4 th MPIA Student Workshop – March 26, 2007 The nucleus of Centaurus A Almudena Prieto, Klaus Meisenheimer Michele Cappellari Paul van der Werf, Juha Reunanen, Tim de Zeeuw Nadine Neumayer, Hans-Walter Rix Ric Davies

4 th MPIA Student Workshop – March 26, 2007 Motivation ◊ Nearest elliptical with AGN and jet (1”~17pc) ◊ Ideal laboratory to test AGN models ◊ Evidence of recent merger (~0.5 Gyr ago) ◊ Binary black hole? ESO / WFI CTIO / Peng et al. 2002

4 th MPIA Student Workshop – March 26, 2007 Cen A on the M bh relations Tremaine et al. 2002Häring & Rix 2004Marconi et al M bh - σM bh -M bulge σ ~138 km/s ● Silge et al ● M sph ~6.5×10 10 M 

4 th MPIA Student Workshop – March 26, 2007 WFPC2 3.8’ 3.7kpc Closer look J-band FWHM = 0.10” 7” ~ 115pc K-band FWHM = 0.06” < 1pc! Core size: <1 pc FWHM

4 th MPIA Student Workshop – March 26, 2007 Stellar mass model K-band FWHM = 0.06” NACO + NICMOS + 2MASS Multi-Gaussian Expansion  stellar potential

4 th MPIA Student Workshop – March 26, 2007 λ [μm] Central kinematics Marconi et al [FeII] aperture: 86mas x 54mas

4 th MPIA Student Workshop – March 26, 2007 Central kinematics Marconi et al. 2001

4 th MPIA Student Workshop – March 26, 2007 The dynamical model ◊ Thin disk model ◊ Gas in hydrostatic equilibrium ◊ Potential from stars + black hole ◊ Three parameters: BH mass, two angles for disk: i, ζ

4 th MPIA Student Workshop – March 26, 2007 Best-fitting model Hot disk model M bh = (6.1± 0.8) x 10 7 M  i = 45° ζ = -27° Häring-Neumayer et al. 2006

4 th MPIA Student Workshop – March 26, 2007 IFU data – SINFONI/VLT K-band H-band

4 th MPIA Student Workshop – March 26, 2007 [FeII] λ=1.644μm

4 th MPIA Student Workshop – March 26, 2007 [SiVI] λ=1.964μm

4 th MPIA Student Workshop – March 26, 2007 Brγ λ=2.166μm

4 th MPIA Student Workshop – March 26, 2007 H 2 λ=2.121μm

4 th MPIA Student Workshop – March 26, 2007 Disk parameters - Kinemetry Using kinemetry routine by Krajnović et al. 2006

4 th MPIA Student Workshop – March 26, 2007 Warped disk structure

4 th MPIA Student Workshop – March 26, 2007 The dynamical model ◊ Tilted ring model ◊ Gas in hydrostatic equilibrium ◊ Potential from stars + black hole ◊ Two parameters: BH mass disk inclination angle

4 th MPIA Student Workshop – March 26, 2007 IFU data and model M bh = (7.0±1.5) × 10 7 M  = 27º±5º

4 th MPIA Student Workshop – March 26, 2007 Symmetrised data & model

4 th MPIA Student Workshop – March 26, 2007 No black hole? ruled out by over 5 σ!

4 th MPIA Student Workshop – March 26, 2007 Cen A on the M bh relations Tremaine et al. 2002Häring & Rix 2004Marconi et al M bh - σM bh -M bulge σ ~138 km/s M sph ~6.5×10 10 M  Silge et al ● ● ● ●

4 th MPIA Student Workshop – March 26, 2007 Stellar vs. gas motion

4 th MPIA Student Workshop – March 26, 2007 Summary ◊ high resolution gas and stellar kinematics ◊ counter-rotation ◊ thin, warped disk model ◊ Mbh = 7 x 10 7 M sun ◊ In agreement with M- σ