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The SED of the nearby H i-massive LIRG HIZOA J0836–43: from the NIR to the radio domain

Published online by Cambridge University Press:  17 August 2012

Renée C. Kraan-Korteweg  and
Michelle E. Cluver
Renée C. Kraan-Korteweg
Affiliation:
Astronomy Department, Astrophysics, Cosmology and Gravity Centre (ACGC), University of Cape Town, Rondebosch 7700, South Africa email: [email protected]
Michelle E. Cluver
Affiliation:
IPAC, California Institute of Technology, Pasadena, CA 91125, USA email: [email protected]
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Abstract

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HIZOA J0836–43 is one of the most H i-massive galaxies in the local (z < 0.1) Universe. Not only are such galaxies extremely rare, but this “coelacanth” galaxy exhibits characteristics – in particular its active, inside-out stellar disk-building – that appear more typical of past (z ~ 1) star formation, when large gas fractions were more common. Unlike most local giant H i galaxies, it is actively star forming. Moreover, the strong infrared emission is not induced by a merger event or AGN, as is commonly found in other local LIRGs. The galaxy is suggestive of a scaled-up version of local spiral galaxies; its extended star formation activity likely being fueled by its large gas reservoir and, as such, can aid our understanding of star formation in systems expected to dominate at higher redshifts. The multi-wavelength imaging and spectroscopic observations that have led to these deductions will be presented. These include NIR (JHK) and MIR (Spitzer; 3 – 24μm) imaging and photometry, MIR spectroscopy, ATCA H i-interferometry and Mopra CO line emission observations. But no optical data, as the galaxy is heavily obscured due to its location in Vela behind the Milky Way.

Keywords

galaxies: individual (HIZOA J0836–43)galaxies: evolutioninfrared: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 213 - 217
Copyright
Copyright © International Astronomical Union 2012

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