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SDSS-C43028: THE NEAREST BLUE GALAXY CLUSTER DEVOID OF AN INTRACLUSTER MEDIUM

  • Shweta Jain
  • , Yuanyuan Su
  • , Andra Stroe
  • , Paul Nulsen
  • , Hyejeon Cho
  • , Kim Hyeonghan
  • , M. James Jee
  • , Ralph P. Kraft
  • , Scott Randall
  • , Jimmy A. Irwin
  • , Ryan L. Sanders
  • , Christine Jones

Research output: Contribution to journal › Article › peer-review

Abstract

SDSS-C43028 is a galaxy cluster at z=0.061, notable for its unusually high fraction of star-forming galaxies with 19 star-forming and 11 quiescent spectroscopically-confirmed member galaxies. From Subaru/HSC imaging, we derived a weak lensing mass of M200=(1.3±0.9)×1014 M⊙, indicating a low-mass cluster. This is in excellent agreement with its dynamical mass of M200=(1.0±0.4)×1014M⊙, derived from SDSS spectroscopic data. XMM-Newton observations reveal that its X-ray emission is uniform and fully consistent with the astrophysical X-ray background, with no evidence for an intracluster medium (ICM). The 3σ upper limit of LX(0.1−2.4keV)=7.7×1042erg s−1 on the cluster’s X-ray luminosity falls below the value expected from the LX−Mhalo scaling relation of nearby galaxy clusters. We derived star-formation histories for its member galaxies using the photometric spectral energy distribution from SDSS, 2MASS, and WISE data. Most of its quiescent galaxies reside within the central 300kpc, while star-forming ones dominate the outer region (300kpc–1Mpc). The core region has formed the bulk of its stellar mass approximately 1.5Gyr earlier than the outskirts. We infer a long quenching time of > 3Gyr for its quiescent galaxies, consistent with slow quenching mechanisms such as galaxy-galaxy interaction or strangulation. These findings suggest that SDSS-C43028 may have undergone an “inside-out” formation and quenching process. Its ICM may have been expelled by intense AGN feedback after core formation but before full cluster assembly. The high fraction (∼0.63) of star-forming members likely results from the absence of ram pressure stripping in this blue cluster, supporting the important role of ram pressure stripping in quenching galaxies in clusters.

Original languageEnglish
JournalOpen Journal of Astrophysics
Volume8
DOIs
StatePublished - 2025

Bibliographical note

Publisher Copyright:
© 2025, National University of Ireland Maynooth. All Rights reserved.

Funding

We thank the anonymous reviewer for their constructive feedback, which helped improve the manuscript. S.J. and Y.S. acknowledge the support of NASA grant 80NSSC22K0856. This work uses observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. H. Cho acknowledges support for the current research from the National Research Foundation of Korea (NRF) under the programs RS-2022 NR070872 and RS-2023-00219959. This work was supported in part by the K-GMT Science Program (PID: GEMINI-KR-2022B-011) of Korea Astronomy and Space Science Institute (KASI). This research is based in part on data collected at the Subaru Telescope (PID: S22B TE011-GQ), via the time exchange program between Subaru and the international Gemini Observatory, a program of NSF’s NOIRLab. The Subaru Telescope is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the Universe from Maunakea, which has the cultural, historical, and natural significance in Hawaii. This research used data obtained with the Dark Energy Spectroscopic Instrument (DESI). DESI construction and operations is managed by the Lawrence Berk ley National Laboratory. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of High-Energy Physics, under Contract No. DE–AC02–05CH11231, and by the Na tional Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI was provided by the U.S. National Science Foundation (NSF), Division of As tronomical Sciences under Contract No. AST-0950945 to the NSF’s National Optical-Infrared Astronomy Research Laboratory; the Science and Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Humanities, Science and Technology of Mexico (CONAHCYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions: www.desi.lbl. gov/collaborating-institutions. The DESI collaboration is honored to be permitted to conduct scientific research on I’oligam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham Nation. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the U.S. National Science Foundation, the U.S. Department of Energy, or any of the listed funding agencies. We thank the anonymous reviewer for their constructive feedback, which helped improve the manuscript. S.J. and Y.S. acknowledge the support of NASA grant 80NSSC22K0856. This work uses observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. H. Cho acknowledges support for the current research from the National Research Foundation of Korea (NRF) under the programs RS-2022-NR070872 and RS-2023-00219959. This work was supported in part by the K-GMT Science Program (PID: GEMINI-KR-2022B-011) of Korea Astronomy and Space Science Institute (KASI). This research is based in part on data collected at the Subaru Telescope (PID: S22B-TE011-GQ), via the time exchange program between Subaru and the international Gemini Observatory, a program of NSF’s NOIRLab. The Subaru Telescope is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the Universe from Maunakea, which has the cultural, historical, and natural significance in Hawaii. This research used data obtained with the Dark Energy Spectroscopic Instrument (DESI). DESI construction and operations is managed by the Lawrence Berkeley National Laboratory. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of High-Energy Physics, under Contract No. DE–AC02–05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI was provided by the U.S. National Science Foundation (NSF), Division of Astronomical Sciences under Contract No. AST-0950945 to the NSF’s National Optical-Infrared Astronomy Research Laboratory; the Science and Technology Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising-Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Humanities, Science and Technology of Mexico (CONAHCYT); the Ministry of Science and Innovation of Spain (MICINN), and by the DESI Member Institutions: www.desi.lbl. gov/collaborating-institutions. The DESI collaboration is honored to be permitted to conduct scientific research on I’oligam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham Nation. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the U.S. National Science Foundation, the U.S. Department of Energy, or any of the listed funding agencies.

FundersFunder number
National Science Foundation Arctic Social Science Program
Science and Technology Facilities Council
Ministerio de Ciencia, Innovación y Universidades
National Energy Research Scientific Computing Center
Consejo Nacional de Humanidades, Ciencias y Tecnologías
Commissariat à l'Énergie Atomique et aux Énergies Alternatives
Heising-Simons Foundation
U.S. Department of Energy
Lawrence Berkeley National Laboratory
Endocrine Society of Australia
Office of Science Programs
Gordon and Betty Moore Foundation
National Research Foundation of KoreaRS-2023-00219959, GEMINI-KR-2022B-011, RS-2022-NR070872
National Aeronautics and Space Administration80NSSC22K0856
Korea Astronomy and Space Science InstituteS22B TE011-GQ
Division of Astronomical SciencesAST-0950945
Institute for High Energy PhysicsDE–AC02–05CH11231

    Keywords

    • Galaxy clusters
    • Intracluster medium
    • SDSS-C43028
    • Weak gravitational lensing
    • X-ray astronomy

    ASJC Scopus subject areas

    • Astronomy and Astrophysics

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