Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (58) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (4)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
A massive young embedded object associated with the UC H II region G31.41+0.31
Authors:
Cesaroni, R.; Olmi, L.; Walmsley, C. M.; Churchwell, E.; Hofner, P.
Affiliation:
AA(Osservatorio Astrofiscio di Arcetri, Firenze, Italy), AB(Osservatorio Astrofiscio di Arcetri, Firenze, Italy), AC(Max-Planck-Institut für Radioastronomie, Bonn, Germany), AD(Max-Planck-Institut für Radioastronomie, Bonn, Germany), AE(University of Wisconsin-Madison, Madison, WI, US)
Publication:
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 435, no. 2, p. L137-L140 (ApJL Homepage)
Publication Date:
11/1994
Category:
Astronomy
Origin:
STI
NASA/STI Keywords:
Acetonitrile, Astronomical Maps, Galactic Evolution, H Ii Regions, Interferometers, Interstellar Matter, Star Formation, Stellar Cores, Ammonia, Astronomical Observatories, Infrared Astronomy Satellite, Molecular Gases, Radio Jets (Astronomy)
DOI:
10.1086/187613
Bibliographic Code:
1994ApJ...435L.137C

Abstract

We have used the institute for radio astronomy in the millimeter range (IRAM) Plateau de Bure Interferometer to make high angular resolution observations of the star-forming region surrounding the ultracompact H II region G31.41+0.31. We have produced maps in the ground state CH3CN(6-5), CH3(13)CN(6-5) and vibrationally excited CH3CN(6-5) transitions, and in the 3 mm continuum emission. From these, we derive estimates of the size and mass of the hot molecular core known from earlier ammonia observations. The core angular diameter as measured in both methyl cyanide and the 3 mm continuum is approximately 1 sec corresponding to approximately 0.04 pc. If the continuum emission is due to heated dust, we derive a mass of approximately 1000 solar mass, but with large uncertainties. A remarkable velocity gradient (approximately 400 km/s/pc) in the SW-NE direction is observed in CH3CN implying an equilibrium mass approximately 1000 solar mass, consistent with the value quoted above. We discuss two possible scenarios (disk or outflow) for explaining this gradient and conclude that the molecular core must be dynamically unstable.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences



More Article Retrieval Options

HELP for Article Retrieval


Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints