2007A&A...469..539C


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.07CET03:38:09

2007A&A...469..539C - Astronomy and Astrophysics, volume 469, 539-551 (2007/7-2)

ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud.

CONTURSI A., RUBIO M., SAUVAGE M., CESARSKY D., BARBA R. and BOULANGER F.

Abstract (from CDS):

We present the analysis of ISOCAM-CVF and the J, H, and Ks photometry data for the HII region complex N4 in the Large Magellanic Cloud (LMC). The aim is twofold: 1) to study the connection between the interstellar medium and the star content of this region; 2) to investigate the effects of the lower-than-Galactic metallicity on dust properties. A dust-features - gas lines - continuum fitting technique on the whole ISOCAM-CVF data cube allows the production of images in each single emission and detailed analysis of dust (both continuum and bands), and ionized gas. The near infrared (NIR) photometry provides, for the first time, information on the stellar content of N4. The mid-infrared (MIR) spectral characteristics of N4 are those expected for an HII region complex, i.e. very similar to those observed in galactic HII regions. The images in single dust feature bands and gas lines clearly show that the HII region core is completely devoid of the carriers responsible for the aromatic features (AFs). On the other hand, the ionized gas arises almost completely in this dust cavity, where the two main exciting stars of N4 are also located. The HII region models from Stasinska (1982A&AS...48..299S) predict an HII region size that corresponds to the observed size of the dust cavity. We find evidence that the effect of lower-than-Galactic metallicity (although not as extreme as in the case of LMC) on the carriers responsible for the AFs is not to prevent their formation or to modify their chemical properties, but to enhance their destruction by the high and hard interstellar radiation field. We argue that this is the dominant process responsible for the absence of AFs in the HII region core. We show that this mechanism is more efficient on smaller dust particles/molecules thus affecting the dust-size distribution. We argue that effects on dust-size distribution, rather than the different dust properties due to a lower metallicity, should be taken into account when analyzing more distant, relatively low-metallicity galaxies. Finally, the analysis of the stellar content of N4 reveals 7 stars: 4 reddened O MS stars and three stars with envelopes. In particular, one of these seems to be an ultra compact HIIregion containing an embedded young stellar object.

Abstract Copyright:

Journal keyword(s): HII regions - ISM: lines and bands - ISM: structure

Nomenclature: Fig.1: [CRS2007] Star A (Nos A-B). Fig.3: [CRS2007] Knot N (Nos 1-2). Fig.5, Table 1: [CRS2007] Star N (Nos 1-7).

Simbad objects: 20

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Number of rows : 20

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 [RLB93] SMC-B1 1 MoC 00 45 32.7 -73 18 46           ~ 33 0
2 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3002 2
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9710 1
4 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5868 1
5 WOH S 53 * 04 51 58.3447456204 -66 54 52.443848861   12.75 10.97     M2 7 0
6 NGC 1714 EmO 04 52 08.4 -66 55 23   11.51 11.61     ~ 81 2
7 NGC 1715 EmO 04 52 11.7 -66 54 29           ~ 23 0
8 NGC 1731 As* 04 53 15 -66 55.6           ~ 40 0
9 LHA 120-N 11 HII 04 56 51.4 -66 24 24           ~ 238 0
10 NGC 1808 Sy2 05 07 42.343 -37 30 46.98 11.05 10.80 9.94 9.36 10.2 ~ 663 3
11 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15214 1
12 2MASS J05383461-6905569 Y*O 05 38 34.619 -69 05 56.92     18.41   16.75 ~ 16 0
13 NAME 30 Dor Nebula SFR 05 38 36.0 -69 05 11           ~ 1060 2
14 SSTISAGEMA J053846.84-690505.4 IR 05 38 46.84 -69 05 05.4           ~ 9 0
15 30Dor-NIC 12d Y*O 05 38 47.02 -69 05 01.7           ~ 11 0
16 LEDA 42639 G 12 42 11.394 +33 45 32.76   14.5       ~ 11 0
17 GRS G308.60 +00.60 HII 13 39.9 -61 45           ~ 96 0
18 NGC 5253 AGN 13 39 55.990 -31 38 24.11 11.48 10.94 10.49 10.33   ~ 1282 4
19 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3138 1
20 NGC 7023 RNe 21 01 36.9 +68 09 48           ~ 642 0

    Equat.    Gal    SGal    Ecl

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