How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions
Herczeg,Gregory J.1; Johnstone,Doug2,3; Mairs,Steve2,3; Hatchell,Jennifer4; Lee,Jeong-Eun5; Bower,Geoffrey C.6; Chen,Huei-Ru Vivien7; Aikawa,Yuri8; Yoo,Hyunju5,9; Kang,Sung-Ju10; Kang,Miju10; Chen,Wen-Ping11; Williams,Jonathan P.12; Bae,Jaehan13; Dunham,Michael M.14,15; Vorobyov,Eduard I.16,17,18; Zhu,Zhaohuan19; Rao,Ramprasad20; Kirk,Helen2; Takahashi,Satoko21,22; Morata,Oscar20; Lacaille,Kevin23; Lane,James3; Pon,Andy24; Scholz,Aleks25; Samal,Manash R.11; Bell,Graham S.26; Graves,Sarah26; Lee,E’lisa M.26; Parsons,Harriet26; He,Yuxin27; Zhou,Jianjun27; Kim,Mi-Ryang28; Chapman,Scott23; Drabek-Maunder,Emily29; Chung,Eun Jung10; Eyres,Stewart P. S.30; Forbrich,Jan15,31; Hillenbrand,Lynne A.32; Inutsuka,Shu-ichiro33; Kim,Gwanjeong10; Kim,Kyoung Hee34; Kuan,Yi-Jehng20,35; Kwon,Woojin10,36; Lai,Shih-Ping7,20; Lalchand,Bhavana11; Lee,Chang Won10,36; Lee,Chin-Fei20; Long,Feng1,37; Lyo,A-Ran10; Qian,Lei38; Scicluna,Peter20; Soam,Archana10; Stamatellos,Dimitris30; Takakuwa,Shigehisa39; Tang,Ya-Wen20; Wang,Hongchi40; Wang,Yiren1,37
Source PublicationThe Astrophysical Journal
AbstractAbstract Most protostars have luminosities that are fainter than expected from steady accretion over the protostellar lifetime. The solution to this problem may lie in episodic mass accretion—prolonged periods of very low accretion punctuated by short bursts of rapid accretion. However, the timescale and amplitude for variability at the protostellar phase is almost entirely unconstrained. In A James Clerk Maxwell Telescope/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions, we are monitoring monthly with SCUBA-2 the submillimeter emission in eight fields within nearby ( < 500 pc) star-forming regions to measure the accretion variability of protostars. The total survey area of ~1.6 deg2 includes ~105 peaks with peaks brighter than 0.5 Jy/beam (43 associated with embedded protostars or disks) and 237 peaks of 0.125–0.5 Jy/beam (50 with embedded protostars or disks). Each field has enough bright peaks for flux calibration relative to other peaks in the same field, which improves upon the nominal flux calibration uncertainties of submillimeter observations to reach a precision of ~2%–3% rms, and also provides quantified confidence in any measured variability. The timescales and amplitudes of any submillimeter variation will then be converted into variations in accretion rate and subsequently used to infer the physical causes of the variability. This survey is the first dedicated survey for submillimeter variability and complements other transient surveys at optical and near-IR wavelengths, which are not sensitive to accretion variability of deeply embedded protostars.
Keywordstars: formation stars: protostars stars: variables: T Tauri, Herbig Ae/Be submillimeter: stars
WOS IDIOP:0004-637X-849-1-aa8b62
PublisherThe American Astronomical Society
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Document Type期刊论文
Affiliation1.Kavli Institute for Astronomy and Astrophysics, Peking University, Yiheyuan 5, Haidian Qu, 100871 Beijing, China
2.NRC Herzberg Astronomy and Astrophysics, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada
3.Department of Physics and Astronomy, University of Victoria, Victoria, BC, V8P 5C2, Canada
4.Physics and Astronomy, University of Exeter, Stocker Road, Exeter EX4 4QL, UK
5.School of Space Research, Kyung Hee University, 1732, Deogyeong-Daero, Giheung-gu Yongin-shi, Gyunggi-do 17104, Korea
6.Academia Sinica Institute of Astronomy and Astrophysics, 645 N. A’ohoku Place, Hilo, HI 96720, USA
7.Department of Physics and Institute of Astronomy, National Tsing Hua University, Taiwan
8.Department of Astronomy, University of Tokyo, Tokyo, Japan
9.Chungnam National University, Korea
10.Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Korea
11.Graduate Institute of Astronomy, National Central University, 300 Jhongda Road, Zhongli, Taoyuan, Taiwan
12.Institute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822, USA
13.Department of Astronomy, University of Michigan, 1085 S. University Avenue, Ann Arbor, MI 48109, USA
14.Department of Physics, The State University of New York at Fredonia, Fredonia, NY 14063, USA
15.Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
16.Institute of Fluid Mechanics and Heat Transfer, TU Wien, Vienna, A-1060, Austria
17.Research Institute of Physics, Southern Federal University, Stachki Ave. 194, Rostov-on-Don, 344090, Russia
18.University of Vienna, Department of Astrophysics, Vienna, A-1180, Austria
19.Physics and Astronomy Department, University of Nevada, Las Vegas, USA
20.Academia Sinica Institute of Astronomy and Astrophysics, P. O. Box 23-141, Taipei 10617, Taiwan
21.Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile
22.National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
23.Department of Physics and Atmospheric Science, Dalhousie University, Halifax, NS, B3H 4R2, Canada
24.Department of Physics and Astronomy, The University of Western Ontario, 1151 Richmond Street, London, N6A 3K7, Canada
25.SUPA, School of Physics & Astronomy, North Haugh, St. Andrews, KY16 9SS, UK
26.East Asian Observatory, 660 N. A‘ohōkū Place, Hilo, HI 96720, USA
27.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
28.Department of Physics, Institute for Astrophysics, Chungbuk National University, Korea
29.Cardiff University, School of Physics and Astronomy, The Parade, Cardiff, CF24 3AA, UK
30.Jeremiah Horrocks Institute for Mathematics, Physics & Astronomy, University of Central Lancashire, Preston, PR1 2HE, UK
31.Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
32.Department of Astronomy; MC 249-17, California Institute of Technology, Pasadena, CA 91125, USA
33.Department of Physics, Graduate School of Science, Nagoya University, 464-8602, Nagoya, Japan
34.Korea National University of Education, Taeseongtabyeon-ro, Grangnae-myeon, Heungdeok-gu, Cheongju-si, Chungbuk 28173, Korea
35.Department of Earth Sciences, National Taiwan Normal University, Taipei 116, Taiwan
36.Korea University of Science and Technology, 217 Gajang-ro, Yuseong-gu, Daejeon 34113, Korea
37.Department of Astronomy, Peking University, Yiheyuan 5, Haidian Qu, 100871 Beijing, China
38.National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
39.Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan
40.Purple Mountain Observatory, & Key Laboratory for Radio Astronomy, Chinese Academy of Sciences, 2 West Beijing Road, Nanjing 210008, China
Recommended Citation
GB/T 7714
Herczeg,Gregory J.,Johnstone,Doug,Mairs,Steve,et al. How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions[J]. The Astrophysical Journal,2017,849(1).
APA Herczeg,Gregory J..,Johnstone,Doug.,Mairs,Steve.,Hatchell,Jennifer.,Lee,Jeong-Eun.,...&Wang,Yiren.(2017).How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions.The Astrophysical Journal,849(1).
MLA Herczeg,Gregory J.,et al."How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions".The Astrophysical Journal 849.1(2017).
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