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Spitzer Infrared Properties of Lyman α Emitters

Colbert, James W. and Scarlata, Claudia and Atek, Hakim and Teplitz, Harry (2011) Spitzer Infrared Properties of Lyman α Emitters. In: Galaxy Evolution: Infrared to Millimeter Wavelength Perspective. ASP Conference Series. No.446. Astronomical Society of the Pacific , San Francisco, CA, pp. 369-375. ISBN 978-1-58381-772-8. https://resolver.caltech.edu/CaltechAUTHORS:20120103-080133270

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Abstract

We present results on the infrared properties of Lyman α emitters. At z=0.3 we demonstrate that our sample of 50 GALEX-identified emitters possess the same extinction properties as similarly ultraviolet-bright galaxies at the same redshift. The AGN fraction for these z=0.3 sources is low, 10-20%, and they show no correlation between Lyα flux and total infrared luminosity. At z=2.4-3.1 we discuss a sample of Lyman α blobs. Roughly two thirds of these blobs have infrared counterparts with infrared and sub-mm colors indicating they are dominated by star formation. Of the six IRS spectra taken of blob counterparts, four show PAH features. Their equivalent widths indicate two are strongly star formation dominated, while the other two are mixed sources with a significant contribution from an AGN.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
http://www.aspbooks.org/a/volumes/article_details/?paper_id=33476PublisherArticle
ORCID:
AuthorORCID
Scarlata, Claudia0000-0002-9136-8876
Atek, Hakim0000-0002-7570-0824
Teplitz, Harry0000-0002-7064-5424
Additional Information:© 2011 Astronomical Society of the Pacific.
Group:Infrared Processing and Analysis Center (IPAC)
Series Name:ASP Conference Series
Issue or Number:446
Record Number:CaltechAUTHORS:20120103-080133270
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20120103-080133270
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:28599
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:04 Jan 2012 17:56
Last Modified:03 Oct 2019 03:33

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