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REVIEW 4 major objections 5 minor 16 references

Voyage through the Hidden Physics of the Cosmic Web

T0 review · 4 major / 5 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read The paper proposes a 'Cosmic Web Explorer' X-ray observatory whose combination of roughly 10 m^2 effective area, a 1 square-degree field of view, R=2000 soft-band spectroscopy, and low detector background would, if realized, detect and…

desk verdict A well-argued Voyage 2050 mission white paper with a real science case for a next-generation soft X-ray observatory; the load-bearing weak spot is the unproven foreground-modeling accuracy it acknowledges but does not demonstrate. read the letter →

arxiv 1908.01778 v2 pith:QJXXAISS submitted 2019-08-05 astro-ph.CO astro-ph.HE

A. Simionescu , S. Ettori , N. Werner , D. Nagai , F. Vazza , H. Akamatsu , C. Pinto , J. de Plaa
show 22 more authors
N. Wijers D. Nelson E. Pointecouteau G. W. Pratt D. Spiga G. Vacanti E. Lau M. Rossetti F. Gastaldello V. Biffi E. Bulbul M. J. Collon J. W. den Herder D. Eckert F. Fraternali B. Mingo G. Pareschi G. Pezzulli T. H. Reiprich J. Schaye S. A. Walker J. Werk
This is my paper · ORCID
classification astro-ph.COastro-ph.HE
keywords warm-hotintergalacticmediumcircumgalacticX-rayspectroscopycosmicwebmissingbaryonsgalaxyclusteroutskirtsaccretionshocksintegralfieldunit
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Most of the ordinary matter in the local Universe is neither stars nor cold gas but a hot, diffuse plasma that current X-ray telescopes cannot see: it is too faint, too extended, and its key spectral lines sit in a soft band where existing spectrometers have poor resolution. The paper argues that a single next-generation X-ray observatory, the 'Cosmic Web Explorer', can bring this hidden baryon population into view. Combining roughly $10\,\mathrm{m}^2$ of collecting area at 1 keV, a 1 square-degree field of view, high spectral resolution at the OVII/OVIII lines, and a very low detector background, the mission would detect and map the warm-hot intergalactic medium, the accretion shocks around galaxy clusters, and the hot circumgalactic medium of Milky Way-mass galaxies. If the mission performs as claimed, it would map essentially all diffuse gas hotter than $10^6$ K in low-redshift cosmic-web filaments and survey about 1600 square degrees over five years, answering long-standing questions about where the missing baryons are and how metals circulate through large-scale structure.

What carries the argument

The load-bearing object is a proposed instrument package whose four coupled capabilities—large collecting area ($\sim 10\,\mathrm{m}^2$ at 1 keV), wide field of view ($1\,\mathrm{deg}^2$), high spectral resolution in the soft band ($E/\Delta E=2000$ at 0.6 keV), and low, stable detector background ($\le 1.5\times10^{-4}\,\mathrm{cts/s/keV/arcmin}^2$)—together define a 'grasp' roughly 16 times larger than the Athena Wide Field Imager. This combination lets the mission do two things at once: image faint diffuse emission over wide fields at 5 arcsec resolution, and use the same detector as a non-dispersive spectrometer for absorption studies against the cosmic X-ray background and against cluster cores. The named capability carrying the argument is the X-ray integral field unit, a megapixel cryogenic microcalorimeter array, which provides spatially resolved spectra of every point in the field and makes simultaneous emission–absorption tomography possible.

What would settle it

A flight-like prototype of the megapixel microcalorimeter array that fails to reach $E/\Delta E=2000$ at 0.6 keV with a background below $1.5\times10^{-4}\,\mathrm{cts/s/keV/arcmin}^2$ would refute the mission's feasibility; so would existing deep observations of a nearby cluster's outskirts if they showed that 0.3–2 keV foregrounds vary by several percent across arcminute scales, since that would push the claimed $10^{-18}\,\mathrm{erg/s/cm^2/arcmin^2}$ sensitivity out of reach.

