CARMA-NRO Orion Survey: Core Emergence and Kinematics in the Orion A Cloud

Creators: Kong, Shuo; Arce, Héctor G.; Sargent, Anneila I.; Mairs, Steve; Klessen, Ralf S.; Bally, John; Padoan, Paolo; Smith, Rowan J.; Maureira, María José; Carpenter, John M.; Ginsburg, Adam; Stutz, Amelia M.; Goldsmith, Paul; Meingast, Stefan; McGehee, Peregrine; Sánchez-Monge, Álvaro; Suri, Sümeyye; Pineda, Jaime E.; Alves, João; Feddersen, Jesse R.; Kauffmann, Jens; Schilke, Peter

Abstract

We have investigated the formation and kinematics of submillimeter (submm) continuum cores in the Orion A molecular cloud. A comparison between submm continuum and near-infrared extinction shows a continuum core detection threshold of A_V ~ 5–10 mag. The threshold is similar to the star formation extinction threshold of A_V ~ 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 ≾ A V ≾ 60 mag. Using data from the CARMA-NRO Orion Survey, we find that dense cores in the integral-shaped filament (ISF) show subsonic 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.

Additional Information

© 2019 The American Astronomical Society. Received 2018 November 26; revised 2019 July 9; accepted 2019 July 9; published 2019 August 30. We thank the anonymous referee for constructive reports that significantly improve the quality of the paper. We acknowledge the fruitful discussions with James Lane and Helen Kirk. S.K. and H.G.A. were funded by NSF award AST-1140063 while conducting this study. R.S.K. thanks the support from the German Science Foundation (DFG) via the Collaborative Research Center SFB 881 "The Milky Way System" (subproject B1 and B2). A.S. acknowledges funding through Fondecyt regular (project code 1180350), "Concurso Proyectos Internacionales de Investigación" (project code PII20150171), and Chilean Centro de Excelencia en Astrofísica y Tecnologías Afines (CATA) BASAL grant AFB-170002. The JCMT has historically been operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the National Research Council of Canada, and the Netherlands Organisation for Scientific Research. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. The identification number for the programme under which the SCUBA-2 data used in this paper is MJLSG313. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. This research was carried out in part at the Jet Propulsion Laboratory which is operated for NASA by the California Institute of Technology. Facilities: CARMA - Combined Array for Research in Millimeter-Wave Astronomy, No:45m - , JCMT - , GBT - , VISTA - , Herschel. - Software: The data analysis in this paper uses python packages Astropy (Astropy Collaboration et al. 2013), SciPy (Jones et al. 2001), and Numpy (van der Walt et al. 2011). The figures are plotted using python packages APLpy (Robitaille & Bressert 2012) and Matplotlib (Hunter 2007).

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