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Title:
Spectroscopy of luminous infrared galaxies at 2 microns: 1. The ultraluminous galaxies (LIR approximately greater than 10 12 solar luminosity)
Authors:
Goldader, Jeffrey D.; Joseph, R. D.; Doyon, Rene; Sanders, D. B.
Affiliation:
AA(University of Hawaii, Honolulu, Hawaii, US), AB(University of Hawaii, Honolulu, Hawaii, US), AC(Universite de Montreal, Montreal, Quebec, Canada), AD(Universite de Montreal, Montreal, Quebec, Canada)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 444, no. 1, p. 97-112 (ApJ Homepage)
Publication Date:
05/1995
Category:
Astronomy
Origin:
STI
NASA/STI Keywords:
Astronomical Spectroscopy, Extremely High Frequencies, Galaxies, Infrared Astronomy, Infrared Spectroscopy, Stellar Luminosity, Active Galactic Nuclei, Emission Spectra, Far Infrared Radiation, Hydrogen, Star Formation, Starburst Galaxies
DOI:
10.1086/175585
Bibliographic Code:
1995ApJ...444...97G

Abstract

We present high-quality spectra covering the K window at a resolving power of 340 for a sample of 13 ultraluminous (LIR approximately greater than 1012 solar luminosity) infrared-selected galaxies, and line fluxes for a comparison sample of 24 lower luminosity galaxies. The 2 micrometers spectra of 10 of the ultraluminous galaxies are characterized by emission and absorption features commonly associated with stars and star formation; two others have the red power-law spectra and Br gamma line widths of Seyfert 1 galaxies; the final galaxy has strong emission from hot dust. We have found no broad-line active nuclei not already known from optical observations, despite the fact that the extinction at 2 micrometers is 1/10 that at optical wavelengths; any putative Seyfert 1 nuclei must be deeply buried. Powerful continua and emission lines from H2 and Br gamma are detected in all the ultraluminous galaxies. Comparing the H2 1-0 S(1), Br gamma, and 2 micrometers and far-infrared luminosities to those of the lower luminosity galaxies yields several major results. First, the dereddened Br gamma emission, relative to the far-infrared luminosity is significantly depressed in the ultraluminous sample, when compared to the lower luminosity galaxies. Five of the ultraluminous galaxies have LBr gammaLIR ratios lower than for any of the comparison objects. Second, the H2 1-0 S(1) luminosity is also responsible, directly or indirectly, for producing the excited H2, and that the H2 apparently comes from optically thin regions in both classes of objects. Third, eight of the 13 ultraluminous systems have lower 2 micrometers/far-infrared luminosity ratios than any of the lower luminosity galaxies, and five of these are the galaxies also deficient in Br gamma. These three findings may be understood if the the H2, Br gamma, and 2 mircometers continua in the ultraluminous galaxies arise from spatially distinct regions, with the continuum and Br gamma largely coming from volumes optically thick even at 2 micrometers, and obscured in such a fashion that the extinctions measured using optical spectroscopy do not properly measure the true optical depths. If this is the case, then even near-infrared spectroscopy may be unable to exclude the presence of undetected powerful active galactive nuclei in the ultraluminous galaxies.

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