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Extended reading notes

Core claim

The paper's central claim is that a single X-ray observatory—the 'Cosmic Web Explorer'—can, for the first time, detect and characterize the diffuse baryons that dominate the ordinary matter budget of the local Universe: the warm-hot intergalactic medium in cosmic-web filaments, the shocked gas in galaxy-cluster outskirts beyond the virial radius, and the hot halos of Milky Way-mass galaxies. With an effective area of roughly $10\,\mathrm{m}^2$ at 1 keV, a $1\,\mathrm{deg}^2$ field of view, a megapixel cryogenic microcalorimeter providing $E/\Delta E=2000$ at 0.6 keV, 5 arcsec spatial resolution, and a detector background no higher than $1.5\times10^{-4}\,\mathrm{cts/s/keV/arcmin}^2$, the mission would reach a surface-brightness sensitivity of about $10^{-18}\,\mathrm{erg/s/cm^2/arcmin^2}$ in the 0.3–2 keV band. The paper argues this is sufficient to map essentially 100% of the diffuse gas hotter than $10^6$ K in low-redshift filaments down to overdensity $\sim 1$, both in emission and in absorption against the cosmic X-ray background, while surveying at least 1600 square degrees over five years. It further claims this would constitute a complete and exhaustive understanding of these unseen baryons and reveal the out-of-equilibrium physics of cosmic accretion.

Load-bearing premise

The central claim rests on the assumption that the instrument background can be kept at or below $1.5\times10^{-4}\,\mathrm{cts/s/keV/arcmin}^2$ while the Milky Way halo, Local Hot Bubble, and cosmic X-ray background can be modelled to sub-percent accuracy across a 1-degree field, a capability the paper asserts is paramount but does not demonstrate.

Editorial extensions

If this is right

  • A mission with these capabilities would make the first direct X-ray detections of cluster accretion shocks, revealing where and how most baryons were heated.
  • It would map OVII and OVIII line emission and kinematics in the circumgalactic medium of Milky Way-mass galaxies, distinguishing between competing galaxy-formation simulations.
  • A five-year survey of about 1600 square degrees at $10^{-18}$ erg/s/cm^2/arcmin^2 would detect essentially all diffuse gas hotter than $10^6$ K in low-redshift cosmic-web filaments, down to overdensity about 1.
  • Absorption studies against the cosmic X-ray background and cluster cores would reach column densities near $10^{19}$ cm^-2 without requiring rare bright background beacons.
  • Measuring metal abundances and abundance ratios in cluster outskirts would test whether early supermassive black hole feedback enriched the intergalactic medium uniformly.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The same survey would yield a tomographic, three-dimensional map of the local cosmic web in emission, a dataset that could be cross-correlated with future Sunyaev-Zel'dovich and galaxy surveys to separate the WHIM from unresolved AGN foregrounds.
  • The required sub-percent foreground modelling would probably force the development of open, data-driven models of the Milky Way's X-ray halo and Local Hot Bubble, methods that would benefit any faint diffuse X-ray science.
  • A scaled-down mission that gives up the 1-degree field of view might still reach the CGM science goals but would lose the filament survey; the paper's scientific case is the combination of grasp, resolution, and background, not any single parameter.
  • The proposed stacking of faint sources against the cosmic X-ray background for absorption measurements could in principle be tested with existing deep X-ray fields before the mission is built.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 5 minor

Summary. The manuscript proposes a next-generation X-ray mission concept, the "Cosmic Web Explorer," designed to map the warm-hot intergalactic medium (WHIM), cluster accretion shocks, and the circumgalactic medium (CGM) of L* galaxies. The central claim is that a mission with ~10 m² effective area at 1 keV, a 1 deg² field of view, spectral resolution E/ΔE = 2000 at 0.6 keV, 5 arcsec angular resolution, and a detector background ≤ 1.5×10^-4 cts/s/keV/arcmin² can reach a surface-brightness sensitivity of ~10^-18 erg/s/cm²/arcmin² in the 0.3–2 keV band, survey 1600 deg² in five years, and map "as much as 100%" of the diffuse gas hotter than 10^6 K in cosmic-web filaments. The paper develops the science case for cluster outskirts, CGM, galaxy groups, and the WHIM; derives mission requirements; describes two mirror concepts (segmented glass foils and silicon pore optics) and a megapixel microcalorimeter detector; and presents spectral simulations and comparisons with Athena. It also proposes absorption studies against the cosmic X-ray background and galaxy cluster cores as a complement to emission mapping.

