期刊
ASTROPHYSICAL JOURNAL
卷 724, 期 1, 页码 493-501出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/724/1/493
关键词
circumstellar matter; stars: individual (PP 13S*); stars: pre-main sequence; techniques: interferometric
资金
- Gordon and Betty Moore Foundation
- Kenneth T. and Eileen L. Norris Foundation
- James S. McDonnell Foundation
- Associates of the California Institute of Technology
- University of Chicago
- State of California
- State of Maryland
- National Science Foundation [AST 08-38260]
- CARMA
- NSF
- Fulbright-CONICYT
- State of Illinois
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0838226] Funding Source: National Science Foundation
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-circle dot, 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.
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