Deeply cooled core of the Phoenix galaxy cluster imaged by ALMA with the Sunyaev–Zel’dovich effect

Kitayama, Tetsu; Ueda, Shutaro; Akahori, Takuya; Komatsu, Eiichiro; Kawabe, Ryohei; Kohno, Kotaro; Takakuwa, Shigehisa; Takizawa, Motokazu; Tsutsumi, Takahiro; Yoshikawa, Kohji

doi:10.1093/pasj/psaa009

Cited by 13 publications

(5 citation statements)

References 40 publications

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“…We note that several other systems also exhibit a hint of flattening in their VSF, especially for the outer filaments. These include 2A 0335 + 096, Centaurus, RXJ 1539.5, and Abell S1101, as well as the outer filaments in Abell 2,597 which is noted in Li Y. et al (2020). Abell 1795 happens to be a nearby system with one of the most spatially extended Hα filaments observed, and therefore, it shows the most convincing flattening in its outer VSF.…”

Section: Kolmogorov Slopes On Small Scalesmentioning

confidence: 75%

“…The VSF for the outer filaments is much shallower, but is still slightly steeper than Kolmogorov. At ℓ < 1 kpc, the slope becomes very close to Kolmogorov. The steep slopes of the VSFs found in Li Y. et al (2020) have been a puzzle. Two of the systems have slopes even steeper than supersonic turbulence.…”

Section: Kolmogorov Slopes On Small Scalesmentioning

confidence: 84%

“…Numerical simulations in Li M. et al (2020) show that SNIa can drive turbulence with velocities of ∼10 − 20 km s −1 at ∼0.1 kpc scale in typical massive elliptical galaxy environments. This is smaller than the scales we can probe in our sample except for Centaurus, and may in fact have contributed to the flattening of the Centaurus VSF on small scales.…”

Section: Sources Of Turbulence In Cluster Centersmentioning

confidence: 99%

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The nature of the motions of multiphase filaments in the centers of galaxy clusters

Ganguly

Olivares

et al. 2023

Front. Astron. Space Sci.

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The intracluster medium (ICM) in the centers of galaxy clusters is heavily influenced by the “feedback” from supermassive black holes (SMBHs). Feedback can drive turbulence in the ICM and turbulent dissipation can potentially be an important source of heating. Due to the limited spatial and spectral resolutions of X-ray telescopes, direct observations of turbulence in the hot ICM have been challenging. Recently, we developed a new method to measure turbulence in the ICM using multiphase filaments as tracers. These filaments are ubiquitous in cluster centers and can be observed at very high resolution using optical and radio telescopes. We study the kinematics of the filaments by measuring their velocity structure functions (VSFs) over a wide range of scales in the centers of ∼10 galaxy clusters. We find features of the VSFs that correlate with the SMBHs activities, suggesting that SMBHs are the main driver of gas motions in the centers of galaxy clusters. In all systems, the VSF is steeper than the classical Kolmogorov expectation and the slopes vary from system to system. One theoretical explanation is that the VSFs we have measured so far mostly reflect the motion of the driver (jets and bubbles) rather than the cascade of turbulence. We show that in Abell 1795, the VSF of the outer filaments far from the SMBH flattens on small scales to a Kolmogorov slope, suggesting that the cascade is only detectable farther out with the current telescope resolution. The level of turbulent heating computed at small scales is typically an order of magnitude lower than that estimated at the driving scale. Even though SMBH feedback heavily influences the kinematics of the ICM in cluster centers, the level of turbulence it drives is rather low, and turbulent heating can only offset ≲ 10% of the cooling loss, consistent with the findings of numerical simulations.

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Section: Kolmogorov Slopes On Small Scalesmentioning

confidence: 75%

Section: Kolmogorov Slopes On Small Scalesmentioning

confidence: 84%

Section: Sources Of Turbulence In Cluster Centersmentioning

confidence: 99%

See 1 more Smart Citation

The nature of the motions of multiphase filaments in the centers of galaxy clusters

Ganguly

Olivares

et al. 2023

Front. Astron. Space Sci.

