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Early Planet Formation in Embedded Disks (eDisk). IX. High-resolution ALMA Observations of the Class 0 Protostar R CrA IRS5N and Its Surroundings

Authors :
Rajeeb Sharma
Jes K. Jørgensen
Sacha Gavino
Nagayoshi Ohashi
John J. Tobin
Zhe-Yu Daniel Lin
Zhi-Yun Li
Shigehisa Takakuwa
Chang Won Lee
Jinshi Sai (Insa Choi)
Woojin Kwon
Itziar de Gregorio-Monsalvo
Alejandro Santamaría-Miranda
Hsi-Wei Yen
Yuri Aikawa
Yusuke Aso
Shih-Ping Lai
Jeong-Eun Lee
Leslie W. Looney
Nguyen Thi Phuong
Travis J. Thieme
Jonathan P. Williams
Source :
The Astrophysical Journal, Vol 954, Iss 1, p 69 (2023)
Publication Year :
2023
Publisher :
IOP Publishing, 2023.

Abstract

We present high-resolution high-sensitivity observations of the Class 0 protostar RCrA IRS5N as part of the Atacama Large Milimeter/submilimeter Array large program Early Planet Formation in Embedded Disks. The 1.3 mm continuum emission reveals a flattened continuum structure around IRS5N, consistent with a protostellar disk in the early phases of evolution. The continuum emission appears smooth and shows no substructures. However, a brightness asymmetry is observed along the minor axis of the disk, suggesting that the disk is optically and geometrically thick. We estimate the disk mass to be between 0.007 and 0.02 M _⊙ . Furthermore, molecular emission has been detected from various species, including C ^18 O (2–1), ^12 CO (2–1), ^13 CO (2–1), and H _2 CO (3 _0,3 − 2 _0,2 , 3 _2,1 − 2 _2,0 , and 3 _2,2 − 2 _2,1 ). By conducting a position–velocity analysis of the C ^18 O (2–1) emission, we find that the disk of IRS5N exhibits characteristics consistent with Keplerian rotation around a central protostar with a mass of approximately 0.3 M _⊙ . Additionally, we observe dust continuum emission from the nearby binary source IRS5a/b. The emission in ^12 CO toward IRS5a/b seems to emanate from IRS5b and flow into IRS5a, suggesting material transport between their mutual orbits. The lack of a detected outflow and large-scale negatives in ^12 CO observed toward IRS5N suggests that much of the flux from IRS5N is being resolved out. Using a 1D radiative transfer model, we infer the mass of the envelope surrounding IRS5N to be ∼1.2 M _⊙ . Due to this substantial surrounding envelope, the central IRS5N protostar is expected to be significantly more massive in the future.

Details

Language :
English
ISSN :
15384357
Volume :
954
Issue :
1
Database :
Directory of Open Access Journals
Journal :
The Astrophysical Journal
Publication Type :
Academic Journal
Accession number :
edsdoj.8d42728f70b4bcda189d0b8b6b6d542
Document Type :
article
Full Text :
https://doi.org/10.3847/1538-4357/ace35c