The Formation of Galaxy Nuclei
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1 The Formation of Galaxy Nuclei Anil Seth (Harvard-Smithsonian CfA University of Utah) Collaborators: Nadine Neumayer (ESO) Michele Cappellari (Oxford) Nelson Caldwell (Harvard-Smithsonian CfA), Bob Blum (NOAO), Victor Debattista (U. Central Lancashire), Markus Hartmann (U. Central Lancashire), Knut Olsen (NOAO), Nate Bastian (Cambridge IOA), Richard McDermid (Gemini), Thomas Puzia (DAO), Andrew Stephens (Gemini) Marcel Agüeros (Columbia), Duane Lee (Columbia) Hubble Space Telescope image of NGC 3621 Anil Seth, Ciera, Sept. 2011
2 Anil Seth, Aug. 2011
3 Galaxy Anatomy Elliptical Spiral Nucleus disk Black Hole bulge Nuclear Star Cluster 10 kpc 30 kly Msun 5 pc 15 ly 10 7 Msun 10 kpc 30 kly Msun Anil Seth, Missouri, Mar. 2011
4 NGC 4244 Anil Seth, UMass, Oct Ciera, Sept.
5 All galaxies have black holes! 75% of galaxies have nuclear star clusters. Black holes are hard to find! Elliptical/ Bulge Disk Data from: Böker+ 2002, Côté+ 2006, Carollo Seth+ 2006, 2008a, Gültekin 2009 Anil Seth, Ciera, Sept. 2011
6 NSCs & BHs commonly coexist Kewley 2006 classification Star-forming galaxies Composite/ Transition Active Galactic Nuclei (AGN) >10% of NSCs have AGN-type spectra suggesting black hole accretion Seth+ 2008a Anil Seth, Ciera, Sept. 2011
7 Anil Seth, Ciera, Sept A surprisingly simple relationship Nuclear Cluster or Black Hole Mass [Msol] Nuclear Clusters Black Holes Galaxy Mass [Msol] Ferrarese (for Elliptical Galaxies) NSC and black hole masses correlated with galaxy masses and bulge velocity dispersions. (Wehner & Harris 2006, Rossa+ 2006, Ferrarese+ 2006, Graham & Driver, 2007 Erwin & Gadotti 2010) Suggests links between galaxies, nuclear star clusters and black holes
8 Anil Seth, Ciera, Sept Resolving Nearby Nuclear Star Clusters 1) Morphology Hubble Space Telescope Imaging 2) Stellar Ages Text Optical Spectra (Magellan, MMT, VLT) 3) Kinematics Adaptive optics infrared spectra (Gemini, VLT)
9 Anil Seth, Ciera, Sept Nearby Nuclear Star Cluster Survey Primary Collaborators: Nadine Neumayer (ESO) Michele Cappellari (Oxford) Seth+ 2008b, Seth+ 2010, Seth 2010, Neumayer+ in prep
10 Anil Seth, Ciera, Sept Survey Goals Study the formation of nuclear star clusters Find and measure the mass of the smallest central black holes
11 Anil Seth, Ciera, Sept The BH - NSC connection Both are fed from the same events? (e.g. Hopkins & Quataert 2010a,b) NSC formation results in BH formation? (e.g. Portegies Zwart 2004, Vespirini 2010, Davies+ 2011) Need to study systems with nuclear star clusters and black holes
12 Anil Seth, Ciera, Sept Black Hole Mass 10 6 Nearby Nuclear Star Velocity Dispersion (σ; ~Galaxy Mass) Gultekin Cluster Sample
13 Anil Seth, Ciera, Sept The number of low mass galaxies with black holes is sensitive to how black holes formed in the early universe Occupation Fraction 0 High Mass Seed Low Mass Seed Velocity Dispersion (σ; ~Galaxy Mass) Volonteri+ 2008
14 NGC404: (D~3 Mpc, σ=35 km/s) Nearest S0-type galaxy Mstellar ~10 9 M Strong evidence for black hole accretion: variable UV emission, compact dust & hard X- ray emission (Maoz+ 2005, Seth+ 2010, Binder+ 2011) GALEX UV Image of NGC 404 Anil Seth, Aug. 2011
15 Dynamical detection of black holes (NGC404) Ingredients: Surface Brightness Nuclear Star Cluster Text 1)Stellar Mass Profile Luminosity Profile fit a Mass-to-Light ratio for stellar light 2)Dynamical Tracer Seth Anil Seth, Ciera, Sept. 2011
16 Anil Seth, Missouri, Mar Anil Seth, UMass, Oct. 2010
17 Anil Seth, Ciera, Sept Stars H 2 Emission
18 Anil Seth, Ciera, Sept Limits on the BH mass: Stars Model using Jeans Eq. (Cappellari 2008) Fit M BH, anistropy & mass-to-light ratio M BH < 1x10 5 M at 3σ (~0.5x10 5 M ) 10 6 Msol BH model No BH model Data Vrms=(V 2 +σ 2 ) ½
19 Anil Seth, Ciera, Sept Limits on the BH mass: H 2 Gas Data require two thin disks Fit inner inclination, and M BH Best fit 4.5±3x10 5 M (3σ) Data Model Resid
20 Anil Seth, Ciera, UMass, Sept. Oct NGC 3621, Sd galaxy [NeV] lines detected (Satyapal+ 2007) Integrated dispersion of 43 km/sec, M BH < 3x10 6 M (Barth+ 2009) X-ray source suggests M BH > 10 3 M (Gliozzi+ 2009)
21 NGC 3621 best fit BH mass is 6.5x10 5 M Neumayer+ in prep Anil Seth, Aug. 2011
22 Anil Seth, Ciera, Sept Scaling Relations Nuclear Cluster or Black Hole Mass Nuclear Clusters Bulgeless Galaxies Black Holes Probing below the mass of previously detected black holes. Dynamical NSC masses What galaxy components are correlated? More to come! Ferrarese Galaxy OR Bulge Mass
23 Anil Seth, Ciera, Sept Occupation Fraction 0 High Mass Seed High Mass Seed Low Mass Seed Low Mass Seed Velocity Dispersion / Galaxy Mass Volonteri+ 2008
24 The Future is Bright Low mass galaxies with nuclear star clusters are abundant in the nearby universe! Future adaptive optics technology will enable resolution of nuclear star clusters and low mass black holes in ~150 lower mass systems Large Synoptic Survey Telescope will enable detection of low-mass black holes via tidal disruption of stars and variability Anil Seth, Ciera, Sept. 2011
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