Protostars and Planets VI, Heidelberg, July 15-20, 2013

Poster 1S044

Two Mass Distributions in the L 1641 Molecular Clouds: The Herschel connection of Dense Cores and Filaments in Orion A

Polychroni, Danae (University of Athens, Department of Astrophysics, Astronomy and Mechanics, Faculty of Physics, Panepistimiopolis, 15784 Zografos, Athens, Greece.)
Schisano, Eugenio (Infrared Processing and Analysis Center, California In stitute of Technology, Pasadena, CA, 91125, USA)
Elia, Davide (Istituto di Astrofisica e Planetologia Spaziali (INAF- IAPS), via del Fosso del Cavaliere 100, 00133 Roma, Italy)
Roy, Arabindo (Laboratoire AIM, CEA/IRFU CNRS/INSU Universit ́ e Paris Diderot, Paris-Saclay, 91191 Gif-sur-Yvette, France)
Molinari, Sergio (Istituto di Astrofisica e Planetologia Spaziali (INAF- IAPS), via del Fosso del Cavaliere 100, 00133 Roma, Italy)
Martin, Peter (Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada)
Andre, Philippe (Laboratoire AIM, CEA/IRFU CNRS/INSU Universit ́ e Paris Diderot, Paris-Saclay, 91191 Gif-sur-Yvette, France)
Turrini, Diego (Istituto di Astrofisica e Planetologia Spaziali (INAF- IAPS), via del Fosso del Cavaliere 100, 00133 Roma, Italy)
Rygl, Kazi (Istituto di Astrofisica e Planetologia Spaziali (INAF- IAPS), via del Fosso del Cavaliere 100, 00133 Roma, Italy)
Benedettini, Milena (Istituto di Astrofisica e Planetologia Spaziali (INAF- IAPS), via del Fosso del Cavaliere 100, 00133 Roma, Italy)
Busquet, Gemma (Istituto di Astrofisica e Planetologia Spaziali (INAF- IAPS), via del Fosso del Cavaliere 100, 00133 Roma, Italy)
di Giorgio, Anna Maria (Istituto di Astrofisica e Planetologia Spaziali (INAF- IAPS), via del Fosso del Cavaliere 100, 00133 Roma, Italy)
Pestalozzi, Michele (Istituto di Astrofisica e Planetologia Spaziali (INAF- IAPS), via del Fosso del Cavaliere 100, 00133 Roma, Italy)
Pezzuto, Stefano (Istituto di Astrofisica e Planetologia Spaziali (INAF- IAPS), via del Fosso del Cavaliere 100, 00133 Roma, Italy)
Arzoumanian, Doris (IAS, CNRS (UMR 8617), Universit ́ e Paris-Sud, Batiment 121, 91400 Orsay, France)
Bontemps, Silvain (Universit ́ e de Bordeaux, Laboratoire dAstrophysique de Bordeaux, CNRS/INSU, UMR 5804, BP 89, 33271, Floirac Cedex, France)
Di Francesco, James (Department of Physics & Astronomy, University of Victoria, PO Box 355, STN, CSC, Victoria BC, V8W 3p6, Canada)
Hennemann, Martin (MPIA Heidelberg, Germany)
Hill, Tracy (Laboratoire AIM, CEA/IRFU CNRS/INSU Universit ́ e Paris Diderot, Paris-Saclay, 91191 Gif-sur-Yvette, France)
Konyves, Vera (Laboratoire AIM, CEA/IRFU CNRS/INSU Universit ́ e Paris Diderot, Paris-Saclay, 91191 Gif-sur-Yvette, France)
Men\'shchikov, Alexander (Laboratoire AIM, CEA/IRFU CNRS/INSU Universit ́ e Paris Diderot, Paris-Saclay, 91191 Gif-sur-Yvette, France)
Motte, Frederique (Laboratoire AIM, CEA/IRFU CNRS/INSU Universit ́ e Paris Diderot, Paris-Saclay, 91191 Gif-sur-Yvette, France)
Nguyen-Luong, Quang (Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada)
Peretto, Nicolas (Cardiff School of Physics and Astronomy, Cardiff Uni- versity, Queens Buildings, The Parade, Cardiff, Wales, CF24 3AA, UK)
Schneider , Nicola (Laboratoire AIM, CEA/IRFU CNRS/INSU Universit ́ e Paris Diderot, Paris-Saclay, 91191 Gif-sur-Yvette, France)
White, Glenn (Space Science and Technology Department, Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX, UK)

Abstract:
We present the Herschel Gould Belt survey maps of the L 1641 molecular clouds in Orion A. We extracted both the filaments and dense cores in the region. We identified which of dense sources are proto- or pre-stellar, and studied their association with the identified filaments. We find that although most (71%) of the pre-stellar sources are located on filaments there is still a significant fraction of sources not associated with such structures. We find that these two populations (on and off the identified filaments) have distinctly different mass distributions. The mass distribution of the sources on the filaments is found to peak at 4 Solar Masses and drives the shape of the CMF at higher masses, which we fit with a power law of the form dN /dlogM ∝ M −1.40.4 . The mass distribution of the sources off the filaments, on the other hand, peaks at 0.8 Solar Masses and leads to a flattening of the CMF at masses lower than ∼4 Solar Masses. We postulate that this difference between the mass distributions is due to the higher proportion of gas that is available in the filaments, rather than in the diffuse cloud.

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