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dc.contributor.authorSeo, Young Min
dc.contributor.authorMajumdar, Liton
dc.contributor.authorGoldsmith, Paul F.
dc.contributor.authorShirley, Yancy L.
dc.contributor.authorWillacy, Karen
dc.contributor.authorWard-Thompson, Derek
dc.contributor.authorFriesen, Rachel
dc.contributor.authorFrayer, David
dc.contributor.authorChurch, Sarah E.
dc.contributor.authorChung, Dongwoo
dc.contributor.authorCleary, Kieran
dc.contributor.authorCunningham, Nichol
dc.contributor.authorDevaraj, Kiruthika
dc.contributor.authorEgan, Dennis
dc.contributor.authorGaier, Todd
dc.contributor.authorGawande, Rohit
dc.contributor.authorGundersen, Joshua O.
dc.contributor.authorHarris, Andrew I.
dc.contributor.authorKangaslahti, Pekka
dc.contributor.authorReadhead, Anthony C. S.
dc.contributor.authorSamoska, Lorene
dc.contributor.authorSieth, Matthew
dc.contributor.authorStennes, Michael
dc.contributor.authorVoll, Patricia
dc.contributor.authorWhite, Steve
dc.date.accessioned2019-05-28T22:41:47Z
dc.date.available2019-05-28T22:41:47Z
dc.date.issued2019-02-01
dc.identifier.citationYoung Min Seo et al 2019 ApJ 871 134en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aaf887
dc.identifier.urihttp://hdl.handle.net/10150/632407
dc.description.abstractWe present deep CCS and HC7N observations of the L1495-B218 filaments in the Taurus molecular cloud obtained using the K-band focal plane array on the 100 m Green Bank Telescope. We observed the L1495-B218 filaments in CCS J(N) = 2(1)-1(0) and HC7N J = 21-20 with a spectral resolution of 0.038 km s(-1) and an angular resolution of 31" We observed strong CCS emission in both evolved and young regions and weak emission in two evolved regions. HC7N emission is observed only in L1495A-N and L1521D. We find that CCS and HC7N intensity peaks do not coincide with NH3 or dust continuum intensity peaks. We also find that the fractional abundance of CCS does not show a clear correlation with the dynamical evolutionary stage of dense cores. Our findings and chemical modeling indicate that the fractional abundances of CCS and HC7N are sensitive to the initial gas-phase C/O ratio, and they are good tracers of young condensed gas only when the initial C/O is close to solar value. Kinematic analysis using multiple lines, including NH3, HC7N, CCS, CO, HCN, and HCO+, suggests that there may be three different star formation modes in the L1495-B218 filaments. At the hub of the filaments, L1495A/B7N has formed a stellar cluster with large-scale inward flows (fast mode), whereas L1521D, a core embedded in a filament, is slowly contracting because of its self-gravity (slow mode). There is also one isolated core that appears to be marginally stable and may undergo quasi-static evolution (isolated mode).en_US
dc.description.sponsorshipNSF [AST-1410190]; NASA postdoctoral programen_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0004-637X/871/i=2/a=134?key=crossref.605185043c6db2afd00b3d1fb29c9fd6en_US
dc.rights© 2019. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectISM: cloudsen_US
dc.subjectISM: moleculesen_US
dc.subjectradio lines: ISMen_US
dc.subjectstars: formationen_US
dc.subjectsurveysen_US
dc.titleAn Ammonia Spectral Map of the L1495-B218 Filaments in the Taurus Molecular Cloud. II. CCS and HC7N Chemistry and Three Modes of Star Formation in the Filamentsen_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Steward Observen_US
dc.contributor.departmentUniv Arizona, Dept Astronen_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.journaltitleThe Astrophysical Journal
dc.source.volume871
dc.source.issue2
dc.source.beginpage134
refterms.dateFOA2019-05-28T22:41:48Z


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