TY - JOUR
T1 - ALMA Observations of SMM11 Reveal an Extremely Young Protostar in Serpens Main Cluster
AU - Aso, Yusuke
AU - Ohashi, Nagayoshi
AU - Aikawa, Yuri
AU - Machida, Masahiro N.
AU - Saigo, Kazuya
AU - Saito, Masao
AU - Takakuwa, Shigehisa
AU - Tomida, Kengo
AU - Tomisaka, Kohji
AU - Yen, Hsi Wei
AU - Williams, Jonathan P.
N1 - Funding Information:
Is supported by the Subaru Telescope Internship Program and acknowledges a grant from the Ministry of Science and Technology (MoST) of Taiwan (MOST 106-2119-M-001-013). Y.A. acknowledges JSPS KAKENHI Grant Number JP16H00931 in support of this work. K.S. and M.S. acknowledge JSPS KAKENHI grant Number JP16K05303 in support of this work S.T. acknowledges a grant from the Ministry of Science and Technology (MOST) of Taiwan (MOST 102-2119-M-001-012-MY3), and JSPS KAKENHI grant Number JP16H07086, in support of this work. K.T. acknowledges JSPS KAKENHI grant Number JP16H05998 in support of this work.
Funding Information:
NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We thank all of the ALMA staff for making our observations successful. We also thank the anonymous referee, who gave us invaluable comments with which to improve the paper. Data analysis were in part carried out on common-use data analysis computer system at the Astronomy Data Center, ADC, of the National Astronomical Observatory of Japan. Y.A. is supported by the Subaru Telescope Internship Program and acknowledges a grant from the Ministry of Science and Technology (MoST) of Taiwan (MOST 106-2119-M-001-013). Y.A. acknowledges JSPS KAKENHI Grant Number JP16H00931 in support of this work. K.S. and M.S. acknowledge JSPS KAKENHI grant Number JP16K05303 in support of this work S.T. acknowledges a grant from the Ministry of Science and Technology (MOST) of Taiwan (MOST 102-2119-M-001-012-MY3), and JSPS KAKENHI grant Number JP16H07086, in support of this work. K.T. acknowledges JSPS KAKENHI grant Number JP16H05998 in support of this work. Facility: ALMA. Software: CASA, MIRIAD.
Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.
PY - 2017/11/20
Y1 - 2017/11/20
N2 - We report the discovery of an extremely young protostar, SMM11, located in the associated submillimeter condensation in the Serpens Main cluster using the Atacama Large Millimeter/submillimeter Array (ALMA) during its Cycle 3 at 1.3 mm and an angular resolution of . SMM11 is a Class 0 protostar without any counterpart at 70 μm or shorter wavelengths. The ALMA observations show 1.3 mm continuum emission associated with a collimated 12CO bipolar outflow. Spitzer and Herschel data show that SMM11 is extremely cold ( 26 K) and faint ( 0.9 ). We estimate the inclination angle of the outflow to be , almost parallel to the plane of the sky, from simple fitting using a wind-driven-shell model. The continuum visibilities consist of Gaussian and power-law components, suggesting a spherical envelope with a radius of ∼600 au around the protostar. The estimated low C18O abundance, X(C18O) = 1.5-3 , is also consistent with its youth. The high outflow velocity, a few 10 at a few 1000 au, is much higher than theoretical simulations of first hydrostatic cores, and we suggest that SMM11 is a transitional object right after the second collapse of the first core.
AB - We report the discovery of an extremely young protostar, SMM11, located in the associated submillimeter condensation in the Serpens Main cluster using the Atacama Large Millimeter/submillimeter Array (ALMA) during its Cycle 3 at 1.3 mm and an angular resolution of . SMM11 is a Class 0 protostar without any counterpart at 70 μm or shorter wavelengths. The ALMA observations show 1.3 mm continuum emission associated with a collimated 12CO bipolar outflow. Spitzer and Herschel data show that SMM11 is extremely cold ( 26 K) and faint ( 0.9 ). We estimate the inclination angle of the outflow to be , almost parallel to the plane of the sky, from simple fitting using a wind-driven-shell model. The continuum visibilities consist of Gaussian and power-law components, suggesting a spherical envelope with a radius of ∼600 au around the protostar. The estimated low C18O abundance, X(C18O) = 1.5-3 , is also consistent with its youth. The high outflow velocity, a few 10 at a few 1000 au, is much higher than theoretical simulations of first hydrostatic cores, and we suggest that SMM11 is a transitional object right after the second collapse of the first core.
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U2 - 10.3847/2041-8213/aa9701
DO - 10.3847/2041-8213/aa9701
M3 - Article
AN - SCOPUS:85035358734
SN - 2041-8205
VL - 850
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L2
ER -