Black Holes in Giant Elliptical Galaxies
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- Abigail Stafford
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1 Gemini Observatory/AURA artwork by Lynette Cook Black Holes in Giant Elliptical Galaxies Chung-Pei Ma (UC Berkeley) Nicholas McConnell (UCB) Shelley Wright (UToronto) James Graham (UCB) Karl Gebhardt (UTexas) Tod Lauer (NOAO) Jeremy Murphy (UTexas) Doug Richstone (UMich)
2 Simulations of Binary Major Mergers! Scaling relations are a function of energy and angular momentum of merger orbit.! Bulge loses less energy to dark matter halo on a more radial orbit! R! L "! L! " # (M BH! " # ) x x Boylan-Kolchin et al (2006)
3 Local Black Holes Direct Mass Measurements Major updates since Gultekin 09 compilation: Text 18 new masses 17 updated masses different slopes M BH σ 4.12±0.38 Gultekin et al (2009) Ferrarese & Merritt (2000) Gebhardt et al (2000)
4 High-z QSOs?? Text
5 Why hadn t the Biggest Galaxies been measured? Challenge 1 Detecting black hole s influence Massive galaxies are rare. Must go beyond Virgo cluster. (Sauron/ATLAS probes < 40 Mpc) Black hole s gravity dominates within the sphere of influence r = GM BH σ 2 50 pc M BH 10 9 M 0.1 arcsec at 100 Mpc 300 km s 1 σ 2
6 Challenge 2 Massive galaxies have shallow inner stellar profile Faber et al (1997)
7 Integral Field Spectrographs Keck OSIRIS (0.05 to 0.7 arcsec) Gemini GMOS-N & S (0.2 to 3.8 arcsec) + McDonald Mitchell/VIRUS-P (4 to 35 arcsec)
8 Ongoing Survey Published BCG D σ Mv MBH NGC 6086 (A2162) 139 Mpc 318 km/s e9 ApJ 2011 NGC 3842 (A1367) 98 Mpc 270 km/s e9 Nature 2011 NGC 4889 (Coma) 103 Mpc 347 km/s e10 Nature 2011 NGC 7768 (A2666) 120 Mpc 313 km/s e9 ApJ 2012 NGC 2832 (A0779) 97 Mpc 334 km/s < 9.0e9 ApJ 2012 Analyzing NGC 4552 (M89) 15 Mpc 254 km/s GMOS, VP NGC 4365 (in Virgo) 20 Mpc 256 km/s GMOS, VP NGC 4696 (A3526) 40 Mpc 254 km/s GMOS-S NGC Mpc 349 km/s GMOS-S NGC 910 (A0347) 81 Mpc 249 km/s OSIRIS, NIFS, GMOS,VP NGC 7578 (A2572) 172 Mpc 214 km/s OSIRIS, VP U9767 (A2040) 176 Mpc 223 km/s OSIRIS, GMOS, VP NGC 6166 (A2199) 129 Mpc 307 km/s GMOS 10 more scheduled (Gemini)
9 HST Photometry Major challenge: Shallow inner stellar profile McConnell et al (2011,2012)
10 Continuum - Divided Flux N3842 N4889 Template star ! rest (nm) GMOS Spectra (r<0.25 arcsec) CaII triplet Continuum - Divided Flux N3842 Template star ! rest (nm) OSIRIS Spectra CO band heads McConnell et al (2011)
11 VIRUS-P Spectra McConnell et al (2012)
12 2-D Map of LOS Velocity Dispersion 3 2 a NGC b NGC 4889 Y (arc sec) E N y (arc sec) N E X (arc sec) x (arc sec) ! (km/s)! (km/s) McConnell et al (2011)
