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Envelope Structure on 700 AU Scales and the Molecular Outflows of Low-Mass Young Stellar Objects

Hogerheijde, Michiel R. and van Dishoeck, Ewine F. and Blake, Geoffrey A. and van Langevelde, Huib Jan (1998) Envelope Structure on 700 AU Scales and the Molecular Outflows of Low-Mass Young Stellar Objects. Astrophysical Journal, 502 (1). pp. 315-336. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20120913-113949968

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Abstract

Aperture synthesis observations of HCO^+ J = 1-0,^(13)CO 1-0, and C18O 1-0 obtained with the Owens Valley Millimeter Array are used to probe the small-scale (5" ≈ 700 AU) structure of the molecular envelopes of a well-defined sample of nine embedded low-mass young stellar objects in Taurus. The interferometer results can be understood in terms of: (1) a core of radius ≾1000 AU surrounding the central star, possibly flattened and rotating; (2) condensations scattered throughout the envelope that may be left over from the inhomogeneous structure of the original cloud core or that may have grown during collapse; and (3) material within the outflow or along the walls of the outflow cavity. Masses of the central cores are 0.001-0.1 M_☉, and agree well with dust continuum measurements. Averaged over the central 20" (3000 AU) region, an HCO^+ abundance of 4 × 10^(-8) is inferred, with a spread of a factor of 3 between the different sources. Reanalysis of previously presented single-dish data yields an HCO^+ abundance of (5.0 ± 1.7) × 10^(-9), which may indicate an average increase by a factor of a few on the smaller scales sampled by the interferometer. Part of this apparent abundance variation could be explained by contributions from extended cloud emission to the single-dish C^(18)O lines, and uncertainties in the assumed excitation temperatures and opacities. The properties of the molecular envelopes and outflows are further investigated through single-dish observations of ^(12)CO J = 6-5, 4-3, and 3-2,^(13)CO 6-5 and 3-2, and C^(18)O 3-2 and 2-1, obtained with the James Clerk Maxwell and IRAM 30 m telescopes, along with the Caltech Submillimeter Observatory. Ratios of the mid-J CO lines are used to estimate the excitation temperature, with values of 25-80 K derived for the gas near line center. The outflow wings show a similar range, although T_(ex) is enhanced by a factor of 2-3 in at least two sources. In contrast to the well-studied L1551 IRS 5 outflow, which extends over 10' (0.4 pc), seven of the remaining eight sources are found to drive ^(12)CO 3-2 outflows over ≤1' (0.04 pc); only L1527 IRS has a well-developed outflow of some 3' (0.12 pc). Estimates are obtained for the outflow kinetic luminosity, L_(kin), and the flow momentum rate, F_(CO), applying corrections for line opacity and source inclination. The flow force F_(CO) correlates with the envelope mass and with the 2.7 mm flux of the circumstellar disk. Only a weak correlation is seen with L_(bol), while none is found with the relative age of the object as measured by ∫ T_(mb)(HCO^+ 3-2)dV/L_(bol). These trends support the hypothesis that outflows are driven by accretion through a disk, with a global mass infall rate determined by the mass and density of the envelope. The association of compact HCO^+ emission with the walls of the outflow cavities indicates that outflows in turn influence the appearance of the envelopes. It is not yet clear, however, whether they are actively involved in sweeping up envelope material, or merely provide a low-opacity pathway for heating radiation to reach into the envelope.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/305885DOIUNSPECIFIED
http://iopscience.iop.org/0004-637X/502/1/315/PublisherUNSPECIFIED
Additional Information:© 1998 American Astronomical Society. Received 1997 September 11; accepted 1998 February 26. The authors wish to thank the staffs of the JCMT, CSO, IRAM 30 m, and OVRO telescopes for their assistance. Remo Tilanus and Fred Baas are thanked for carrying out part of the JCMT observations. Jocelyn Keene kindly assisted in calibrating the CSO data. Lee Mundy is acknowledged for useful discussions. M. R. H. is indebted to the Caltech Divisions of Geological and Planetary Sciences and Mathematics, Physics and Astronomy, and the Owens Valley Radio Observatory for hospitality, and to the Netherlands Organization for Scientific Research (NWO) and the Leids Kerkhoven-Bosscha Fonds for travel support. Research in Astrochemistry in Leiden is supported by NWO/NFRA through grant 781-76-015. G. A. B. gratefully acknowledges support provided by NASA grants NAGW-2297 and NAGW-1955. H. J. v. L. acknowledges support for his research from the European Union under contract CHGECT920011. The referee is thanked for providing constructive comments that improved the manuscript.
Funders:
Funding AgencyGrant Number
NWO/NFRA781-76-015
NASANAGW-2297
NASANAGW-1955
European UnionCHGECT920011
Leids Kerkhoven-Bosscha FondsUNSPECIFIED
Subject Keywords:ISM: molecules; radio lines: stars; stars: formation; stars: low mass, brown dwarfs; stars: pre-main sequence
Record Number:CaltechAUTHORS:20120913-113949968
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20120913-113949968
Official Citation: Envelope Structure on 700 AU Scales and the Molecular Outflows of Low-Mass Young Stellar Objects Michiel R. Hogerheijde et al. 1998 ApJ 502 315
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:34068
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:13 Sep 2012 19:01
Last Modified:26 Dec 2012 16:10

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