Voyage through the Hidden Physics of the Cosmic Web

Simionescu, A.; Ettori, S.; Werner, N.; Nagai, D.; Vazza, F.; Akamatsu, H.; Pinto, C.; de Plaa, J.; Wijers, N.; Nelson, D.; Pointecouteau, E.; Pratt, G. W.; Spiga, D.; Vacanti, G.; Lau, E.; Rossetti, M.; Gastaldello, F.; Biffi, V.; Bulbul, E.; Collon, M. J.; Herder, J. W. den; Eckert, D.; Fraternali, F.; Mingo, B.; Pareschi, G.; Pezzulli, G.; Reiprich, T. H.; Schaye, J.; Walker, S. A.; Werk, J.

doi:10.48550/arxiv.1908.01778

Cited by 7 publications

(7 citation statements)

References 89 publications

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“…For the most distant future, the youngest members of our community have already engaged in the voyage2050 exercise for the long term science planning of ESA to prepare the follow-up mission to Athena, e.g. Simionescu et al (2019b) and Uttley et al (2019).…”

Section: Discussionmentioning

confidence: 99%

The Athena space X‐ray observatory and the astrophysics of hot plasma^†

et al. 2020

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The properties (temperature, density, chemical composition, velocity) of hot astrophysical plasma and the physical processes affecting them (heating/cooling, turbulence, shocks, acceleration) can be probed by high‐resolution X‐ray spectroscopy, to be complemented by high‐spatial‐resolution imaging. The paper presents the status of the European Space Agency's Advanced Telescope for High Energy Astrophysics (Athena) mission, particularly focusing on the science performance of its two focal‐plane instruments for studies of extended X‐ray sources: the wide‐field imager and the X‐ray integral field unit. This paper then provides a brief summary of the breakthroughs expected with Athena on the astrophysics of hot plasma, building on the vast heritage of the discoveries and revolutionary results obtained by Chandra and XMM‐Newton in this field. As of November 12, 2019, Athena successfully concluded its feasibility study, and has since then moved into the definition phase, with a launch date scheduled in the early 2030s.

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Section: Discussionmentioning

confidence: 99%

The Athena space X‐ray observatory and the astrophysics of hot plasma^†

et al. 2020

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“…In the near future, XRISM/Resolve (Tashiro et al 2018) and Athena/X-IFU (Barret et al 2016) will measure the turbulence in the ICM for many nearby clusters and within the cores of more distant clusters, providing an opportunity to check the f nth (r) model, correct for the HSE mass bias, and properly calibrate the mass scale (Ota et al 2018). Furthermore, the Lynx X-ray Surveyor (Gaskin et al 2019) and Cosmic Web Explorer (Simionescu et al 2019a) have been proposed as future-generation X-ray telescopes that would enable exquisite measurements of turbulence out to the halo outskirts of an unprecedentedly large sample down to the galaxy mass scale.…”

Section: Conclusion and Future Outlookmentioning

confidence: 99%

Scatter in Sunyaev--Zel'dovich effect scaling relations explained by inter-cluster variance in mass accretion histories

Green,

Aung,

Nagai

et al. 2020

Preprint

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The X-ray and microwave observable-mass scaling relations of galaxy clusters are immensely valuable tools for cosmological analysis, but their power is currently limited by astrophysical systematic uncertainties that bias cluster mass estimates and introduce additional scatter. Turbulent energy injected into the intracluster medium via mass assembly contributes substantially to the cluster's non-thermal pressure support, which is a significant source of such uncertainties. We use a simple analytical model to compute the mass assembly-driven non-thermal pressure profiles of individual haloes based on Monte Carlo-generated halo assembly histories from extended Press-Schechter theory. After combining this with the Komatsu-Seljak model for the total pressure to obtain thermal pressure profiles, we predict deviations from selfsimilarity and the intrinsic scatter in the Sunyaev-Zel'dovich effect observable-mass scaling relation (Y SZ − M) due solely to inter-cluster variations in halo mass assembly histories. We study the dependence of the slope, normalization, and scatter of Y SZ − M on aperture radius, cosmology, redshift, and halo mass limit. The model predicts 5 − 9% scatter in Y SZ − M at z = 0, increasing as the aperture used to compute Y SZ increases from r 500c to 5r 500c . The predicted scatter lies slightly below that of studies based on non-radiative hydrodynamical simulations, illustrating that assembly history variance alone is likely to be responsible for a substantial fraction of the scatter in Y SZ − M. As redshift increases, Y SZ − M deviates more from self-similarity and scatter increases. Lastly, we show that the residuals of Y SZ − M correlate strongly with the recent halo mass accretion rate, potentially providing an opportunity to infer the latter.

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“…On the other hand, imaging the hot diffuse gas in the cosmic web seems to remain a challenge also in the future (e.g. Nevalainen et al 2015;Eckert et al 2015;Connor et al 2019;Simionescu et al 2019). In summary, while on one hand complexity is likely an unobservable property of cosmic structures, it is useful to theoretically characterize the dynamics of regions which existing and future observation can efficiently target and detect in the radio domain.…”

Section: Practical Applicationsmentioning

confidence: 99%

How complex is the cosmic web?

Vazza

2019

Monthly Notices of the Royal Astronomical Society

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The growth of large-scale cosmic structure is a beautiful exemplification of how complexity can emerge in our Universe, starting from simple initial conditions and simple physical laws. Using ENZO cosmological numerical simulations, I applied tools from Information Theory (namely, "statistical complexity") to quantify the amount of complexity in the simulated cosmic volume, as a function of cosmic epoch and environment. This analysis can quantify how much difficult to predict, at least in a statistical sense, is the evolution of the thermal, kinetic and magnetic energy of the dominant component of ordinary matter in the Universe (the intragalactic medium plasma). The most complex environment in the simulated cosmic web is generally found to be the periphery of large-scale structures (e.g. galaxy clusters and filaments), where the complexity is on average ∼ 10 − 10 2 times larger than in more rarefied regions, even if the latter dominate the volume-integrated complexity of the simulated Universe. If the energy evolution of gas in the cosmic web is measured on a ≈ 100 kpc/h resolution and over a ≈ 200 Myr timescale, its total complexity is the range of ∼ 10 16 − 10 17 bits, with little dependence on the assumed gas physics, cosmology or cosmic variance.

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Voyage through the Hidden Physics of the Cosmic Web

Cited by 7 publications

References 89 publications

The Athena space X‐ray observatory and the astrophysics of hot plasma^†

The Athena space X‐ray observatory and the astrophysics of hot plasma^†

Scatter in Sunyaev--Zel'dovich effect scaling relations explained by inter-cluster variance in mass accretion histories

How complex is the cosmic web?

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Voyage through the Hidden Physics of the Cosmic Web

Cited by 7 publications

References 89 publications

The Athena space X‐ray observatory and the astrophysics of hot plasma†

The Athena space X‐ray observatory and the astrophysics of hot plasma†

Scatter in Sunyaev--Zel'dovich effect scaling relations explained by inter-cluster variance in mass accretion histories

How complex is the cosmic web?

Contact Info

Product

Resources

About

The Athena space X‐ray observatory and the astrophysics of hot plasma^†

The Athena space X‐ray observatory and the astrophysics of hot plasma^†