Molecular gas content in strongly lensed z ~ 1.5−3 star-forming galaxies with low infrared luminosities^⋆

¹ Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Versoix, Switzerland
e-mail: miroslava.dessauges@unige.ch
² CNRS, IRAP, 14 Avenue E. Belin, 31400 Toulouse, France
³ Observatoire de Paris, LERMA, 61 Avenue de l’Observatoire, 75014 Paris, France
⁴ Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
⁵ Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK
⁶ CRAL, Observatoire de Lyon, Université Lyon 1, 9 Avenue Ch. André, 69561 Saint Genis Laval Cedex, France
⁷ ESAC, ESA, PO Box 78, Villanueva de la Canada, 28691 Madrid, Spain
⁸ Laboratoire d’Astrophysique, École Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland
⁹ Aix Marseille Université, CNRS, LAM, UMR 7326, 13388 Marseille, France
¹⁰ Department of Physics & Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK

Received: 23 July 2014
Accepted: 12 February 2015

Abstract

To extend the molecular gas measurements to more typical star-forming galaxies (SFGs) with star formation rates SFR< 40 M_⊙ yr^-1 and stellar masses M_∗< 2.5 × 10¹⁰M_⊙ at z ~ 1.5−3, we have observed CO emission with the IRAM Plateau de Bure Interferometer and the IRAM 30 m telescope for five strongly lensed galaxies, selected from the Herschel Lensing Survey. These observations are combined with a compilation of CO measurements from the literature. From this, we infer the CO luminosity correction factors r_2,1 = 0.81 ± 0.20 and r_3,1 = 0.57 ± 0.15 for the J = 2 and J = 3 CO transitions, respectively, valid for SFGs at z> 1. The combined sample of CO-detected SFGs at z> 1 shows a large spread in star formation efficiency (SFE) with a dispersion of 0.33 dex, such that the SFE extends well beyond the low values of local spirals and overlaps the distribution of z> 1 submm galaxies. We find that the spread in SFE (or equivalently in molecular gas depletion timescale) is due to the variations of several physical parameters, primarily the specific star formation rate, and also stellar mass and redshift. The dependence of SFE on the offset from the main sequence and the compactness of the starburst is less clear. The possible increase of the molecular gas depletion timescale with stellar mass, now revealed by low M_∗ SFGs at z> 1 and also observed at z = 0, contrasts with the generally acknowledged constant molecular gas depletion timescale and refutes the linearity of the Kennicutt-Schmidt relation. A net rise of the molecular gas fraction (f_gas) is observed from z ~ 0.2 to z ~ 1.2, followed by a very mild increase toward higher redshifts, as found in earlier studies. At each redshift the molecular gas fraction shows a large dispersion, mainly due to the dependence of f_gas on stellar mass, producing a gradient of increasing f_gas with decreasing M_∗. We provide the first measurement of the molecular gas fraction of z> 1 SFGs at the low-M_∗ end between 10^9.4<M_∗/M_⊙< 10^9.9, reaching a mean ⟨ f_gas ⟩ = 0.69 ± 0.18, which shows a clear f_gas upturn at these lower stellar masses. Finally, we find evidence for a nonuniversal dust-to-gas ratio among high-redshift SFGs, high-redshift submm galaxies, local spirals, and local ultraluminous IR galaxies with near-solar metallicities, as inferred from a homogeneous analysis of their rest-frame 850 μm luminosity per unit gas mass. The SFGs with z> 1 show a trend for a lower L_ν(850 μm) /M_gas mean by 0.33 dex compared to the other galaxy populations.