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An atlas of z = 5.7 and z = 6.5 Lyα emitters

Hu, E. M. and Cowie, L. L. and Barger, A. J. and Capak, P. and Kakazu, Y. and Trouille, L. (2010) An atlas of z = 5.7 and z = 6.5 Lyα emitters. Astrophysical Journal, 725 (1). pp. 394-423. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20110112-144431112

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Abstract

We present an atlas of 88 z ~ 5.7 and 30 z ~ 6.5 Lyα emitters obtained from a wide-field narrowband survey. We combined deep narrowband imaging in 120 Å bandpass filters centered at 8150 Å and 9140 Å with deep B V R I z broadband imaging to select high-redshift galaxy candidates over an area of 4180 arcmin^2. The goal was to obtain a uniform selection of comparable depth over the seven targeted fields in the two filters. For the GOODS-North region of the Hubble Deep Field-North field, we also selected candidates using a 120 Å filter centered at 9210 Å. We made spectroscopic observations with Keck DEIMOS of nearly all the candidates to obtain the final sample of Lyα emitters. At the 3.3 Å resolution of the DEIMOS observations the asymmetric profile for Lyα emission can be clearly seen in the spectra of nearly all the galaxies. We show that the spectral profiles are surprisingly similar for many of the galaxies and that the composite spectral profiles are nearly identical at z = 5.7 and z = 6.5.We analyze the distributions of line widths and Lyα equivalent widths and find that the lines are marginally narrower at the higher redshift, with median values of 0.77 Å at z = 6.5 and 0.92 Å at z = 5.7. The line widths have a dependence on the Lyα luminosity of the form ~L^(0.3)_α . We compare the surface densities and the luminosity functions at the two redshifts and find that there is a multiplicative factor of two decrease in the number density of bright Lyα emitters from z = 5.7 to z = 6.5, while the characteristic luminosity is unchanged.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/725/1/394DOIArticle
http://iopscience.iop.org/0004-637X/725/1/394/PublisherArticle
Additional Information:© 2010 American Astronomical Society. Received 2010 July 7; accepted 2010 August 31; published 2010 November 18. Based in part on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Based in part on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA and was made possible by the generous financial support of the W. M. Keck Foundation. We are indebted to the staff of the Subaru and Keck Observatories for their excellent assistance with the observations. We thank Yoshi Taniguchi and Masami Ouchi for useful conversations. We gratefully acknowledge support from NSF grants AST 0687850 (E.M.H.), AST 0709356 (L.L.C.), and AST 0708793 (A.J.B.), a grant from NASA through an award issued by JPL 1289080 (E.M.H.), the University of Wisconsin Research Committee with funds granted by the Wisconsin Alumni Research Foundation, and the David and Lucile Packard Foundation (A.J.B.).
Group:COSMOS, Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NSF AST-0687850
NSF AST-0709356
NSF AST-0708793
NASA/JPL1289080
Wisconsin Alumni Research FoundationUNSPECIFIED
David and Lucile Packard Foundation UNSPECIFIED
W. M. Keck Foundation UNSPECIFIED
Subject Keywords:cosmology: observations – galaxies: distances and redshifts – galaxies: evolution – galaxies: formation – galaxies: high-redshift – galaxies: luminosity function, mass function
Classification Code:PACS: 98.62.Py; 95.30.Ky; 98.62.Ra; 98.62.Qz
Record Number:CaltechAUTHORS:20110112-144431112
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20110112-144431112
Official Citation:E. M. Hu et al. 2010 ApJ 725 394 doi: 10.1088/0004-637X/725/1/394
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21738
Collection:CaltechAUTHORS
Deposited By: Benjamin Perez
Deposited On:12 Jan 2011 23:30
Last Modified:19 May 2017 19:03

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