgrA* size/motion relative S2 size X-ray/ IR flare emission region S2 orbit SgrA* cluster proper motions fermion ball (17 kev) 1996 density stellar cusp at.5" 1986 gas motions mini-spiral density (g cm -3 ) >1 1 yrs density nuclear star cluster at.3 pc size (pc)
53 black hole or no black hole? size (R s (3x1 6 M )) x1 6 M BH boson star 1 2 density (M pc -3 ) SgrA* size/motion relative S2 >1 5 yrs >1 9 yrs size X- ray/ IR flare emission region S2 orbit SgrA* cluster proper motions fermion ball (17 kev) density stellar cusp at.5" gas motions mini-spiral density (g cm -3 ) >1 1 yrs density nuclear star cluster at.3 pc size (pc) Schödel et al. 22, 23, Ghez et al. 24, Reid et al. 24
54 surface density (sources per sq.-arcsec per mag) Constraints on cusp properties & mass Galactic center KLF Zoccali et al. Bulge KLF 1S2-orbit allows 3-7x1 5 M of extended O/B mass V supergiants AGB HB K/M giants p 9" A/F V K-band luminosity function NACO Galactic center Zoccali et al. Bulge KLF p 1.5" K-mag Mouawad Genzel et et al. al , A&A in press (astro-ph 42338) K-mag
55 X- and γ-rays from SgrA* 6 kev INTEGRAL cont. & 6.4 kev ASCA FeK SgrA* Chandra 2-8 kev why is the BH so faint: L~1-6 8 L Edd? May 22 campaign: ~ flares/day TeV source Aharonian et al hours low accretion rate low conversion efficiency to radiation low efficiency of removal of angular momentum Baganoff et al. 1, 4, Muno et al. 4, Mayer-Hasselwander et al. 99, Porquet et al. 23, Goldwurm et al. 1998, 23, Sunyaev et al. 1993, Koyama et al. 1996, Revnivtsev et al. 24
56 Distance to Galactic Center NACO 1 SPIFFI Distance Galactic Center: 7.94±.42 kpc Rotation velocity of sun: km/s GC Eisenhauer et al. 23
57 radio/mm SgrA*: diameter ~ 1 AU ~ 2 R s accretion onto the black hole 1 min. 2-8 kev 3 (.1 pc) why is the BH so faint: L~1-6 8 L Edd? low accretion rate low conversion efficiency to radiation low efficiency of removal of angular momentum 2 hours May 22 campaign: ~ flares/day Baganoff et al. 2, 21,23, Porquet et al. 23, Aschenbach et al. 24, Yusef- Zadeh, Zhao et al. 2, 23,Aitken et al. 99, Bower et al. 23
58 radio/mm 2-8 kev SgrA*: diameter ~ 1 AU ~ 2 R s 1 min. Accretion onto the Black Hole Why is the BH so faint: L~1-9 L Edd? 3 (.1 pc) 2 hours May 22 campaign: ~ flares/day X-rays low accretion rate low conversion efficiency to radiation low efficiency of removal of angular momentum Baganoff et al. 2, 21,23, Porquet et al. 23, Aschenbach et al. 24 Baganoff, Bower, Doeleman, Lo, Yusef-Zadeh days Yusef-Zadeh, Zhao et al. 2, 23,Aitken et al. 99, Bower et al. 23
59 infrared flares & BH spin location of black hole.22 (1 light days) May 9, 23: NACO (VLT) H-band, 4 mas resolution (adaptive optics), 1 min per image
