DISK AND ENVELOPE STRUCTURE IN CLASS 0 PROTOSTARS. II. HIGH-RESOLUTION MILLIMETER MAPPING OF THE SERPENS SAMPLE
- Department of Astronomy, University of California at Berkeley, 601 Campbell Hall, Berkeley, CA 94720 (United States)
- NRAO/ALMA-JAO, Av. Apoquindo 3650, Piso 18, Las Condes, Santiago (Chile)
- Combined Array for Research in Millimeter-wave Astronomy, Big Pine, CA 93513 (United States)
- Department of Astronomy and Laboratory for Millimeter-wave Astronomy, University of Maryland, College Park, MD 20742 (United States)
- Owens Valley Radio Observatory, California Institute of Technology, Big Pine, CA 93513 (United States)
- Department of Astronomy, University of Illinois, Urbana, IL 61801 (United States)
- Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Ave. Chicago, IL 60637 (United States)
- Department of Astronomy, California Institute of Technology, 1200 East California Blvd, Pasadena, CA 91125 (United States)
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{lambda}), allowing us to trace spatial scales from 10{sup 2} to 10{sup 4} 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{lambda}, where the contribution from the envelope should be negligible, assuming an unresolved disk. The resulting disk masses range from 0.04 M{sub sun} to 1.7 M{sub sun}, with a mean of approximately 0.2 M{sub sun}. Our high-resolution maps are also sensitive to binary or multiple sources with separations {approx}> 250 AU, but significant evidence of multiplicity on scales <2000 AU is seen in only one source.
- OSTI ID:
- 21560342
- Journal Information:
- Astrophysical Journal, Supplement Series, Vol. 195, Issue 2; Other Information: DOI: 10.1088/0067-0049/195/2/21; ISSN 0067-0049
- Country of Publication:
- United States
- Language:
- English
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