Significance. If realized, the proposed mission would be a genuinely transformative step for X-ray astrophysics: it would open cluster outskirts, the CGM of L* galaxies, and the WHIM to direct imaging spectroscopy, complementing Athena and eROSITA. The paper's quantitative requirements table (Table 1) and its comparisons with Athena (Figures 5 and 7) are concrete and useful, and the absorption-line strategy of stacking faint point sources against the unresolved cosmic X-ray background is an original and practical idea. The sensitivity estimates are anchored in current cosmological simulations (Omega500, IllustrisTNG, EAGLE, ENZO) and are presented in a falsifiable way, e.g., the claim that a 50 ks exposure detects at least two WHIM emission lines at 5σ per 1000 arcmin². However, the central feasibility claim depends on two unproven pillars: sub-percent-level modeling and subtraction of the Milky Way foreground and cosmic X-ray background, and the realization of a megapixel cryogenic calorimeter array with very low instrumental background.

major comments (4)
  1. [§2.4, Fig. 2 caption, §2.1.2] The claim that a surface-brightness sensitivity of ~10^-18 erg/s/cm²/arcmin² will map "as much as 100%" of gas hotter than 10^6 K (Abstract, §2.4) is explicitly conditioned on "an accurate understanding of the cosmic foregrounds and backgrounds" and on modeling the Milky Way halo, local hot bubble, and unresolved AGN at "sub-percent level accuracy" (§2.1.2). No calculation is given to show that such accuracy is achievable or that foreground residuals can be kept below the source signal. For z≈0 WHIM, the target OVII and OVIII lines fall at the same wavelengths as the same ionic lines from the Galactic halo and the local hot bubble, so the separation is not purely spectral. Please add a quantitative sensitivity analysis, e.g., the maximum allowed foreground normalization error as a function of detection significance, and demonstrate with a concrete spectral-spatial decomposition or a reference to published work that the proposed survey design can deliver the required accuracy without circularity.
  2. [Table 1, §2.4] Table 1 sets the detector background requirement at ≤ 1.5×10^-4 cts/s/keV/arcmin², about four times lower than the Athena X-IFU nominal value quoted in the same table, yet the paper does not describe how this background is to be achieved (e.g., anticoincidence, passive shielding, low-Earth orbit) and does not provide a preliminary background budget or an assessment of its systematic uncertainty. The spectral simulations in Figures 2 and 4 assume this background without an error analysis. Given that the faint diffuse signals are comparable to or weaker than the instrumental background, a quantitative background model and an explicit sensitivity to background-rate and spectral-shape uncertainties are needed to support the forecasted detection significances.
  3. [§3.3] The proposed quasi-megapixel calorimeter array (~4×10^5 pixels) is a thousandfold increase in readout elements over Athena X-IFU and an order of magnitude beyond Lynx, and §3.3 acknowledges that "R&D components will need to be addressed" (microwave SQUID multiplexing, hydra multi-absorber TES, optical/thermal blocking filters). This technology is load-bearing for the entire mission concept, yet the paper does not specify which requirements are at demonstrated TRL and which are extrapolations, nor does it identify a critical-path development plan with milestones. Please add a technology readiness assessment and a statement of which capabilities must be demonstrated before the mission requirements in Table 1 can be considered feasible.
  4. [§2.4, Fig. 4] The survey depth of 50 ks per pointing and the resulting 1600 deg² coverage assume a WHIM metallicity of 0.3 Solar in collisional ionization equilibrium at kT ~ 0.2 keV. Observed WHIM metallicities are poorly constrained and non-equilibrium ionization can reduce line emissivities substantially; footnote 4 notes that deeper observations can compensate in some cases, but the headline "100% mapping" claim is tied to the baseline assumption. Please provide a scaling of the detectable gas mass fraction with metallicity and ionization state, and show the sensitivity of the Fig. 4 right panel to a metallicity of 0.1 Solar and to non-equilibrium ionization, so the reader can judge how robust the completeness claim is.
minor comments (5)
  1. [§3.3, Eq. (1)] The text states that 0.5–0.7 eV resolution at 1.5 keV has been achieved in the laboratory and that E/ΔE = 2000 at 0.6 keV is feasible, but the relation between the quoted saturation energy E_Max ~ 0.6 keV, the operating temperature T ~ 60–70 mK, and the resolving power at 0.6 keV is not explained; please clarify the derivation or add a reference that performs this scaling explicitly.
  2. [Fig. 4 caption] The left panel is described as a "comoving 85 Mpc^3 volume"; please specify whether this is an 85 Mpc box, an 85 h^-1 Mpc box, or a cubic volume of 85 Mpc^3, since the simulation resolution and the interpretation of the phase diagram depend on this.
  3. [Table 1, §3.3] The paper alternately calls the detector a "megapixel" array and a "quasi-mega-pixel" array; Table 1 and §3.3 derive ~4×10^5 pixels for a 1 deg² FoV with 5 arcsec pixels, so please use a consistent descriptor and state the exact pixel count and format used in the sensitivity estimates.
  4. [§2.1.2] The statement that the proposed mission has 16 times the grasp of the Athena WFI would be clearer if the grasp comparison were defined as effective area times field of view at a reference energy, since the WFI and the proposed instrument have different spectral responses.
  5. [§2.4, Fig. 6] The absorption simulations assume specific column densities and velocity offsets for the WHIM filaments; please state whether these values are derived from the same cosmological simulations used elsewhere in the paper or chosen as representative, and how the detection significance would change for a range of line-of-sight column densities.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the mission capability forecasts are forward-model calculations against cosmological simulations and assumed foregrounds, with no fitted parameter renamed as a prediction.

