2012A&A...548A..91L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.15CEST11:24:20

2012A&A...548A..91L - Astronomy and Astrophysics, volume 548A, 91-91 (2012/12-1)

Physical conditions in the gas phases of the giant H II region LMC-N11 unveiled by Herschel. I. Diffuse [C II] and [O III] emission in LMC-N11B.

LEBOUTEILLER V., CORMIER D., MADDEN S.C., GALLIANO F., INDEBETOUW R., ABEL N., SAUVAGE M., HONY S., CONTURSI A., POGLITSCH A., REMY A., STURM E. and WU R.

Abstract (from CDS):

The Magellanic Clouds provide a nearby laboratory for metal-poor dwarf galaxies. The low dust abundance enhances the penetration of UV photons into the interstellar medium (ISM), resulting in a relatively larger filling factor of the ionized gas. Furthermore, there is very likely a molecular gas reservoir probed by the [CII] 157µm line not traced by CO(1-0), the so-called ``dark'' gas. The Herschel Space Telescope allows us to observe far-infrared (FIR) cooling lines and to examine the physical conditions in the gas phases of a low-metallicity environment to unprecedented, small spatial scales. Our objective is to interpret the origin of the diffuse emission of FIR cooling lines in the H region N11B in the Large Magellanic Cloud. We first investigate the filling factor of the ionized gas. We then constrain the origin of the [CII] line by comparing to tracers of the low-excitation ionized gas and of photodissociation regions (PDRs). We present Herschel/PACS maps of N11B in several tracers, [CII] 157µm, [OI] 63µm and 145µm, [NII] 122µm, [NIII] 57µm, and [OIII] 88µm. Optical images in Hα and [OIII] 5007Å were used as complementary data to investigate the effect of dust extinction. Observations were interpreted with photoionization models to infer the gas conditions and estimate the ionized gas contribution to the [CII] emission. PDRs were probed through polycyclic aromatic hydrocarbons (PAHs) observed with the Spitzer Space Telescope. [OIII] 88µm is dominated by extended emission from the high-excitation diffuse ionized gas. This is the brightest FIR line throughout N11B, ∼4 times brighter than [CII]. We find that about half of the emission from the ionized gas is extinguished by dust. We modeled [OIII] around each O-type star and find that the density of the ISM is ≲16cm–3 on large scales. The extent of the [OIII] emission suggests that the medium is rather fragmented, allowing far-UV photons to permeates the ISM to scales of >30pc. Furthermore, by comparing [CII] with [NII] 122µm, we find that 95% of [CII] arises in PDRs, except toward the stellar cluster for which as much as 15% could arise in the ionized gas. We find a remarkable correlation between [CII]+[OI] and PAH emission, with [CII] dominating the cooling in diffuse PDRs and [OI] dominating in the densest PDRs. The combination of [CII] and [OI] provides a proxy for the total gas cooling. Our results suggest that PAH emission describes better the gas heating in PDRs as compared to the total infrared emission.

Abstract Copyright:

Journal keyword(s): infrared: ISM - HII regions - ISM: lines and bands - dust, extinction - methods: data analysis

CDS comments: Y shaped Cloud not in Simbad. Paragraph 2.2 star A from Walborn & Parker 1992 not in Simbad.

