SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 345, 949-964 (1999)

Next Section Table of Contents

Unveiling the disk-jet system in the massive (proto)star IRAS 20126+4104

R. Cesaroni 1, M. Felli 1, T. Jenness 2, R. Neri 3, L. Olmi 4, M. Robberto 5,6, L. Testi 1,7 and C.M. Walmsley 1

1 Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy
2 Joint Astronomy Centre, 660 N. A`ohoku Place, Hilo, HI 96720, USA
3 IRAM, 300 Rue de la Piscine, Domaine Universitaire, F-38406 St. Martin d'Hères Cedex, France
4 LMT Project and FCRAO, University of Massachusetts, 630 L.G.R.C., Amherst, MA 01003, USA
5 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
6 Osservatorio Astronomico di Torino, Str. Osservatorio 20, I-10025 Pino Torinese, Italy
7 Division of Mathematics, Physics and Astronomy, MS105-24, California Institute of Technology, Pasadena, CA 91125, USA

Received 18 December 1998 / Accepted 9 March 1999

Abstract

We present the results of line and continuum observations towards the source IRAS 20126+4104, performed at 1.3 mm and 3.5 mm with the Plateau de Bure interferometer, from 350 µm to 2 mm with the James Clerk Maxwell telescope, and at 10 and 20 µm with the United Kingdom infrared telescope. The results fully confirm the findings of Cesaroni et al. (1997), namely that IRAS 20126+4104 is a very young stellar object embedded in a dense, hot core and lying at the centre of a rotating disk. The bipolar jet imaged by Cesaroni et al. (1997) in the 2.122 µm H2 line is seen also in the SiO(2-1) transition, which allows to study the velocity field in the jet. A simple model is developed to obtain the inclination angle of the jet (and hence of the disk axis), which turns out to be almost perpendicular to the line of sight. By studying the diameter of the disk in different transitions and the corresponding line widths and peak velocities, one can demonstrate that the disk is Keplerian and collapsing, and thus compute the mass of the central object and the accretion luminosity. We show that if all the mass inducing the Keplerian rotation is concentrated in a single star, then this cannot be a ZAMS star, but more likely a massive protostar which derives its luminosity from accretion.

Key words: ISM: clouds – ISM: individual objects: IRAS 20126+4104 – ISM: molecules – radio lines: ISM

Send offprint requests to: R. Cesaroni (cesa@arcetri.astro.it)

SIMBAD Objects

Contents

Next Section Table of Contents

© European Southern Observatory (ESO) 1999

Online publication: April 28, 1999
helpdesk.link@springer.de