Matching dust emission structures and magnetic field in high-latitude cloud L1642 : comparing Herschel and Planck maps

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http://hdl.handle.net/10138/184148

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Malinen , J , Montier , L , Montillaud , J , Juvela , M , Ristorcelli , I , Clark , S E , Berne , O , Bernard , J-P , Pelkonen , V-M & Collins , D C 2016 , ' Matching dust emission structures and magnetic field in high-latitude cloud L1642 : comparing Herschel and Planck maps ' Monthly Notices of the Royal Astronomical Society , vol. 460 , no. 2 , pp. 1934-1945 . DOI: 10.1093/mnras/stw1061

Title: Matching dust emission structures and magnetic field in high-latitude cloud L1642 : comparing Herschel and Planck maps
Author: Malinen, J.; Montier, L.; Montillaud, J.; Juvela, M.; Ristorcelli, I.; Clark, S. E.; Berne, O.; Bernard, J.-Ph.; Pelkonen, V.-M.; Collins, D. C.
Contributor: University of Helsinki, Department of Astronomy (-2009)
University of Helsinki, Department of Physics
Date: 2016-08-01
Language: eng
Number of pages: 12
Belongs to series: Monthly Notices of the Royal Astronomical Society
ISSN: 0035-8711
URI: http://hdl.handle.net/10138/184148
Abstract: The nearby cloud L1642 is one of only two known very high latitude (b| > 30 deg) clouds actively forming stars. It is a rare example of star formation in isolated conditions, and can reveal important details of star formation in general, e.g. of the effect of magnetic fields. We compareHerschel dust emission structures and magnetic field orientation revealed byPlanck polarization maps in L1642. The high-resolution (similar to 20 arcsec)Herschel data reveal a complex structure including a dense, compressed central clump, and low-density striations. ThePlanck polarization data (at 10 arcmin resolution) reveal an ordered magnetic field pervading the cloud and aligned with the surrounding striations. There is a complex interplay between the cloud structure and large-scale magnetic field. This suggests that the magnetic field is closely linked to the formation and evolution of the cloud. CO rotational emission confirms that the striations are connected with the main clumps and likely to contain material either falling into or flowing out of the clumps. There is a clear transition from aligned to perpendicular structures approximately at a column density ofN(H) = 1.6 x 10(21) cm(-2). Comparing theHerschel maps with thePlanck polarization maps shows the close connection between the magnetic field and cloud structure even in the finest details of the cloud.
Subject: polarization
ISM: clouds
ISM: magnetic fields
submillimetre: ISM
POSITIVE MATRIX FACTORIZATION
STAR-FORMATION
POLARIZATION FRACTION
MOLECULAR CLOUDS
PRESTELLAR CORES
CATALOG
MORPHOLOGY
OBJECTS
GRAINS
ANGLE
115 Astronomy, Space science
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