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dc.contributor.authorLee, YH
dc.contributor.authorJohnstone, D
dc.contributor.authorLee, JE
dc.contributor.authorHerczeg, G
dc.contributor.authorMairs, S
dc.contributor.authorContreras-Pena, C
dc.contributor.authorHatchell, J
dc.contributor.authorNaylor, T
dc.contributor.authorBell, GS
dc.contributor.authorBourke, TL
dc.contributor.authorBroughton, C
dc.contributor.authorFrancis, L
dc.contributor.authorGupta, A
dc.contributor.authorHarsono, D
dc.contributor.authorLiu, SY
dc.contributor.authorPark, G
dc.contributor.authorPlovie, S
dc.contributor.authorMoriarty-Schieven, GH
dc.contributor.authorScholz, A
dc.contributor.authorSharma, T
dc.contributor.authorTeixeira, PS
dc.contributor.authorWang, YT
dc.contributor.authorAikawa, Y
dc.contributor.authorBower, GC
dc.contributor.authorChen, HRV
dc.contributor.authorBae, J
dc.contributor.authorBaek, G
dc.contributor.authorChapman, S
dc.contributor.authorChen, WP
dc.contributor.authorDu, FJ
dc.contributor.authorDutta, S
dc.contributor.authorForbrich, J
dc.contributor.authorGuo, Z
dc.contributor.authorInutsuka, S
dc.contributor.authorKang, M
dc.contributor.authorKirk, H
dc.contributor.authorKuan, YJ
dc.contributor.authorKwon, W
dc.contributor.authorLai, SP
dc.contributor.authorLalchand, B
dc.contributor.authorLane, JMM
dc.contributor.authorLee, CF
dc.contributor.authorLiu, T
dc.contributor.authorMorata, O
dc.contributor.authorPearson, S
dc.contributor.authorPon, A
dc.contributor.authorSahu, D
dc.contributor.authorShang, H
dc.contributor.authorStamatellos, D
dc.contributor.authorTang, SY
dc.contributor.authorXu, Z
dc.contributor.authorYoo, H
dc.contributor.authorRawlings, JMC
dc.date.accessioned2022-10-20T23:36:16Z
dc.date.available2022-10-20T23:36:16Z
dc.date.issued2021-10
dc.identifier.citationLee , YH , Johnstone , D , Lee , JE , Herczeg , G , Mairs , S , Contreras-Pena , C , Hatchell , J , Naylor , T , Bell , GS , Bourke , TL , Broughton , C , Francis , L , Gupta , A , Harsono , D , Liu , SY , Park , G , Plovie , S , Moriarty-Schieven , GH , Scholz , A , Sharma , T , Teixeira , PS , Wang , YT , Aikawa , Y , Bower , GC , Chen , HRV , Bae , J , Baek , G , Chapman , S , Chen , WP , Du , FJ , Dutta , S , Forbrich , J , Guo , Z , Inutsuka , S , Kang , M , Kirk , H , Kuan , YJ , Kwon , W , Lai , SP , Lalchand , B , Lane , JMM , Lee , CF , Liu , T , Morata , O , Pearson , S , Pon , A , Sahu , D , Shang , H , Stamatellos , D , Tang , SY , Xu , Z , Yoo , H & Rawlings , JMC 2021 , ' The JCMT Transient Survey : four-year summary of monitoring the submillimeter variability of protostars ' , Astrophysical Journal , vol. 920 , no. 2 , 119 . https://doi.org/10.3847/1538-4357/ac1679en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 276566177
dc.identifier.otherPURE UUID: 7446c8f3-52f4-493a-af18-ee210d4340de
dc.identifier.otherRIS: urn:05DB13A7ECBC1B26D6D3791EEFF42D39
dc.identifier.otherWOS: 000709555900001
dc.identifier.otherORCID: /0000-0002-3665-5784/work/102725902
dc.identifier.otherScopus: 85118507254
dc.identifier.urihttps://hdl.handle.net/10023/26228
dc.descriptionThe contribution of C.C.P. was funded by a Leverhulme Trust Research Project Grant. D.S. recognizes support from STFC grants ST/N504014/1 and ST/M000877/1.en
dc.description.abstractWe present the four-year survey results of monthly submillimeter monitoring of eight nearby (<500 pc) star-forming regions by the JCMT Transient Survey. We apply the Lomb–Scargle Periodogram technique to search for and characterize variability on 295 submillimeter peaks brighter than 0.14 Jy beam−1, including 22 disk sources (Class II), 83 protostars (Class 0/I), and 190 starless sources. We uncover 18 secular variables, all of them protostars. No single-epoch burst or drop events and no inherently stochastic sources are observed. We classify the secular variables by their timescales into three groups: Periodic, Curved, and Linear. For the Curved and Periodic cases, the detectable fractional amplitude, with respect to mean peak brightness, is ∼4% for sources brighter than ∼0.5 Jy beam−1. Limiting our sample to only these bright sources, the observed variable fraction is 37% (16 out of 43). Considering source evolution, we find a similar fraction of bright variables for both Class 0 and Class I. Using an empirically motivated conversion from submillimeter variability to variation in mass accretion rate, six sources (7% of our full sample) are predicted to have years-long accretion events during which the excess mass accreted reaches more than 40% above the total quiescently accreted mass: two previously known eruptive Class I sources, V1647 Ori and EC 53 (V371 Ser), and four Class 0 sources, HOPS 356, HOPS 373, HOPS 383, and West 40. Considering the full protostellar ensemble, the importance of episodic accretion on few years timescale is negligible—only a few percent of the assembled mass. However, given that this accretion is dominated by events on the order of the observing time window, it remains uncertain as to whether the importance of episodic events will continue to rise with decades-long monitoring.
dc.format.extent23
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rightsCopyright © 2021 The American Astronomical Society. All rights reserved. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-4357/ac1679.en
dc.subjectProtostarsen
dc.subjectYoung stellar objectsen
dc.subjectPre-main sequence starsen
dc.subjectFU Orionis starsen
dc.subjectSubmillimeter astronomyen
dc.subjectStar formationen
dc.subjectVariable starsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe JCMT Transient Survey : four-year summary of monitoring the submillimeter variability of protostarsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.3847/1538-4357/ac1679
dc.description.statusPeer revieweden
dc.date.embargoedUntil2022-10-21
dc.identifier.urlhttps://arxiv.org/abs/2107.10750en


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