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dc.contributor.authorOh, Heeyoung
dc.contributor.authorPyo, Tae-Soo
dc.contributor.authorKoo, Bon-Chul
dc.contributor.authorYuk, In-Soo
dc.contributor.authorKaplan, Kyle F.
dc.contributor.authorLee, Yong-Hyun
dc.contributor.authorSokal, Kimberly R.
dc.contributor.authorMace, Gregory N.
dc.contributor.authorPark, Chan
dc.contributor.authorLee, Jae-Joon
dc.contributor.authorPark, Byeong-Gon
dc.contributor.authorHwang, Narae
dc.contributor.authorKim, Hwihyun
dc.contributor.authorJaffe, Daniel T.
dc.date.accessioned2018-05-23T15:49:25Z
dc.date.available2018-05-23T15:49:25Z
dc.date.issued2018-05
dc.identifier.citationHeeyoung Oh et al 2018 ApJ 858 23en_US
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aabba4
dc.identifier.urihttp://hdl.handle.net/10150/627755
dc.description.abstractWe present a high-resolution, near-IR spectroscopic study of multiple outflows in the LkH alpha 234 star formation region using the Immersion GRating INfrared Spectrometer (IGRINS). Spectral mapping over the blueshifted emission of HH 167 allowed us to distinguish at least three separate, spatially overlapped outflows in H-2 and [Fe II] emission. We show that the H-2 emission represents not a single jet but rather complex multiple outflows driven by three known embedded sources: MM1, VLA 2, and VLA 3. There is a redshifted H-2 outflow at a low velocity, V-LSR < +50 km s(-1), with respect to the systemic velocity of V-LSR = -11.5 km s(-1), that coincides with the H2O masers seen in earlier radio observations 2 '' southwest of VLA 2. We found that the previously detected [Fe II] jet with vertical bar V-LSR vertical bar > 100 km s(-1) driven by VLA 3B is also detected in H-2 emission and confirm that this jet has a position angle of about 240 degrees. Spectra of the redshifted knots at 14 ''-65 '' northeast of LkH alpha 234 are presented for the first time. These spectra also provide clues to the existence of multiple outflows. We detected high-velocity (50-120 km s(-1)) H-2 gas in the multiple outflows around LkH alpha 234. Since these gases move at speeds well over the dissociation velocity (> 40 km s(-1)), the emission must originate from the jet itself rather than H-2 gas in the ambient medium. Also, position-velocity and excitation diagrams indicate that emission from knot C in HH 167 comes from two different phenomena, shocks and photodissociation.en_US
dc.description.sponsorshipUS National Science Foundation [AST-1229522]; University of Texas at Austin; Korean GMT Project of KASI; National Research Foundation of Korea (NRF) - Korean government (MSIP) [2012R1A4A1028713]en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.relation.urlhttp://stacks.iop.org/0004-637X/858/i=1/a=23?key=crossref.47895c23921a0f1922e84fbf131cb50een_US
dc.rights© 2018. The American Astronomical Society. All rights reserved.en_US
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectISM: individual objects (LkH alpha 234, HH 167)en_US
dc.subjectISM: jets and outflowsen_US
dc.subjectISM: moleculesen_US
dc.subjectstars: formationen_US
dc.subjecttechniques: spectroscopicen_US
dc.titleHigh-resolution Near-IR Spectral Mapping with H-2 and [Fe II] Lines of Multiple Outflows around LkH alpha 234en_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Astron, Steward Observen_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.volume858
dc.source.issue1
dc.source.beginpage23
refterms.dateFOA2018-05-23T15:49:26Z


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