2003/06/04 by Sozo Yokogawa, S. Yokogawa, Yoshimi Kitamura +4 · 2 citations
Chemistry · Earth and Planetary Sciences · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atmospheric Ozone and Climate #Bipolar outflow #Molecular Spectroscopy and Structure #Outflow #Physics #Protostar #Star formation #Stars #astro-ph
paper · pdf · doi:10.1086/377302
published as Astrophys.J. 595 (2003) 266-278 · 29 pages, 12 figures, Accepted for Publication in the Astrophysical Journal
arxiv created 2003/06/04 · openalex publication_date 2003/09/16 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
High angular resolution and sensitive aperture synthesis observations of CS ( J = 2-1) and CS ( J = 3-2) emissions toward L1551 NE, the second brightest protostar in the Taurus molecular cloud, made with the Nobeyama Millimeter Array are presented. L1551 NE is categorized as a Class 0 object deeply embedded in the redshifted outflow lobe of L1551 IRS 5. Previous studies of the L1551 NE region in CS emission revealed the presence of shell-like components open toward L1551 IRS 5, which seem to trace low-velocity shocks in the swept-up shell driven by the outflow from L1551 IRS 5. In this study, significant CS emission around L1551 NE was detected at the eastern tip of the swept-up shell from V lsr = 5.3 to 10.1 km s -1 , and the total mass of the dense gas is estimated to be 0.14 ± 0.02 M ☉ . In addition, the following new structures were successfully revealed: a compact disklike component with a size of ≈1000 AU just at L1551 NE, an arc-shaped structure around L1551 NE, open toward L1551 NE, with a size of ~5000 AU, i.e., a bow shock, and a distinct velocity gradient of the dense gas, i.e., deceleration along the outflow axis of L1551 IRS 5. These features suggest that the CS emission traces the postshocked region where the dense gas associated with L1551 NE and the swept-up shell of the outflow from L1551 IRS 5 interact. Since the age of L1551 NE is comparable to the timescale of the interaction, it is plausible that the formation of L1551 NE was induced by the outflow impact. The compact structure of L1551 NE with a tiny envelope was also revealed, suggesting that the outer envelope of L1551 NE has been blown off by the outflow from L1551 IRS 5.