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Published June 2018 | Published + Accepted Version
Journal Article Open

The CARMA-NRO Orion Survey


We present the first results from a new, high-resolution ^(12)CO(1–0), ^(13)CO(1–0), and C^(18)O(1–0) molecular-line survey of the Orion A cloud, hereafter referred to as the CARMA-NRO Orion Survey. CARMA observations have been combined with single-dish data from the Nobeyama 45 m telescope to provide extended images at about 0.01 pc resolution, with a dynamic range of approximately 1200 in spatial scale. Here we describe the practical details of the data combination in uv space, including flux scale matching, the conversion of single-dish data to visibilities, and joint deconvolution of single-dish and interferometric data. A Δ-variance analysis indicates that no artifacts are caused by combining data from the two instruments. Initial analysis of the data cubes, including moment maps, average spectra, channel maps, position–velocity diagrams, excitation temperature, column density, and line ratio maps, provides evidence of complex and interesting structures such as filaments, bipolar outflows, shells, bubbles, and photo-eroded pillars. The implications for star formation processes are profound, and follow-up scientific studies by the CARMA-NRO Orion team are now underway. We plan to make all the data products described here generally accessible; some are already available at https://dataverse.harvard.edu/dataverse/CARMA-NRO-Orion.

Additional Information

© 2018 The American Astronomical Society. Received 2018 February 6; revised 2018 March 28; accepted 2018 March 29; published 2018 May 17. We thank the anonymous referee for a thorough check on the paper and helpful comments. We thank Amelia Stutz for fruitful discussions. This research was supported by the National Science Foundation, award AST-1140063, which also provided partial support for CARMA operations. CARMA operations were also supported by the California Institute of Technology, the University of California–Berkeley, the University of Illinois at Urbana-Champaign, the University of Maryland College Park, and the University of Chicago. The Nobeyama 45 m telescope is operated by the Nobeyama Radio Observatory, a branch of the National Astronomical Observatory of Japan. We are grateful to the staff at both NRO and CARMA for all their contributions. We also thank the Yale Center for Research Computing and the staff of their HPC facilities for their support. We thank Rob Gutermuth for providing the Spitzer images. We thank Alvaro Hacar for providing the ALMA data. HGA and JRF were partially funded by NSF award AST-1311825 while conducting this study. JEP acknowledges the financial support of the European Research Council (ERC; project PALs 320620). RJS acknowledges an STFC Ernest Rutherford fellowship. VO was supported by the Deutsche Forschungsgemeinschaft (DFG) through project number 177/2-2 and central funds of the DFG priority program 1573 (ISM-SPP). STS and ASM acknowledge funding by the DFG via the Sonderforschungsbereich SFB 956 Conditions and Impact of Star Formation (subproject A4 and A6) and the Bonn-Cologne Graduate School. RSK acknowledges financial support from the DFG via SFB 881, "The Milky Way System" (subprojects B1, B2, and B8) and SPP 1573, "Physics of the Interstellar Medium." He is also grateful for funding from the European Research Council via the ERC Advanced Grant "STARLIGHT: Formation of the First Stars" (project number 339177). P.P. is supported by the Spanish MINECO under project AYA2017-88754-P. This research was carried out in part at the Jet Propulsion Laboratory, operated for NASA by the California Institute of Technology. Facilities: CARMA - Combined Array for Research in Millimeter-Wave Astronomy, No:45m. - Software: Astropy (Astropy Collaboration et al. 2013), Numpy (van der Walt et al. 2011), APLpy (Robitaille & Bressert 2012), Matplotlib (Hunter 2007).

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Published - Kong_2018_ApJS_236_25.pdf

Accepted Version - 1803.11522.pdf


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