Nuclear Star Clusters and Black Holes · Nuclear Star Clusters and Black Holes Anil Seth (10 min)...
Transcript of Nuclear Star Clusters and Black Holes · Nuclear Star Clusters and Black Holes Anil Seth (10 min)...
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HST im
age
of N
GC 3
621
Nuclear Star Clusters and Black Holes
Anil Seth (10 min) Harvard-Smithsonian Center for Astrophysics
Nadine Neumayer (10 min) European Southern Observatory
Collaborators: Michele Cappellari (Oxford), Nelson Caldwell (Harvard-Smithsonian CfA), Aaron Barth (UC Irvine), Jakob Walcher (ESTEC), Torsten Böker (ESTEC), Richard McDermid (Gemini), Bob Blum (NOAO), Victor Debattista (U. Central Lancashire), Markus Hartmann (U. Central Lancashire), Knut Olsen (NOAO), Nate Bastian (Cambridge IOA), Thomas Puzia (DAO), Hans-Walter Rix (MPIA), Andrew Stephens (Gemini)
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Nearby Nuclear Star Clusters
Seth+ 2008b, Seth+ 2010, Neumayer+, in prep
25 Mly
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Resolving Nuclear Star Clusters
HST Imaging
Optical Spectra (Magellan, MMT, VLT)
Adaptive Optics IFU spectra (Gemini, VLT)
1) Morphology
2) Stellar Populations
3) Kinematics
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The Formation of Nuclear Star Clusters
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V-‐I Color
Morphology In edge-on spirals: • Flattened clusters
aligned with galaxy disks.
• Bluer disks/rings near midplane
• Multiple pops/continuous SFH from spectra
Seth+ 2006
Central 40 pc of NGC4244
Evidence for episodic accretion
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Rotation Dominated
Seth+ 2008b
See also, Milky Way (Trippe+ 2008, Schoedel+ 2009)
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Episodic Disk Accretion
• Accretion of gas or stars from the galaxy into a disk
• Older stars get puffed up by accretion event
• Recurs ~100 Myr • Cluster or Gas
Accretion? See Markus Hartmann’s talk tomorrow!
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Evidence for Merger Accretion • NGC404 nearest S0 galaxy ~109 M. • Galaxy is old (>10 Gyr) (Williams+ 2010) • Nuclear star cluster has dominant ~1 Gyr old population
(50% of mass) • HI Gas in outskirts merger ~1 Gyr ago! (del Rio+ 2004)
Seth+ 2010
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Evidence for Merger Accretion
Seth+ 2010
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Two Pathways To Similar Objects
Episodic Disk Accretion vs. Merger Accretion
• Primary difference is the stellar population.
• Both rotate strongly.
• Scaling relations?
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Black Holes in Nuclear Star Clusters
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Data from: Böker+ 2002, Côté+ 2006, Carollo+ 1998-2002, Seth+ 2006, 2008a, Gültekin 2009
All (?) galaxies have BHs
Hard to Detect Black Holes
Most (~75%) galaxies have NSCs
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Gültekin+ 2009 Our Galaxy
Sample
(Bulge) Velocity Dispersion [km/sec]
Black Hole Mass
106
109
1010
60 500
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GALEX Thilker et al. 2010
Close look at NGC 404
Nearest S0 galaxy D=3Mpc, σ=35km/s
Some evidence for an accreting black hole:
✔ LINER like nucleus ✔ compact X-ray source ✔ High excitation lines in
Mid-IR ✔ variable UV emission ✔ compact dust emission
Ho+ 1997, Eracleous+ 2002, Satyapal+ 2004, Maoz+ 2005, Seth+ 2010
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Dynamical black hole detection
Ingredients:
1) Stellar Mass Profile • Luminosity Profile • Mass-to-light ratio
2) Dynamical Tracer
Seth+ 2010
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NGC404 - Stellar Kinematics
Seth+ 2010
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NGC404 - Stellar Kinematic Model
Jeans anisotropic model Fit MBH, βz, M/L MBH < 1×105 M (~ 0.5 ×105 M )
Seth+ 2010
Vrms=(Vrot2+σ2)½
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NGC404 - H2 Gas Kinematics
Seth+ 2010
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NGC404 – Gas Kinematic Model
MBH ~ (4.5±3)×105 M Degeneracy due to
vrot ~ √MBH × sin(i)
Inclination i~37°±10°
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NGC 3621 - Sd galaxy
Bulge-less spiral
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NGC 3621 / ESO
NGC 3621 - Sd galaxy
Bulge-less spiral hosts nuclear cluster… …plus detected AGN
– in MIR (Satyapal et al. 2007) – and X-rays (Gliozzi et al. 2009)
MBH > 2×104 M MBH < 3×106 M
SINFONI data resolve the cluster
Can dynamically detect MBH ~ 3×105 M
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(Gliozzi et al. 2009)
NGC 3621 - Sd galaxy
Bulge-less spiral hosts nuclear cluster… …plus detected AGN
– in MIR (Satyapal et al. 2007) – and X-rays (Gliozzi et al. 2009)
MBH > 2×104 M MBH < 3×106 M
SINFONI data resolve the cluster
Can dynamically detect MBH ~ 3×105 M
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Barth et al. 2009 Barth et al. 2009
NGC 3621 - Sd galaxy
Bulge-less spiral hosts nuclear cluster… …plus detected AGN
– in MIR (Satyapal et al. 2007) – and X-rays (Gliozzi et al. 2009)
MBH > 2×104 M MBH < 3×106 M
SINFONI data resolve the cluster
Can dynamically detect MBH ~ 3×105 M
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Ferrarese+ 2006
Nucl
ear
Clu
ster
or
Bla
ck H
ole
Mas
s [M
]
Galaxy/Bulge Mass [M]
NGC4
04
NGC 3621
• Probing below the mass of previously detected black holes.
• Nuclear star clusters more massive than black holes.
• What mass to plot on x-axis?
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Summary
• Nuclear star clusters are common
• They co-exist with black holes
• Mixed evidence for a black hole in NGC404
• Detection of a black hole in NGC3621
• More to come!