Simbad objects: 44

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Number of rows : 44

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 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9447 1
2 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5669 1
3 LHA 120-N 11I HII 04 55 50 -66 34.4           ~ 16 0
4 NGC 1760 HII 04 56 20.8 -66 32 13           ~ 29 0
5 HD 32228 WR* 04 56 34.666 -66 28 26.34   10.685 10.830     WC4+O9.5II: 90 0
6 NGC 1761 As* 04 56 39 -66 29.0     9.94     ~ 96 0
7 PGMW 3042 * 04 56 39.176 -66 24 49.94 13.590 14.514 14.461   14.708 O9.5Vn 11 0
8 PGMW 3053 * 04 56 41.0477932862 -66 24 40.540750469   13.04 13.13     O6II(f+) 11 0
9 PGMW 3058 * 04 56 42.146 -66 24 54.61 12.901 14.092 14.089   13.991 O3V((f*)) 16 0
10 [L72] LH 10-3061 * 04 56 42.460 -66 25 18.09 12.699 13.595 13.491   13.405 ON2III(f*) 25 0
11 [HT83] alf * 04 56 43.209 -66 25 02.57 11.057 12.335 12.47   10.944 O6V 16 1
12 PGMW 3073 * 04 56 43.334 -66 24 54.55 12.895 14.734 13.868   14.181 O6.5V 10 0
13 PGMW 3090 * 04 56 44.536 -66 24 56.28 12.522 14.311 13.303   13.764 B0:V 5 0
14 PGMW 3089 * 04 56 44.5485567603 -66 24 33.717269326   14.528 14.650     O8V 5 0
15 PGMW 3100 * 04 56 45.2038993380 -66 25 10.779707928 13.007 13.736 13.648   13.547 O5III(f+) 12 0
16 PGMW 3102 * 04 56 45.3658193611 -66 24 46.427644821 12.601 13.319 13.416   13.502 O7V 11 0
17 PGMW 3103 * 04 56 45.433 -66 24 38.26   15.64 15.781     O9.5:IV: 4 0
18 PGMW 3115 * 04 56 46.548 -66 24 51.56 14.103 14.942 14.771   15.005 O9V 4 0
19 PGMW 3120 * 04 56 46.812 -66 24 46.72 11.700 12.496 12.466   12.464 O5.5V((f*)) 25 0
20 PGMW 3123 * 04 56 47.08 -66 24 31.2   14.464 14.570     O8.5V 8 0
21 PGMW 3126 * 04 56 47.107 -66 24 59.33 13.391 14.371 14.050   14.034 O6.5V 6 0
22 PGMW 3128 * 04 56 47.2379973322 -66 24 42.203919645   14.59 14.71     B0.2V 10 0
23 IRAS 04566-6629 mul 04 56 47.4 -66 24 30           ~ 3 0
24 BRRG I1 IR 04 56 47.5 -66 24 43           ~ 1 0
25 [IJC2004] B0456-6629(W2) Rad 04 56 47.8 -66 24 34           ~ 2 0
26 BRRG I2 IR 04 56 48.5 -66 24 30           ~ 1 0
27 BRRG I3 IR 04 56 49.0 -66 24 22           ~ 1 0
28 IC 2115 HII 04 56 50 -66 24.9           ~ 7 2
29 LHA 120-N 11 HII 04 56 51.4 -66 24 24           ~ 234 0
30 NGC 1763 As* 04 56 51.5 -66 24 25     9.40     ~ 154 3
31 PGMW 3168 * 04 56 54.4601951589 -66 24 15.871362997   13.57 13.68     O7II(f) 16 0
32 PGMW 3173 * 04 56 54.7169427454 -66 24 54.517643598   14.56 14.71     O4-O6V 5 0
33 NAME Kiwi Shaped Cloud ISM 04 56 57.5 -66 24 40           ~ 2 0
34 PGMW 3204 * 04 56 58.7897 -66 24 40.710   13.85 14.02     O6.5V((f)) 15 0
35 HD 268721 * 04 56 58.971 -66 24 38.16 11.374 11.935 11.859   11.281 O3III(f*)+OB 21 0
36 PGMW 3211 *i* 04 56 59.09 -66 24 36.6   15.568 15.739     ~ 3 0
37 BI 42 * 04 57 00.859 -66 24 25.12 11.998 12.768 12.896   12.663 O8V 20 0
38 PGMW 3224 EB* 04 57 00.8736795052 -66 23 57.319380258 13.369 14.167 14.043   13.820 O6III 9 0
39 [GC2009] J045702.52-662503.3 IR 04 57 02.52 -66 25 03.3           ~ 3 0
40 IRAS 04571-6627 mul 04 57 15.5 -66 23 14           ~ 52 1
41 HD 32340 Em* 04 57 16.253 -66 23 20.94   13.11 12.45 14.00   O3-O6V 77 0
42 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14833 1
43 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 716 0
44 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1736 1

    Equat.    Gal    SGal    Ecl

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2020.07.15-11:24:20

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