The Evolution of Stars seen with ISOCAM - the Need for NICMOS and VLT Follow Up.

Details The Evolution of Stars seen with ISOCAM - the Need for NICMOS and VLT Follow Up. The Evolution of Stars seen with ISOCAM - the Need for NICMOS and VLT Follow Up.

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998esoc...55..110s&link_type=abstract

NICMOS and the VLT: A New Era of High Resolution Near Infrared Imaging and Spectroscopy, Pula, Sardinia, Italy, June 26-27th 199

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Scientific paper

Three examples are presented of how ISOCAM sees the process of stellar evolution. i) Standard staring and coronographic observations with ISOCAM towards BD+31 643 are presented. The morphology of the detected emission is quite similar to a proto-planetary disk. ii) The class 0 object HH108MMS is detected at 15 mic. in absorption against the diffuse interstellar background. This detection confirms its protostellar nature. iii) A ring of organic matter is detected around the pre--main--sequence Herbig AeBe star HD97300. The images show extended emission, an elliptical ring structure of size about 0.045x0.03 pc as well as two peaks of emission, separated by about 3" (240 AU). One of the two peaks coincides with the position of HD97300, while the other may be an embedded companion. The data show that the emission in this region is dominated by the infrared emission bands centered at 6.2, 7.7, 8.7, 11.3 and 12.5 microns, with a very small contribution from continuum emission at longer wavelengths. The spectra are fit with a three component dust model which includes organic molecules such as polycyclic aromatic hydrocarbons, very small graphite and very small silicates, as well as large grains. The fit to the ISOCAM data is very good if one applies a classical oscillator model for the infrared emission bands. The new fitting procedure allows to estimate the total mass of the ring, which is ~0.03 Msun.

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