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Astron. Astrophys. 354, 439-452 (2000)

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Near infrared imaging spectroscopy of NGC 1275

A. Krabbe 1,2, B.J. SamsIII 2, R. Genzel 2, N. Thatte 2 and F. Prada 3

1 Deutsches Zentrum für Luft- und Raumfahrt, Institut für Weltraumsensorik und Planetenerkundung, Rutherfordstrasse 2, 12489 Berlin-Adlershof, Germany
2 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany
3 Centro Astronomico Hispano-Aleman, Almeria, Spain

Received 6 July 1999 / Accepted 9 December 1999


We present H and K band imaging spectroscopy of the core regions of the cD/AGN galaxy NGC 1275. The spectra, including lines from H2, H, 12CO bandheads, [Fe II], and [Fe III], are exploited to constrain the star formation and excitation mechanisms in the galaxy's nucleus. The near-infrared properties can largely be accounted for by ionized gas in the NLR, dense molecular gas, and hot dust concentrated near the active nucleus of NGC 1275. The strong and compact H2 emission is mostly from circumnuclear gas excited by the AGN and not from the cooling flow. The extended emission of late-type stars is diluted in the center by the thermal emission of hot dust. The line ratios [Fe II]/Br[FORMULA], as well as [Fe II]/H2 can be explained with X-ray excitation from the central AGN.

Key words: instrumentation: spectrographs – galaxies: active – galaxies: cooling flows – galaxies: individual: NGC 1275 – infrared: galaxies – infrared: ISM: lines and bands

Send offprint requests to: A. Krabbe (krabbe@dlr.de)

© European Southern Observatory (ESO) 2000

Online publication: February 9, 2000