The Astrophysical Journal (Jan 2024)

LoVoCCS. II. Weak Lensing Mass Distributions, Red-sequence Galaxy Distributions, and Their Alignment with the Brightest Cluster Galaxy in 58 Nearby X-Ray-luminous Galaxy Clusters

  • Shenming Fu,
  • Ian Dell’Antonio,
  • Zacharias Escalante,
  • Jessica Nelson,
  • Anthony Englert,
  • Søren Helhoski,
  • Rahul Shinde,
  • Julia Brockland,
  • Philip LaDuca,
  • Christelyn Larkin,
  • Lucca Paris,
  • Shane Weiner,
  • William K. Black,
  • Ranga-Ram Chary,
  • Douglas Clowe,
  • M. C. Cooper,
  • Megan Donahue,
  • August Evrard,
  • Mark Lacy,
  • Tod Lauer,
  • Binyang Liu,
  • Jacqueline McCleary,
  • Massimo Meneghetti,
  • Hironao Miyatake,
  • Mireia Montes,
  • Priyamvada Natarajan,
  • Michelle Ntampaka,
  • Elena Pierpaoli,
  • Marc Postman,
  • Jubee Sohn,
  • David Turner,
  • Keiichi Umetsu,
  • Yousuke Utsumi,
  • Gillian Wilson

DOI
https://doi.org/10.3847/1538-4357/ad67c6
Journal volume & issue
Vol. 974, no. 1
p. 69

Abstract

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The Local Volume Complete Cluster Survey is an ongoing program to observe nearly a hundred low-redshift X-ray-luminous galaxy clusters (redshifts 0.03 10 ^44 erg s ^−1 ) with the Dark Energy Camera, capturing data in the u , g , r , i , z bands with a 5 σ point source depth of approximately 25th–26th AB magnitudes. Here, we map the aperture masses in 58 galaxy cluster fields using weak gravitational lensing. These clusters span a variety of dynamical states, from nearly relaxed to merging systems, and approximately half of them have not been subject to detailed weak lensing analysis before. In each cluster field, we analyze the alignment between the 2D mass distribution described by the aperture mass map, the 2D red-sequence (RS) galaxy distribution, and the brightest cluster galaxy (BCG). We find that the orientations of the BCG and the RS distribution are strongly aligned throughout the interiors of the clusters: the median misalignment angle is 19° within 2 Mpc. We also observe the alignment between the orientations of the RS distribution and the overall cluster mass distribution (by a median difference of 32° within 1 Mpc), although this is constrained by galaxy shape noise and the limitations of our cluster sample size. These types of alignment suggest long-term dynamical evolution within the clusters over cosmic timescales.

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