Toward the low-scatter selection of X-ray clusters

Käfer, Florian; Finoguenov, A.; Eckert, D.; Clerc, N.; Ramos-Ceja, M. E.; Sanders, J. S.; Ghirardini, Vittorio

doi:10.1051/0004-6361/201936131

Cited by 18 publications

(15 citation statements)

References 48 publications

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“…More massive groups with luminosities ∼10 42 erg s −1 should be detectable to z ∼ 0.1 in the final eRASS:8 survey. Käfer et al [343] performed detailed simulations to evaluate the sensitivity of eRASS:8 to galaxy groups. The authors used a wavelet decomposition algorithm sensitive to large-scale diffuse emission.…”

Section: Impact On Cosmological Probesmentioning

confidence: 99%

“…Expected sensitivity curve of the final eROSITA survey (eRASS:8) compared to the sensitivity of existing and upcoming X-ray and SZ surveys. The eROSITA sensitivity curve was computed from synthetic data using a wavelet decomposition algorithm[343] sensitive to scales of 1-4 (solid blue curve) and 1-16 (dashed blue curve). For comparison, the dashed black curve shows the sensitivity of the ROSAT all-sky survey assuming a fixed soft X-ray flux threshold of 1.8 × 10 −12 erg s −1 , which is the typical sensitivity of the REFLEX and NORAS samples (green asterisks,[345]).…”

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confidence: 99%

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Feedback from Active Galactic Nuclei in Galaxy Groups

et al. 2021

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The co-evolution between supermassive black holes and their environment is most directly traced by the hot atmospheres of dark matter halos. The cooling of the hot atmosphere supplies the central regions with fresh gas, igniting active galactic nuclei (AGN) with long duty cycles. Outflows from the central engine tightly couple with the surrounding gaseous medium and provide the dominant heating source preventing runaway cooling by carving cavities and driving shocks across the medium. The AGN feedback loop is a key feature of all modern galaxy evolution models. Here, we review our knowledge of the AGN feedback process in the specific context of galaxy groups. Galaxy groups are uniquely suited to constrain the mechanisms governing the cooling–heating balance. Unlike in more massive halos, the energy that is supplied by the central AGN to the hot intragroup medium can exceed the gravitational binding energy of halo gas particles. We report on the state-of-the-art in observations of the feedback phenomenon and in theoretical models of the heating-cooling balance in galaxy groups. We also describe how our knowledge of the AGN feedback process impacts galaxy evolution models and large-scale baryon distributions. Finally, we discuss how new instrumentation will answer key open questions on the topic.

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Section: Impact On Cosmological Probesmentioning

confidence: 99%

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confidence: 99%

Feedback from Active Galactic Nuclei in Galaxy Groups

et al. 2021

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“…The multiplicity functions of the two samples cross each other at 10 14.5 M h −1 , then the unrelaxed structures take over at the high-mass end. This approach offers a possible connection to selection effects in observations, such as the cool core bias in X-rays (Eckert et al 2011;Käfer et al 2019Käfer et al , 2020. It possibly offers a solution to mitigate biases in a cosmological interpretation of clusters abundance.…”

