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Astron. Astrophys. 346, 205-210 (1999)

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Infrared spectra of young stars in Chamaeleon *

J. Gürtler 1, K. Schreyer 1, Th. Henning 1, D. Lemke 2 and W. Pfau 1

1 Astrophysikalisches Institut und Universitäts-Sternwarte an der Friedrich-Schiller-Universität Jena, Schillergässchen 2-3, D-07745 Jena, Germany
2 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany

Received 1 December 1998 / Accepted 19 February 1999

Abstract

We present infrared spectra covering the wavelength ranges 3.1-5.0 µm and 5.8-11.6 µm for 9 young stars located in the Chamaeleon I dark cloud. The spectra were taken with the spectrophotometer of ISO (ISOPHOT-S). The spectra of three stars which illuminate reflection nebulae are dominated by the series of strong emission features generally ascribed to polycyclic aromatic hydrocarbons. Three or possibly four stars classified as T Tauri stars show the 10 µm silicate band in emission, whereas another object, T42, shows the silicate band in absorption and could be a T Tau star with a disk seen edge-on. The last source, Cha IRN, is a deeply embedded young stellar object. Its spectrum is characterized by deep absorption bands due to various interstellar ices, but shows a very weak silicate band only.

Key words: stars: circumstellar matter – ISM: dust, extinction – ISM: individual objects: Chamaeleon clouds – infrared: ISM: lines and bands

* Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, Netherlands and the United Kingdom) with the participation of ISAS and NASA

Send offprint requests to: J. Gürtler (guertler@astro.uni-jena.de)

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© European Southern Observatory (ESO) 1999

Online publication: May 6, 1999
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