Testing the Limits of AGN Feedback and the Onset of Thermal Instability in the Most Rapidly Star-forming Brightest Cluster Galaxies

Calzadilla, Michael S.; McDonald, Michael; Donahue, M.; McNamara, B. R.; Fogarty, Kevin; Gaspari, M.; Gitti, Myriam; Russell, H. R.; Tremblay, G. R.; Voit, G. Mark; Ubertosi, Francesco

doi:10.3847/1538-4357/ac9790

Cited by 14 publications

(14 citation statements)

References 144 publications

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“…In this context, Cavagnolo et al (2011) noted filamentary structures in the residual optical image of the BCG extending 8-10 kpc southward. These structures were recently confirmed by Calzadilla et al (2022), who produced continuum-subtracted [O II] maps of nebular emission using the Hubble Space Telescope. The overlay of [O II] contours on the t cool /t ff map (see lower right panel in Figure 5) reveals that cool gas at ∼10 4 keV is coincident with the region where the minimum in t cool /t ff is found (within ∼20 kpc S from the center).…”

Section: Thermodynamic Maps Of the Icmmentioning

confidence: 60%

“…The low-entropy (30 keV cm 2 ) and short cooling time (t cool 1 Gyr) ICM is preferentially found between and behind the X-ray cavities, which may indicate that the bubbles are stimulating cooling. In this context, the region with the shortest cooling time (∼440 Myr) and minimum t cool /t ff ratio (∼18) is located within 20 kpc S of the center, where filamentary patches of [O II] nebular emission tracing star-forming gas were recently detected (Calzadilla et al 2022). 3.…”

Section: Discussionmentioning

confidence: 99%

“…Alternatively, the turbulence injected by the nuclear activity may trigger local compressions of the gas (e.g., Brighenti & Mathews 2002;Gaspari et al 2011Gaspari et al , 2012. In such cases, as thermal instabilities may ensue, further cooling of the ICM can be stimulated, creating warm or cold filaments (e.g., McDonald et al 2010;Russell et al 2019;Calzadilla et al 2022;Temi et al 2022;Olivares et al 2022).…”

Section: Introductionmentioning

confidence: 99%

“…In the lower panels, cyan ellipses show the positions of the X-ray cavities. In the lower right panel, white contours fromCalzadilla et al (2022) trace the morphology of the central [O II]-emitting nebulae, and the red dashed wedge shows the region where the minimum in t cool /t ff is found. Relative uncertainties in temperature, pressure, and cooling time are on the order of ∼10%, while those in t cool /t ff are on the order of ∼20%.…”

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confidence: 99%

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Multiple Shock Fronts in RBS 797: The Chandra Window on Shock Heating in Galaxy Clusters

Ubertosi

Gitti

Brighenti

et al. 2023

ApJ

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Using ∼427 ks of Chandra observations, we present a study of shock heating and intracluster medium (ICM) cooling in the galaxy cluster RBS 797. We discover three nested pairs of weak shocks at roughly 50, 80, and 130 kpc from the center. The total energy associated with the shocks is ∼6 × 1061 erg, with the central active galactic nucleus (AGN) driving a pair of weak shocks every 20–30 Myr with a power P sh ≈ 1046 erg s−1. Based on its morphology and age (∼30 Myr), the inner cocoon shock is associated with the four equidistant X-ray cavities previously discovered. From the thermodynamic analysis of the inner 30 kpc, we find evidence for ICM condensation into colder gas between and behind the X-ray cavities. The total AGN mechanical power (cavities and shocks) of 3.4 × 1046 erg s−1 can balance the ICM radiative losses, estimated as L cool = 2.3 × 1045 erg s−1. By building plots of P cav versus L cool, P shock versus L cool, and P tot versus L cool for RBS 797 and 14 other galaxy clusters, galaxy groups, and elliptical galaxies where both cavities and shocks are detected, we verify that the most powerful outbursts are found in the strongest cooling systems. Ultimately, we observe that the mechanical power of the AGN exceeds the gas radiative losses by a factor that is different for FR I and FR II radio galaxies, being less than a few tens for FR Is (as RBS 797) and more than roughly 100 for FR IIs.

