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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 k{\lambda}) matched ALMA andVLA 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 frequencyemission (> 233 GHz) (560 pc * 390 pc), suggesting different physical originsfor the continuum emission. Based on an SED model for a dusty starburst galaxy,it is found that the SED can be explained by three components, (1) non-thermalsynchrotron emission (traced in the 4.81 and 8.36 GHz continuum), (2) thermalfree-free emission (traced in the 108 GHz continuum), and (3) thermal dustemission (traced in the 352 and 691 GHz continuum). We also present thespatially-resolved (sub-kpc scale) Kennicutt-Schmidt relation of NGC 1614. Theresult suggests a systematically shorter molecular gas depletion time in NGC1614 (average {\tau}_gas of 49 - 77 Myr and 70 - 226 Myr at the starburst ringand 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 starformation activities in U/LIRGs are efficiently enhanced as the merger stageproceeds, which is consistent with the results from high-resolution numericalmerger simulations.

Spatially-resolved Radio-to-Far-infrared SED of the Luminous Merger Remnant NGC 1614 with ALMA and VLA