The Hot and Energetic Universe: AGN feedback in galaxy clusters and groups

Croston, J. H.; Sanders, J. S.; Heinz, S.; Hardcastle, Martin; Zhuravleva, I.; Bîrzan, L.; G.,, Bower, R.; Brüggen, M.; Churazov, E.; Edge, A. C.; Ettori, S.; C., Fabian, A.; Finoguenov, A.; Kaastra, J.; Gaspari, M.; Gitti, M.; Nulsen, Paul; McNamara, B. R.; Pointecouteau, E.; Ponman, T. J.; Pratt, G. W.; Rafferty, D. A.; Reiprich, T. H.; Sijacki, D.; Worrall, D. M.; Kraft, R. P.; McCarthy, I.; Wise, M.

doi:10.48550/arxiv.1306.2323

Cited by 6 publications

(9 citation statements)

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“…In local systems, Athena will be also in condition to determine the occurrence and impact of AGN feedback phenomena by searching for ripples in surface brightness in the cores of a statistical sample of objects. Using temperature-sensitive line ratios, Athena's observations will trace how much gas is at each temperature in the cores of these systems, providing a complete description of the gas heating-cooling balance (Croston et al 2013) and transport processes such as turbulence and diffusion (Cucchetti et al 2018;Roncarelli et al 2018;Mernier et al 2020).…”

Section: Galaxy Groups With the Next Generation Instrumentsmentioning

confidence: 99%

Scaling Properties of Galaxy Groups

et al. 2021

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Galaxy groups and poor clusters are more common than rich clusters, and host the largest fraction of matter content in the Universe. Hence, their studies are key to understand the gravitational and thermal evolution of the bulk of the cosmic matter. Moreover, because of their shallower gravitational potential, galaxy groups are systems where non-gravitational processes (e.g., cooling, AGN feedback, star formation) are expected to have a higher impact on the distribution of baryons, and on the general physical properties, than in more massive objects, inducing systematic departures from the expected scaling relations. Despite their paramount importance from the astrophysical and cosmological point of view, the challenges in their detection have limited the studies of galaxy groups. Upcoming large surveys will change this picture, reassigning to galaxy groups their central role in studying the structure formation and evolution in the Universe, and in measuring the cosmic baryonic content. Here, we review the recent literature on various scaling relations between X-ray and optical properties of these systems, focusing on the observational measurements, and the progress in our understanding of the deviations from the self-similar expectations on groups’ scales. We discuss some of the sources of these deviations, and how feedback from supernovae and/or AGNs impacts the general properties and the reconstructed scaling laws. Finally, we discuss future prospects in the study of galaxy groups.

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Section: Galaxy Groups With the Next Generation Instrumentsmentioning

confidence: 99%

Scaling Properties of Galaxy Groups

et al. 2021

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“…One of the primary goals of Athena X-IFU is probing the (astro)physics of the diffuse plasma which fills the potential wells of galaxy clusters (Ettori et al 2013;Croston et al 2013;Pointecouteau et al 2013), also known as the intracluster medium (ICM). The ICM, which formed during the cosmological gravitational collapse in the growing dark matter halo (e.g., Planelles et al 2017), accounts for most of the baryonic mass of a massive galaxy cluster (∼ 12 − 15 % of the total mass of ∼ 10 15 M ), with typical electron temperatures and densities in the core of T e ∼ 5 − 10 keV and n e ∼ 10 −2 − 10 −3 cm −3 , respectively.…”

Section: Introductionmentioning

confidence: 99%

Measuring turbulence and gas motions in galaxy clusters via syntheticAthenaX-IFU observations

Roncarelli

Gaspari

Ettori

et al. 2018

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Context. The X-ray Integral Field Unit (X-IFU) that will be on board the Athena telescope will provide an unprecedented view of the intracluster medium (ICM) kinematics through the observation of gas velocity, v, and velocity dispersion, w, via centroid-shift and broadening of emission lines, respectively. Aims. The improvement of data quality and quantity requires an assessment of the systematics associated with this new data analysis, namely biases, statistical and systematic errors, and possible correlations between the different measured quantities. Methods. We have developed an end-to-end X-IFU simulator that mimics a full X-ray spectral fitting analysis on a set of mock event lists, obtained using sixte. We have applied it to three hydrodynamical simulations of a Coma-like cluster that include the injection of turbulence. This allowed us to assess the ability of X-IFU to map five physical quantities in the cluster core: emission measure, temperature, metal abundance, velocity, and velocity dispersion. Finally, starting from our measurements maps, we computed the 2D structure function (SF) of emission measure fluctuations, v and w, and compared them with those derived directly from the simulations. Results. All quantities match with the input projected values without bias; the systematic errors were below 5%, except for velocity dispersion whose error reaches about 15%. Moreover, all measurements prove to be statistically independent, indicating the robustness of the fitting method. Most importantly, we recover the slope of the SFs in the inertial regime with excellent accuracy, but we observe a systematic excess in the normalization of both SF v and SF w ascribed to the simplistic assumption of uniform and (bi-)Gaussian measurement errors. Conclusions. Our work highlights the excellent capabilities of Athena X-IFU in probing the thermodynamic and kinematic properties of the ICM. This will allow us to access the physics of its turbulent motions with unprecedented precision.

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“…-Athena 17 (Nandra et al 2013) is ESA's second Large Mission after the planetary mission Juice, and before the gravitational wave mission LISA. Details of cluster science expectations are provided in Pointecouteau et al (2013); Ettori et al (2013b); Croston et al (2013). The expected launch is in the early 2030s.…”

Section: Xrism and Athenamentioning

confidence: 99%

The Galaxy Cluster Mass Scale and Its Impact on Cosmological Constraints from the Cluster Population

et al. 2019

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The total mass of a galaxy cluster is one of its most fundamental properties. Together with the redshift, the mass links observation and theory, allowing us to use the cluster population to test models of structure formation and to constrain cosmological parameters. Building on the rich heritage from X-ray surveys, new results from Sunyaev-Zeldovich and optical surveys have stimulated a resurgence of interest in cluster cosmology. These studies have generally found fewer clusters than predicted by the baseline Planck ΛCDM model, prompting a renewed effort on the part of the commu-nity to obtain a definitive measure of the true cluster mass scale. Here we review recent progress on this front. Our theoretical understanding continues to advance, with numerical simulations being the cornerstone of this effort. On the observational side, new, sophisticated techniques are being deployed in individual mass measurements and to account for selection biases in cluster surveys. We summarise the state of the art in cluster mass estimation methods and the systematic uncertainties and biases inherent in each approach, which are now well identified and understood, and explore how current uncertainties propagate into the cosmological parameter analysis. We discuss the prospects for improvements to the measurement of the mass scale using upcoming multiwavelength data, and the future use of the cluster population as a cosmological probe.

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The Hot and Energetic Universe: AGN feedback in galaxy clusters and groups

Cited by 6 publications

References 0 publications

Scaling Properties of Galaxy Groups

Scaling Properties of Galaxy Groups

Measuring turbulence and gas motions in galaxy clusters via syntheticAthenaX-IFU observations

The Galaxy Cluster Mass Scale and Its Impact on Cosmological Constraints from the Cluster Population

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