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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, Kevin13; 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, Hongchi40,41; Wang, Yiren1,37
Contribution Rank27

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 JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star Forming Regions", we are monitoring monthly with SCUBA-2 the sub-mm emission in eight fields within nearby (<500 pc) star forming regions to measure the accretion variability of protostars. The total survey area of similar to 1.6 sq.deg. includes similar to 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 sub-mm observations to reach a precision of similar to 2-3% rms, and also provides quantified confidence in any measured variability. The timescales and amplitudes of any sub-mm 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 sub-mm 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 Submillimeter: Stars Stars: Variables: t Tauri Herbig Ae/be
WOS HeadingsScience & Technology ; Physical Sciences
Indexed BySCI
WOS KeywordGould Belt Survey ; Clerk Maxwell Telescope ; Perseus Molecular Cloud ; Young Stellar Objects ; Spitzer C2d Survey ; Survey Scuba-2 Observations ; Dust Continuum Emission ; Small-scale Structures ; Fu-orionis Objects ; Rho-ophiuchi Cloud
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000413865300014
Funding OrganizationNational Science Foundation of China(11473005) ; Natural Sciences and Engineering Research Council (NSERC) of Canada ; National Research Council of Canada ; NSERC ; National Research Foundation of Korea (NRF)(NRF-2015R1A2A2A01004769) ; Korea Astronomy and Space Science Institute(2015-1-320-18) ; Canadian Institute for Theoretical Astrophysics (CITA) ; National Research Foundation of Korea(NRF) - Ministry of Science, ICT & Future Planning(NRF-2015R1C1A1A01052160) ; National Research Foundation of Korea (NRF) - Ministry of Science, ICT & Future Planning(NRF-2016R1C1B2013642) ; National Research Foundation of Korea (NRF) - Ministry of Education, Science, and Technology(NRF-2016R1A2B4012593) ; Austrian Science Fund (FWF)(I2549-N27) ; Ministry of Science and Technology (MoST) of Taiwan(102-2119-M-007-004-MY3, 105-2119-M-007-024) ; Chinese Academy of Sciences(XDB09000000) ; Science and Technology Facilities Council of the United Kingdom ; Canadian Space Agency ; CANARIE ; Compute Canada ; University of Victoria
Citation statistics
Cited Times:23[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Affiliation1.Peking Univ, Kavli Inst Astron & Astrophys, Yiheyuan 5, Beijing 100871, Peoples R China
2.NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada
3.Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada
4.Univ Exeter, Phys & Astron, Stocker Rd, Exeter EX4 4QL, Devon, England
5.Kyung Hee Univ, Sch Space Res, 1732,Deogyeong Daero, Yongin 17104, Gyunggi Do, South Korea
6.Acad Sinica, Inst Astron & Astrophys, 645 N Aohoku Pl, Hilo, HI 96720 USA
7.Natl Tsing Hua Univ, Dept Phys & Inst Astron, Hsinchu, Taiwan
8.Univ Tokyo, Dept Astron, Tokyo, Japan
9.Chungnam Natl Univ, Daejeon, South Korea
10.Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea
11.Natl Cent Univ, Grad Inst Astron, 300 Jhongda Rd, Taoyuan, Taiwan
12.Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA
13.Univ Michigan, Dept Astron, 1085 S Univ Ave, Ann Arbor, MI 48109 USA
14.SUNY Coll Fredonia, Dept Phys, Fredonia, NY 14063 USA
15.Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA
16.TU Wien, Inst Fluid Mech & Heat Transfer, A-1060 Vienna, Austria
17.Southern Fed Univ, Inst Phys Res, Stachki Ave 194, Rostov Na Donu 344090, Russia
18.Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria
19.Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA
20.Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan
21.Joint ALMA Observ, Alonso de Cordova 3107, Santiago, Chile
22.Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
23.Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada
24.Univ Western Ontario, Dept Phys & Astron, 1151 Richmond St, London, ON N6A 3K7, Canada
25.Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland
26.East Asian Observ, 660 N Aohoku Pl, Hilo, HI 96720 USA
27.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi, Peoples R China
28.Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju, South Korea
29.Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales
30.Univ Cent Lancashire, Jeremiah Horrocks Inst Math Phys & Astron, Preston PR1 2HE, Lancs, England
31.Univ Hertfordshire, Sch Phys Astron & Math, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England
32.CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA
33.Nagoya Univ, Grad Sch Sci, Dept Phys, Nagoya, Aichi 4648602, Japan
34.Korea Natl Univ Educ, Cheongju 28173, Chungbuk, South Korea
35.Natl Taiwan Normal Univ, Dept Earth Sci, Taipei 116, Taiwan
36.Korea Univ Sci & Technol, 217 Gajang Ro, Daejeon 34113, South Korea
37.Peking Univ, Dept Astron, Yiheyuan 5, Beijing 100871, Peoples R China
38.Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China
39.Kagoshima Univ, Grad Sch Sci & Engn, Dept Phys & Astron, 1-21-35 Korimoto, Kagoshima, Kagoshima 8900065, Japan
40.Chinese Acad Sci, Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China
41.Chinese Acad Sci, Key Lab Radio Astron, 2 West Beijing Rd, Nanjing 210008, Jiangsu, Peoples R 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]. ASTROPHYSICAL JOURNAL,2017,849(1):43.
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.ASTROPHYSICAL JOURNAL,849(1),43.
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".ASTROPHYSICAL JOURNAL 849.1(2017):43.
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