Atmospheric Phase Correction Using CARMA-PACS: High Angular Resolution Observations of the FU Orionis Star PP 13S

• Published in: The Astrophysical journal Vol. 724; no. 1; pp. 493 - 501
• Main Authors: Pérez, Laura M, Lamb, James W, Woody, David P, Carpenter, John M, Zauderer, B. Ashley, Isella, Andrea, Bock, Douglas C, Bolatto, Alberto D, Carlstrom, John, Culverhouse, Thomas L, Joy, Marshall, Kwon, Woojin, Leitch, Erik M, Marrone, Daniel P, Muchovej, Stephen J, Plambeck, Richard L, Scott, Stephen L, Teuben, Peter J, Wright, Melvyn C. H
• Format: Journal Article
• Language: English
• Published: Bristol IOP Publishing 20.11.2010; IOP
• Subjects: ASTRONOMY; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BINARY STARS; CALIBRATION; Earth, ocean, space; ERUPTIVE VARIABLE STARS; Exact sciences and technology; GRAVITATIONAL INSTABILITY; INSTABILITY; INTERSTELLAR GRAINS; MASS; PARTICLES; PLASMA INSTABILITY; STARS; T TAURI STARS; VARIABLE STARS; stars: individual (PP 13S); Fluctuations; Atmospheric correction; FU Orionis stars; T Tauri stars; Circumstellar matter; Data reduction; Continuum; stars: pre-main sequence; Theoretical model; Gravitational instability; Visibility; Circumstellar disks; techniques: interferometric
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/724/1/493

We present 015 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.