60 K t o =3 h 1 m 7 s (UT) 12 infrared flares K t o =4 h 47 m 46 s (UT) dereddened flux density (mjy) d 8 S1 SgrA* 5 1 J u ly 8 th, 2 4, t o = 2 h 3 7 m 5 7 s 4 4 e 5 1 S (mjy) 2 Genzel et al. 23, Nature 425, Ghez et al. 24 ApJL t - t o (m in)
61 Infrared flares: quasi-periodicity 12 K t o =4 h 47 m 46 s (UT) S1 SgrA* normalized power spectrum 4 2 period: 16.8±2 min S1 June16th all June15th flare June16th flare e 5 1 spin parameter: a=.52± x x1-3 5x Frequency (Hz) Genzel et al. 23, Nature 425, 934
62 IR variability VLT/Keck H t o = 2 h 1 8 m 2 ( U T ) Dereddened flux density (mjy) Genzel et al. 23 Nature 425, S1 x2 5 1 t-t o (min) K, 15 Jun. 23, t o =3 h 1 m 7s (UT) S (mjy) 12 L -band 8 4 S1 SgrA* Ghez et al. 24, ApJ 61, L t-t o (min) K, 16 Jun. 23, t o =4h 47m 46 s (UT)
63 Fundamental dynamical frequencies around a black hole fundamental dynamical frequencies for M=3.59x1 6 M sun,a=.52 GM/c 3 2 orbital period at last stable orbit ν orbital n=1 g-mode acoustic oscillation R/R s T lsto (min) 1 a =.52 (±.1,.1,±.7,.7,±.14).14) ν (Hz) ν epicycle a/(gm/c) 1-6 last stable orbit ν Lense-Thirring ν R, precession R(cm)
64 SgrA* * flare variability and evidence for significant BH spin Normalized power spectrum period: 17±2 min S1 June 16 average flares June15/16 average 'quiescent' June 15/July21 5x x1-3 5x1-3 T lsto (min) a =.52 (±.1,.1,±.7,.7,±.14).14) orbital period at last stable orbit a/(gm/c) frequency (Hz) Genzel et al. 24, Aschenbach et al. 24
65 Kerr MHD accretion disk simulation De Villers, Hawley & Krolik, 24, Narayan, Quataert, Blandford, Begelman, Balbus, Stone, Gammie
66 IR SED of flares t= t=6 t= t-t (min)= t-t (min)= t-t (min)= α=-2.2± ν L ν (L sun ) 2.5 α=-3.7± α=-3.5±.4 July 15th, 24: t =3 h 37 m UT July 17th, 24: t =3 h 46 m UT SINFONI 24: Eisenhauer et al x x x x x1 14 frequency (Hz) 1.3x x x1 14 frequency (Hz)
67 SgrA* * SED and models E (ev) ν L ν (3.8x1 33 erg/s) RIAF + 1.5% p=3.5 power law RIAF + SSC jet-disk ν (Hz) Radio: Zhao, Falcke, Bower, Aitken, et al X-ray: Baganoff et al. 21, 23, Goldwurm et al. 23, Porquet et al. 23, models: Markoff, Falcke, Liu, Melia, Narayan, Quataert, Yuan et al Genzel et al. 23, Nature Ghez et al. 24, ApJ 61, L159, Eisenhauer et al. 25
68 Evidence for rotation of the black hole Genzel et al. 23, Nature 425, 934
69 Simultaneous X-/IRX /IR-Flares Eckart et al. 4, 5
70
71
72 overall SgrA* * spectral July 4 (2) July 4 (1) July 3 j RIAF + 1.5% p=3.5 power law energy distribution E(eV) E RIAF + SSC jet-disk XMM 2 ν L ν (3.8x1 33 erg/s) 1 1 SINFONI flares Jul/Aug4 Chandra.1 Chandra quiescent ν (Hz) Falcke et al. 1999, Zhao et al. 24, Markoff et al. 21, Genzel et al. 23, Ghez et al. 24,Eisenhauer et al. 25, Baganoff et al. 21, 23, Porquet et al. 23, Eckart et al. 24, 25, Yuan et al. 21, 23, 24, Liu et al. 24
73 Kormendy & Ho 21 Black hole demographics
