Bulletin on the Biggest, Baddest Black Hole on the Block

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1 Bulletin on the Biggest, Baddest Black Hole on the Block (SgrA* that is) Scott C. Noble UIUC CTA Lunch Seminar September 21, 2005

2 Outline: Introduction: How Big and Bad is it? M, R, tdyn, d, etc. What can SgrA* do for us? Observations: Models: X rays, IR, Radio and beyond! Thin disk, 2 T disks, ADAF, Jet, CDAF, ADIOS,... Future Methods and Trends Conclusion Alexander 2005 astro ph/ SgrA* KITP conference:

3 It' s a Black Hole, ok?

4 It' s a Black Hole, ok? Very few possible compact sources Who' s seen a scalar boson anyway? Spectra fits well with jet & accretion models Some spectra features seem to indicate variability < 10 Rs Dark star clusters are short lived

5 How Big is it? Ghez et al (UCLA) New Keck diffraction limited observation, adaptive optics Simultaneous 6 orbit fit MSgrA*= 3.7 +/ 0.2 x106 MSun Genzel et al., Nature, 2003 Eisenhauer et al (MPE/UCB) ESO/VLT, adaptive optics MSgrA*= 3.6 +/ 0.3 x106 Msun Ro = 7.6 +/ 0.3 kpc Biggest black hole on the sky!!! 12 7 R SgrA = 1 10 cm = Ghez et al pc = =0.07 AU =

6 How Bad is it? Only sources where Sphere of Influence is resolved. SgrA* shows other spectral similarities to LLAGN Solid: Ferrarese & Ford (2005) Dotted: Tremaine et al. (2002)

7 IR Observations Genzel et al, Nature (2003) VLT

8 IR Observations 30 f u n d a m e n t a l d y n a m ic a l f r e o r b it a l p e r io d a t la s t s ta b le o r b it fo r M = x 1 0 ls to ( m in ) 20 T M sun,a = 10 ν 3 o r b it a l 1.0 a / ( G M et / c ) al, Nature (2003) VLT 4 Genzel a =0.52 (±0.1,±0.07,±0.14) ν e p ic y c le n= g ac os

9 X Ray Observations NASA/UMass/D.Wang et al. (Chandra) 120x48 arcmin or 900x400 light year

10 X Ray Observations 1.23 arcmin 8.4 arcmin NASA/CXC/MIT/ F.K. Baganoff et al. 1.4 arcsec

11 X Ray and Bondi Modelling it as kt~1.3kev hot, optically thin emission: n e = 30 cm 3 2 s c = k T / m = 550 km / s = v wind 2 s R B = 2 G M SgrA /c = 0.1 pc = 2.7 arcsec. R B = 2 R X rays

12 X Ray Variability 45x,4hr 25x,1hr 12x,1.5hr 13x,0.5hr 1hr variability > ~20 Rs Baganoff et al. ( )

13 Radio (VLBA) Position best determined in radio (best res. on the planet) Visible Size 1/ν Optically thin at ~submm λ > horizon images

14 Composite Spectrum

15 The Luminousity Problem 36 L SgrA = 10 erg/s 38 L Edd = 4 c G M e / T = M / M sun erg/s 44 L Edd M Sgr = erg/s 8 L Sgr =10 L Edd 2 B 5 M X rays = 4 R c s = 4 10 M sun / yr 2 43 L = c M X rays = erg /s

16 The Luminousity Problem 6 L SgrA = 5 10 L thin Radio Linear Polarization contraints: 3 3 M =10 M X rays =10 thin

17 The Luminousity Problem 6 L SgrA = 5 10 L thin Radio Linear Polarization contraints: 3 3 M =10 M X rays =10 thin No thermal thin disk emission Bad!

18 Plain BB Bondi Spectrum (more B' s!) Narayan astro ph/

19 Realistic Bondi Spectrum Including Synch., Bremsstrahlung (+IC) At low ρ, e' s & ions decouple since t Coulomb t infall IC Synch. Shapiro, Lightman, & Eardley (1976) Brem. Narayan astro ph/

20 RIAF' s (Radiatively Inefficient Accretion Flows) ADAF's (Advection Dominated Accretion Flows): Narayan & Yi (1994 5), Yuan et al. (2003 4) At least I didn' t name them Type II accretion flows!, Narayan, KITP SgrA* Conf Q diss Q rad. r 2 T flows, ala Shapiro et al., advection stabilizes Thick disks, ~spherical Convectively unstable 3/ 2

21 CDAF' s & ADIOS' s r 3/2 s M in = M out R in / R out s ADIOS (Advection Dominated Inflow/Outflow Sol's) 0 s 1 Blandford & Begelman (1999) Much of the energy is blown away in a wind CDAF (Convection Dominated Accretion Flows) s = 1 Quataert & Gruzinov (2000) Ang. Mom. Transported inward Energy Transported outward Weakest accretion of the RIAF' s

22 RIAF Simulations Igumenshchev, Narayan, Abramowicz (2003) 3D, MHD, Paczynski & Wiita Pot., Viscous, Resistive Toroidal B fed in from outer boundary Similar ρ 1/R close to analytic CDAF

23 RIAF Simulations Goldston, Quataert, Igumenshchev (2005) 3D RIAF Sim. as before Te = a Ttot ne ~ Maxwellian + PLT Opt. thin at 450 GHz torbit timescale for opt. thin emission > torbit timescale for opt. thick emission

24 Jet Models Vr Falcke et al (1995 now) Blandford & Konigl (1979) Free expanding, rel. jet Conical confinement due to rel. vel. Jet fed at constant rate Vz φ vz = c, v r = s s c =1/ M =v r /v z small M jet = v A = m p n r c r 2 E B, jet = B v A = B r c r 2 2 n r 1/r B r 1/r 2

25 Jet Models (Synchrotron Absorption) Photons are free to go past the τ = 1 surface sync B =1 φ 1 Get a flat spectrum B r r 1 r sync 3 3 r 1 r =1

26 Composite Spectrum (comparison) RIAF' s have problem with var. of brem. since Rbrem ~ 105 Rs Instead, add PL ne gives hard IC/SSC photons Solves Radio under lum. Modern RIAF' s have many parameters, need better constraints: simult. wide freq. survey, submm VLBI Jets lack a mechanism, no launching mechanism Reliant on a disk model of some type Can it predict X ray flare state? SgrA* may have been more active in the past...?

27 Conclusion? Not until submm VLBI and see or

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