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Atmospheric phase correction using CARMA-PACS: high angular resolution observations of the FU Orionis star PP 13S*

Pérez, Laura M. and Lamb, James W. and Woody, David P. and Carpenter, John M. and Zauderer, B. Ashley and Isella, Andrea and Bock, Douglas C. and Bolatto, Alberto D. and Carlstrom, John and Culverhouse, Thomas L. and Joy, Marshall and Kwon, Woojin and Leitch, Erik M. and Marrone, Daniel P. and Muchovej, Stephen J. and Plambeck, Richard L. and Scott, Stephen L. and Teuben, Peter J. and Wright, Melvyn C. H. (2010) Atmospheric phase correction using CARMA-PACS: high angular resolution observations of the FU Orionis star PP 13S*. Astrophysical Journal, 724 (1). pp. 493-501. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20101215-141057173

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Abstract

We present 0".15 resolution observations of the 227 GHz continuum emission from the circumstellar disk around the FU Orionis star PP 13S*. The data were obtained with the Combined Array for Research in Millimeter-wave Astronomy (CARMA) Paired Antenna Calibration System (C-PACS), which measures and corrects the atmospheric delay fluctuations on the longest baselines of the array in order to improve the sensitivity and angular resolution of the observations. A description of the C-PACS technique and the data reduction procedures are presented. C-PACS was applied to CARMA observations of PP 13S*, which led to a factor of 1.6 increase in the observed peak flux of the source, a 36% reduction in the noise of the image, and a 52% decrease in the measured size of the source major axis. The calibrated complex visibilities were fitted with a theoretical disk model to constrain the disk surface density. The total disk mass from the best-fit model corresponds to 0.06 M_⊙, which is larger than the median mass of a disk around a classical T Tauri star. The disk is optically thick at a wavelength of 1.3 mm for orbital radii less than 48 AU. At larger radii, the inferred surface density of the PP 13S* disk is an order of magnitude lower than that needed to develop a gravitational instability.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/724/1/493DOIArticle
http://dx.doi.org/10.1088/0004-637X/724/1/493PublisherArticle
ORCID:
AuthorORCID
Bolatto, Alberto D.0000-0002-5480-5686
Additional Information:© 2010 American Astronomical Society. Received 2010 July 12; accepted 2010 September 13; published 2010 November 3. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of California, Illinois, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement (grant AST 08-38260), and by the CARMA partner universities. L.M.P. acknowledges support for graduate studies through a Fulbright-CONICYT scholarship. S.M. acknowledges support from an NSF Astronomy and Astrophysics Fellowship.
Funders:
Funding AgencyGrant Number
Fulbright FoundationUNSPECIFIED
NSF Astronomy and Astrophysics FellowshipUNSPECIFIED
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)UNSPECIFIED
Subject Keywords:circumstellar matter – stars: individual (PP 13S*) – stars: pre-main sequence – techniques: interferometric
Classification Code:PACS: 97.21.+a; 97.10.Pg; 95.30.Sf; 97.10.Fy; 97.30.Nr; 95.85.Bh
Record Number:CaltechAUTHORS:20101215-141057173
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20101215-141057173
Official Citation:Laura M. Pérez et al 2010 ApJ 724 493 doi: 10.1088/0004-637X/724/1/493
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21384
Collection:CaltechAUTHORS
Deposited By: Benjamin Perez
Deposited On:15 Dec 2010 23:52
Last Modified:25 Mar 2019 19:08

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