Basu-Zych, Antara R. and Schiminovich, David and Johnson, Benjamin D. and Hoopes, Charles and Overzier, Roderik and Treyer, Marie A. and Heckman, Timothy M. and Barlow, Tom A. and Bianchi, Luciana and Conrow, Tim and Donas, José and Forster, Karl and Friedman, Peter G. and Lee, Young-Wook and Madore, Barry F. and Martin, D. Christopher and Milliard, Bruno and Morrissey, Patrick and Neff, Susan G. and Rich, R. Michael and Salim, Samir and Seibert, Mark and Small, Todd A. and Szalay, Alex S. and Wyder, Ted K. and Yi, Sukyoung (2007) The Young and the Dustless: Interpreting Radio Observations of Ultraviolet-Luminous Galaxies. Astrophysical Journal Supplement Series, 173 (2). pp. 457-470. ISSN 0067-0049 http://resolver.caltech.edu/CaltechAUTHORS:20091016-084254435
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Ultraviolet-luminous galaxies (UVLGs) have been identified as intensely star-forming nearby galaxies. A subset of these, the supercompact UVLGs, are believed to be local analogs of high-redshift Lyman break galaxies. Here we investigate the radio continuum properties of this important population for the first time. We have observed 42 supercompact UVLGs with the VLA, all of which have extensive coverage in the UV/optical by GALEX and SDSS. Our analysis includes comparison samples of multiwavelength data from the Spitzer First Look Survey and from the SDSS-GALEX matched catalogs. In addition we have Spitzer MIPS data for 24 of our galaxies and find that they fall on the radio-FIR correlation of normal star-forming galaxies. We find that our galaxies have lower radio to UV ratios and lower Balmer decrements than other local galaxies with similar (high) star formation rates. Optical spectra show they have lower D_n(4000) and Hδ_A indices, higher Hβ emission-line equivalent widths, and higher [O III]5007/Hβ emission-line ratios than normal star-forming galaxies. Comparing these results to galaxy spectral evolution models we conclude that supercompact UVLGs are distinguished from normal star-forming galaxies firstly by their high specific star formation rates. Moreover, compared to other types of galaxies with similar star formation rates, they have significantly less dust attenuation. In both regards they are similar to Lyman break galaxies. This suggests that the process that causes star formation in the supercompact UVLGs differs from other local star-forming galaxies, but may be similar to Lyman break galaxies.
|Additional Information:||© 2007 The American Astronomical Society. Received 2007 February 7; accepted 2007 June 18. GALEX (Galaxy Evolution Explorer) is a NASA small explorer, launched in 2003 April. We gratefully acknowledge NASA’s support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. We thank Michael Blanton for access to the IDL kcorrect (ver. 4.1.4) analysis package.We recognize that funding for the SDSS archive has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society.|
|Subject Keywords:||galaxies : starburst; radio continuum : galaxies; ultraviolet : galaxies|
|Official Citation:||The Young and the Dustless: Interpreting Radio Observations of Ultraviolet-Luminous Galaxies Antara R. Basu-Zych, David Schiminovich, Benjamin D. Johnson, Charles Hoopes, Roderik Overzier, Marie A. Treyer, Timothy M. Heckman, Tom A. Barlow, Luciana Bianchi, Tim Conrow, José Donas, Karl G. Forster, Peter G. Friedman, Young-Wook Lee, Barry F. Madore, D. Christopher Martin, Bruno Milliard, Patrick Morrissey, Susan G. Neff, R. Michael Rich, Samir Salim, Mark Seibert, Todd A. Small, Alex S. Szalay, Ted K. Wyder, and Sukyoung Yi 2007 ApJS 173 457-470 doi: 10.1086/521146|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Tony Diaz|
|Deposited On:||26 Oct 2009 18:24|
|Last Modified:||04 Mar 2013 17:52|
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