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dc.contributor.authorHoq, Sadiaen_US
dc.contributor.authorClemens, D. P.en_US
dc.contributor.authorGuzman, Andres E.en_US
dc.contributor.authorCashman, Lauren R.en_US
dc.date.accessioned2017-12-08T15:47:46Z
dc.date.available2017-12-08T15:47:46Z
dc.date.issued2017-02-20
dc.identifierhttp://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000395797900015&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=6e74115fe3da270499c3d65c9b17d654
dc.identifier.citationSadia Hoq, DP Clemens, Andres E Guzman, Lauren R Cashman. 2017. "Tracing the Magnetic Field of IRDC G028.23-00.19 Using NIR Polarimetry." Astrophysical Journal, v. 836, Issue 2, 20 p.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttps://hdl.handle.net/2144/25895
dc.description.abstractThe importance of the magnetic (B) field in the formation of infrared dark clouds (IRDCs) and massive stars is an ongoing topic of investigation. We studied the plane-of-sky B field for one IRDC, G028.23-00.19, to understand the interaction between the field and the cloud. We used near-IR background starlight polarimetry to probe the B field and performed several observational tests to assess the field importance. The polarimetric data, taken with the Mimir instrument, consisted of H-band and K-band observations, totaling 17,160 stellar measurements. We traced the plane-of-sky B-field morphology with respect to the sky-projected cloud elongation. We also found the relationship between the estimated B-field strength and gas volume density, and we computed estimates of the normalized mass-to-magnetic flux ratio. The B-field orientation with respect to the cloud did not show a preferred alignment, but it did exhibit a large-scale pattern. The plane-of-sky B-field strengths ranged from 10 to 165 μG, and the B-field strength dependence on density followed a power law with an index consistent with 2/3. The mass-to-magnetic flux ratio also increased as a function of density. The relative orientations and relationship between the B field and density imply that the B field was not dynamically important in the formation of the IRDC. The increase in mass-to-flux ratio as a function of density, though, indicates a dynamically important B field. Therefore, it is unclear whether the B field influenced the formation of G28.23. However, it is likely that the presence of the IRDC changed the local B-field morphology.en_US
dc.description.sponsorshipWe thank J. Montgomery, T. Hogge, and I. Stephens for constructive discussions on the analysis. We are grateful to R. Crutcher for permission to include his Zeeman data. This research was conducted in part using the Mimir instrument, jointly developed at Boston University and Lowell Observatory and supported by NASA, NSF, and the W.M. Keck Foundation. This research made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology (Caltech), under contract with NASA. This publication made use of data products from the Two Micron All Sky Survey, which was a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/Caltech, funded by NASA and NSF. This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey. The ATLAS-GAL project is a collaboration between the Max-PlanckGesellschaft, the European Southern Observatory (ESO), and the Universidad de Chile. It includes projects E-181.C-0885, E-078.F-9040(A), M-079.C-9501(A), M-081.C-9501(A), and Chilean data. This publication makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project of Boston University and Five College Radio Astronomy Observatory, funded by the National Science Foundation under grants AST-9800334, 0098562, 0100793, 0228993, and. 0507657. A.E.G. acknowledges support from FONDECYT 3150570. This work was supported under NSF grants AST 09-07790 and 14-12269 and NASA grant NNX15AE51G to Boston University. We thank the anonymous referee for valuable feedback, which improved the quality of this work. (NASA; NSF; W.M. Keck Foundation; E-181.C-0885 - Max-Planck-Gesellschaft; E-078.F-9040(A) - Max-Planck-Gesellschaft; M-079.C-9501(A) - Max-Planck-Gesellschaft; M-081.C-9501(A) - Max-Planck-Gesellschaft; E-181.C-0885 - European Southern Observatory (ESO); E-078.F-9040(A) - European Southern Observatory (ESO); M-079.C-9501(A) - European Southern Observatory (ESO); M-081.C-9501(A) - European Southern Observatory (ESO); E-181.C-0885 - Universidad de Chile; E-078.F-9040(A) - Universidad de Chile; M-079.C-9501(A) - Universidad de Chile; M-081.C-9501(A) - Universidad de Chile; AST-9800334 - National Science Foundation; 0098562 - National Science Foundation; 0100793 - National Science Foundation; 0228993 - National Science Foundation; 0507657 - National Science Foundation; 3150570 - FONDECYT; AST 09-07790 - NSF; 14-12269 - NSF; NNX15AE51G - NASA)en_US
dc.format.extentp. 1-20en_US
dc.languageEnglish
dc.language.isoen_US
dc.publisherInstitute of Physics Publishing Ltden_US
dc.relation.ispartofAstrophysical Journal
dc.rights© 2017. The American Astronomical Society. All rights reserved.en_US
dc.subjectScience & technologyen_US
dc.subjectPhysical sciencesen_US
dc.subjectAstronomy & astrophysicsen_US
dc.subjectDust, extinctionen_US
dc.subjectISM: cloudsen_US
dc.subjectISM: individual objects (G028.23-00.19)en_US
dc.subjectISM: magnetic fieldsen_US
dc.subjectStars: formationen_US
dc.subjectTechniques: polarimetricen_US
dc.subjectFilamentary molecular cloudsen_US
dc.subjectPolarization survey GPIPSen_US
dc.subjectRegulated star-formationen_US
dc.subjectInfrared dark cloudsen_US
dc.subjectGalactic planeen_US
dc.subjectAmbipolar diffusionen_US
dc.subjectZeeman observationsen_US
dc.subjectInterstellar dusten_US
dc.subjectMilky Wayen_US
dc.titleTracing the magnetic field of IRDC G028.23-00.19 using NIR polarimetryen_US
dc.typeArticleen_US
dc.identifier.doi10.3847/1538-4357/836/2/199
pubs.elements-sourceweb-of-scienceen_US
pubs.notesEmbargo: No embargoen_US
pubs.organisational-groupBoston Universityen_US
pubs.organisational-groupBoston University, College of Arts & Sciencesen_US
pubs.organisational-groupBoston University, College of Arts & Sciences, Department of Astronomyen_US
pubs.publication-statusPublisheden_US
dc.identifier.orcid0000-0002-9947-4956 (Clemens, DP)


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