2009ApJ...707..988W


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.06CEST01:09:23

2009ApJ...707..988W - Astrophys. J., 707, 988-999 (2009/December-3)

Continuum observations at 350 microns of high-redshift molecular emission line galaxies.

WU J., VANDEN BOUT P.A., EVANS N.J. and DUNHAM M.M.

Abstract (from CDS):

We report observations of 15 high-redshift (z = 1 - 5) galaxies at 350 µm using the Caltech Submillimeter Observatory and Submillimeter High Angular Resolution Camera II array detector. Emission was detected from eight galaxies, for which far-infrared luminosities, star formation rates (SFRs), total dust masses, and minimum source size estimates are derived. These galaxies have SFRs and star formation efficiencies comparable to other high-redshift molecular emission line galaxies. The results are used to test the idea that star formation in these galaxies occurs in a large number of basic units, the units being similar to star-forming clumps in the Milky Way. The luminosity of these extreme galaxies can be reproduced in a simple model with (0.9-30)x106 dense clumps, each with a luminosity of 5x105 L, the mean value for such clumps in the Milky Way. Radiative transfer models of such clumps can provide reasonable matches to the overall spectral energy distributions (SEDs) of the galaxies. They indicate that the individual clumps are quite opaque in the far-infrared. Luminosity-to-mass ratios vary over two orders of magnitude, correlating strongly with the dust temperature derived from simple fits to the SED. The gas masses derived from the dust modeling are in remarkable agreement with those from CO luminosities, suggesting that the assumptions going into both calculations are reasonable.

Abstract Copyright:

Journal keyword(s): galaxies: formation - galaxies: high-redshift - galaxies: ISM - galaxies: starburst - infrared: galaxies

Simbad objects: 23

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Number of rows : 23

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 LBQS 0018-0220 QSO 00 21 27.3596452464 -02 03 33.553093015   17.48 17.10     ~ 30 0
2 ACO 370 ClG 02 39 50.5 -01 35 08           ~ 654 0
3 NAME SMM J023952-0136 Sy2 02 39 51.9 -01 35 58     21.90     ~ 39 0
4 [BCS99b] ACO 370 L5 smm 02 39 56.51 -01 34 25.7   20.44       ~ 50 0
5 NAME LRG J0239-0134 Sy2 02 39 56.568 -01 34 26.49   20.44       ~ 56 0
6 QSO J0338+0021 QSO 03 38 29.3152522955 +00 21 56.242586538   25.10 23.26     ~ 88 0
7 4C 05.19 QSO 04 14 37.7673624 +05 34 42.328449   24.100 23.800 21.270   ~ 336 2
8 RAFGL 618 pA* 04 42 53.6245215366 +36 06 53.397219192   16.32   12.59   C-rich 966 0
9 4C 60.07 rG 05 12 54.80 +60 30 51.7           ~ 88 1
10 QSO J0751+2716 QSO 07 51 41.517 +27 16 31.79     18.7     ~ 73 2
11 QSO B0908+0603 QSO 09 11 27.6052 +05 50 54.281   18.44 18.16     ~ 215 2
12 SDSS J092721.82+200123.7 QSO 09 27 21.821 +20 01 23.63   24.97 23.89     ~ 52 0
13 NAME SMM J09431+4700 AGN 09 43 03.96 +47 00 16.0       23.80   ~ 41 0
14 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2189 0
15 QSO B0952-0115 QSO 09 55 00.1037541106 -01 30 06.549307797     18.7     ~ 131 0
16 NAME SMM J14011+0252 GiC 14 01 04.95 +02 52 24.0           ~ 152 1
17 NAME SMM J16359+6613 G 16 35 55.62 +66 12 59.5           ~ 59 1
18 W 31 SFR 18 10 28.6 -19 55 51           ~ 243 0
19 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 464 0
20 NAME TX J1908+7220 rG 19 08 23.50 +72 20 09.8           ~ 53 1
21 W 49 SFR 19 10 20 +09 07.7           ~ 523 1
22 W 51 SNR 19 23 50 +14 06.0           ~ 1179 1
23 87GB 232800.5+391033 EmG 23 30 24.94 +39 27 12.0   24.70 23.97     ~ 50 2

    Equat.    Gal    SGal    Ecl

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2021.05.06-01:09:23

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