Multiwavelength Analysis of A1240, the Double Radio-relic Merging Galaxy Cluster Embedded in an ∼80 Mpc-long Cosmic Filament

Hyejeon Cho; M. James Jee; Rory Smith; Kyle Finner; Wonki Lee

doi:10.3847/1538-4357/ac36c8

Multiwavelength Analysis of A1240, the Double Radio-relic Merging Galaxy Cluster Embedded in an ∼80 Mpc-long Cosmic Filament

Hyejeon Cho, M. James Jee, Rory Smith, Kyle Finner, Wonki Lee

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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=2.61-0.60+0.51×1014M⊙) and middle ( M200=1.09-0.43+0.34×1014M⊙) 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=1.78-0.55+0.44×1014M⊙), ∼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.

Original language	English
Article number	68
Journal	Astrophysical Journal
Volume	925
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/ac36c8
Publication status	Published - 2022 Jan 1

Bibliographical note

Funding Information:
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.

Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/ac36c8

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title = "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=2.61-0.60+0.51×1014M⊙) and middle ( M200=1.09-0.43+0.34×1014M⊙) 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=1.78-0.55+0.44×1014M⊙), ∼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.",

author = "Hyejeon Cho and {James Jee}, M. and Rory Smith and Kyle Finner and Wonki Lee",

note = "Funding Information: 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. Publisher Copyright: {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society.",

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doi = "10.3847/1538-4357/ac36c8",

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AU - James Jee, M.

AU - Smith, Rory

AU - Finner, Kyle

AU - Lee, Wonki

N1 - Funding Information: 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. Publisher Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

PY - 2022/1/1

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N2 - 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=2.61-0.60+0.51×1014M⊙) and middle ( M200=1.09-0.43+0.34×1014M⊙) 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=1.78-0.55+0.44×1014M⊙), ∼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.

AB - 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=2.61-0.60+0.51×1014M⊙) and middle ( M200=1.09-0.43+0.34×1014M⊙) 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=1.78-0.55+0.44×1014M⊙), ∼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.

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ER -

Multiwavelength Analysis of A1240, the Double Radio-relic Merging Galaxy Cluster Embedded in an ∼80 Mpc-long Cosmic Filament

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