We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.

Durham Research Online
You are in:

The core of the massive cluster merger MACS J0417.5-1154 as seen by VLT/MUSE.

Jauzac, Mathilde and Mahler, Guillaume and Edge, Alastair C and Sharon, Keren and Gillman, Steven and Ebeling, Harald and Harvey, David and Richard, Johan and Hamer, Stephen L and Fumagalli, Michele and Swinbank, A Mark and Kneib, Jean-Paul and Massey, Richard and Salomé, Philippe (2018) 'The core of the massive cluster merger MACS J0417.5-1154 as seen by VLT/MUSE.', Monthly notices of the Royal Astronomical Society., 483 (3). pp. 3082-3097.


We present a multiwavelength analysis of the core of the massive galaxy cluster MACS J0417.5−1154 (⁠z = 0.441). Our analysis takes advantage of Very Large Telescope/Multi-Unit Spectroscopic Explorer observations which allow the spectroscopic confirmation of three strongly lensed systems. System #1, nicknamed The Doughnut, consists of three images of a complex ring galaxy at z = 0.8718 and a fourth, partial and radial image close to the brightest cluster galaxy (BCG) only discernible thanks to its strong [O II] line emission. The best-fitting mass model (rms of 0.38 arcsec) yields a two-dimensional enclosed mass of M(R<200kpc)=(1.77±0.03)×1014M⊙ and almost perfect alignment between the peaks of the BCG light and the dark matter of (0.5 ± 0.5) arcsec. We observe a significant misalignment when system #1 radial image is omitted. The result serves as an important caveat for studies of BCG–dark-matter offsets in galaxy clusters. Using Chandra to map the intracluster gas, we observe an offset between gas and dark matter of (1.7 ± 0.5) arcsec, and excellent alignment of the X-ray peak with the location of optical emission line associated with the BCG. We interpret all observational evidences in the framework of ongoing cluster merger activity, noting specifically that the coincidence between the gas and optical line peaks may be evidence of dense, cold gas cooled directly from the intracluster gas. Finally, we measure the surface area, σμ, above a given magnification factor μ, a metric to estimate the lensing power of a lens, σ(μ > 3) = 0.22 arcmin2, which confirms MACS J0417 as an efficient gravitational lens.

Item Type:Article
Full text:(VoR) Version of Record
Download PDF
Publisher Web site:
Publisher statement:© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society
Date accepted:30 November 2018
Date deposited:08 January 2019
Date of first online publication:07 December 2018
Date first made open access:08 January 2019

Save or Share this output

Look up in GoogleScholar