13 Stellar Orbit Modeling 1. Assume a black hole mass MBH and stellar mass-to-light ratio (ϒ=M*/L) 2. Generate stellar orbits in gravitational potential ρ = MBH δ(r) + ϒ ρ* + ρdm 3. For a MBH and ϒ, determine the combination of orbits that (a) reproduces the observed light profile ρ* (b) best fits the LOS velocity distributions derived from spectra at multiple spatial points 4. Compute ϰ 2 for the best-fit orbits 5+. Repeat for different MBH and M*/L e.g. Schwarzschild (1979); Gebhardt et al (2003) N. Minimize ϰ 2 to obtain best-fit MBH and M*/L
14 NGC3842! 2 -! 2 min M BH (10 9 M Sun ) 10 5 M BH =(9.7 ± 2.5) 10 9 M M /L R =(5.2 ± 0.8) M /L M * /L R ( M Sun /L Sun )
15 M BH σ Relation All 65 galaxies M BH σ 5.12±0.36 ( 0 =0.43) 45 early-type galaxies M BH σ 4.53±0.40 ( 0 =0.38) 20 late-type galaxies M BH σ 4.58±1.25 ( 0 =0.47) McConnell et al (2011)
16 M BH σ Relation M BH L v Relation M BH σ 5.12±0.36 M BH L 1.16±0.14 McConnell et al (2011)
17 Power-law vs Core Early-Type McConnell & Ma (2012, in prep)
18 Scatter in Mbh does not decrease at high end McConnell & Ma (2012, in prep)
19 Caveats on Velocity Dispersions Exclude sphere of influence? Our value G 09 Lauer 07 Hyperleda (km/s) M M NGC IC Our published sample NGC n/a NGC n/a NGC n/a NGC n/a n/a 313 NGC n/a
20 Ongoing Survey Published BCG D σ Mv MBH NGC 6086 (A2162) 139 Mpc 318 km/s e9 ApJ 2011 NGC 3842 (A1367) 98 Mpc 270 km/s e9 Nature 2011 NGC 4889 (Coma) 103 Mpc 347 km/s e10 Nature 2011 NGC 7768 (A2666) 120 Mpc 313 km/s e9 ApJ 2012 NGC 2832 (A0779) 97 Mpc 334 km/s < 9.0e9 ApJ 2012 Analyzing NGC 4552 (M89) 15 Mpc 254 km/s GMOS, VP NGC 4365 (in Virgo) 20 Mpc 256 km/s GMOS, VP NGC 4696 (A3526) 40 Mpc 254 km/s GMOS-S NGC Mpc 349 km/s GMOS-S NGC 910 (A0347) 81 Mpc 249 km/s OSIRIS, NIFS, GMOS,VP NGC 7578 (A2572) 172 Mpc 214 km/s OSIRIS, VP U9767 (A2040) 176 Mpc 223 km/s OSIRIS, GMOS, VP NGC 6166 (A2199) 129 Mpc 307 km/s GMOS
21 Ongoing Gemini GMOS Survey Incoming Data 2012A IC 4329 (A3574) D 57 Mpc σ 275 km/s Mv MBH (from σ or L) 9.0 / 9.7e9 NGC Mpc 389 km/s / 8.5e9 2012B NGC Mpc 291 km/s / 9.4e9 NGC Mpc 321 km/s / 9.2e9 NGC Mpc 414 km/s / 8.9e9 IC 1633 (A2877) 98 Mpc 355 km/s / 9.7e9 IC 4931 (A3656) 83 Mpc 273 km/s / 9.5e9 NGC Mpc 279 km/s / 9.5e9 NGC Mpc 291 km/s / 9.4e9 NGC Mpc 246 km/s / 9.5e9
22 Summary Major recent update to Gultekin 09 compilation. See BH website. Gemini + IFU + AO make it feasible to extract MBH and stellar populations at centers of nearby massive galaxies. BCGs can host massive black holes >~ 10 billion solar masses. NGC 3842 and 4889 are new record holders. Remnants of massive high-z QSOs? Expect 10+ more new measurements Time to move beyond a single global fit to scaling relations of MBH with galaxy properties. e.g. Late vs early type Core vs power-law MBH - σ relation. Which σ? Modelers pay attention to σ. Scatter does not decrease at high mass - some models ruled out. BIG thanks to Gemini staff and TAC!
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