Poidevin, Frédérick, Ade, Peter A. R., Angile, Francesco E., Benton, Steven J., Chapin, Edward L., Devlin, Mark J., Fissel, Laura M., Fukui, Yasuo, Gandilo, Natalie N., Gundersen, Joshua O., Hargrave, Peter C., Klein, Jeffrey, Korotkov, Andrei L., Matthews, Tristan G., Moncelsi, Lorenzo, Mroczkowski, Tony K., Netterfield, Calvin B., Novak, Giles, Nutter, David, Olmi, Luca, Pascale, Enzo, Savini, Giorgio, Scott, Douglas, Shariff, Jamil A., Soler, Juan Diego, Tachihara, Kengo, Thomas, Nicholas E., Truch, Matthew D. P., Tucker, Carole E., Tucker, Gregory S. and Ward-Thompson, Derek (2014) Comparison of prestellar core elongations and large-scale molecular cloud structures in the Lupus 1 region. Astrophysical Journal, 791 (1). p. 43. ISSN 0004-637X
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Official URL: http://dx.doi.org/10.1088/0004-637x/791/1/43
Turbulence and magnetic fields are expected to be important for regulating molecular cloud formation and evolution. However, their effects on sub-parsec to 100 parsec scales, leading to the formation of starless cores, are not well understood. We investigate the prestellar core structure morphologies obtained from analysis of the Herschel-SPIRE 350 mum maps of the Lupus I cloud. This distribution is first compared on a statistical basis to the large-scale shape of the main filament. We find the distribution of the elongation position angle of the cores to be consistent with a random distribution, which means no specific orientation of the morphology of the cores is observed with respect to the mean orientation of the large-scale filament in Lupus I, nor relative to a large-scale bent filament model. This distribution is also compared to the mean orientation of the large-scale magnetic fields probed at 350 mum with the Balloon-borne Large Aperture Telescope for Polarimetry during its 2010 campaign. Here again we do not find any correlation between the core morphology distribution and the average orientation of the magnetic fields on parsec scales. Our main conclusion is that the local filament dynamics---including secondary filaments that often run orthogonally to the primary filament---and possibly small-scale variations in the local magnetic field direction, could be the dominant factors for explaining the final orientation of each core.
|Uncontrolled Keywords (separate with ;):||ISM: clouds, ISM: individual objects: Lupus I, ISM: magnetic fields, polarization, submillimeter:|
|Subjects:||Physical sciences > Astronomy|
|Schools:||Faculty of Science and Technology > School of Physical Sciences and Computing > Jeremiah Horrocks Institute|
|Deposited By:||Nuala Jones|
|Deposited On:||02 Apr 2015 12:00|
|Last Modified:||19 Oct 2016 12:42|
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