The peculiar cluster MACS J0417.5-1154 in the C and X-bands

  • Pritpal Sandhu
  • Siddharth MaluEmail author
  • Ramij Raja
  • Abhirup Datta
Original Paper


We present 5.5 and 9.0 GHz Australia Telescope Compact Array (ATCA) observations of the cluster MACSJ0417.5-1154, one of the most massive galaxy clusters and one of the brightest in X-ray in the Massive Cluster Survey (MACS). We estimate diffuse emission at 5.5 and 9.0 GHz from our ATCA observations, and compare the results with the 235 MHz and 610 MHz GMRT observations and 1575 MHz VLA observations. We also estimate the diffuse emission at low frequencies from existing GLEAM survey data (using the MWA telescope (, and find that the steepening reported in earlier studies may have been an artefact of underestimates of diffuse emission at low frequencies. High-frequency radio observations of galaxy cluster mergers therefore provide an important complement to low-frequency observations, not only for a probing the ‘on’ and ‘off’ state of radio halos in these mergers, but also to constrain energetics of cluster mergers. We comment on the future directions that further studies of this cluster can take.


Cosmic microwave background Galaxies: clusters: individual (MACSJ0417.5-1154) Intergalactic medium Radio continuum: general Techniques: interferometric 



The Australia Telescope Compact Array is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Analysis and observations were made possible by a generous grant for Astronomy by IIT Indore. GLEAM Postage Stamp Service: The GaLactic and Extragalactic MWA Survey Postage Stamp Service was used for this paper. We are grateful to the anonymous referee for their comments, which helped improve this paper.


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Authors and Affiliations

  1. 1.Centre of AstronomyIndian Institute of Technology IndoreIndoreIndia
  2. 2.Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary ScienceUniversity of ColoradoBoulderUSA

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