2017A&A...602A..49H


Query : 2017A&A...602A..49H

2017A&A...602A..49H - Astronomy and Astrophysics, volume 602A, 49-49 (2017/6-1)

VALES. II. The physical conditions of interstellar gas in normal star-forming galaxies up to z = 0.2 revealed by ALMA.

HUGHES T.M., IBAR E., VILLANUEVA V., ARAVENA M., BAES M., BOURNE N., COORAY A., DUNNE L., DYE S., EALES S., FURLANETTO C., HERRERA-CAMUS R., IVISON R.J., VAN KAMPEN E., LARA-LOPEZ M.A., MADDOX S.J., MICHALOWSKI M.J., SMITH M.W.L., VALIANTE E., VAN DER WERF P. and XUE Y.Q.

Abstract (from CDS):

We use new Band 3 CO(1-0) observations taken with the Atacama Large Millimeter/submillimeter Array (ALMA) to study the physical conditions in the interstellar gas of a sample of 27 dusty main-sequence star-forming galaxies at 0.03<z<0.2 present in the Valparaiso ALMA Line Emission Survey (VALES). The sample is drawn from far-IR bright galaxies over ∼160deg2 in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), which is covered by high-quality ancillary data including Herschel [CII] 158µm spectroscopy and far-infrared (FIR) photometry. The [CII] and CO(1-0) lines are both detected at >5σ in 26 sources. We find an average [CII] to CO(1-0) luminosity ratio of 3500±1200 for our sample that is consistent with previous studies. Using the [CII], CO(1-0) and FIR measurements as diagnostics of the physical conditions of the interstellar medium, we compare these observations to the predictions of a photodissociation region (PDR) model to determine the gas density, surface temperature, pressure, and the strength of the incident far-ultraviolet (FUV) radiation field, G0, normalised to the Habing Field. The majority of our sample exhibit hydrogen densities of 4<logn/cm3<5.5 and experience an incident FUV radiation field with strengths of 2<logG0<3 when adopting standard adjustments. A comparison to galaxy samples at different redshifts indicates that the average strength of the FUV radiation field appears constant up to redshift z∼6.4, yet the neutral gas density increases as a function of redshift by a factor of ∼100 from z=0 to z=0.2 that persists regardless of various adjustments to our observable quantities. Whilst this evolution could provide an explanation for the observed evolution of the star formation rate density with cosmic time, the result most likely arises from a combination of observational biases when using different suites of emission lines as diagnostic tracers of PDR gas.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: high-redshift - galaxies: ISM - infrared: galaxies - submillimeter: galaxies - ISM: lines and bands - ISM: lines and bands

Simbad objects: 40

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Number of rows : 40
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3193 2
2 NGC 891 H2G 02 22 32.907 +42 20 53.95 11.08 10.81 9.93 7.86   ~ 1612 2
3 NGC 1097 LIN 02 46 19.059 -30 16 29.68 10.46 9.97 9.48 8.72 9.8 ~ 1277 3
4 QSO B0736+01 QSO 07 39 18.03389906 +01 37 04.6177501   16.90 16.47 16.19   ~ 659 1
5 QSO B0748+126 QSO 07 50 52.04573865 +12 31 04.8282079   17.67 17.28 17.16   ~ 309 1
6 LEDA 180962 G 08 36 01.537 +00 26 17.08           ~ 12 0
7 Z 4-89 G 08 37 45.1170513360 -00 51 41.832228564   15.5       ~ 16 0
8 IRAS F08359+0011 G 08 38 31.8062940336 +00 00 44.699785416           ~ 11 0
9 IRAS F08390+0204 G 08 41 39.5490718848 +01 53 46.533031908           ~ 9 0
10 LEDA 1219472 G 08 42 17.8808890920 +02 12 23.218974396           ~ 10 0
11 FIRST J084305.1+010855 LIN 08 43 05.153 +01 08 55.58           ~ 12 0
12 IRAS F08412+0106 G 08 43 50.8281642792 +00 55 34.595857452           ~ 10 0
13 FIRST J084428.4+020659 G 08 44 28.427 +02 06 59.35           ~ 10 0
14 Z 5-4 G 08 44 28.4526107496 +02 03 50.209940664   15.7       ~ 23 0
15 SDSS J084630.85+005055.0 G 08 46 30.8515975896 +00 50 55.070244744           ~ 8 0
16 IRAS 08465-0040 G 08 49 07.1026806192 -00 51 38.123428284           ~ 10 0
17 LEDA 1196839 G 08 51 11.4078099072 +01 30 06.070297716           ~ 15 0
18 IRAS 08486+0114 G 08 51 12.865 +01 03 42.87           ~ 15 0
19 IRAS F08499+0145 G 08 52 34.30704 +01 34 19.4124   20.0   18.8 18.32 ~ 7 1
20 Z 5-23 AGN 08 53 40.7278281216 +01 33 48.644674452   15.20       ~ 38 0
21 IRAS F08511+0024 G 08 53 46.3844650368 +00 12 52.201757196           ~ 16 0
22 NPM1G +00.0231 G 08 53 56.4521887896 +00 12 56.064921408           ~ 17 0
23 IRAS F08515+0123 G 08 54 05.9034906144 +01 11 30.723389664           ~ 18 0
24 LEDA 1219302 G 08 54 50.2112079240 +02 12 08.593127208           ~ 14 0
25 IRAS 08552+0058 rG 08 57 48.0593483352 +00 46 41.385658080           ~ 14 0
26 NPM1G +00.0234 G 08 58 28.5998204904 +00 38 13.637605668           ~ 23 0
27 NPM1G +01.0223 Sy1 08 58 35.9855275488 +01 31 49.507529448   18.57 17.98     ~ 24 0
28 NPM1G +00.0239 rG 09 00 05.0433499416 +00 04 46.769547972           ~ 20 0
29 [VV2006] J090125.8-003703 QSO 09 01 25.8398690376 -00 37 03.125460324   20.20 20.05 19.5   ~ 35 1
30 Z 5-54 rG 09 05 32.5991707680 +02 02 21.890956704   15.6       ~ 15 0
31 IRAS F09052+0113 rG 09 07 50.070 +01 01 41.01           ~ 13 0
32 4C 01.24B QSO 09 09 10.09159883 +01 21 35.6176206   17.63 17.29 17.04   ~ 402 2
33 SDSS J090949.72+014845.6 rG 09 09 49.609 +01 48 47.40           ~ 15 0
34 IRAS 09095+0039 G 09 12 05.8528271184 +00 26 55.918271472           ~ 16 0
35 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5677 6
36 NGC 3372 HII 10 45 02.23 -59 41 59.8           ~ 975 2
37 NGC 4559 H2G 12 35 57.6402869976 +27 57 35.859278160   10.46 10.01     ~ 593 1
38 NAME Centaurus A Sy2 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4320 3
39 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 4160 4
40 M 83 SBG 13 37 00.91920 -29 51 56.7400 8.85 8.11 7.52 7.21   ~ 2453 2

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2023.01.31-09:05:16

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