S315p.207 — Influence of Interstellar FUV Radiation on the Abundance Ratio of13CO to C18O in L 1551

Date & Time

Aug 4th at 6:00 PM until 6:00 PM




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Author(s): Sheng-Jun Lin6, Yoshito Shimajiri1, Chihomi Hara7, Shih-Ping Lai6, Fumitaka Nakamura5, Koji Sugitani4, Ryohei Kawabe5, Yoshimi Kitamura3, Atsushi Yoshida8, Hidefumi Tatei8, Toshiya Akashi8, Takashi Tsukagushi2

Institution(s): 1. CEA Saclay, 2. Ibaraki University, 3. Japan Aerospace Exploration Agency, 4. Nagoya City University, 5. National Astronomical Observatory of Japan, 6. National Tsing Hua University, 7. The University of Tokyo, 8. Tokyo Institute of Technology

To investigate the relationship between the far-ultraviolet (FUV) radiation and the abundance ratios between 13CO and C18O, we observed L 1551 in 12CO (J=1-0), 13CO (J=1-0) and C18O (J=1-0) using the Nobeyama Radio Observatory 45 m telescope with an angular resolution of ~22" (corresponding to 0.017 pc at a distance of 160 pc). L 1551 is chosen because it is relatively isolated in Taurus-Auriga complex, providing an ideal environment for studying the variation of abundance ratio due to the penetration of the FUV photons. L 1551 is a young star-forming region containing at least 6 young protostars between Class I and Class III stages and a quiescent elongated starless core. The distribution of 12CO emission shows the outflows coming from 2 youngest protostars IRS5 and NE. The 13CO and C18O are detected throughout the whole region with enhancement around the outflows and depletion in the outflow cavities. To avoid the influence of outflows, we exclude the outflow regions for X(13CO)/X(C18O) abundance ratio calculation. X(13CO)/X(C18O) is found in the range of 3.2 -- 36.2 with a mean value of 7.6. Comparing to the extinction map derived from Herschel observations, we found that the abundance ratio reaches its maximum at low AV and decreases to typical solar system value of 5.5 within the starless core. The high X(13CO)/X(C18O) value at the low AV value in L 1551 is most likely due to the selective FUV photodissociation of C18O. This is in contrast with Orion-A region where its internal OB stars keep the abundance ratio at a high level greater than ~10.