full rationale

The paper's derivation chain is a mission-feasibility forecast, not a parameter fit: it selects instrumental parameters (effective area, field of view, spectral resolution, background) and computes whether assumed diffuse sources would be detectable in synthetic spectra. The detection claims in Figure 2 start from an input source surface brightness of 10^-18 erg/s/cm^2/arcmin^2 and add the Galactic halo, local hot bubble, cosmic X-ray background, and instrumental background components; the residual line detections are forward calculations, not inversions of the target quantities. The '100% of gas hotter than 10^6 K' statement in Section 2.4 is obtained by post-processing a hydrodynamical simulation (Figure 4), i.e., by cutting simulated gas distributions at the proposed sensitivity, which again is a forward model rather than an equivalence-by-construction. Several simulations (Omega500, ENZO, IllustrisTNG, EAGLE) are co-authored by paper authors, but they are independent physical models used as external benchmarks; none of them is constructed from the mission's sensitivity target, and no uniqueness theorem or self-citation is invoked to forbid alternatives. The admitted foreground-modeling challenge in Section 2.4 ('the expected signal is much weaker than the cosmic foregrounds and backgrounds') is a real scientific risk and is weighed as such, but an unproven assumption is not circularity. No equation, fitted parameter, or self-referential step can be quoted that reduces a prediction to its input, so the circularity score is 0.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central feasibility claims rest on assumed instrument performance and foreground models; no new physical entities are introduced.

free parameters (3)
  • Instrumental background requirement = ≤ 1.5e-4 cts/s/keV/arcmin^2
    Chosen as a mission requirement (Table 1) to reach the surface brightness sensitivity; not yet demonstrated and critical to the detection claims.
  • WHIM metallicity assumption = 0.3 Solar
    Used in spectral simulations (Figures 2 and 6) to estimate line detection significances; WHIM metallicity is largely unconstrained.
  • Survey area and exposure = 1600 deg^2 at 50 ks over 5 years
    Assumed observing efficiency in LEO and mission duration; drives the survey completeness claims.
assumptions (5)
  • domain assumption The warm-hot intergalactic medium exists and contains a significant fraction of the missing baryons, as predicted by cosmological simulations.
    Section 2.4 and Figure 4 assume the WHIM phase (T > 10^6 K) is present with mass fractions from simulations (Cen and Ostriker 2006; Vazza et al. 2019).
  • domain assumption Collisional ionization equilibrium and a metallicity of 0.3 Solar apply to the WHIM and cluster outskirts.
    Assumed in the spectral simulations in Section 2.4 and Figure 2; deviations would change predicted line fluxes.
  • domain assumption Cosmic X-ray background can be modeled to sub-percent accuracy and used as a backlight for absorption studies.
    Section 2.4 states that detailed modeling of foregrounds and backgrounds is paramount; this is an unproven capability.
  • ad hoc to paper The proposed instrument technologies (megapixel microcalorimeter array, low background, large mirror) can be realized.
    Section 3.3 acknowledges R&D needed; the science case depends on these capabilities being achieved.
  • domain assumption Simulations used for predictions (Omega500, Illustris, EAGLE, ENZO) reliably represent the diffuse baryon distribution.
    Figures 1, 3, 4, 5 rely on these simulations; model spread (Figure 3 lower right) is large for CGM predictions.

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Cite this review

Pith. "Pith review of Voyage through the Hidden Physics of the Cosmic Web." pith.science (2026). https://pith.science/paper/QJXXAISS

@misc{pith2026190801778,
  author       = {Pith},
  title        = {Pith review of: Voyage through the Hidden Physics of the Cosmic Web},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/QJXXAISS}},
  note         = {Machine review of arXiv:1908.01778}
}
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 $10^6$ 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 (~10 m$^2$ at 1 keV) over a large field of view ($\sim1$ deg$^2$), a megapixel cryogenic microcalorimeter array providing integral field spectroscopy with a resolving power $E/\Delta E$ = 2000 at 0.6 keV and a spatial resolution of 5 arcsec in the soft X-ray band, and a low and stable instrumental background ensuring high sensitivity to faint, extended emission.

