For, Bi-QingStaveley-Smith, ListerHurley-Walker, NatashaFranzen, T. M. O.Kapińska, A. D.Filipovic, M DCollier, J.D.Wu, ChenGrieve, K.Callingham, J.R.Briggs, Franklin2019-12-172019-12-170035-8711http://hdl.handle.net/1885/195679We present the first low-frequency Murchison Widefield Array (MWA) radio continuum maps of the Magellanic Clouds (MCs), using mosaics from the GaLactic Extragalactic All-Sky MWA (GLEAM) survey. In this paper, we discuss the overall radio continuum morphology between 76 and 227 MHz and compare them with neutral hydrogen maps, 1.4 GHz continuum maps and optical images. Variation of diffuse emission is noticeable across the Large Magellanic Cloud (LMC) but absent across the bar of the Small Magellanic Cloud (SMC). We also measure the integrated flux densities and derive the spectral indices for the MCs. A double power-law model with fixed α1 = −0.1 fit between 19.7 MHz and 8.55 GHz yields α0 = −0.66 ± 0.08 for the LMC. A power-law model yields α85.5MHz8.55GHz=−0.82±0.03 for the SMC. The radio spectral index maps reveal distinctive flat and steep spectral indices for the H II regions and supernova remnants, respectively. We find strong correlation between H II regions and Hα emission. Using a new 150 MHz–Hα relation as a star formation rate indicator, we estimate global star formation rates of 0.068–0.161 M⊙ yr−1 and 0.021–0.050 M⊙ yr−1 for the LMC and SMC, respectively. Images in 20 frequency bands, and wideband averages are made available via the GLEAM virtual observatory server.This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the operation of the Murchison Widefield Array is provided by the Australian Government (NCRIS), under a contract to Curtin University administered by Astronomy Australia Limited. We acknowledge the Pawsey Supercomputing Centre which is supported by the Western Australian and Australian Governments and the Centre of Excellence for All-sky Astrophysics (CAASTRO), which is an Australian Research Council Centre of Excellence, funded by grant CE110001020. Parts of this research were conducted with the support of Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. This research also made use of Montage. Montage is funded by the National Science Foundation under Grant Number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration’s Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology.application/pdfen-AU© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society201810.1093/MNRAS/STY19602019-07-21