2019A&A...626A..23C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST22:19:19

2019A&A...626A..23C - Astronomy and Astrophysics, volume 626A, 23-23 (2019/6-1)

The Herschel Dwarf Galaxy Survey. II. Physical conditions, origin of [C II] emission, and porosity of the multiphase low-metallicity ISM.

CORMIER D., ABEL N.P., HONY S., LEBOUTEILLER V., MADDEN S.C., POLLES F.L., GALLIANO F., DE LOOZE I., GALAMETZ M. and LAMBERT-HUYGHE A.

Abstract (from CDS):

The sensitive infrared telescopes, Spitzer and Herschel, have been used to target low-metallicity star-forming galaxies, allowing us to investigate the properties of their interstellar medium (ISM) in unprecedented detail. Interpretation of the observations in physical terms relies on careful modeling of those properties. We have employed a multiphase approach to model the ISM phases (HII region and photodissociation region) with the spectral synthesis code Cloudy. Our goal is to characterize the physical conditions (gas densities, radiation fields, etc.) in the ISM of the galaxies from the Herschel Dwarf Galaxy Survey. We are particularly interested in correlations between those physical conditions and metallicity or star-formation activity. Other key issues we have addressed are the contribution of different ISM phases to the total line emission, especially of the [CII]157 µm line, and the characterization of the porosity of the ISM. We find that the lower-metallicity galaxies of our sample tend to have higher ionization parameters and galaxies with higher specific star-formation rates have higher gas densities. The [CII] emission arises mainly from PDRs and the contribution from the ionized gas phases is small, typically less than 30% of the observed emission. We also find a correlation - though with scatter - between metallicity and both the PDR covering factor and the fraction of [CII] from the ionized gas. Overall, the low metal abundances appear to be driving most of the changes in the ISM structure and conditions of these galaxies, and not the high specific star-formation rates. These results demonstrate in a quantitative way the increase of ISM porosity at low metallicity. Such porosity may be typical of galaxies in the young Universe.

Abstract Copyright: © D. Cormier et al. 2019

Journal keyword(s): radiative transfer - HII regions - photon-dominated region - galaxies: dwarf - galaxies: ISM - infrared: ISM

VizieR on-line data: <Available at CDS (J/A+A/626/A23): obs.dat model1.dat model2.dat>

Status at CDS:   Tables of objects will be appraised for possible ingestion in SIMBAD.

