Multiwavelength Analysis of A1240, the Double Radio-relic Merging Galaxy Cluster Embedded in an ∼80 Mpc-long Cosmic Filament
Abstract
We present a multiwavelength study of the double radio-relic cluster A1240 at z = 0.195. Our Subaru-based weak-lensing analysis detects three mass clumps forming an ∼4 Mpc filamentary structure elongated in a north–south orientation. The northern (M₂₀₀ = 2.61^(+0.51)_(−0.60) × 10¹⁴ M_⊙) and middle (M₂₀₀ = 1.09^(+0.34)_(−0.43) × 10¹⁴ M_⊙) mass clumps separated by ∼1.3 Mpc are associated with A1240 and colocated with the X-ray peaks and cluster galaxy overdensities revealed by Chandra and MMT/Hectospec observations, respectively. The southern mass clump (M₂₀₀ = 1.78^(+0.44)_(−0.55) × 10¹⁴ M_⊙), ∼1.5 Mpc to the south of the middle clump, coincides with the galaxy overdensity in A1237, the A1240 companion cluster at z = 0.194. Considering the positions, orientations, and polarization fractions of the double radio relics measured by the LOFAR study, we suggest that A1240 is a postmerger binary system in the returning phase with a time since collision of ∼1.7 Gyr. With the SDSS DR16 data analysis, we also find that A1240 is embedded in the much larger scale (∼80 Mpc) filamentary structure whose orientation is in remarkable agreement with the hypothesized merger axis of A1240.
Additional Information
© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 September 13; revised 2021 October 25; accepted 2021 November 3; published 2022 January 26. This work was supported by the K-GMT Science Program (PID: MMT-2019A-004) of the Korea Astronomy and Space Science Institute (KASI). The observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This work is based in part on data collected at the Subaru Telescope and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. H.C. and K.F. thank Ho Seong Hwang for providing guidance on the MMT/Hectospec data reduction. H.C. acknowledges support from the Brain Korea 21 FOUR Program. M.J.J. acknowledges support for the current research from the National Research Foundation (NRF) of Korea under programs 2017R1A2B2004644 and 2020R1A4A2002885. Facilities: Subaru(Suprime-Cam) - Subaru Telescope, MMT(Hectospec) - , CXO - , LOFAR. - Software: Astropy (Astropy Collaboration et al. 2013, 2018), CIAO (Fruscione et al. 2006), emcee (Foreman-Mackey et al. 2013), FIATMAP (Fischer & Tyson 1997), GetDist (Lewis 2019), HSRED (https://github.com/MMTObservatory/hsred), IRAF/RVSAO (Kurtz & Mink 1998), Matplotlib (Hunter 2007), MPFIT (Markwardt 2009), MCMAC (Dawson 2014), NumPy (Harris et al. 2020), SCAMP (Bertin 2006), SciPy (Virtanen et al. 2020), SDFRED2 (Ouchi et al. 2004), SExtractor (Bertin & Arnouts 1996), SWarp (Bertin et al. 2002).Attached Files
Published - Cho_2022_ApJ_925_68.pdf
Accepted Version - 2109.06879.pdf
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Additional details
- Eprint ID
- 113255
- Resolver ID
- CaltechAUTHORS:20220203-317939000
- MMT-2019A-004
- Korea Astronomy and Space Science Institute (KASI)
- 2017R1A2B2004644
- National Research Foundation of Korea
- 2020R1A4A2002885
- National Research Foundation of Korea
- Created
-
2022-02-03Created from EPrint's datestamp field
- Updated
-
2022-02-03Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)