EDP Sciences
Free access
Issue
A&A
Volume 371, Number 1, May III 2001
Page(s) 312 - 327
Section Diffuse matter in space
DOI http://dx.doi.org/10.1051/0004-6361:20010356


A&A 371, 312-327 (2001)
DOI: 10.1051/0004-6361:20010356

ISOCAM 3-12 $\mu$m imaging of five galactic compact HII regions

A. Zavagno and V. Ducci

Observatoire de Marseille, 2 place Le Verrier, 13248 Marseille Cedex 4, France

(Received 23 September 1999 / Accepted 7 March 2001)

Abstract
We present 3-12 $\mu$m ISOCAM observations of the five Galactic compact H II regions Sh 61, Sh 138, Sh 152, Sh 156 and Sh 186. The unidentified infrared bands (UIBs) centred at 3.3, 6.2, 7.7, 8.6 and 11.2 $\mu$m -and underlying continuum -are imaged using the SW1, SW2, LW4, LW6 and LW8 filters. Images are also obtained at 5.985, 6.911, 8.222, 10.520 and 12.000 $\mu$m using the circular variable filter (CVF). We show that the 5.985 $\mu$m emission represents a true continuum reference for the 6.2 $\mu$m band, allowing a derivation of this band's properties. Due to uncertainties in the continuum estimates, only lower limits can be given for the 3.3, 7.7 and 11.3 $\mu$m band fluxes. These limits agree with previous results found in the literature. The distribution of the bands coincide. The 3.3 $\mu$m emission is not observed in high extinction zones, suggesting a lower temperature of the carriers and/or a higher abundance of larger molecules in those zones. The 6.2 $\mu$m band emission peaks outside the ionized zone, in the photodissociation region. The 6.2 $\mu$m band luminosity correlates with the far UV field intensity, suggesting a UV excitation. We also find a correlation between the spatial distribution of the 6.2 $\mu$m band emission and zones of strong 2.122 $\mu$m H2 emission due to ultraviolet fluorescence. This suggests that both emissions are due to UV excitation. The 6.2 $\mu$m emission is slightly closer to the exciting star. This suggests that the band carriers survive in the H I zone. The 12 $\mu$m emission traces the continuum emission from very small grains, when present, and follows well the distribution of UIB emission. This suggests a link between the two emission carriers. The emission peak observed on the star in Sh 61 and Sh 156 indicates that the continuum from very small grains dominates the emission in highly excited regions.


Key words: ISM: H II regions -- Dust ISM: extinction -- ISM: lines and bands

Offprint request: A. Zavagno, Zavagno@observatoire.cnrs-mrs.fr

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