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Section: Thermodynamic Maps Of the Icmmentioning

confidence: 60%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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Multiple Shock Fronts in RBS 797: The Chandra Window on Shock Heating in Galaxy Clusters

Ubertosi

Gitti

Brighenti

et al. 2023

ApJ

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“…The latest gain and charge transfer inefficiency corrections were applied, with improved background screening for the VFAINT telemetry mode. Modeling of the global ICM properties was done as in Calzadilla et al (2022), and the thermodynamic profiles are shown and discussed in Section 3.1.…”

Section: X-ray (Chandra)mentioning

confidence: 99%

SPT-CL J2215−3537: A Massive Starburst at the Center of the Most Distant Relaxed Galaxy Cluster

Calzadilla

Bleem

McDonald

et al. 2023

ApJ

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We present the discovery of the most distant, dynamically relaxed cool core cluster, SPT-CL J2215−3537 (SPT2215), and its central brightest cluster galaxy (BCG) at z = 1.16. Using new X-ray observations, we demonstrate that SPT2215 harbors a strong cool core with a central cooling time of 200 Myr (at 10 kpc) and a maximal intracluster medium cooling rate of 1900 ± 400 M ⊙ yr−1. This prodigious cooling may be responsible for fueling the extended, star-forming filaments observed in Hubble Space Telescope imaging. Based on new spectrophotometric data, we detect bright [O ii] emission in the BCG, implying an unobscured star formation rate (SFR) of 320 − 140 + 230 M ⊙ yr−1. The detection of a weak radio source (2.0 ± 0.8 mJy at 0.8 GHz) suggests ongoing feedback from an active galactic nucleus (AGN), though the implied jet power is less than half the cooling luminosity of the hot gas, consistent with cooling overpowering heating. The extreme cooling and SFR of SPT2215 are rare among known cool core clusters, and it is even more remarkable that we observe these at such high redshift, when most clusters are still dynamically disturbed. The high mass of this cluster, coupled with the fact that it is dynamically relaxed with a highly isolated BCG, suggests that it is an exceptionally rare system that must have formed very rapidly in the early universe. Combined with the high SFR, SPT2215 may be a high-z analog of the Phoenix cluster, potentially providing insight into the limits of AGN feedback and star formation in the most massive galaxies.

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Waking the monster: The onset of AGN feedback in galaxy clusters hosting young central radio galaxies

Ubertosi

Gitti

Brighenti

et al. 2023

A&A

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Aims. The investigation of the feedback cycle in galaxy clusters has historically been performed for systems where feedback is ongoing (“mature-feedback” clusters), that is where the central radio galaxy has inflated radio lobes, pushing aside the intracluster medium (ICM). In this pilot study, we present results from “pre-feedback” clusters, where the central newly active radio galaxies (age < 103 yr) may not yet have had time to alter the thermodynamic state of the ICM. Methods. We analyze Chandra and MUSE observations of two such systems, evaluating the hot gas entropy and cooling time profiles, and characterizing the morphology and kinematics of the warm gas. Results. Based on our exploratory study of these two sources, we find that the hot gas meets the expectations for an as of yet unheated ICM. Specifically, the entropy and cooling time of pre-feedback clusters within 20 kpc from the center fall below those of mature-feedback clusters by a factor ∼2. We speculate that with an estimated mechanical power of ∼1044 − 1045 erg s−1, the two young radio galaxies may restore the entropy levels in a few tens of millions of years, which are typical values of power outbursts and lifetimes for radio galaxies in clusters. Conversely, the properties of the gas at ∼104 K seem to remain invariant between the two feedback stages, possibly suggesting that the warm gas reservoir accumulates over long periods (107 − 108 yr) during the growth of the radio galaxy. We conclude that the exploratory results obtained from our analysis of two cluster-central young radio galaxies are crucial in the context of understanding the onset of active galactic nuclei feedback, and they provide enough motivation for further investigation of similar cases.

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Testing the Limits of AGN Feedback and the Onset of Thermal Instability in the Most Rapidly Star-forming Brightest Cluster Galaxies

Cited by 14 publications

References 144 publications

Multiple Shock Fronts in RBS 797: The Chandra Window on Shock Heating in Galaxy Clusters

Multiple Shock Fronts in RBS 797: The Chandra Window on Shock Heating in Galaxy Clusters

SPT-CL J2215−3537: A Massive Starburst at the Center of the Most Distant Relaxed Galaxy Cluster

Waking the monster: The onset of AGN feedback in galaxy clusters hosting young central radio galaxies

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