Volume 407, Number 1, August III 2003
|Page(s)||225 - 235|
|Section||Interstellar and circumstellar matter|
|Published online||17 November 2003|
High resolution observations of the hot core in G29.96–0.02
University of Puerto Rico, Physics Department, PO Box 23343 University Station, San Juan, PR 00931-3343, USA
2 Istituto di Radio Astronomia, CNR Sezione di Firenze, Largo E. Fermi 5, 50125 Firenze, Italy
3 Osservatorio Astrofisico di Arcetri, INAF, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: firstname.lastname@example.org; email@example.com
4 Arecibo Observatory, Cornell University, HC3 Box 53995, Arecibo, PR 00612, USA e-mail: firstname.lastname@example.org
5 Instituto de Astronomia, Universidad Nacional Autónoma de México, Apdo. Postal 3-72, C.P. 58090, Morelia, Michoacán, Mexico e-mail: email@example.com
6 Washburn Observatory, University of Wisconsin-Madison, 475 North Charter Street, Madison, WI 53706, USA e-mail: firstname.lastname@example.org
Corresponding author: L. Olmi, email@example.com
Accepted: 21 May 2003
We present high angular resolution observations obtained with the Owens Valley and the IRAM Plateau de Bure millimeter-wave interferometers toward the hot core in G29.96–0.02. We observed the ground state (6–5), (6–5), vibrationally excited () (6–5), and the (1–0) rotational transitions, as well as the 2.7 mm continuum emission. Our continuum maps show evidence of a compact source barely resolved whose diameter we estimate to be about 0.06 pc and whose emission mechanism is dominated by thermal emission from warm dust. Both the ground state and the methyl cyanide lines, as well as other serendipituosly detected molecular transitions, arise from a compact source at the same position as the 2.7 mm continuum emission. The observations sample the structure and kinematics of the molecular surroundings of the hot core and from the data we estimate a gas mass of about in a region with a diameter of 0.32 pc, corresponding to an average number density of about 106 cm-3. Our data show evidence of both a temperature and density gradient in the hot core and its molecular surroundings. The density gradient, in particular, is consistent with the infalling scenario suggested by the presence of an East-West oriented velocity gradient, which is however of opposite sign in and . We tentatively interpret the velocity gradient as associated with infall, whereas the gradient, consistent with that measured in by Cesaroni et al. ([CITE]), is likely to trace a massive rotating disk.
Key words: stars: formation / radio lines: ISM / ISM: individual objects: G29.96–0.02 / ISM: molecules
© ESO, 2003
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