Section: Introductionmentioning

confidence: 99%

The mass function dependence on the dynamical state of dark matter haloes

Seppi

Comparat

Nandra

et al. 2021

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Context. Galaxy clusters are luminous tracers of the most massive dark matter haloes in the Universe. To use them as a cosmological probe, a detailed description of the properties of dark matter haloes is required. Aims. We characterize how the dynamical state of haloes impacts the dark matter halo mass function at the high-mass end (i.e., for haloes hosting clusters of galaxies). Methods. We used the dark matter-only MultiDark suite of simulations and the high-mass objects M > 2.7 × 1013 M⊙ h−1 therein. We measured the mean relations of concentration, offset, and spin as a function of dark matter halo mass and redshift. We investigated the distributions around the mean relations. We measured the dark matter halo mass function as a function of offset, spin, and redshift. We formulated a generalized mass function framework that accounts for the dynamical state of the dark matter haloes. Results. We confirm the recent discovery of the concentration upturn at high masses and provide a model that predicts the concentration for different values of mass and redshift with one single equation. We model the distributions around the mean values of concentration, offset, and spin with modified Schechter functions. We find that the concentration of low-mass haloes shows a faster redshift evolution compared to high-mass haloes, especially in the high-concentration regime. We find that the offset parameter is systematically smaller at low redshift, in agreement with the relaxation of structures at recent times. The peak of its distribution shifts by a factor of ∼1.5 from z = 1.4 to z = 0. The individual models are combined into a comprehensive mass function model, which predicts the mass function as a function of spin and offset. Our model recovers the fiducial mass function with ∼3% accuracy at redshift 0 and accounts for redshift evolution up to z ∼ 1.5. Results. This new approach accounts for the dynamical state of the halo when measuring the halo mass function. It offers a connection with dynamical selection effects in galaxy cluster observations. This is key toward precision cosmology using cluster counts as a probe.

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“…As a consequence, only the deepest existing X-ray survey, that is, the Chandra Deep Field-South (CDF-S) 7 Ms survey (Luo et al 2017), reaches 0.5-2 keV fluxes where the number of nonactive galaxies becomes non-negligible (i.e., f 0.5−2 10 −17 erg s −1 cm −2 ): in all the other X-ray surveys, AGNs make up almost the totality of the detected sources. Characterizing the properties of the diffuse medium in clusters of galaxies, which are the largest virialized structures in the Universe, also requires deep X-ray surveys over large areas of the sky (see, e.g., Finoguenov et al 2015;Käfer et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Mock catalogs for the extragalactic X-ray sky: Simulating AGN surveys with ATHENA and with the AXIS probe

Marchesi

Gilli

Lanzuisi

et al. 2020

A&A

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We present a series of new, publicly available mock catalogs of X-ray selected active galactic nuclei (AGNs), nonactive galaxies, and clusters of galaxies. These mocks are based on up-to-date observational results on the demographic of extragalactic X-ray sources and their extrapolations. They reach fluxes below 10−20 erg cm−2 s−1 in the 0.5–2 keV band, that is, more than an order of magnitude below the predicted limits of future deep fields, and they therefore represent an important tool for simulating extragalactic X-ray surveys with both current and future telescopes. We used our mocks to perform a set of end-to-end simulations of X-ray surveys with the forthcoming ATHENA mission and with the AXIS probe, a subarcsecond resolution X-ray mission concept proposed to the Astro 2020 Decadal Survey. We find that these proposed, next generation surveys may transform our knowledge of the deep X-ray Universe. As an example, in a total observing time of 15 Ms, AXIS would detect ∼225 000 AGNs and ∼50 000 nonactive galaxies, reaching a flux limit of f0.5−2 ∼ 5 × 10−19 erg cm−2 s−1 in the 0.5–2 keV band, with an improvement of over an order of magnitude with respect to surveys with current X-ray facilities. Consequently, 90% of these sources would be detected for the first time in the X-rays. Furthermore, we show that deep and wide X-ray surveys with instruments such as AXIS and ATHENA are expected to detect ∼20 000 z > 3 AGNs and ∼250 sources at redshift z > 6, thus opening a new window of knowledge on the evolution of AGNs over cosmic time and putting strong constraints on the predictions of theoretical models of black hole seed accretion in the early universe.

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Toward the low-scatter selection of X-ray clusters

Cited by 18 publications

References 48 publications

Feedback from Active Galactic Nuclei in Galaxy Groups

Feedback from Active Galactic Nuclei in Galaxy Groups

The mass function dependence on the dynamical state of dark matter haloes

Mock catalogs for the extragalactic X-ray sky: Simulating AGN surveys with ATHENA and with the AXIS probe

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