Prof. Niranjan Thatte: Publications

Near-IR imaging spectroscopy of CD galaxy NGC1275

IAU SYMP (1996) 440-440

Authors:

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

Observational Evidence for a Compact Dark Mass at the Galactic Center

Chapter in Spiral Galaxies in the Near-IR, Springer Nature (1996) 117-123

Authors:

A Eckart, R Genzel, A Krabbe, R Hofmann, LE Tacconi-Garman, H Kroker, N Thatte, L Weitzel

The nature of nuclear starbursts: M82

Chapter in Spiral Galaxies in the Near-IR, Springer Nature (1996) 328-330

Authors:

NM Förster, T Böker, A Krabbe, N Thatte, H Kroker, R Genzel

The stellar cluster at the center of the Galaxy

ASTR SOC P 98 (1996) 386-387

Authors:

A Eckart, R Genzel, A Krabbe, R Hofmann, LE TacconiGarman, H Kroker, N Thatte

The nuclear cluster of the milky way: Star formation and velocity dispersion in the central 0.5 parsec

Astrophysical Journal 447:2 (1995) L95-L99

Authors:

A Krabbe, R Genzel, A Eckart, F Najarro, D Lutz, M Cameron, H Kroker, LE Tacconi-Garman, N Thatte, L Weitzel, S Drapatz, T Geballe, A Sternberg, R Kudritzki

Abstract:

We report the first results of an extensive new study of the Galactic center stellar cluster. The central parsec is powered by a cluster of about two dozen luminous and helium-rich blue supergiants/Wolf-Rayet stars (Teff i 20,000-30,000 K) with ZAMS masses up to -100 MQ. The most likely scenario for the formation of the massive stars is a small star formation burst between 3 X 106 and 7 X 106 years ago. In this scenario the Galactic center is presently in a short-lived, post-main-sequence “wind phase.” In addition, there is evidence for another star formation event about 108 years ago, as well as for recently formed massive stars that may have been transported into the central core along with orbiting gas streamers. The radial velocity dispersion of 35 early- and late-type stars with distances of 1"-12" from Sgr A* is 154 ± 19 km s-1. Our new results strongly favor the existence of a central dark mass of -3 X 106 M⊙ (density > 108.5 M⊙ pc-3, M/L > 10 M⊙/L⊙) within 0.14 pc of the dynamic center. © 1995 The American Astronomical Society.

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