Mid-infrared imaging and spectrophotometry of N 66 in the SMC with ISOCAM

Details Mid-infrared imaging and spectrophotometry of N 66 in the SMC with ISOCAM Mid-infrared imaging and spectrophotometry of N 66 in the SMC with ISOCAM

2000-06-13

arxiv.org/abs/astro-ph/0006185v1

Astron.Astrophys.362:310-324,2000

Astronomy and Astrophysics

Astrophysics

14 pages, 17 figures, accepted to A&A

Scientific paper

We present observations with the mid-infrared camera ISOCAM on board ISO of the major star-forming region N66 in the Small Magellanic Cloud and of its surroundings. These observations were performed with broad filters and the CVF giving a spectral resolution of about 40. In addition, CO(2-1) data are presented, allowing us to identify and study how hot dust relates with the different phases of the Interstellar Medium present in N66. The spectra are dominated by the strong emission of fine structure line. Monochromatic maps have been made in the [NeIII] 15.6 microns and [SIV] 10.5 microns line. There are significant differences between their distributions, due to the effects of density and of shocks. Aromatic Infrared Bands are seen at various places in the field but they are generally faint. They exhibit a variety of shapes and relative intensities, suggesting that a diversity of carbonaceous materials are present. Silicate emission is also clearly visible in the central condensation and in a few others and emission from hot small grains longward of 10 microns is present in the whole region. All these dust components are heated by the very strong far UV radiation of the many young, massive stars contained in the region. The interstellar radiation field (ISRF) at 1600 A is >= 10^5 times the ISRF of the solar neighborhood in the peaks of MIR emission. The relative contributions of the dust components to the MIR spectra seem to depend on the intensity and the hardness of the far UV field. In general the 15/6.75 microns intensity ratio is higher than in relatively quiescent galactic regions but it is not as high as expected for a linear increase with ISRF. We interpret this behavior as due to the destruction of both AIBs carriers and VSGs in a very high ISRF.

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