The CARMA-NRO Orion Survey: Core Emergence and Kinematics in the Orion A Cloud. (arXiv:1908.04488v1 [astro-ph.SR])

The CARMA-NRO Orion Survey: Core Emergence and Kinematics in the Orion A Cloud. (arXiv:1908.04488v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kong_S/0/1/0/all/0/1">Shuo Kong</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Arce_H/0/1/0/all/0/1">H&#xe9;ctor G. Arce</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Sargent_A/0/1/0/all/0/1">Anneila I. Sargent</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Mairs_S/0/1/0/all/0/1">Steve Mairs</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Klessen_R/0/1/0/all/0/1">Ralf S. Klessen</a> (4,5), <a href="http://arxiv.org/find/astro-ph/1/au:+Bally_J/0/1/0/all/0/1">John Bally</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Padoan_P/0/1/0/all/0/1">Paolo Padoan</a> (7,8), <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">Rowan J. Smith</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Maureira_M/0/1/0/all/0/1">Mar&#xed;a Jos&#xe9; Maureira</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Carpenter_J/0/1/0/all/0/1">John M. Carpenter</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Ginsburg_A/0/1/0/all/0/1">Adam Ginsburg</a> (11), <a href="http://arxiv.org/find/astro-ph/1/au:+Stutz_A/0/1/0/all/0/1">Amelia M. Stutz</a> (12,13), <a href="http://arxiv.org/find/astro-ph/1/au:+Goldsmith_P/0/1/0/all/0/1">Paul Goldsmith</a> (14), <a href="http://arxiv.org/find/astro-ph/1/au:+Meingast_S/0/1/0/all/0/1">Stefan Meingast</a> (15), <a href="http://arxiv.org/find/astro-ph/1/au:+McGehee_P/0/1/0/all/0/1">Peregrine McGehee</a> (16), <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_Monge_A/0/1/0/all/0/1">&#xc1;lvaro S&#xe1;nchez-Monge</a> (17), <a href="http://arxiv.org/find/astro-ph/1/au:+Suri_S/0/1/0/all/0/1">S&#xfc;meyye Suri</a> (17), <a href="http://arxiv.org/find/astro-ph/1/au:+Pineda_J/0/1/0/all/0/1">Jaime E. Pineda</a> (18), <a href="http://arxiv.org/find/astro-ph/1/au:+Alves_J/0/1/0/all/0/1">Jo&#xe3;o Alves</a> (15,19), <a href="http://arxiv.org/find/astro-ph/1/au:+Feddersen_J/0/1/0/all/0/1">Jesse R. Feddersen</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kauffmann_J/0/1/0/all/0/1">Jens Kauffmann</a> (20), <a href="http://arxiv.org/find/astro-ph/1/au:+Schilke_P/0/1/0/all/0/1">Peter Schilke</a> (17) ((1) Department of Astronomy, Yale University, New Haven, CT 06511, USA, (2) Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 249-17, Pasadena, CA 91125, USA, (3) East Asian Observatory, 660 N. A&#x27;ohoku Place, Hilo, HI 96720, USA, (4) Universit&#xe4;t Heidelberg, Zentrum f&#xfc;r Astronomie, Albert-Ueberle-Str. 2, D-69120 Heidelberg, Germany, (5) Universit&#xe4;t Heidelberg, Interdisziplin&#xe4;res Zentrum f&#xfc;r Wissenschaftliches Rechnen, INF 205, D-69120 Heidelberg, Germany, (6) Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO, USA, (7) Institut de Ci&#xe8;ncies del Cosmos, Universitat de Barcelona, IEEC-UB, Mart&#xed; i Franqu&#xe8;s 1, E08028 Barcelona, Spain, (8) ICREA, Pg. Llu&#xed;s Companys 23, E-08010 Barcelona, Spain, (9) Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK, (10) Joint ALMA Observatory, Alonso de C&#xf3;rdova 3107 Vitacura, Santiago, Chile, (11) National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA, (12) Departmento de Astronom&#xed;a, Facultad de Ciencias F&#xed;sicas y Matem&#xe1;ticas, Universidad de Concepci&#xf3;n, Concepci&#xf3;n, Chile, (13) Max-Planck-Institute for Astronomy, K&#xf6;nigstuhl 17, D-69117 Heidelberg, Germany, (14) Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA, (15) Department of Astrophysics, University of Vienna, T&#xfc;rkenschanzstrasse 17, A-1180 Wien, Austria, (16) Department of Earth and Space Sciences, College of the Canyons, Santa Clarita, CA 91355, USA, (17) I. Physikalisches Institut, Universit&#xe4;t zu K&#xf6;ln, Z&#xfc;lpicher Str. 77, D-50937 K&#xf6;ln, Germany, (18) Max-Planck-Institut f&#xfc;r extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, Germany, (19) Radcliffe Institute for Advanced Study, Harvard University, 10 Garden Street, Cambridge, MA 02138, USA, (20) Haystack Observatory, Massachusetts Institute of Technology, 99 Millstone Road, Westford, MA 01886, USA)

We have investigated the formation and kinematics of sub-mm continuum cores
in the Orion A molecular cloud. A comparison between sub-mm continuum and near
infrared extinction shows a continuum core detection threshold of $A_Vsim$
5-10 mag. The threshold is similar to the star formation extinction threshold
of $A_Vsim$ 7 mag proposed by recent work, suggesting a universal star
formation extinction threshold among clouds within 500 pc to the Sun. A
comparison between the Orion A cloud and a massive infrared dark cloud
G28.37+0.07 indicates that Orion A produces more dense gas within the
extinction range 15 mag $lesssim A_V lesssim$ 60 mag. Using data from the
CARMA-NRO Orion Survey, we find that dense cores in the integral-shaped
filament (ISF) show sub-sonic core-to-envelope velocity dispersion that is
significantly less than the local envelope line dispersion, similar to what has
been found in nearby clouds. Dynamical analysis indicates that the cores are
bound to the ISF. An oscillatory core-to-envelope motion is detected along the
ISF. Its origin is to be further explored.

We have investigated the formation and kinematics of sub-mm continuum cores
in the Orion A molecular cloud. A comparison between sub-mm continuum and near
infrared extinction shows a continuum core detection threshold of $A_Vsim$
5-10 mag. The threshold is similar to the star formation extinction threshold
of $A_Vsim$ 7 mag proposed by recent work, suggesting a universal star
formation extinction threshold among clouds within 500 pc to the Sun. A
comparison between the Orion A cloud and a massive infrared dark cloud
G28.37+0.07 indicates that Orion A produces more dense gas within the
extinction range 15 mag $lesssim A_V lesssim$ 60 mag. Using data from the
CARMA-NRO Orion Survey, we find that dense cores in the integral-shaped
filament (ISF) show sub-sonic core-to-envelope velocity dispersion that is
significantly less than the local envelope line dispersion, similar to what has
been found in nearby clouds. Dynamical analysis indicates that the cores are
bound to the ISF. An oscillatory core-to-envelope motion is detected along the
ISF. Its origin is to be further explored.

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