The disk-outflow system around the high-mass (proto)star IRAS 20126+4104


R. Cesaroni (1), M. Felli (1), L. Testi (2), C.M. Walmsley (1,3), L. Olmi (4)

(1) Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125 Firenze, Italy

(2) Dipartimento di Astronomia e Scienza dello Spazio, Universitá di Firenze, Largo E. Fermi, 5, I-50125 Firenze, Italy

(3) I. Physikalisches Institut der Universitaet zu Koeln, Zuelpicherstrasse 77, D-50937 Koeln, Germany

(4) Cornell University, NAIC, Arecibo Observatory, P.O. Box 995, Arecibo, P.R. 00613


We have used the Pico Veleta 30-m telescope and the Plateau de Bure interferometer to obtain maps of the molecular gas associated with \I\ in 11 rotational transitions. We also present near infrared images of the same region taken with the TIRGO and NOT telescopes. A molecular clump centred on the \WAT\ masers associated with the IRAS source is found. A molecular bipolar outflow is clearly evidenced by the interferometer maps in the \HCOp(1--0) line, originating at the center of the clump; also, the images in the K-band continuum and in the \HM\ $v=1\rightarrow0$ $S(0)$ vibrational line trace the same bipolar structure seen in \HCOp. A flattened structure elongated in the direction perpendicular to the outflow axis is seen in the \MCN(5--4) line: we interpret this as a rotating disk with a very young massive early type star at its centre. We conclude that \I\ represents a beautiful example of a disk-outflow system associated with an early type (proto)star, prior to the development of an ultracompact \HII\ region.

Mantained by: Leonardo Testi