TY - JOUR
T1 - Revealing a detailed mass distribution of a high-density core MC27/L1521F in Taurus with ALMA
AU - Tokuda, Kazuki
AU - Onishi, Toshikazu
AU - Matsumoto, Tomoaki
AU - Saigo, Kazuya
AU - Kawamura, Akiko
AU - Fukui, Yasuo
AU - Inutsuka, Shu Ichiro
AU - Machida, Masahiro N.
AU - Tomida, Kengo
AU - Tachihara, Kengo
AU - André, Philippe
N1 - Funding Information:
This paper makes use of the following ALMA data: ADS/ JAO.ALMA#2011.0.00611.S and 2012.1.00239.S. ALMA is a partnership of the ESO, NSF, NINS, NRC, NSC, and ASIAA. The Joint ALMA Observatory is operated by the ESO, AUI/NRAO, and NAOJ. This work was financially supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant nos. 16H02160, 22244014, 23103005, 23244027, 23403001, 23540270, 24244017, 26247026, 26287030, and 26400233. K. Tokuda is supported by a JSPS Research Fellow. T. Onishi is supported by the ALMA Japan Research Grant of NAOJ Chile Observatory, NAOJ-ALMA-0013 and NAOJ-ALMA-0032. P. André is partly supported by the European Research Council under the European Union's Seventh Framework Programme (ERC Grant Agreement no. 291294). This work is partly based on observations carried out with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).
Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.
PY - 2016/7/20
Y1 - 2016/7/20
N2 - We present the results of ALMA observations of dust continuum emission and molecular rotational lines toward a dense core MC27 (aka L1521F) in Taurus, which is considered to be at a very early stage of star formation. The detailed column density distributions on size scales from a few tens to ∼10,000 AU are revealed by combining the ALMA (12 m array + 7 m array) data with the published/unpublished single-dish data. The high angular resolution observations at 0.87 mm with a synthesized beam size of ∼0.″74 × 0.″32 reveal that a protostellar source, MMS-1, is not spatially resolved and lacks associated gas emission, while a starless high-density core, MMS-2, has substructures in both dust and molecular emission. The averaged radial column density distribution of the inner part of MC27/L1521F (r ≲ 3000 AU) is ∼ , clearly flatter than that of the outer part, ∼. The complex velocity/spatial structure obtained with previous ALMA observations is located inside the inner flatter region, which may reflect the dynamical status of the dense core.
AB - We present the results of ALMA observations of dust continuum emission and molecular rotational lines toward a dense core MC27 (aka L1521F) in Taurus, which is considered to be at a very early stage of star formation. The detailed column density distributions on size scales from a few tens to ∼10,000 AU are revealed by combining the ALMA (12 m array + 7 m array) data with the published/unpublished single-dish data. The high angular resolution observations at 0.87 mm with a synthesized beam size of ∼0.″74 × 0.″32 reveal that a protostellar source, MMS-1, is not spatially resolved and lacks associated gas emission, while a starless high-density core, MMS-2, has substructures in both dust and molecular emission. The averaged radial column density distribution of the inner part of MC27/L1521F (r ≲ 3000 AU) is ∼ , clearly flatter than that of the outer part, ∼. The complex velocity/spatial structure obtained with previous ALMA observations is located inside the inner flatter region, which may reflect the dynamical status of the dense core.
KW - ISM: clouds
KW - ISM: kinematics and dynamics
KW - ISM: molecules
KW - stars: formation
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U2 - 10.3847/0004-637X/826/1/26
DO - 10.3847/0004-637X/826/1/26
M3 - Article
AN - SCOPUS:84979578307
SN - 0004-637X
VL - 826
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 26
ER -