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FMOS near-IR spectroscopy of Herschel-selected galaxies: star formation rates, metallicity and dust attenuation at z ∼ 1

Roseboom, I. G. and Bock, J. and Cooray, A. and Schulz, B. and Zemcov, M. (2012) FMOS near-IR spectroscopy of Herschel-selected galaxies: star formation rates, metallicity and dust attenuation at z ∼ 1. Monthly Notices of the Royal Astronomical Society, 426 (3). pp. 1782-1792. ISSN 0035-8711.

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We investigate the properties (e.g. star formation rate, dust attenuation, stellar mass and metallicity) of a sample of infrared (IR) luminous galaxies at z ∼ 1 via near-IR spectroscopy with Subaru-FMOS. Our sample consists of Herschel SPIRE and Spitzer MIPS selected sources in the COSMOS field with photometric redshifts in the range of 0.7 < z_phot < 1.8, which have been targeted in two pointings (0.5 deg^2) with FMOS. We find a modest success rate for emission-line detections, with candidate Hα emission lines detected for 57 of 168 SPIRE sources (34 per cent). By stacking the near-IR spectra we directly measure the mean Balmer decrement for the Hα and Hβ lines, finding a value of 〈E(B − V)〉 = 0.51 ± 0.27 for 〈LIR〉 = 10^12  L_⊙ sources at 〈z〉 = 1.36. By comparing star formation rates estimated from the IR and from the dust-uncorrected Hα line we find a strong relationship between dust attenuation and star formation rate. This relation is broadly consistent with that previously seen in star-forming galaxies at z ∼ 0.1. Finally, we investigate the metallicity via the N2 ratio, finding that z ∼ 1 IR-selected sources are indistinguishable from the local mass–metallicity relation. We also find a strong correlation between dust attenuation and metallicity, with the most metal-rich IR sources experiencing the largest levels of dust attenuation.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Bock, J.0000-0002-5710-5212
Cooray, A.0000-0002-3892-0190
Zemcov, M.0000-0001-8253-1451
Additional Information:© 2012 The Authors. Monthly Notices of the Royal Astronomical Society © 2012 RAS. Accepted 2012 July 23. Received 2012 July 23; in original form 2012 January 26. Article first published online: 8 Oct. 2012. We thank the anonymous referee for suggestions which greatly enhanced this work. IGR, SJO and LW acknowledge support from the Science and Technology Facilities Council (grant Nos ST/F002858/1 and ST/I000976/1). JSD acknowledges the support of the Royal Society via aWolfson Research Merit award and the support of the European Research Council via the award of an Advanced Grant. Based on zCOSMOS observations carried out using the Very Large Telescope at the ESO Paranal Observatory under Programme ID: LP175.A-0839. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, theMax Planck Society and theHigher Education Funding Council for England. The SDSS website is The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) including University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UK ATC, University of Sussex (UK); and Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy);MCINN (Spain); SNSB (Sweden); STFC and UKSA (UK); and NASA (USA). FMOS was funded jointly by STFC and the Japanese Monbukagakusho, and we gratefully acknowledge the support of the staff at the Subaru Telescope throughout the instrument commissioning phase. The data presented in this paper will be released through the Herschel Database inMarseille HeDaM (
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)ST/F002858/1
Science and Technology Facilities Council (STFC)ST/I000976/1
European Research Council (ERC)UNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
Japanese MonbukagakushoUNSPECIFIED
Max Planck SocietyUNSPECIFIED
Higher Education Funding Council for EnglandUNSPECIFIED
Subject Keywords:galaxies: evolution; submillimetre: galaxies
Issue or Number:3
Record Number:CaltechAUTHORS:20121129-084742065
Persistent URL:
Official Citation:Roseboom, I. G., Bunker, A., Sumiyoshi, M., Wang, L., Dalton, G., Akiyama, M., Bock, J., Bonfield, D., Buat, V., Casey, C., Chapin, E., Clements, D. L., Conley, A., Curtis-Lake, E., Cooray, A., Dunlop, J. S., Farrah, D., Ham, S. J., Ibar, E., Iwamuro, F., Kimura, M., Lewis, I., Macaulay, E., Magdis, G., Maihara, T., Marsden, G., Mauch, T., Moritani, Y., Ohta, K., Oliver, S. J., Page, M. J., Schulz, B., Scott, D., Symeonidis, M., Takato, N., Tamura, N., Totani, T., Yabe, K. and Zemcov, M. (2012), FMOS near-IR spectroscopy of Herschel-selected galaxies: star formation rates, metallicity and dust attenuation at z ∼ 1. Monthly Notices of the Royal Astronomical Society, 426: 1782–1792. doi: 10.1111/j.1365-2966.2012.21777.x
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:35722
Deposited By: Jason Perez
Deposited On:29 Nov 2012 18:57
Last Modified:29 Jan 2020 21:48

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