Fridlund, C. V. M.; Bergman, P.; White, G. J.; Pilbratt, G. L. and Tauber, J. A.
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|DOI (Digital Object Identifier) Link:||https://doi.org/10.1051/0004-6361:20011519|
|Google Scholar:||Look up in Google Scholar|
The inner three arcminutes surrounding the Class 0/1 binary protostar L1551 IRS5 have been observed using the J=1→0 transitions of the HCO+, H13CO+, 12CO and 13CO molecular species. Since the line core of HCO+ is self reversed over a substantial part of our map, observations of isotopomers such as H13CO+ 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⊙ 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⊙) clumps. One of these features appears to be kinematically disconnected from both the disk and the molecular outflow.
|Item Type:||Journal Article|
|Copyright Holders:||2002 ESO|
|Keywords:||clouds; L1551; jets; outflows; stellar formation; pre-main sequence; radio lines|
|Academic Unit/School:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||G. J. White|
|Date Deposited:||06 Feb 2007|
|Last Modified:||29 Nov 2016 21:39|
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