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Spatially resolved radio-to-far-infrared SED of the luminous merger remnant NGC 1614 with ALMA and VLA

Saito, Toshiki and Iono, Daisuke and Xu, Cong K. and Ueda, Junko and Nakanishi, Kouichiro and Yun, Min S. and Kaneko, Hiroyuki and Yamashita, Takuji and Lee, Minju and Espada, Daniel and Motohara, Kentaro and Kawabe, Ryohei (2016) Spatially resolved radio-to-far-infrared SED of the luminous merger remnant NGC 1614 with ALMA and VLA. Publications of the Astronomical Society of Japan, 68 (2). Art. No. 20. ISSN 0004-6264.

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We present the results of Atacama Large Millimeter/Submillimeter Array (ALMA) 108-, 233-, 352-, and 691-GHz continuum observations and Very Large Array (VLA) 4.81- and 8.36-GHz observations of the nearby luminous merger remnant NGC 1614. By analyzing the beam (1′′.0 × 1′′.0) and uv (≥45 kλ) matched ALMA and VLA maps, we find that the deconvolved source size of lower-frequency emission (≤108 GHz) is more compact (420 pc × 380 pc) compared to the higher-frequency emission (≥233 GHz) (560 pc × 390 pc), suggesting different physical origins for the continuum emission. Based on a spectral energy distribution (SED) model for a dusty starburst galaxy, it is found that the SED can be explained by three components: (1) non-thermal synchrotron emission (traced in the 4.81- and 8.36-GHz continua), (2) thermal free–free emission (traced in the 108-GHz continuum), and (3) thermal dust emission (traced in the 352- and 691-GHz continua). We also present the spatially resolved (sub-kpc scale) Kennicutt–Schmidt relation of NGC 1614. The result suggests a systematically shorter molecular gas depletion time in NGC 1614 (average τ_(gas) of 49–77 Myr and 70–226 Myr at the starburst ring and the outer region, respectively) than that of normal disk galaxies (∼2 Gyr) and a mid-stage merger VV 114 (= 0.1–1 Gyr). This implies that the star formation activities in (ultra-)luminous infrared galaxies are efficiently enhanced as the merger stage proceeds, which is consistent with the results from high-resolution numerical merger simulations.

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Additional Information:© The Author 2016. Published by Oxford University Press on behalf of the Astronomical Society of Japan. Received September 10, 2015. Accepted December 16, 2015. First published online February 1, 2016. The authors thank the anonymous referee for comments that improved this paper. TS and other authors thank ALMA staff for their kind support. TS and ML are financially supported by a Research Fellowship from the Japan Society for the Promotion of Science for Young Scientists. TS was supported by the ALMA Japan Research Grant of NAOJ Chile Observatory, NAOJ-ALMA-0114. DI was supported by the ALMA Japan Research Grant of NAOJ Chile Observatory, NAOJ-ALMA-0011, JSPS KAKENHI Grant Number 15H02074, and the 2015 Inamori Research Grants Program. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00182.S, ADS/JAO.ALMA#2011.0.00768.S, and ADS/JAO.ALMA#2013.1.01172.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research has made extensive use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Japan Society for the Promotion of Science (JSPS)15340059
NAOJ Chile ObservatoryNAOJ-ALMA-0114
NAOJ Chile ObservatoryNAOJ-ALMA-0011
Japan Society for the Promotion of Science (JSPS)15H02074
2015 Inamori Research Grants ProgramUNSPECIFIED
Record Number:CaltechAUTHORS:20160603-110021963
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Official Citation:Toshiki Saito, Daisuke Iono, Cong K. Xu, Junko Ueda, Kouichiro Nakanishi, Min S. Yun, Hiroyuki Kaneko, Takuji Yamashita, Minju Lee, Daniel Espada, Kentaro Motohara, and Ryohei Kawabe Spatially resolved radio-to-far-infrared SED of the luminous merger remnant NGC 1614 with ALMA and VLA Publ Astron Soc Jpn (April 2016) 68 (2), 20, doi:10.1093/pasj/psv136 first published online February 1, 2016 (11 pages)
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:67652
Deposited By: Tony Diaz
Deposited On:03 Jun 2016 18:28
Last Modified:03 Jun 2016 18:28

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