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Black Hole

Lensing of space time around a black hole. At Oxford we study black holes observationally and theoretically on all size and time scales - it is some of our core work.

Credit: ALAIN RIAZUELO, IAP/UPMC/CNRS. CLICK HERE TO VIEW MORE IMAGES.

Prof. Niranjan Thatte

Professor of Astrophysics

Research theme

  • Astronomy and astrophysics
  • Instrumentation
  • Exoplanets and planetary physics

Sub department

  • Astrophysics

Research groups

  • Astronomical instrumentation
  • Exoplanets and Stellar Physics
  • Galaxy formation and evolution
  • Extremely Large Telescope
Niranjan.Thatte@physics.ox.ac.uk
Telephone: 01865 (2)73412
Denys Wilkinson Building, room 709
  • About
  • Teaching
  • Publications

The dark mass concentration in the central parsec of the milky way

Astrophysical Journal 472:1 PART I (1996) 153-172

Authors:

R Genzel, N Thatte, A Krabbe, H Kroker, LE Tacconi-Garman

Abstract:

We report ∼1″ resolution K-band (2 μm) imaging spectroscopy of the central parsec of our Galaxy. The derived radial velocities for 223 early- and late-type stars probe the nuclear mass distribution to spatial scales of 0.1 pc. We find a statistically very significant increase of projected stellar velocity dispersion from about 55 km s-1 at p ∼ 5 pc to 180 km s-1 at p ∼ 0.1 pc. The stars are also rotating about the dynamic center. The late-type stars follow general Galactic rotation, while the early-type stars show counter-rotation. Fitting simultaneously the observed projected surface densities and velocity dispersions, we derive the intrinsic volume densities and radial velocity dispersions as a function of distance from the dynamic center for both types of stars. We then derive the mass distribution between 0.1 and 5 pc from the Jeans equation assuming an isotropic velocity field. Our analysis requires a compact central dark mass of 2.5-3.2 × 106 M⊙, at 6-8 σ significance. The dark mass has a density of 109 M⊙ pc-3 or greater and a mass to 2 μm luminosity of ≥ 100. The increase in mass-to-luminosity ratio can be reduced but not eliminated even if extreme anisotropic velocity destributions are considered. The dark mass cannot be a cluster of solar mass remnants (such as neutron stars). It is either a compact cluster of 10-20 M⊙ black holes or a single massive black hole. © 1996. The American Astronomical Society. All rights reserved.
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NIR Imaging Spectroscopy of F10214: Evidence for a Starburst Around an AGN at Z = 2.284

Chapter in Spiral Galaxies in the Near-IR, Springer Nature (1996) 336-338

Authors:

H Kroker, R Genzel, A Krabbe, LE Tacconi-Garman, M Tecza, N Thatte
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Near IR and mm Imaging Spectroscopy of the Nuclear Region of NGC 1068

Chapter in Spiral Galaxies in the Near-IR, Springer Nature (1996) 333-335

Authors:

N Thatte, L Tacconi, H Kroker, A Krabbe, LE Tacconi-Garman, R Genzel
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Near infrared imaging spectroscopy of cD galaxy NGC1275

ASTR SOC P 98 (1996) 515-516

Authors:

BJ Sams, R Genzel, A Krabbe, N Thatte, F Prada
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Near-IR imaging spectroscopy of CD galaxy NGC1275

IAU SYMP (1996) 440-440

Authors:

BJ Sams, R Genzel, A Krabbe, N Thatte, H Kroker
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