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Observational Constraints on Submillimeter Dust Opacity

Shirley, Yancy L. and Huard, Tracy L. and Pontoppidan, Klaus M. and Wilner, David J. and Stutz, Amelia M. and Bieging, John H. and Evans, Neal J., II (2011) Observational Constraints on Submillimeter Dust Opacity. Astrophysical Journal, 728 (2). Art. No. 143. ISSN 0004-637X.

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Infrared extinction maps and submillimeter dust continuum maps are powerful probes of the density structure in the envelope of star-forming cores. We make a direct comparison between infrared and submillimeter dust continuum observations of the low-mass Class 0 core, B335, to constrain the ratio of submillimeter to infrared opacity (κ_(smm)/κ_(ir)) and the submillimeter opacity power-law index (κ ∝ λ–β). Using the average value of theoretical dust opacity models at 2.2 μm, we constrain the dust opacity at 850 and 450 μm. Using new dust continuum models based upon the broken power-law density structure derived from interferometric observations of B335 and the infall model derived from molecular line observations of B335, we find that the opacity ratios are ^κ_(850)_κ_(2.2) = (3.21 - 4.80)^(+0.44)_(-0.30) x 10^(-4) ^κ_(450)_κ(2.0) = (12.8-24.8)^(+2.4)_(-1.3) x 10^(-4) with a submillimeter opacity power-law index of β_(smm) = (2.18-2.58)^(+0.30)_(–0.30). The range of quoted values is determined from the uncertainty in the physical model for B335. For an average 2.2 μm opacity of 3800 ± 700 cm^2 g^(–1), we find a dust opacity at 850 and 450 μm of κ_(850) = (1.18-1.77)^9+0.36)_(–0.24) and κ_(450) = (4.72-9.13)^(+1.9)_(–0.98) cm^2 g^(–1) of dust. These opacities are from (0.65-0.97)κ^(OH5)_(850) of the widely used theoretical opacities of Ossenkopf and Henning for coagulated ice grains with thin mantles at 850 μm.

Item Type:Article
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URLURL TypeDescription
Pontoppidan, Klaus M.0000-0001-7552-1562
Wilner, David J.0000-0003-1526-7587
Stutz, Amelia M.0000-0003-2300-8200
Evans, Neal J., II0000-0001-5175-1777
Additional Information:© 2011 American Astronomical Society. Received 2010 July 24; accepted 2010 December 16; published 2011 February 1. We sincerely thank the referee for a very thorough and careful reading of the manuscript. We thank Brandon Kelly for comments that improved this paper. Guest User, Canadian Astronomy Data Centre, is operated by the Dominion Astrophysical Observatory for the National Research Council of Canada’s Herzberg Institute of Astrophysics. K.M.P. is supported by NASA through Hubble Fellowship grant no. 01201.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Additional support came from NASA Origins grant NNG04GG24G and the Spitzer Legacy Science Program, provided by NASA through contracts 1224608 and 1230779 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407 to N.J.E.
Funding AgencyGrant Number
NASANAS 5-26555
Subject Keywords:dust, extinction – ISM: clouds – stars: formation
Issue or Number:2
Classification Code:PACS: 98.38.Dq, 95.85.Fm, 98.58.Db, 98.38.Cp, 98.58.Ca
Record Number:CaltechAUTHORS:20110321-155432977
Persistent URL:
Official Citation:Yancy L. Shirley et al. 2011 ApJ 728 143 doi: 10.1088/0004-637X/728/2/143
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:23019
Deposited By: Benjamin Perez
Deposited On:22 Mar 2011 15:19
Last Modified:18 Nov 2019 00:12

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