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“…Cross-contamination may in fact cause both an underestimation of the flux of the former when using CLEAN-like algorithms 81 , and—at the same time—introduce a notable suppression of the underlying SZ footprint. Also, common approaches exploiting scale separation between the signature from the radio sources and the ICM in galaxy clusters 82 , 83 would not be able to provide a robust characterization of the two signals, as their characteristic scales exhibit a broad overlap in the case of the Spiderweb protocluster.…”

Section: Methodsmentioning

confidence: 99%

Forming intracluster gas in a galaxy protocluster at a redshift of 2.16

Mascolo

Saro

Mroczkowski

et al. 2023

Nature

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Galaxy clusters are the most massive gravitationally bound structures in the Universe, comprising thousands of galaxies and pervaded by a diffuse, hot intracluster medium (ICM) that dominates the baryonic content of these systems. The formation and evolution of the ICM across cosmic time1 is thought to be driven by the continuous accretion of matter from the large-scale filamentary surroundings and energetic merger events with other clusters or groups. Until now, however, direct observations of the intracluster gas have been limited only to mature clusters in the later three-quarters of the history of the Universe, and we have been lacking a direct view of the hot, thermalized cluster atmosphere at the epoch when the first massive clusters formed. Here we report the detection (about 6σ) of the thermal Sunyaev–Zeldovich (SZ) effect2 in the direction of a protocluster. In fact, the SZ signal reveals the ICM thermal energy in a way that is insensitive to cosmological dimming, making it ideal for tracing the thermal history of cosmic structures3. This result indicates the presence of a nascent ICM within the Spiderweb protocluster at redshift z = 2.156, around 10 billion years ago. The amplitude and morphology of the detected signal show that the SZ effect from the protocluster is lower than expected from dynamical considerations and comparable with that of lower-redshift group-scale systems, consistent with expectations for a dynamically active progenitor of a local galaxy cluster.

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“…It has been studied that thermodynamic perturbations in the ICM are a good proxy for examining gas motions, including turbulence (e.g., Gaspari et al 2014;Churazov et al 2016;Hofmann et al 2016;Ueda et al 2018;Zhuravleva et al 2018;Kitayama et al 2020;Ueda et al 2021;Zhuravleva et al 2023). Gaspari et al (2014) presented that entropy perturbations in the ICM can be used to infer one-dimensional Mach numbers of turbulence ( 1D ), assuming that pressure perturbations in the ICM are negligible.…”

Section: Analysis Of Thermodynamic Perturbationsmentioning

confidence: 99%

The Relation between the Cool-core Radius and the Host Galaxy Clusters: Thermodynamic Properties and Cluster Mass

Ng,

Ueda

2024

ApJ

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We present a detailed study of cool-core systems in a sample of four galaxy clusters (RXCJ1504.1-0248, A3112, A4059, and A478) using archival X-ray data from the Chandra X-ray Observatory. Cool cores are frequently observed at the centers of galaxy clusters and are considered to be formed by radiative cooling of the intracluster medium (ICM). Cool cores are characterized by a significant drop in the ICM temperature toward the cluster center. We extract and analyze X-ray spectra of the ICM to measure the radial profiles of the ICM thermodynamic properties, including temperature, density, pressure, entropy, and radiative cooling time. We define the cool-core radius as the turnover radius in the ICM temperature profile and investigate the relation between the cool-core radius and the properties of the host galaxy clusters. In our sample, we observe that the radiative cooling time of the ICM at the cool-core radius exceeds 10 Gyr, with RXCJ1504.1-0248 exhibiting a radiative cooling time of 32 − 11 + 5 Gyr at its cool-core radius. These results indicate that not only radiative cooling but also additional mechanisms, such as gas sloshing, may play an important role in determining the size of cool cores. Additionally, we might find that the best-fit relation between the cool-core radius and the cluster mass (M 500) is consistent with a linear relation. Our findings may suggest that cool cores are linked to the evolution of their host galaxy clusters.

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Deeply cooled core of the Phoenix galaxy cluster imaged by ALMA with the Sunyaev–Zel’dovich effect

Cited by 13 publications

References 40 publications

The nature of the motions of multiphase filaments in the centers of galaxy clusters

The nature of the motions of multiphase filaments in the centers of galaxy clusters

Forming intracluster gas in a galaxy protocluster at a redshift of 2.16

The Relation between the Cool-core Radius and the Host Galaxy Clusters: Thermodynamic Properties and Cluster Mass

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