1 / 23

The nucleus of Centaurus A

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. Motivation. Nearest elliptical with AGN and jet (1”~17pc) Ideal laboratory to test AGN models

colleen-murphy
Download Presentation

The nucleus of Centaurus A

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 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

  2. 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

  3. ● ● Cen A on the Mbh relations Mbh - σ Mbh-Mbulge • • • Msph~6.5×1010 M σ ~138 km/s Tremaine et al. 2002 Silge et al. 2005 Marconi et al. 2001 Häring & Rix 2004

  4. J-band FWHM = 0.10” WFPC2 7” ~ 115pc 3.8’ 3.7kpc Closer look < 1pc! K-band FWHM = 0.06” Core size: <1 pc FWHM

  5. Stellar mass model Multi-Gaussian Expansion NACO + NICMOS + 2MASS K-band FWHM = 0.06”  stellar potential

  6. [FeII] λ [μm] Central kinematics aperture: 86mas x 54mas Marconi et al. 2001

  7. Central kinematics Marconi et al. 2001

  8. 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

  9. Best-fitting model Hot disk model Mbh = (6.1± 0.8) x 107 M i = 45° ζ = -27° Häring-Neumayer et al. 2006

  10. IFU data – SINFONI/VLT H-band K-band

  11. [FeII] λ=1.644μm

  12. [SiVI] λ=1.964μm

  13. Brγλ=2.166μm

  14. H2λ=2.121μm

  15. Disk parameters - Kinemetry Using kinemetry routine by Krajnović et al. 2006

  16. Warped disk structure

  17. The dynamical model • Tilted ring model • Gas in hydrostatic equilibrium • Potential from stars + black hole • Two parameters: • BH mass • disk inclination angle

  18. IFU data and model Mbh= (7.0±1.5) × 107 M <i> = 27º±5º

  19. Symmetrised data & model

  20. No black hole? ruled out by over 5σ!

  21. ● ● ● ● Cen A on the Mbh relations Mbh - σ Mbh-Mbulge • • • Msph~6.5×1010 M σ ~138 km/s Tremaine et al. 2002 Silge et al. 2005 Marconi et al. 2001 Häring & Rix 2004

  22. Stellar vs. gas motion

  23. Summary • high resolution gas and stellar kinematics • counter-rotation • thin, warped disk model • Mbh = 7 x 107 Msun • In agreement with M-σ

More Related