ATMOSPHERIC PHASE CORRECTION USING CARMA-PACS: HIGH ANGULAR RESOLUTION OBSERVATIONS OF THE FU ORIONIS STAR PP 13S*
- Department of Astronomy, California Institute of Technology, 1200 East California Blvd, Pasadena, CA 91125 (United States)
- Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA 93513 (United States)
- Department of Astronomy, University of Maryland, College Park, MD 20742-2421 (United States)
- Combined Array for Research in Millimeter-wave Astronomy, P.O. Box 968, Big Pine, CA 93513 (United States)
- Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Ave. Chicago, IL 60637 (United States)
- Space Sciences-VP62, NASA Marshall Space Flight Center, Huntsville, AL 35812 (United States)
- Department of Astronomy, University of Illinois, Urbana, IL 61801 (United States)
- Astronomy Department, University of California at Berkeley, Berkeley, CA 94720-3411 (United States)
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{sub sun}, 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.
- OSTI ID:
- 21471172
- Journal Information:
- Astrophysical Journal, Vol. 724, Issue 1; Other Information: DOI: 10.1088/0004-637X/724/1/493; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
Similar Records
VARIABILITY AT THE EDGE: OPTICAL NEAR/IR RAPID-CADENCE MONITORING OF NEWLY OUTBURSTING FU ORIONIS OBJECT HBC 722
RESOLVING THE SUB-AU-SCALE GAS AND DUST DISTRIBUTION IN FU ORIONIS SOURCES