Abstract
The majority of the ordinary matter in the local Universe has been heated by strong structure formation shocks and resides in a largely unexplored hot, diffuse, X-ray emitting plasma that permeates the halos of galaxies, galaxy groups and clusters, and the cosmic web. We propose a next-generation “Cosmic Web Explorer” that will permit a complete and exhaustive understanding of these unseen baryons. This will be the first mission capable to reach the accretion shocks located several times farther than the virial radii of galaxy clusters, and reveal the out-of-equilibrium parts of the intra-cluster medium which are live witnesses to the physics of cosmic accretion. It will also enable a view of the thermodynamics, kinematics, and chemical composition of the circumgalactic medium in galaxies with masses similar to the Milky Way, at the same level of detail that Athena will unravel for the virialized regions of massive galaxy clusters, delivering a transformative understanding of the evolution of those galaxies in which most of the stars and metals in the Universe were formed. Finally, the proposed X-ray satellite will connect the dots of the large-scale structure by mapping, at high spectral resolution, as much as 100% of the diffuse gas hotter than 106 K that fills the filaments of the cosmic web at low redshifts, down to an over-density of 1, both in emission and in absorption against the ubiquitous cosmic X-ray background, surveying at least 1600 square degrees over 5 years in orbit. This requires a large effective area (\(\sim \)10 m2 at 1 keV) over a large field of view (\(\sim 1\) deg2), a megapixel cryogenic microcalorimeter array providing integral field spectroscopy with a resolving power E/ΔE = 2000 at 0.6 keV and a spatial resolution of 5\(^{\prime \prime }\) in the soft X-ray band, and a low and stable instrumental background ensuring high sensitivity to faint, extended emission.
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Notes
the radius within which the mean enclosed density is 200 times the critical density at the redshift of the cluster.
Observations of 1 Ms can probe OVIII emission down to a limiting flux of 6 × 10− 12 photons/s/cm2/arcmin2.
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Acknowledgements
We thank F. Nicastro, J.S. Kaastra, G. M. Voit, M. Donahue, J. Green, W. Cui, N. Hatch, D. Fielding, J. Sayers, J. P. Breuer, L. di Mascolo, F. Mernier and J. Croston, in no particular order, for fruitful discussions and support towards preparing this manuscript. A.S. gratefully acknowledges support by the Women In Science Excel (WISE) programme of the Netherlands Organisation for Scientific Research (NWO). S.E., M.R. and F.G. acknowledge financial contribution from the contracts ASI-INAF Athena 2015-046-R.0, ASI-INAF Athena 2019-27-HH.0, “Attività di Studio per la comunità scientifica di Astrofisica delle Alte Energie e Fisica Astroparticellare” (Accordo Attuativo ASI-INAF n. 2017-14-H.0), and from INAF “Call per interventi aggiuntivi a sostegno della ricerca di main stream di INAF”. D.N. acknowledges Yale University for granting a triennial leave and the Max-Planck-Institut für Astrophysik for hospitality. GWP acknowledges support from the French space agency, CNES. B.M. acknowledges support from the UK STFC under grants ST/R00109X/1, ST/R000794/1, and ST/T000295/1. F.V. acknowledges financial support from the ERC Starting Grant “MAGCOW”, no. 714196, the usage of Piz Daint supercomputer at CSCS-ETHZ (Lugano, Switzerland) under project s805, and the usage of online storage tools kindly provided by the INAF Astronomical Archive (IA2) initiative (http://www.ia2.inaf.it). VB acknowledges support by the Deutsche Forschungsgemeinschaft (DFG) project nr. 415510302.
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Simionescu, A., Ettori, S., Werner, N. et al. Voyage through the hidden physics of the cosmic web. Exp Astron 51, 1043–1079 (2021). https://doi.org/10.1007/s10686-021-09720-0
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DOI: https://doi.org/10.1007/s10686-021-09720-0