TY - JOUR
T1 - Tentative detection of deuterated methane toward the low-mass protostar iras 04368+2557 in L1527
AU - Sakai, Nami
AU - Shirley, Yancy L.
AU - Sakai, Takeshi
AU - Hirota, Tomoya
AU - Watanabe, Yoshimasa
AU - Yamamoto, Satoshi
PY - 2012/10/10
Y1 - 2012/10/10
N2 - The millimeter-wave rotational transition line (JK = 1 0-00) of deuterated methane CH3D has tentatively been detected toward the low-mass Class 0 protostar IRAS 04368+2557 in L1527 with the Heinrich Hertz Submillimeter Telescope. This is the first detection of CH3D in interstellar clouds, if confirmed. The column density and fractional abundance of CH3D are determined to be (9.1 ± 3.4) × 1015cm-2 and (3.0 ± 1.1) × 10-7, respectively, where we assume the rotational temperature of 25K. The column density and fractional abundance of the gaseous CH4 are estimated to be (1.3-4.6) × 1017cm -2 and (4.3-15.2) × 10-6, respectively, by adopting the molecular D/H ratios of 2%-7% reported for various molecules in L1527. The fractional abundance of CH4 is higher than or comparable to that found in high-mass star-forming cores by infrared observations. It is sufficiently high to trigger the efficient production of various carbon-chain molecules in a lukewarm region near the protostar, which supports the scenario of warm carbon-chain chemistry.
AB - The millimeter-wave rotational transition line (JK = 1 0-00) of deuterated methane CH3D has tentatively been detected toward the low-mass Class 0 protostar IRAS 04368+2557 in L1527 with the Heinrich Hertz Submillimeter Telescope. This is the first detection of CH3D in interstellar clouds, if confirmed. The column density and fractional abundance of CH3D are determined to be (9.1 ± 3.4) × 1015cm-2 and (3.0 ± 1.1) × 10-7, respectively, where we assume the rotational temperature of 25K. The column density and fractional abundance of the gaseous CH4 are estimated to be (1.3-4.6) × 1017cm -2 and (4.3-15.2) × 10-6, respectively, by adopting the molecular D/H ratios of 2%-7% reported for various molecules in L1527. The fractional abundance of CH4 is higher than or comparable to that found in high-mass star-forming cores by infrared observations. It is sufficiently high to trigger the efficient production of various carbon-chain molecules in a lukewarm region near the protostar, which supports the scenario of warm carbon-chain chemistry.
KW - ISM
KW - individual objects (L1527) ISM
KW - molecules
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U2 - 10.1088/2041-8205/758/1/L4
DO - 10.1088/2041-8205/758/1/L4
M3 - Article
AN - SCOPUS:84866707120
VL - 758
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
IS - 1
M1 - L4
ER -