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Title:
Submillimeter spectrum and dust mass of the primeval galaxy IRAS 10214 + 4724
Authors:
Downes, D.; Radford, J. E.; Greve, A.; Thum, C.; Solomon, P. M.; Wink, J. E.
Affiliation:
AA(Inst. de Radioastronomie Millimetrique, Saint-Martin-d'Heres, France), AB(Inst. de Radioastronomie Millimetrique, Saint-Martin-d'Heres, France), AC(Inst. de Radioastronomia Milimetrica, Granada, Spain), AD(Inst. de Radioastronomie Millimetrique, Saint-Martin-d'Heres, France), AE(New York, State Univ., Stony Brook), AF(Inst. de Radioastronomie Millimetrique, Saint-Martin-d'Heres, France)
Publication:
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 398, no. 1, p. L25-L27. (ApJL Homepage)
Publication Date:
10/1992
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
COSMIC DUST, INFRARED SOURCES (ASTRONOMY), STARBURST GALAXIES, SUBMILLIMETER WAVES, ABUNDANCE, ASTRONOMICAL MODELS, CARBON MONOXIDE, INTERSTELLAR EXTINCTION, METALLICITY
DOI:
10.1086/186568
Bibliographic Code:
1992ApJ...398L..25D

Abstract

We measured with the IRAM 30 m telescope the continuum flux of the extremely luminous primeval galaxy IRAS 10214 +4724 at a wavelength of 1.2 mm. This is the longest wavelength at which this galaxy's thermal continuum radiation has been detected; at z = 2.286, it corresponds to a rest wavelength of 370 microns. From the entire continuum spectrum we estimate a dust temperature of 80 K, and from the optically thin radiation at 370 microns (rest frame) we find a dust mass of 2.5 x 10 exp 8/sq h solar masses. For the H2 mass of 1 x 10 exp 11/sq h solar masses implied by the CO line luminosity, this yields a ratio of the mass of gas (H2 + He) to warm dust of 500, which is surprisingly normal for a galaxy at z = 2.3. It is the same value as observed in the central regions of nearby luminous galaxies that have solar metallicity. The ratio of observed CO and 370 microns (rest-frame) luminosities in 10214 + 4724, essentially the gas-to-dust mass ratio, is the same as in nearby galaxies. Hence, in this galaxy, most of the heavy elements have already been produced, at nearly present-day abundances.

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