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Active Disk Building in a Local H I-massive LIRG: The Synergy Between Gas, Dust, and Star Formation

Cluver, M. E. and Jarrett, T. H. and Kraan-Korteweg, R. C. and Koribalski, B. S. and Appleton, P. N. and Melbourne, J. and Emonts, B. and Woudt, P. A. (2010) Active Disk Building in a Local H I-massive LIRG: The Synergy Between Gas, Dust, and Star Formation. Astrophysical Journal, 725 (2). pp. 1550-1562. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20110308-123057283

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Abstract

HIZOA J0836-43 is the most Hi-massive (M_(Hi) = 7.5 × 10^(10)M_⊙) galaxy detected in the HIPASS volume (δ = −90◦ to + 25◦ , v <12,700 km s^(−1)) and lies optically hidden behind the Milky Way. Markedly different from other extreme Hi disks in the local universe, it is a luminous infrared galaxy (LIRG) with an actively star-forming disk (>50 kpc), central to its ~130 kpc gas disk, with a total star formation rate (SFR) of ~20.5M_⊙ yr^(−1). Spitzer spectroscopy reveals an unusual combination of powerful polycyclic aromatic hydrocarbon (PAH) emission coupled to a relatively weak warm dust continuum, suggesting photodissociation-region-dominated emission. Compared to a typical LIRG with similar total infrared luminosity (L_(TIR) = 10^(11) L_⊙), the PAHs in HIZOA J0836-43 are more than twice as strong, whereas the warm dust continuum (λ > 20 μm) is best fit by a star-forming galaxy with L_(TIR) = 10^(10) L_⊙. Mopra CO observations suggest an extended molecular gas component (H -2+He > 3.7×10^9 M_⊙ and a lower limit of ~64% for the gas-mass fraction; this is above average compared to local disk systems, but similar to that of z ~ 1.5 BzK galaxies (~57%). However, the star formation efficiency (SFE = L_(IR)/L'_(CO)) for HIZOA J0836-43 of 140 L_⊙ (K km s^(−1) pc^2)^(−1) is similar to that of local spirals and other disk galaxies at high redshift, in strong contrast to the increased SFE seen in merging and strongly interacting systems. HIZOA J0836-43 is actively forming stars and building a massive stellar disk. Its evolutionary phase of star formation (M_(stellar), SFR, and gas fraction) compared to more distant systems suggests that it would be considered typical at redshift z ~ 1. This galaxy provides a rare opportunity in the nearby universe for studying (at z ~ 0.036) how disks were building and galaxies evolving at z ~ 1, when similarly large gas fractions were likely more common.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/725/2/1550DOIArticle
http://iopscience.iop.org/0004-637X/725/2/1550PublisherArticle
ORCID:
AuthorORCID
Appleton, P. N.0000-0002-7607-8766
Additional Information:© 2010 American Astronomical Society. Received 2010 August 30; accepted 2010 October 15; published 2010 November 30. We thank Danny Dale and SINGS, Lee Armus and GOALS for data access. We are grateful to Steve Lord, Ray Norris, Joe Mazzarella, and Justin Howell for valuable discussions and inputs. We thank the ATNF for hosting us (in Epping and Narrabri), and in particular Balt Indermuehle for his input regarding our Mopra observations. Support for this work was provided by NASA through an award issued by JPL/Caltech. M.E.C., R.K.-K., and P.A.W. thank the NRF (South Africa) for financial support.
Funders:
Funding AgencyGrant Number
NASAUNSPECIFIED
National Research Foundation (South Africa)UNSPECIFIED
Subject Keywords:galaxies: individual (HIZOA J0836-43); galaxies: starburst; infrared: galaxies
Classification Code:PACS: 98.54.Ep; 98.62.Ai; 95.85.Hp; 98.58.Ca; 98.58.Bz
Record Number:CaltechAUTHORS:20110308-123057283
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20110308-123057283
Official Citation:M. E. Cluver et al. 2010 ApJ 725 1550 doi: 10.1088/0004-637X/725/2/1550
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:22718
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:09 Mar 2011 19:20
Last Modified:18 Aug 2017 01:24

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