Free Access
Issue
Astron. Astrophys. Suppl. Ser.
Volume 129, Number 3, May_I 1998
Page(s) 495 - 504
DOI https://doi.org/10.1051/aas:1998403
Published online 15 May 1998
DOI: 10.1051/aas:1998403

A&A Supplement series, Vol. 129, May I 1998, 495-504

Received July 17; accepted October 24, 1997

Near-infrared images of star forming regions containing masers

Las Campanas observations of 31 southern sourcesgif,gif

L. Testitex2html_wrap518 - M. Fellitex2html_wrap520 - P. Persitex2html_wrap522 - M. Rothtex2html_wrap524

Send offprint request: Testi: Caltech, lt@astro.caltech.edu

tex2html_wrap526  Division of Physics, Mathematics and Astronomy, California Institute of Technology, MS105-24, Pasadena, CA 91125, U.S.A.
tex2html_wrap528  Dipartimento di Astronomia e Scienza dello Spazio, Università degli Studi di Firenze, Largo E. Fermi 5, I-50125 Firenze, Italy
tex2html_wrap530  Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy
tex2html_wrap532  Istituto di Astrofisica Spaziale, C.N.R., C.P. 67, I-00044 Frascati, Italy
tex2html_wrap534  Las Campanas Observatory, Casilla 601, La Serena, Chile

Abstract:

We present sensitive high resolution near infrared (NIR) broad band (J, H, and K) observations of a sample of 31 Star Forming Regions (SFRs) which contain H2O and OH maser sources.

The observations are aimed at the detection and characterization of Young Stellar Objects (YSOs) which may be the source of excitation of the maser emission. In spite of the large number of sources detected in the regions, using positional coincidence and NIR colours we are able to reliably identify K-band sources related to the masing gas in a large fraction of the observed regions.

The NIR infrared sources selected from close positional coincidence with the maser show strong NIR excesses and most probably represent the YSOs still embedded in their parental cocoon where the maser emission occurs.

keywords: masers -- star formation -- circumstellar matter -- infrared: ISM: continuum; stars

SIMBAD Objects

Copyright by the European Southern Observatory (ESO)

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