Simbad objects: 47

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Number of rows : 47

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 HS 0017+1055 G 00 20 21.0 +11 12 21           ~ 16 0
2 IC 10 G 00 20 23.16 +59 17 34.7   13.6 9.5     ~ 1008 0
3 ESO 350-38 AGN 00 36 52.489 -33 33 17.23   14.31 14.41 13.49   ~ 289 0
4 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9440 1
5 SDSS J005456.38+255307.8 G 00 54 56.387 +25 53 07.85           ~ 14 0
6 NGC 450 H2G 01 15 30.470 -00 51 38.98   13.4   13.3 13.2 ~ 202 0
7 NGC 625 AGN 01 35 04.632 -41 26 10.32 12.37 11.78 11.25 11.03 11.5 ~ 247 2
8 MCG+01-05-030 H2G 01 44 41.3 +04 53 26 15.07 15.50 15.16 14.86 14.58 ~ 79 0
9 NGC 1140 EmG 02 54 33.5258827369 -10 01 43.135585379 12.41 12.84 12.49 13.6 13.5 ~ 260 1
10 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5665 1
11 SBSG 0335-052 bCG 03 37 44.04 -05 02 38.5     16.65     ~ 433 1
12 NGC 1569 IG 04 30 49.186 +64 50 52.52 11.72 11.86 11.03     ~ 1147 3
13 NGC 1705 SBG 04 54 13.500 -53 21 39.82 12.32 12.96 12.56 12.58 12.9 ~ 593 1
14 NGC 1741 IG 05 01 38.3 -04 15 25   13.7   13.02 13.6 ~ 250 0
15 UGCA 116 H2G 05 55 42.645 +03 23 32.23 10.74 11.68 11.46   11.82 ~ 500 0
16 NGC 2366 H2G 07 28 51.85 +69 12 31.1 12.25 11.86 11.39 11.33   ~ 702 0
17 LEDA 2790884 bCG 08 25 55.521 +35 32 31.96   18.2       ~ 102 1
18 ESO 495-21 bCG 08 36 15.190 -26 24 33.66 12.04 11.93 11.45 11.09 12.3 ~ 499 3
19 UGC 4483 GiG 08 37 03.29 +69 46 29.2 15.70 15.46 14.98 14.89   ~ 265 0
20 Mrk 116 PaG 09 34 02.1 +55 14 25           ~ 996 1
21 Mrk 33 IG 10 32 31.956 +54 24 03.53 13.29 13.66 13.13 12.71 12.27 ~ 322 1
22 NGC 3353 AGN 10 45 22.390 +55 57 37.36 12.90 13.25 12.79     ~ 319 1
23 Mrk 153 G 10 49 05.036 +52 20 07.77   14.6       ~ 67 0
24 UGC 6456 bCG 11 28 00.43 +78 59 38.4   14.50       ~ 305 1
25 Mrk 1450 H2G 11 38 35.6604109660 +57 52 26.730510064   15.5       ~ 101 1
26 Mrk 1304 IG 11 42 12.253 +00 20 03.68   14.16 13.67 13.41 13.03 ~ 150 0
27 LEDA 37102 Sy1 11 51 33.3534243441 -02 22 21.893770899   17       ~ 143 0
28 LEDA 2815986 G 12 02 02.493 +54 15 51.05   18.0       ~ 63 0
29 LEDA 39055 EmG 12 14 02.479 +53 45 17.35   18       ~ 68 0
30 NGC 4228 SBG 12 15 39.174 +36 19 36.80 10.63 10.30 9.93 9.74   ~ 863 1
31 LEDA 39402 H2G 12 17 17.093 -28 02 32.67   17       ~ 123 0
32 LEDA 101471 EmG 12 24 36.7369432538 +37 24 35.833921444           ~ 27 0
33 Mrk 209 bCG 12 26 16.02 +48 29 36.6   15.3       ~ 301 0
34 2MASX J12390403+3920437 H2G 12 39 04.039 +39 20 43.42   18.7       ~ 21 0
35 LEDA 2790846 EmG 12 51 52.4 +49 03 25   18.0       ~ 47 0
36 NGC 4861 H2G 12 59 02.340 +34 51 33.98   12.90 12.32     ~ 355 2
37 LEDA 101484 EmG 13 06 24.193 +35 13 43.00           ~ 27 0
38 LEDA 169741 H2G 13 21 19.704 +32 08 25.17   19.123       ~ 21 0
39 LEDA 46982 bCG 13 25 48.60 -11 36 38.0           ~ 71 0
40 LEDA 101493 EmG 13 33 08.394 +36 36 32.45   16.7       ~ 21 0
41 NGC 5253 AGN 13 39 55.990 -31 38 24.11 11.48 10.94 10.49 10.33   ~ 1269 4
42 MCG+07-29-060 QSO 14 17 01.716 +43 30 13.52   15.6       ~ 152 0
43 UGC 9497 H2G 14 44 12.8032800372 +42 37 43.773570223   16.0       ~ 60 0
44 NVSS J153412+571655 rG 15 34 13.3860337334 +57 17 07.294760490   15.8       ~ 65 1
45 Mrk 930 AGN 23 31 58.630 +28 56 50.51 14.27 15.04 14.63 14.56 14.46 ~ 120 0
46 HS 2352+2733 bCG 23 54 56.7 +27 49 59           ~ 12 0
47 NAME Local Group GrG ~ ~           ~ 6970 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-22:19:19

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