DISK AND ENVELOPE STRUCTURE IN CLASS 0 PROTOSTARS. II. HIGH-RESOLUTION MILLIMETER MAPPING OF THE SERPENS SAMPLE

• Published in: The Astrophysical journal. Supplement series Vol. 195; no. 2; pp. 21 - jQuery1323919777801='48'
• Main Authors: Enoch, Melissa L., Corder, Stuartt, Duchêne, Gaspard, Bock, Douglas C., Bolatto, Alberto D., Culverhouse, Thomas L., Kwon, Woojin, Lamb, James W., Leitch, Erik M., Marrone, Daniel P., Muchovej, Stephen J., Pérez, Laura M., Scott, Stephen L., Teuben, Peter J., Wright, Melvyn C. H., Zauderer, B. Ashley
• Format: Journal Article
• Language: English
• Published: United States 01.08.2011
• Subjects: ANTENNAS; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CALIBRATION; ELECTRICAL EQUIPMENT; ELECTROMAGNETIC RADIATION; INSTRUMENTATION RELATED TO NUCLEAR SCIENCE AND TECHNOLOGY; INTERFEROMETRY; MAPPING; PROTOSTARS; RADIATIONS; ULTRAVIOLET RADIATION
• ISSN: 0067-0049; 1538-4365
• DOI: 10.1088/0067-0049/195/2/21

We present high-resolution CARMA 230 GHz continuum imaging of nine deeply embedded protostars in the Serpens Molecular Cloud, including six of the nine known Class 0 protostars in Serpens. This work is part of a program to characterize disk and envelope properties for a complete sample of Class 0 protostars in nearby low-mass star-forming regions. Here, we present CARMA maps and visibility amplitudes as a function of uv-distance for the Serpens sample. Observations are made in the B, C, D, and E antenna configurations, with B configuration observations utilizing the CARMA Paired Antenna Calibration System. Combining data from multiple configurations provides excellent uv-coverage (4-500 k Delta *l), allowing us to trace spatial scales from 102 to 104 AU. We find evidence for compact disk components in all of the observed Class 0 protostars, suggesting that disks form at very early times (t < 0.2 Myr) in Serpens. We make a first estimate of disk masses using the flux at 50 k Delta *l, where the contribution from the envelope should be negligible, assuming an unresolved disk. The resulting disk masses range from 0.04 M to 1.7 M , with a mean of approximately 0.2 M . Our high-resolution maps are also sensitive to binary or multiple sources with separations 250 AU, but significant evidence of multiplicity on scales <2000 AU is seen in only one source.