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The Bright and Dark Sides of High-redshift Starburst Galaxies from Herschel and Subaru Observations

Puglisi, A. and Daddi, E. and Renzini, A. and Rodighiero, G. and Silverman, J. D. and Kashino, D. and Rodríguez-Muñoz, L. and Mancini, C. and Mainieri, V. and Man, A. and Franceschini, A. and Valentino, F. and Calabrò, A. and Jin, S. and Darvish, B. and Maier, C. and Kartaltepe, J. S. and Sanders, D. B. (2017) The Bright and Dark Sides of High-redshift Starburst Galaxies from Herschel and Subaru Observations. Astrophysical Journal Letters, 838 (2). Art. No. L18. ISSN 2041-8213. https://resolver.caltech.edu/CaltechAUTHORS:20170331-091528326

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Abstract

We present rest-frame optical spectra from the FMOS-COSMOS survey of 12 z ~ 1.6 Herschel starburst galaxies, with star formation rate (SFR) elevated by ×8, on average, above the star-forming main sequence (MS). Comparing the Hα to IR luminosity ratio and the Balmer decrement, we find that the optically thin regions of the sources contain on average only ~10% of the total SFR, whereas ~90% come from an extremely obscured component that is revealed only by far-IR observations and is optically thick even in Hα. We measure the [N ii]_(6583)/Hα ratio, suggesting that the less obscured regions have a metal content similar to that of the MS population at the same stellar masses and redshifts. However, our objects appear to be metal-rich outliers from the metallicity–SFR anticorrelation observed at fixed stellar mass for the MS population. The [S ii]_(6732)/[S ii]_(6717) ratio from the average spectrum indicates an electron density n_e ~ 1100 cm^(−3) , larger than what was estimated for MS galaxies but only at the 1.5σ level. Our results provide supporting evidence that high-z MS outliers are analogous of local ULIRGs and are consistent with a major-merger origin for the starburst event.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/2041-8213/aa66c9DOIArticle
http://iopscience.iop.org/article/10.3847/2041-8213/aa66c9/metaPublisherArticle
https://arxiv.org/abs/1703.04801arXivDiscussion Paper
ORCID:
AuthorORCID
Puglisi, A.0000-0001-9369-1805
Daddi, E.0000-0002-3331-9590
Renzini, A.0000-0002-7093-7355
Rodighiero, G.0000-0002-9415-2296
Silverman, J. D. 0000-0002-0000-6977
Kashino, D.0000-0001-9044-1747
Mancini, C.0000-0002-4297-0561
Calabrò, A.0000-0003-2536-1614
Darvish, B.0000-0003-4919-9017
Kartaltepe, J. S.0000-0001-9187-3605
Sanders, D. B.0000-0002-1233-9998
Additional Information:© 2017. The American Astronomical Society. Received 2017 January 18; revised 2017 February 27; accepted 2017 March 11; published 2017 March 30. A.R. acknowledges partial support by the DFG Cluster of Excellence Origin and Structure of the Universe (www.universe-cluster.de). B.D. acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. We thank the referee for the careful reading of the manuscript and for giving valuable comments and insights. The authors thank Rob Ivison for useful discussions and Margherita Talia for reading the manuscript and providing useful comments. A.P. also thanks Suhail Dhawan and Miguel Querejeta for helpful discussions and support while this Letter was completed.
Funders:
Funding AgencyGrant Number
Deutsche Forschungsgemeinschaft (DFG)UNSPECIFIED
NASANNX12AE20G
Subject Keywords:galaxies: evolution; galaxies: high-redshift; galaxies: interactions; galaxies: ISM; galaxies: starburst; infrared: galaxies
Issue or Number:2
Record Number:CaltechAUTHORS:20170331-091528326
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170331-091528326
Official Citation:A. Puglisi et al 2017 ApJL 838 L18
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:75567
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:31 Mar 2017 16:45
Last Modified:10 Oct 2019 20:21

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