Comparison of prestellar core elongations and large-scale molecular cloud structures in the Lupus I region
- UCL, KLB, Department of Physics and Astronomy, Gower Place, London WC1E 6BT (United Kingdom)
- School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA (United Kingdom)
- Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104 (United States)
- Department of Physics, University of Toronto, 60 St. George Street, Toronto, ON M5S 1A7 (Canada)
- XMM SOC, ESAC, Apartado 78, E-28691 Villanueva de la Canãda, Madrid (Spain)
- Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4 (Canada)
- Department of Physics, Nagoya University, Chikusa-ku, Nagoya, Aichi 464-8601 (Japan)
- Department of Physics, University of Miami, 1320 Campo Sano Drive, Coral Gables, FL 33146 (United States)
- Department of Physics, Brown University, 182 Hope Street, Providence, RI 02912 (United States)
- Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 (United States)
- California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125 (United States)
- Physics Department, University of Puerto Rico, Rio Piedras Campus, Box 23343, UPR station, San Juan, PR 00931 (United States)
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 μm 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 μm 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.
- OSTI ID:
- 22365390
- Journal Information:
- Astrophysical Journal, Vol. 791, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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