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dc.contributor.authorChoudhury, S.en
dc.contributor.authorPineda, J. E.en
dc.contributor.authorCaselli, P.en
dc.contributor.authorOffner, S. S. R.en
dc.contributor.authorRosolowsky, E.en
dc.contributor.authorFriesen, R. K.en
dc.contributor.authorRedaelli, E.en
dc.contributor.authorChacón-Tanarro, A.en
dc.contributor.authorShirley, Y.en
dc.contributor.authorPunanova, A.en
dc.contributor.authorKirk, H.en
dc.date.accessioned2021-08-31T15:06:30Z-
dc.date.available2021-08-31T15:06:30Z-
dc.date.issued2021-
dc.identifier.citationTransition from coherent cores to surrounding cloud in L1688 / S. Choudhury, J. E. Pineda, P. Caselli, et al. — DOI 10.1051/0004-6361/202039897 // Astronomy and Astrophysics. — 2021. — Vol. 648. — A114.en
dc.identifier.issn46361-
dc.identifier.otherFinal2
dc.identifier.otherAll Open Access, Hybrid Gold, Green3
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85104988265&doi=10.1051%2f0004-6361%2f202039897&partnerID=40&md5=c13143abe8b2aaedf9c64298daece5d1
dc.identifier.otherhttps://www.aanda.org/articles/aa/pdf/2021/04/aa39897-20.pdfm
dc.identifier.urihttp://elar.urfu.ru/handle/10995/102940-
dc.description.abstractContext. Stars form in cold dense cores showing subsonic velocity dispersions. The parental molecular clouds display higher temperatures and supersonic velocity dispersions. The transition from core to cloud has been observed in velocity dispersion, but temperature and abundance variations are unknown. Aims. We aim to measure the temperature and velocity dispersion across cores and ambient cloud in a single tracer to study the transition between the two regions. Methods. We use NH3 (1,1) and (2,2) maps in L1688 from the Green Bank Ammonia Survey, smoothed to 1′, and determine the physical properties by fitting the spectra. We identify the coherent cores and study the changes in temperature and velocity dispersion from the cores to the surrounding cloud. Results. We obtain a kinetic temperature map extending beyond dense cores and tracing the cloud, improving from previous maps tracing mostly the cores. The cloud is 4-6 K warmer than the cores, and shows a larger velocity dispersion (Δσv = 0.15-0.25 km s-1). Comparing to Herschel-based dust temperatures, we find that cores show kinetic temperatures that are ≈1.8 K lower than the dust temperature, while the gas temperature is higher than the dust temperature in the cloud. We find an average p-NH3 fractional abundance (with respect to H2) of (4.2 ± 0.2) × 10-9 towards the coherent cores, and (1.4 ± 0.1) × 10-9 outside the core boundaries. Using stacked spectra, we detect two components, one narrow and one broad, towards cores and their neighbourhoods. We find the turbulence in the narrow component to be correlated with the size of the structure (Pearson-r = 0.54). With these unresolved regional measurements, we obtain a turbulence-size relation of σv,NT ∝ r0.5, which is similar to previous findings using multiple tracers. Conclusions. We discover that the subsonic component extends up to 0.15 pc beyond the typical coherent boundaries, unveiling larger extents of the coherent cores and showing gradual transition to coherence over ∼0.2 pc. © S. Choudhury et al. 2021.en
dc.description.sponsorshipAcknowledgemen. S.C., J.E.P., and P.C. acknowledge the support by the Max Planck Society. This material is based upon work supported by the Green Bank Observatory which is a major facility funded by the National Science Foundation operated by Associated Universities, Inc. A.C.-T. acknowledges the support from MINECO projects AYA2016-79006-P and PID2019-108765GB-I00. AP acknowledges the support from the Russian Ministry of Science and Higher Education via the State Assignment Project FEUZ-2020-0038. A.P. is a member of the Max Planck Partner Group at the Ural Federal University.en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherEDP Sciencesen
