Volume 469, Number 2, July II 2007
|Page(s)||539 - 551|
|Section||Interstellar and circumstellar matter|
|Published online||05 March 2007|
ISOCAM mid-infrared spectroscopy and NIR photometry of the HII complex N4 in the Large Magellanic Cloud*
Max-Planck-Institut für Extraterrestrische Physik (MPE), Postfach 1312, 85741 Garching, Germany e-mail: firstname.lastname@example.org
2 Departamento de Astronomía Universidad de Chile, Casilla 36–D, Santiago, Chile
3 CEA/DSM/DAPNIA/Service d'Astrophysique, CE Saclay, 91191 Gif-sur-Yvette Cedex, France
4 Institut d'Astrophysique Spatiale, Bat. 121, Université Paris XI, 91450 Orsay Cedex, France
5 Departamento de Física, Universidad de La Serena, Chile
Accepted: 16 January 2007
Context.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).
Aims. 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.
Methods.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.
Results. 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 Stasińska (1982, A&AS, 48, 2999) 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 HII region containing an embedded young stellar object.
Key words: HII regions / ISM: lines and bands / ISM: structure
© ESO, 2007
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