X-Ray Cavity Dynamics and Their Role in the Gas Precipitation in Planck Sunyaev-Zeldovich (SZ) Selected Clusters

V. Olivares, Y. Su, W. Forman, M. Gaspari, F. Andrade-Santos, P. Salome, P. Nulsen, A. Edge, F. Combes, C. Jones

Research output: Contribution to journalArticlepeer-review

2 Scopus citations

Abstract

We study active galactic nucleus (AGN) feedback in nearby (z < 0.35) galaxy clusters from the Planck Sunyaev-Zeldovich sample using Chandra observations. This nearly unbiased mass-selected sample includes both relaxed and disturbed clusters and may reflect the entire AGN feedback cycle. We find that relaxed clusters better follow the one-to-one relation of cavity power versus cooling luminosity, while disturbed clusters display higher cavity power for a given cooling luminosity, likely reflecting a difference in cooling and feedback efficiency. Disturbed clusters are also found to contain asymmetric cavities when compared to relaxed clusters, hinting toward the influence of the intracluster medium (ICM) "weather"on the distribution and morphology of the cavities. Disturbed clusters do not have fewer cavities than relaxed clusters, suggesting that cavities are difficult to disrupt. Thus, multiple cavities are a natural outcome of recurrent AGN outbursts. As in previous studies, we confirm that clusters with short central cooling times, t cool, and low central entropy values, K 0, contain warm ionized (10,000 K) or cold molecular (<100 K) gas, consistent with ICM cooling and a precipitation/chaotic cold accretion scenario. We analyzed archival Multi-Unit Spectroscopic Explorer observations that are available for 18 clusters. In 11/18 of the cases, the projected optical line emission filaments appear to be located beneath or around the cavity rims, indicating that AGN feedback plays an important role in forming the warm filaments by likely enhancing turbulence or uplift. In the remaining cases (7/18), the clusters either lack cavities or their association of filaments with cavities is vague, suggesting alternative turbulence-driven mechanisms (sloshing/mergers) or physical time delays are involved.

Original languageEnglish
Article number56
JournalAstrophysical Journal
Volume954
Issue number1
DOIs
StatePublished - Sep 1 2023

Bibliographical note

Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.

Funding

The authors would like to thank the referee for providing useful and detailed comments on the manuscript. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO. V.O. and Y.S. were supported by NSF grant 2107711, Chandra X-ray Observatory grant GO1-22126X, and NASA grant 80NSSC21K0714. M.G. acknowledges partial support by HST GO-15890.020/023-A and the BlackHoleWeather program. W.F., C.J., and P.N. acknowledge support from the Smithsonian Institution and the Chandra High Resolution Camera Project through NASA contract NAS8-03060. W.F. also acknowledges support from NASA grants 80NSSC19K0116, GO1-22132X, and GO9-20109X. P.S. acknowledges support by the Agence Nationale De La Recherche (ANR) grant LYRICS (ANR-16-CE31-0011).

FundersFunder number
Chandra High Resolution Camera ProjectGO1-22132X, NAS8-03060, GO9-20109X, 80NSSC19K0116
HST/STScIGO-15890.020/023-A
National Science Foundation Arctic Social Science Program2107711, GO1-22126X
National Science Foundation Arctic Social Science Program
Smithsonian Institution
National Aeronautics and Space Administration80NSSC21K0714
National Aeronautics and Space Administration
Agence Nationale de la RechercheANR-16-CE31-0011
Agence Nationale de la Recherche

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

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