2015A&A...577A..46D


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.07CET05:47:48

2015A&A...577A..46D - Astronomy and Astrophysics, volume 577A, 46-46 (2015/5-1)

CO excitation of normal star-forming galaxies out to z = 1.5 as regulated by the properties of their interstellar medium.

DADDI E., DANNERBAUER H., LIU D., ARAVENA M., BOURNAUD F., WALTER F., RIECHERS D., MAGDIS G., SARGENT M., BETHERMIN M., CARILLI C., CIBINEL A., DICKINSON M., ELBAZ D., GAO Y., GOBAT R., HODGE J. and KRIPS M.

Abstract (from CDS):

We investigate the CO excitation of normal (near-IR selected BzK) star-forming (SF) disk galaxies at z=1.5 using IRAM Plateau de Bure observations of the CO[2-1], CO[3-2], and CO[5-4] transitions for four galaxies, including VLA observations of CO[1-0] for three of them, with the aim of constraining the average state of H2 gas. By exploiting previous knowledge of the velocity range, spatial extent, and size of the CO emission, we measure reliable line fluxes with a signal-to-noise ratio >4-7 for individual transitions. While the average CO spectral line energy distribution (SLED) has a subthermal excitation similar to the Milky Way (MW) up to CO[3-2], we show that the average CO[5-4] emission is four times stronger than assuming MW excitation. This demonstrates that there is an additional component of more excited, denser, and possibly warmer molecular gas. The ratio of CO[5-4] to lower-J CO emission is lower than in local (ultra-)luminous infrared galaxies (ULIRGs) and high-redshift starbursting submillimeter galaxies, however, and appears to be closely correlated with the average intensity of the radiation field <U> and with the star formation surface density, but not with the star formation efficiency. The luminosity of the CO[5-4] transition is found to be linearly correlated with the bolometric infrared luminosity over four orders of magnitudes. For this transition, z=1.5 BzK galaxies follow the same linear trend as local spirals and (U)LIRGs and high-redshift star-bursting submillimeter galaxies. The CO[5-4] luminosity is thus empirically related to the dense gas and might be a more convenient way to probe it than standard high-density tracers that are much fainter than CO. We see excitation variations among our sample galaxies that can be linked to their evolutionary state and clumpiness in optical rest-frame images. In one galaxy we see spatially resolved excitation variations, where the more highly excited part of the galaxy corresponds to the location of massive SF clumps. This provides support to models that suggest that giant clumps are the main source of the high-excitation CO emission in high-redshift disk-like galaxies.

Abstract Copyright:

Journal keyword(s): galaxies: evolution - galaxies: high-redshift - galaxies: starburst - galaxies: star formation - submillimeter: galaxies

CDS comments: HLSW-01 is HERMES J105751.1+573027 in SIMBAD.

Simbad objects: 33

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Number of rows : 33

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NPM1G +40.0002 Sy2 00 08 20.3669698339 +40 37 55.924594172     16.8     ~ 43 0
2 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 2868 2
3 2MASX J02513583+4315117 LIN 02 51 35.8181246223 +43 15 11.769570316   18.09 17.36     ~ 54 0
4 IC 342 SBG 03 46 48.514 +68 05 45.98   10.5       ~ 1364 1
5 2MASX J04260482+1443360 LIN 04 26 04.829 +14 43 36.01           ~ 25 0
6 ZW VII 31 G 05 16 46.384 +79 40 12.63   15.8       ~ 134 0
7 2MASX J05210136-2521450 Sy2 05 21 01.3987198411 -25 21 45.269338983   15.47 14.75     ~ 420 0
8 NAME IRAS F08572+3915 NW LIN 09 00 25.364 +39 03 54.23     16.66     ~ 360 1
9 UGC 5101 Sy1 09 35 51.694 +61 21 10.52   15.20 15.50     ~ 500 4
10 M 95 GiP 10 43 57.733 +11 42 13.00 10.71 10.51 9.73 9.48   ~ 909 2
11 NAME HLock01 G 10 57 51.1 +57 30 27           ~ 33 0
12 2XMM J105918.1+243234 LIN 10 59 18.128 +24 32 34.74   15.7       ~ 234 1
13 NGC 3521 LSB 11 05 48.5676206040 -00 02 09.228156576 10.06 9.83 9.02 10.1 9.6 ~ 676 2
14 NAME BzK 4171 G 12 36 26.5278 +62 08 35.701 26.53 25.8 25.9   24.39 ~ 25 0
15 NAME BzK 16000 G 12 36 30.0982 +62 14 28.357 24.73 24.57 25.14   23.20 ~ 23 0
16 NAME MM J123633+6214.1 G 12 36 33.2 +62 14 07           ~ 51 0
17 [FRP2015] z4 GNW 18460 G 12 37 08.840 +62 22 02.37     25.150     ~ 38 0
18 [PSD2006] GN20.2b smm 12 37 09.73 +62 22 02.6           ~ 14 0
19 NAME BzK 21000 rG 12 37 10.6429 +62 22 34.555 23.93 25.06     23.76 ~ 44 0
20 NAME SMM J123711+622212 AGN 12 37 11.89 +62 22 12.7   27.2 25.185   24.42 ~ 143 0
21 NAME BzK 17999 G 12 37 51.819 +62 15 20.16           ~ 13 0
22 M 94 SyG 12 50 53.148 +41 07 12.55 9.15 8.96 8.24 7.78   ~ 1184 3
23 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1742 3
24 M 83 SBG 13 37 00.919 -29 51 56.74 8.85 8.11 7.52 7.21   ~ 2167 2
25 Mrk 273 Sy2 13 44 42.070 +55 53 13.17   15.68 14.91     ~ 814 3
26 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2629 4
27 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1450 2
28 6dFGS gJ172322.0-001701 LIN 17 23 21.943 -00 17 00.96   15.1       ~ 368 0
29 EM* MWC 349 Em* 20 32 45.6328 +40 39 36.143   15.88 13.15 12.13   Bep 692 1
30 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2187 2
31 NAME Eyelash LeG 21 35 11.60 -01 02 52.0           ~ 175 0
32 NGC 7331 LIN 22 37 04.102 +34 24 57.31 10.65 10.35 9.48     ~ 1086 2
33 2MASX J23390127+3621087 SyG 23 39 01.274 +36 21 08.77   16.17       ~ 193 1

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2019.12.07-05:47:48

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