THE ROTATING OUTFLOW, ENVELOPE, AND DISK OF THE CLASS-0/I PROTOSTAR [BHB2007] no. 11 IN THE PIPE NEBULA

Journal Article · Wed Jul 10 04:00:00 EDT 2013 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/771/2/128· OSTI ID:22140123

Hara, C. ^[1]; Shimajiri, Y.; Kurono, Y.; Saigo, K.; Nakamura, F.; Saito, M.; Kawabe, R. ^[2]; Tsukagoshi, T. ^[3]; Wilner, David ^[4]

---

1. University of Tokyo, 7-3-1 Hongo Bunkyo, Tokyo 113-0033 (Japan)
2. National Astronomical Observatory of Japan, 2-21-1 Osawa Mitaka, Tokyo 181-0015 (Japan)
3. Ibaraki University, 2-1-1 Bunkyo Mito, Ibaraki Prefecture 310-8512 (Japan)
4. Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)

We present the results of observations toward a low-mass Class-0/I protostar [BHB2007] no. 11 (B59 no. 11) in the nearby (d = 130 pc) star-forming region Barnard 59 (B59), in the Pipe Nebula. We utilize the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope ({approx}22'' resolution), focusing on the CO(3-2), HCO{sup +}, H{sup 13}CO{sup +}(4-3), and 1.1 mm dust-continuum emission transitions. We also show Submillimeter Array (SMA) data with {approx}5'' resolution in {sup 12}CO, {sup 13}CO, C{sup 18}O(2-1), and 1.3 mm dust-continuum emission. From ASTE CO(3-2) observations, we found that B59 no. 11 is blowing a collimated outflow whose axis lies almost on the plane of the sky. The outflow traces well a cavity-like structure seen in the 1.1 mm dust-continuum emission. The results of SMA {sup 13}CO and C{sup 18}O(2-1) observations have revealed that a compact and elongated structure of dense gas is associated with B59 no. 11; the structure is oriented perpendicular to the outflow axis. There is a compact dust condensation with a size of 350 Multiplication-Sign 180 AU seen in the SMA 1.3 mm continuum map, and the direction of its major axis is almost the same as that of the dense gas elongation. The distributions of {sup 13}CO and C{sup 18}O emission also show velocity gradients along their major axes, which are thought to arise from the envelope/disk rotation. From detailed analysis of the SMA data, we infer that B59 no. 11 is surrounded by a Keplerian disk with a radius of less than 350 AU. In addition, the SMA CO(2-1) image shows a velocity gradient in the outflow in the same direction as that of the dense gas rotation. We suggest that this velocity gradient indicates rotation in the outflow.

• OSTI ID: 22140123
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 771; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
CARBON 13
CARBON MONOXIDE
CAVITIES
DISTRIBUTION
DUSTS
ELONGATION
EMISSION
GOLD 180
MASS
MOLECULES
NEBULAE
OXYGEN 18
PROTOSTARS
RESOLUTION
ROTATION
STARS
TELESCOPES
VELOCITY