74 ark central masses in external galaxies NGC 4258 M31 M =4x1 7 M ρ > M pc -3 M =3.6x1 7 M ρ > 1 12 M pc -3 Greenhill, Myoshi, Moran et al Bacon, Bender, Kormendy, Richstone, Tonry, van der Marel, et al
75 Dark central masses in external galaxies: H 2 O maser disk in NGC 4258 M =3.6x1 7 M ρ > 1 12 M pc -3 Greenhill, Herrnstein, Myoshi, Moran et al (e.g. Nature 373, 127)
76 Dark central masses in external galaxies: bulges and ellipticals M31 M =3x1 7 M M84 M =2x1 9 M Bacon, Bender, Bower, Dressler, Kormendy, Richstone, Tonry, van der Marel, et al
77 -ray spectroscopy: relativistic accretion disks XMM-Newton MCG Tanaka et al. 95, Nandra et al. 97, Ballantyne and Fabian 21, Wilms et al. 21, Lee et al. 2, Elvis 2, Fabian et al. 22
78 Relativistic accretion disks in external galaxies Fe KαK MCG (XMM Newton) 15 km/s Tanaka, Nandra et al Fabian et al. 22
79 NGC 4258 Black Holes in the Local Universe M =3.6x1 7 M M =4x1 7 M M31 (Andromeda) Miyoshi et al. 1995, Kormendy & Richstone 1995, Gebhardt et al. 2, Merritt und Ferrarese 2, Tremaine et al. 22, Bender et al. 22, 25
80 Black Holes & Galaxy Formation ROSAT/XMM/Chandra Quasar -density Cosmic star formation rate FORS/VLT M BH ~ a few 1 9 M at t~8 Myrs after Big Bang! Hasinger et al. 1999, 22, Steidel et al. 1999, Bender und FORS Team 22 Fan et al. 21, Becker et al. 22
81 ROSAT/XMM/Chandra Black Holes & Galaxy Formation Quasar -density FORS/VLT cosmic star formation rate M BH ~ a few 1 9 M at t~8 Myrs after Big Bang! redshift z Hasinger et al. 1999, 22, Steidel et al. 1999, Bender und FORS Team 22, Osmer 23, Fan et al. 22
82 ROSAT/XMM/Chandra Black Holes and Galaxy Formation Quasar -density FORS/VLT Cosmic Star formation rate Hasinger et al. 1999, 22, Steidel et al. 1999, Bender und FORS Team 22
83 Nearby Black Holes as Ashes of the QSO Era ρ ρ ε QSO dn( L, z) dt 1 = ( dz ( dl L) ) /( εc ) M Mpc dl dz ε bu lg e, early, theoretical = 2x1 M Mpc ρ 5 bu lg e 5 2 < ε accretion >= 5x1 5x1 x 6 3x1 ρ Gebhardt et al. 2 e.g. Soltan et al. 1982, Yu & Tremaine 22
84 Black Holes and Galaxy formation quasar Density cosmic star formation rate Magorrian et al. 1998, Kormendy and Ho 2, Gebhardt et al. 2, Merritt and Ferrarese 2, Hasinger et al. 1999, Steidel et al. 1999
85 NGC 624 Chandra Formation of Quasars Springel 21 Binary black hole: Komossa & Hasinger 23
86 The future interferometry: : relativistic regime submm VLBI: detection of event horizon simultaneous radio to γ-emission : accretion flow TeV emission: dark matter spike? z~1 QSOs and galaxies ESO-VLTI
87 the future 2 AU VLTI beam 1µas astrometry with PRIMA =3µas per orbit T~2 yrs R min ~2 AU (3 R s, V max ~.2 c ESO-VLT(I)
88 the future shadow of the Black Hole Falcke et al. 2 VLBI 2 AU VLTI beam 1µas astrometry with PRIMA =3µas per orbit T~2 yrs R min ~2 AU (3 R s, V max ~.2 c ESO-VLT(I)
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