ISO-SWS Observations on Proto-Planetary System Candidates

Bibcode
2000ESASP.456..219P
Palacios, J.; Wesselius, P. R.; Eiroa, C.; Mora, A.; Montesinos, B.; Merin, B.; Solano, E.; Alberdi, A.; Collier Cameron, A.; Davies, J. K.; Deeg, H. J.; Ferlet, R.; Garzón, F.; Grady, C. A.; Harris, A.; Horne, K.; Miranda, L. F.; Oudmaijer, R. D.; Penny, A.; Quirrenbach, A.; Rauer, H.; Schneider, J.; Tsapras, Y.; de Winter, D.
Bibliographical reference

ISO beyond the peaks: The 2nd ISO workshop on analytical spectroscopy. Eds. A. Salama, M.F.Kessler, K. Leech & B. Schulz. ESA-SP 456. p.219

Advertised on:
11
2000
Number of authors
24
IAC number of authors
0
Citations
0
Refereed citations
0
Description
We present a preliminary analysis of ISO-SWS spectra of a sample of Vega-type and pre-main sequence stars, which were observed from the ground in a project devoted to the study of formation and evolution of planetary systems, carried out during the 1998 International Time of the Canary Islands Observatories. ISO-SWS covers many interesting features expected to be present in Vega-type and pre-main sequence objects. Most of the Vega-type stars shows photospheric spectral energy distributions up to ≈ 10 μm, while an IR excess is normally observed at wavelengths larger than ≈ 20 μm. Pre-main sequence (PMS) stars usually shows IR excesses along the whole SWS spectral range. The 10 μm silicate feature is observed in emission towards most of the PMS stars, while it is observed in only one Vega-type star in our sample, 51 Oph. The comparison of the silicate features observed towards the protoplanetary systems with the silicate band profiles of the Trapezium and comet Kohoutek suggests a better agreement with the solar system cometary silicates.
Type
Non-refereed
Pre-main sequence stars

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