The Interstellar Medium in High-redshift Submillimeter Galaxies as Probed by Infrared Spectroscopy
- Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham, DH1 3LE (United Kingdom)
- Department of Physics and Astronomy, University of California, Irvine, CA 92697 (United States)
- Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ (United Kingdom)
- Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ (United Kingdom)
- Instituto de Astrofísica de Canarias (IAC), Dpto. Astrofísica, E-38200 La Laguna, Tenerife (Spain)
- School of Physics and Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD (United Kingdom)
- School of Physics and Astronomy, Cardiff University, Queen’s Buildings, The Parade 5, Cardiff CF24 3AA (United Kingdom)
- Department of Physics, Virginia Tech, Blacksburg, VA 24061 (United States)
- Instituto de Física y Astronomía, Universidad de Valparaóso, Avda. Gran Bretaña 1111, Valparaíso (Chile)
- Department of Astronomy, Cornell University, 220 Space Sciences Building, Ithaca, NY 14853 (United States)
- Oxford Astrophysics, Department of Physics, University of Oxford, Keble Rd, Oxford OX1 3RH (United Kingdom)
- Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1 (Canada)
Submillimeter galaxies (SMGs) at z≳1 are luminous in the far-infrared, and have star formation rates, SFR, of hundreds to thousands of solar masses per year. However, it is unclear whether they are true analogs of local ULIRGs or whether the mode of their star formation is more similar to that in local disk galaxies. We target these questions by using Herschel-PACS to examine the conditions in the interstellar medium (ISM) in far-infrared luminous SMGs at z∼1–4. We present 70–160 μm photometry and spectroscopy of the [O iv]26 μm, [Fe ii]26 μm, [S iii]33 μm, [Si ii]34 μm, [O iii]52 μm, [N iii]57 μm, and [O i]63 μm fine-structure lines and the S(0) and S(1) hydrogen rotational lines in 13 lensed SMGs identified by their brightness in early Herschel data. Most of the 13 targets are not individually spectroscopically detected; we instead focus on stacking these spectra with observations of an additional 32 SMGs from the Herschel archive—representing a complete compilation of PACS spectroscopy of SMGs. We detect [O i]63 μm, [Si ii]34 μm, and [N iii]57 μm at ⩾3σ in the stacked spectra, determining that the average strengths of these lines relative to the far-IR continuum are (0.36±0.12)×10{sup −3}, (0.84±0.17)×10{sup −3}, and (0.27±0.10)×10{sup −3}, respectively. Using the [O iii]52 μm/[N iii]57 μm emission line ratio, we show that SMGs have average gas-phase metallicities ≳Z{sub ⊙}. By using PDR modeling and combining the new spectral measurements with integrated far-infrared fluxes and existing [C ii]158 μm data, we show that SMGs have average gas densities, n, of ∼10{sup 1−3} cm{sup −3} and FUV field strengths, G{sub 0}∼10{sup 2.2−4.5} (in Habing units: 1.6×10{sup −3} erg cm{sup −2} s{sup −1}), consistent with both local ULIRGs and lower luminosity star-forming galaxies.
- OSTI ID:
- 22869293
- Journal Information:
- Astrophysical Journal, Vol. 837, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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