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Dust Extinction from Balmer Decrements of Star-forming Galaxies at 0.75 ≤ z ≤ 1.5 with Hubble Space Telescope/Wide-Field-Camera 3 Spectroscopy from the WFC3 Infrared Spectroscopic Parallel Survey

Dominguez, A. and Siana, B. and Henry, A. L. and Scarlata, C. and Bedregal, A. G. and Malkan, M. and Atek, H. and Ross, N. R. and Colbert, J. W. and Teplitz, H. I. and Rafelski, M. and McCarthy, P. and Bunker, A. and Hathi, N. P. and Dressler, A. and Martin, C. L. and Masters, D. (2013) Dust Extinction from Balmer Decrements of Star-forming Galaxies at 0.75 ≤ z ≤ 1.5 with Hubble Space Telescope/Wide-Field-Camera 3 Spectroscopy from the WFC3 Infrared Spectroscopic Parallel Survey. Astrophysical Journal, 763 (2). Art. No. 145. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20150707-145422929

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Abstract

Spectroscopic observations of Hα and Hβ emission lines of 128 star-forming galaxies in the redshift range 0.75 ≤ z ≤ 1.5 are presented. These data were taken with slitless spectroscopy using the G102 and G141 grisms of the Wide-Field-Camera 3 (WFC3) on board the Hubble Space Telescope as part of the WFC3 Infrared Spectroscopic Parallel survey. Interstellar dust extinction is measured from stacked spectra that cover the Balmer decrement (Hα/Hβ). We present dust extinction as a function of Hα luminosity (down to 3 × 10^(41) erg s^(–1)), galaxy stellar mass (reaching 4 × 10^8 M _☉), and rest-frame Hα equivalent width. The faintest galaxies are two times fainter in Hα luminosity than galaxies previously studied at z ~ 1.5. An evolution is observed where galaxies of the same Hα luminosity have lower extinction at higher redshifts, whereas no evolution is found within our error bars with stellar mass. The lower Hα luminosity galaxies in our sample are found to be consistent with no dust extinction. We find an anti-correlation of the [O III] λ5007/Hα flux ratio as a function of luminosity where galaxies with L _(Hα) < 5 × 10^(41) erg s^(–1) are brighter in [O III] λ5007 than Hα. This trend is evident even after extinction correction, suggesting that the increased [O III] λ5007/Hα ratio in low-luminosity galaxies is likely due to lower metallicity and/or higher ionization parameters.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/763/2/145DOIArticle
http://iopscience.iop.org/0004-637X/763/2/145/PublisherArticle
http://arxiv.org/abs/1206.1867arXivDiscussion Paper
ORCID:
AuthorORCID
Siana, B.0000-0002-4935-9511
Henry, A. L.0000-0002-6586-4446
Scarlata, C.0000-0002-9136-8876
Malkan, M.0000-0001-6919-1237
Atek, H.0000-0002-7570-0824
Teplitz, H. I.0000-0002-7064-5424
Rafelski, M.0000-0002-9946-4731
Hathi, N. P.0000-0001-6145-5090
Masters, D.0000-0001-5382-6138
Alternate Title:Dust extinction from Balmer decrements of star-forming galaxies at 0.75 ≤ z ≤ 1.5 with HST/WFC3 spectroscopy from the WISP survey
Additional Information:© 2013 The American Astronomical Society. Received 2012 June 8; Accepted 2012 December 8; Published 2013 January 17. The authors thank Naveen Reddy for reading and improving the paper and David Sobral for fruitful discussions. We also thank the anonymous referee for helpful suggestions. This work is based on observations made with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs 11696, 12283, and 12568.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANAS 5-26555
Subject Keywords:dust, extinction; galaxies: evolution; galaxies: high-redshift
Issue or Number:2
Record Number:CaltechAUTHORS:20150707-145422929
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20150707-145422929
Official Citation:Dust Extinction from Balmer Decrements of Star-forming Galaxies at 0.75 ≤ z ≤ 1.5 with Hubble Space Telescope/Wide-Field-Camera 3 Spectroscopy from the WFC3 Infrared Spectroscopic Parallel Survey. A. Domínguez et al. 2013 ApJ 763 145
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:58795
Collection:CaltechAUTHORS
Deposited By: Joanne McCole
Deposited On:10 Jul 2015 22:00
Last Modified:03 Oct 2019 08:40

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