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Issue A&A
Volume 382, Number 2, February I 2002
Page(s) 573 - 582
Section Diffuse matter in space
DOI http://dx.doi.org/10.1051/0004-6361:20011519



A&A 382, 573-582 (2002)
DOI: 10.1051/0004-6361:20011519

The molecular disk surrounding the protostellar binary L1551 IRS5

C. V. M. Fridlund1, P. Bergman2, G. J. White3, G. L. Pilbratt1 and J. A. Tauber1

1  ESA Astrophysics Mission Division, Research and Scientific Support Department, ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands
2  Centre for Astrophysics and Space Science at Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
3  Unit for Space Sciences and Astronomy, Physics Department, University of Kent, Canterbury CT2 7NR, UK

(Received 24 July 2001 / Accepted 23 October 2001 )

Abstract
The inner three arcminutes surrounding the Class 0/1 binary protostar L1551 IRS5 have been observed using the $J=1\rightarrow0$ transitions of the , , 12CO and 13CO molecular species. Since the line core of is self reversed over a substantial part of our map, observations of isotopomers such as are required in order to estimate the mass of the molecular gas in the immediate vicinity of IRS5. Our observations demonstrate the presence of a large (~7000 AU radius) dense, possibly rotating, molecular disk with a mass of a few $M_{\odot}$ oriented perpendicular to the major axis of an extended molecular outflow. The disk is surrounded by an envelope with a radius of ~10 000 AU that contains two massive (each ~1  $M_{\odot}$) clumps. One of these features appears to be kinematically disconnected from both the disk and the molecular outflow.


Key words: ISM: clouds -- ISM: individual objects: L1551 -- ISM: jets and outflows -- stars: formation -- stars: pre-main sequence -- radio lines: ISM

Offprint request: C. V. M. Fridlund, Malcolm.Fridlund@esa.int

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© ESO 2002


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