The nucleus of Centaurus A Nadine Neumayer HansWalter
![Central kinematics [Fe. II] λ [μm] aperture: 86 mas x 54 mas Marconi et](https://slidetodoc.com/presentation_image/8ffb508b8f0269d26039b79cf473141e/image-6.jpg "Central kinematics [Fe. II] λ [μm] aperture: 86 mas x 54 mas Marconi et")
![[Fe. II] 4 th MPIA Student Workshop – March 26, 2007 λ=1. 644μm](https://slidetodoc.com/presentation_image/8ffb508b8f0269d26039b79cf473141e/image-11.jpg "[Fe. II] 4 th MPIA Student Workshop – March 26, 2007 λ=1. 644μm")
![[Si. VI] 4 th MPIA Student Workshop – March 26, 2007 λ=1. 964μm](https://slidetodoc.com/presentation_image/8ffb508b8f0269d26039b79cf473141e/image-12.jpg "[Si. VI] 4 th MPIA Student Workshop – March 26, 2007 λ=1. 964μm")
- Slides: 23
The nucleus of Centaurus A Nadine Neumayer, Hans-Walter Rix Almudena Prieto, Klaus Meisenheimer Michele Cappellari Paul van der Werf, Juha Reunanen, Tim de Zeeuw Ric Davies 4 th MPIA Student Workshop – March 26, 2007
Motivation ◊ Nearest elliptical with AGN and jet (1”~17 pc) ◊ Ideal laboratory to test AGN models ◊ Evidence of recent merger (~0. 5 Gyr ago) ◊ Binary black hole? WFI CTIO / Peng ESO et al. /2002 4 th MPIA Student Workshop – March 26, 2007
Cen A on the Mbh relations Mbh - σ Mbh-Mbulge ● ● • • • σ ~138 km/s Tremaine et al. 2002 Silge et al. 2005 4 th MPIA Student Workshop – March 26, 2007 Msph~6. 5× 1010 M Marconi et al. 2001 Häring & Rix 2004
J-band Closer look WFPC 2 FWHM = 0. 10” 7” ~ 115 pc < 1 pc! 3. 8’ 3. 7 kpc Core size: <1 pc FWHM 4 th MPIA Student Workshop – March 26, 2007 K-band FWHM = 0. 06”
Stellar mass model Multi-Gaussian Expansion NACO + NICMOS + 2 MASS K-band FWHM = 0. 06” 4 th MPIA Student Workshop – March 26, 2007 stellar potential
Central kinematics [Fe. II] λ [μm] aperture: 86 mas x 54 mas Marconi et al. 2001 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 Mbh = (6. 1± 0. 8) x 107 M i = 45° ζ = -27° Häring-Neumayer et al. 2006 4 th MPIA Student Workshop – March 26, 2007
IFU data – SINFONI/VLT H-band K-band 4 th MPIA Student Workshop – March 26, 2007
[Fe. II] 4 th MPIA Student Workshop – March 26, 2007 λ=1. 644μm
[Si. VI] 4 th MPIA Student Workshop – March 26, 2007 λ=1. 964μm
Brγ 4 th MPIA Student Workshop – March 26, 2007 λ=2. 166μm
H 2 4 th MPIA Student Workshop – March 26, 2007 λ=2. 121μm
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 Mbh= (7. 0± 1. 5) × 107 M <i> = 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 5σ! 4 th MPIA Student Workshop – March 26, 2007
Cen A on the Mbh relations Mbh - σ Mbh-Mbulge ● ● • ● • σ ~138 km/s Tremaine et al. 2002 Silge et al. 2005 4 th MPIA Student Workshop – March 26, 2007 Msph~6. 5× 1010 M Marconi et al. 2001 Häring & Rix 2004
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 107 Msun ◊ In agreement with M-σ 4 th MPIA Student Workshop – March 26, 2007