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceAstron. Astrophys.2
dc.sourceAstronomy and Astrophysicsen
dc.subjectISM: INDIVIDUAL OBJECTS: L1688en
dc.subjectISM: KINEMATICS AND DYNAMICSen
dc.subjectISM: MOLECULESen
dc.subjectSTARS: FORMATIONen
dc.subjectAMMONIAen
dc.subjectDISPERSIONSen
dc.subjectDUSTen
dc.subjectTRACERSen
dc.subjectTURBULENCEen
dc.subjectCOHERENT BOUNDARIESen
dc.subjectDUST TEMPERATURESen
dc.subjectGRADUAL TRANSITIONen
dc.subjectKINETIC TEMPERATURESen
dc.subjectMOLECULAR CLOUDSen
dc.subjectSUBSONIC VELOCITYen
dc.subjectSUPERSONIC VELOCITIESen
dc.subjectVELOCITY DISPERSIONen
dc.subjectVELOCITYen
dc.titleTransition from coherent cores to surrounding cloud in L1688en
dc.typeArticleen
dc.typeinfo:eu-repo/semantics/articleen
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.rsi46030716-
dc.identifier.doi10.1051/0004-6361/202039897-
dc.identifier.scopus85104988265-
local.contributor.employeeChoudhury, S., Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, Garching, 85748, Germany
local.contributor.employeePineda, J.E., Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, Garching, 85748, Germany
local.contributor.employeeCaselli, P., Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, Garching, 85748, Germany
local.contributor.employeeOffner, S.S.R., Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, United States
local.contributor.employeeRosolowsky, E., Department of Physics, 4-181 Ccis, University of Alberta, Edmonton, AB T6G 2E1, Canada
local.contributor.employeeFriesen, R.K., Department of Astronomy and Astrophysics, University of Toronto, 50 St. George St., Toronto, ON M5S 3H4, Canada
local.contributor.employeeRedaelli, E., Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, Garching, 85748, Germany
local.contributor.employeeChacón-Tanarro, A., Observatorio Astronómico Nacional (OAN-IGN), Alfonso XII 3, Madrid, 28014, Spain
local.contributor.employeeShirley, Y., Steward Observatory, 933 North Cherry Ave., Tucson, AZ 85721, United States
local.contributor.employeePunanova, A., Ural Federal University, Mira st. 19, Yekaterinburg, 620002, Russian Federation
local.contributor.employeeKirk, H., Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Rd., Victoria, BC V8P 5C2, Canada, Herzberg Astronomy and Astrophysics, National Research Council of Canada, 5071 West Saanich Rd., Victoria, BC V9E 2E7, Canada
local.volume648-
dc.identifier.wos000642711200002-
local.contributor.departmentMax-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, Garching, 85748, Germany
local.contributor.departmentDepartment of Astronomy, The University of Texas at Austin, Austin, TX 78712, United States
local.contributor.departmentDepartment of Physics, 4-181 Ccis, University of Alberta, Edmonton, AB T6G 2E1, Canada
local.contributor.departmentDepartment of Astronomy and Astrophysics, University of Toronto, 50 St. George St., Toronto, ON M5S 3H4, Canada
local.contributor.departmentObservatorio Astronómico Nacional (OAN-IGN), Alfonso XII 3, Madrid, 28014, Spain
local.contributor.departmentSteward Observatory, 933 North Cherry Ave., Tucson, AZ 85721, United States
local.contributor.departmentUral Federal University, Mira st. 19, Yekaterinburg, 620002, Russian Federation
local.contributor.departmentDepartment of Physics and Astronomy, University of Victoria, 3800 Finnerty Rd., Victoria, BC V8P 5C2, Canada
local.contributor.departmentHerzberg Astronomy and Astrophysics, National Research Council of Canada, 5071 West Saanich Rd., Victoria, BC V9E 2E7, Canada
local.identifier.pure21881180-
local.identifier.pure532bfb02-66f5-4eae-9954-6690affd004fuuid
local.description.orderA114-
local.identifier.eid2-s2.0-85104988265-
local.identifier.wosWOS:000642711200002-
local.fund.feuzFEUZ-2020-0038-
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