000212638 001__ 212638
000212638 005__ 20181203024024.0
000212638 0247_ $$2doi$$a10.1051/0004-6361/201424661
000212638 022__ $$a0004-6361
000212638 02470 $$2ISI$$a000357345900002
000212638 037__ $$aARTICLE
000212638 245__ $$aMolecular gas content in strongly lensed z similar to 1.5-3 star-forming galaxies with low infrared luminosities
000212638 260__ $$bEDP Sciences$$c2015$$aLes Ulis Cedex A
000212638 269__ $$a2015
000212638 300__ $$a20
000212638 336__ $$aJournal Articles
000212638 520__ $$aTo extend the molecular gas measurements to more typical star-forming galaxies (SFGs) with star formation rates SFR < 40 M-circle dot yr(-1) and stellar masses M-* < 2.5 x 10(10) M-circle dot at z similar to 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 similar to 0.2 to z similar to 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-circle dot < 10(9.9), reaching a mean af(gas)o = 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 mu m luminosity per unit gas mass. The SFGs with z > 1 show a trend for a lower L-nu(850 mu m)/M-gas mean by 0.33 dex compared to the other galaxy populations.
000212638 6531_ $$acosmology: observations
000212638 6531_ $$agravitational lensing: strong
000212638 6531_ $$agalaxies: high-redshift
000212638 6531_ $$aISM: molecules
000212638 6531_ $$agalaxies: evolution
000212638 700__ $$uUniv Geneva, Observ Geneve, CH-1290 Versoix, Switzerland$$aDessauges-Zavadsky, M.
000212638 700__ $$aZamojski, M.
000212638 700__ $$uUniv Geneva, Observ Geneve, CH-1290 Versoix, Switzerland$$aSchaerer, D.
000212638 700__ $$uObserv Paris, LERMA, F-75014 Paris, France$$aCombes, F.
000212638 700__ $$uUniv Arizona, Steward Observ, Tucson, AZ 85721 USA$$aEgami, E.
000212638 700__ $$uUniv Durham, Inst Computat Cosmol, Durham DH1 3LE, England$$aSwinbank, A. M.
000212638 700__ $$uUniv Lyon 1, Observ Lyon, CRAL, F-69561 St Genis Laval, France$$aRichard, J.
000212638 700__ $$uUniv Geneva, Observ Geneve, CH-1290 Versoix, Switzerland$$aSklias, P.
000212638 700__ $$uESA, ESAC, Madrid 28691, Spain$$aRawle, T. D.
000212638 700__ $$uUniv Arizona, Steward Observ, Tucson, AZ 85721 USA$$aRex, M.
000212638 700__ $$0246614$$g222189$$uEPFL, Observ Sauverny, Astrophys Lab, CH-1290 Versoix, Switzerland$$aKneib, J-P.
000212638 700__ $$uCNRS, IRAP, F-31400 Toulouse, France$$aBoone, F.
000212638 700__ $$aBlain, A.
000212638 773__ $$j577$$tAstronomy & Astrophysics$$qA50
000212638 909C0 $$xU10933$$0252365$$pLASTRO
000212638 909CO $$pSB$$particle$$ooai:infoscience.tind.io:212638
000212638 917Z8 $$x103317
000212638 937__ $$aEPFL-ARTICLE-212638
000212638 973__ $$rREVIEWED$$sPUBLISHED$$aEPFL
000212638 980__ $$aARTICLE