2017A&A...608A.144Y


Query : 2017A&A...608A.144Y

2017A&A...608A.144Y - Astronomy and Astrophysics, volume 608A, 144-144 (2017/12-1)

Molecular gas in the Herschel-selected strongly lensed submillimeter galaxies at z∼ 2-4 as probed by multi-J CO lines.

YANG C., OMONT A., BEELEN A., GAO Y., VAN DER WERF P., GAVAZZI R., ZHANG Z.-Y., IVISON R., LEHNERT M., LIU D., OTEO I., GONZALEZ-ALFONSO E., DANNERBAUER H., COX P., KRIPS M., NERI R., RIECHERS D., BAKER A.J., MICHALOWSKI M.J., COORAY A. and SMAIL I.

Abstract (from CDS):

We present the IRAM-30 m observations of multiple-J CO (Jup mostly from 3 up to 8) and [C I](3P2-3P1) ([CI](2-1) hereafter) line emission in a sample of redshift ∼2-4 submillimeter galaxies (SMGs). These SMGs are selected among the brightest-lensed galaxies discovered in the Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). Forty-seven CO lines and 7 [CI](2-1) lines have been detected in 15 lensed SMGs. A non-negligible effect of differential lensing is found for the CO emission lines, which could have caused significant underestimations of the linewidths, and hence of the dynamical masses. The CO spectral line energy distributions (SLEDs), peaking around Jup∼5-7, are found to be similar to those of the local starburst-dominated ultra-luminous infrared galaxies and of the previously studied SMGs. After correcting for lensing amplification, we derived the global properties of the bulk of molecular gas in the SMGs using non-LTE radiative transfer modelling, such as the molecular gas density nH2∼102.5-104.1cm–3 and the kinetic temperature Tk∼20-750K. The gas thermal pressure Pth ranging from∼105K/cm3 to 106K/cm3 is found to be correlated with star formation efficiency. Further decomposing the CO SLEDs into two excitation components, we find a low-excitation component with nH2∼102.8-104.6cm–3 and Tk∼20-30K, which is less correlated with star formation, and a high-excitation one (nH2∼102.7-104.2cm–3, Tk∼60-400K) which is tightly related to the on-going star-forming activity. Additionally, tight linear correlations between the far-infrared and CO line luminosities have been confirmed for the Jup≥5 CO lines of these SMGs, implying that these CO lines are good tracers of star formation. The [CI](2-1) lines follow the tight linear correlation between the luminosities of the [CI](2-1) and the CO(1-0) line found in local starbursts, indicating that [CI] lines could serve as good total molecular gas mass tracers for high-redshift SMGs as well. The total mass of the molecular gas reservoir, (1-30)x1010M, derived based on the CO(3-2) fluxes and αCO(1–0)=0.8M/(K.(km/s).pc2), suggests a typical molecular gas depletion time tdep∼20-100Myr and a gas to dust mass ratio δGDR∼30-100 with ∼20%-60% uncertainty for the SMGs. The ratio between CO line luminosity and the dust mass L'CO/Mdust appears to be slowly increasing with redshift for high-redshift SMGs, which need to be further confirmed by a more complete SMG sample at various redshifts. Finally, through comparing the linewidth of CO and H2O lines, we find that they agree well in almost all our SMGs, confirming that the emitting regions of the CO and H2O lines are co-spatially located.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: high-redshift - galaxies: ISM - infrared: galaxies - submillimeter: galaxies - radio lines: ISM - ISM: molecules - ISM: molecules

VizieR on-line data: <Available at CDS (J/A+A/608/A144): list.dat sp/*>

CDS comments: G12v2.890 is H-ATLAS J113243.1-005108 in SIMBAD, NAME G12v2.257 is H-ATLAS J115820.2-013753.

Simbad objects: 32

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Number of rows : 32
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME G09v1.97 G 08 30 51.0 +01 32 24           ~ 19 0
2 QSO J0831+5245 QSO 08 31 41.7108197808 +52 45 17.616994560   19.2   14.5 13.9 ~ 518 1
3 H-ATLAS J084933.4+021443 G 08 49 33.4 +02 14 43           ~ 29 0
4 NAME G09v1.40 G 08 53 58.6749643920 +01 55 35.473138860           ~ 15 0
5 NAME SDP 17b G 09 03 02.9 -01 41 27           ~ 17 0
6 SDP 81 G 09 03 11.574 +00 39 06.55           ~ 89 0
7 H-ATLAS J090740.0-004200 G? 09 07 40.0 -00 42 00           ~ 28 0
8 H-ATLAS J091043.0-000322 G? 09 10 43.1 -00 03 21           ~ 27 0
9 [VV96] J102434.5+470911 Sy1 10 24 34.5 +47 09 11     20.5     ~ 477 0
10 H-ATLAS J113243.0-005108 G 11 32 43.1 -00 51 08           ~ 8 0
11 NAME G12v2.43 G 11 35 26.3 -01 46 05           ~ 15 0
12 NAME G12.v2.30 G 11 46 37.9 -00 11 32           ~ 29 0
13 H-ATLAS J115820.1-013752 G 11 58 20.2 -01 37 53           ~ 11 0
14 NAME Antennae IG 12 01 53.170 -18 52 37.92           ~ 1631 0
15 NAME SMM J123711+622212 AGN 12 37 11.92 +62 22 12.1   27.1786 25.185   24.4196 ~ 184 0
16 NAME NGP reg 12 51 26.275 +27 07 41.70           ~ 1107 0
17 NAME NCv1.268 G 12 51 35.412 +26 14 58.63           ~ 8 0
18 Mrk 231 Sy1 12 56 14.2341182928 +56 52 25.238373852   14.68 13.84     ~ 1907 3
19 NAME NCv1.143 G 12 56 32.544 +23 36 27.63           ~ 15 0
20 NAME NAv1.195 G 13 26 30.216 +33 44 07.60           ~ 10 0
21 NAME NAv1.777 G 13 28 59.246 +29 23 26.13           ~ 9 0
22 NAME NB.v1.78 G 13 30 08.3 +24 59 00           ~ 16 0
23 H-ATLAS J133649.9+291800 G? 13 36 49.9 +29 18 01           ~ 16 0
24 NAME NAv1.56 G 13 44 29.4 +30 30 36           ~ 16 0
25 NAME G15v2.235 G 14 13 51.9 -00 00 26           ~ 15 0
26 QSO J1415+1129 QSO 14 15 46.25 +11 29 43.4   17.63 17.23     ~ 620 0
27 NAME Upper Centaurus Lupus As* 15 24 -41.9           ~ 416 1
28 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2836 4
29 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1565 2
30 NAME HFLS 3 G 17 06 47.8 +58 46 23           ~ 121 0
31 NAME Eyelash LeG 21 35 11.60 -01 02 52.0           ~ 209 0
32 NGC 7771 GiG 23 51 24.880 +20 06 42.57 13.42 13.08 12.25     ~ 326 4

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2022.08.10-19:56:15

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