Volume 606, October 2017
|Number of page(s)||18|
|Published online||17 October 2017|
Interstellar medium conditions in z ~ 0.2 Lyman-break analogs
1 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
2 Department of Physics and Astronomy, Rutgers, The State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019, USA
3 Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
4 Naval Research Laborratory, Remote Sensing Division, 4555 Overlook Ave SW, Washington, DC 20375, USA
5 Oxford University, Dept. of Astrophysics, Oxford OX1 3RH, UK
6 Max-Planck Institut für Astronomie, Königstuhl 17, 69117 Heidelberg; Universität Heidelberg, Zentrum für Astronomie, Inst. für Theor. Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
7 Department of Astronomy and Joint Space Science Institute, University of Maryland, College Park, MD 20742, USA
8 California Institute of Technology, 301-17, 1200 E. California Blvd., Pasadena, CA 91125, USA
9 Tel Aviv University, Sackler School of Physics & Astronomy, 69978 Ramat Aviv, Israel
10 Department of Physics, Faculty of Science, University of Zagreb, Bijenička cesta 32, 10000 Zagreb, Croatia
Received: 13 February 2017
Accepted: 12 June 2017
We present an analysis of far–infrared (FIR) [CII] and [OI] fine structure line and continuum observations obtained with Herschel/PACS, and 12CO(1–0) observations obtained with the IRAM Plateau de Bure Interferometer, of Lyman-break analogs (LBAs) at z ~ 0.2. The principal aim of this work is to determine the typical interstellar medium (ISM) properties of z ~ 1−2 main sequence (MS) galaxies, with stellar masses between 109.5 and 1011M⊙, which are currently not easily detectable in all these lines even with ALMA and NOEMA. We perform PDR modeling and apply different infared diagnostics to derive the main physical parameters of the far-infrared (FIR)-emitting gas and dust and we compare the derived ISM properties to those of galaxies on and above the MS at different redshifts. We find that the ISM properties of LBAs are quite extreme (low gas temperature and high density and thermal pressure) with respect to those found in local normal spirals and more active local galaxies. LBAs have no [CII] deficit despite having the high specific star formation rates (sSFRs) typical of starbursts. Although LBAs lie above the local MS, we show that their ISM properties are more similar to those of high-redshift MS galaxies than of local galaxies above the main sequence. This data set represents an important reference for planning future ALMA [CII] observations of relatively low-mass MS galaxies at the epoch of the peak of the cosmic star formation.
Key words: galaxies: evolution / galaxies: ISM / galaxies: high-redshift / infrared: galaxies
© ESO, 2017
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