Tracing the magnetic field of IRDC G028.23-00.19 using NIR polarimetry
dc.contributor.author | Hoq, Sadia | en_US |
dc.contributor.author | Clemens, D. P. | en_US |
dc.contributor.author | Guzman, Andres E. | en_US |
dc.contributor.author | Cashman, Lauren R. | en_US |
dc.date.accessioned | 2017-12-08T15:47:46Z | |
dc.date.available | 2017-12-08T15:47:46Z | |
dc.date.issued | 2017-02-20 | |
dc.identifier | http://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.citation | Sadia 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.issn | 0004-637X | |
dc.identifier.issn | 1538-4357 | |
dc.identifier.uri | https://hdl.handle.net/2144/25895 | |
dc.description.abstract | The 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.sponsorship | We 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.extent | p. 1-20 | en_US |
dc.language | English | |
dc.language.iso | en_US | |
dc.publisher | Institute of Physics Publishing Ltd | en_US |
dc.relation.ispartof | Astrophysical Journal | |
dc.rights | © 2017. The American Astronomical Society. All rights reserved. | en_US |
dc.subject | Science & technology | en_US |
dc.subject | Physical sciences | en_US |
dc.subject | Astronomy & astrophysics | en_US |
dc.subject | Dust, extinction | en_US |
dc.subject | ISM: clouds | en_US |
dc.subject | ISM: individual objects (G028.23-00.19) | en_US |
dc.subject | ISM: magnetic fields | en_US |
dc.subject | Stars: formation | en_US |
dc.subject | Techniques: polarimetric | en_US |
dc.subject | Filamentary molecular clouds | en_US |
dc.subject | Polarization survey GPIPS | en_US |
dc.subject | Regulated star-formation | en_US |
dc.subject | Infrared dark clouds | en_US |
dc.subject | Galactic plane | en_US |
dc.subject | Ambipolar diffusion | en_US |
dc.subject | Zeeman observations | en_US |
dc.subject | Interstellar dust | en_US |
dc.subject | Milky Way | en_US |
dc.title | Tracing the magnetic field of IRDC G028.23-00.19 using NIR polarimetry | en_US |
dc.type | Article | en_US |
dc.identifier.doi | 10.3847/1538-4357/836/2/199 | |
pubs.elements-source | web-of-science | en_US |
pubs.notes | Embargo: No embargo | en_US |
pubs.organisational-group | Boston University | en_US |
pubs.organisational-group | Boston University, College of Arts & Sciences | en_US |
pubs.organisational-group | Boston University, College of Arts & Sciences, Department of Astronomy | en_US |
pubs.publication-status | Published | en_US |
dc.identifier.orcid | 0000-0002-9947-4956 (Clemens, DP) |
This item appears in the following Collection(s)
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BU Open Access Articles [3866]
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CAS: Astronomy: Scholarly Papers [211]