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Works this paper leans on

16 extracted references · 10 canonical work pages

  1. [1]

    arXiv e-prints 1907.04473 Anderson ME, Churazov E, Bregman JN (2016) A deep XMM-Newton study of the hot gaseous halo around NGC

    Abazajian K, Addison G, Adshead P, Ahmed Z, Allen SW, Alonso D, Alvarez M, Anderson A, Arnold KS, Baccigalupi C, et al (2019) CMB-S4 Science Case, Reference Design, and Project Plan. arXiv e-prints 1907.04473 Anderson ME, Churazov E, Bregman JN (2016) A deep XMM-Newton study of the hot gaseous halo around NGC

    arXiv 2019

  2. [3]

    1051/0004-6361:20010584, astro-ph/0104369 Connor T, Kelson DD, Mulchaey J, Vikhlinin A, Patel SG, Balogh ML, Joshi G, Kraft R, Nagai D, Starikova S (2018) Wide-field Optical Spectroscopy of Abell 133: A Search for Filaments Reported in X-Ray Observations. ApJ867(1):25, DOI 10.3847/1538-4357/aae38b, 1809.08241 Cotroneo V, Spiga D, Barbera M, Bruni R, Chen K...

    work page Pith review arXiv 2018

  3. [5]

    1093/pasj/psx056, 1702.00193 Irwin KD, Hilton GC (2005) Transition-Edge Sensors, vol 99, Springer-Verlag Berlin/Heidelberg, p

    work page Pith review arXiv 2005

  4. [9]

    1093/mnras/stz3075, 1907.00989 Nandra K, Barret D, Barcons X, Fabian A, den Herder JW, Piro L, Watson M, Adami C, Aird J, Afonso JM, et al (2013) The Hot and Energetic Universe: A White Paper presenting the science theme motivating the Athena+ mission. arXiv e-prints arXiv:1306.2307, 1306.2307 Nelson D, Kauffmann G, Pillepich A, Genel S, Springel V, Pakmor...

    arXiv 2013

  5. [10]

    A Deep XMM-Newton Study of the Hot Gaseous Halo Around NGC 1961

    1093/mnras/stv2314, 1508.01514 Armillotta L, Fraternali F, Werk JK, Prochaska JX, Marinacci F (2017) The survival of gas clouds in the circumgalactic medium of Milky Way-like galax- ies. MNRAS470(1):114–125, DOI 10.1093/mnras/stx1239, 1608.05416 Avestruz C, Nagai D, Lau ET, Nelson K (2015) Non-equilibrium Electrons in the Outskirts of Galaxy Clusters. ApJ...

    work page Pith review arXiv 2017

  6. [11]

    1093/pasj/psy040, 1507.02730 Pareschi G, Cotroneo V, Spiga D, Vernani D, Barbera M, Artale A, Col- lura A, Varisco S, Grisoni G, Valsecchi G, Negri B (2004) Astronomical Soft X-ray mirrors Reflectivity Enhancement by Multilayer Coatings with Carbon overcoating. In: Proceedings of SPIE, Society of Photo-Optical In- strumentation Engineers (SPIE) Conference ...

    arXiv 2004

  7. [12]

    Optics for X-ray telescopes: analytical treatment of the off-axis effective area of mirrors in optical modules

    1051/0004-6361/201116430, 1101.0629 Stern J, Hennawi JF, Prochaska JX, Werk JK (2016) A Universal Density Structure for Circumgalactic Gas. ApJ830(2):87, DOI 10.3847/0004-637X/ 830/2/87, 1604.02168 Sun M (2012) Hot gas in galaxy groups: recent observations. New Journal of Physics 14(4):045004, DOI 10.1088/1367-2630/14/4/045004, 1203.4228 Sunyaev RA, Zeldo...

    work page Pith review arXiv 2016

  8. [14]

    1088/0004-637X/789/1/55, 1405.5225 van Daalen MP, Schaye J (2015) The contributions of matter inside and outside of haloes to the matter power spectrum. MNRAS452(3):2247–2257, DOI 10.1093/mnras/stv1456, 1501.05950 van Daalen MP, McCarthy IG, Schaye J (2020) Exploring the effects of galaxy formation on matter clustering through a library of simulation power...

    work page Pith review arXiv 2015

Show all 16 references
  1. [15]

    ApJ788(1):28, DOI 10.1088/0004-637X/788/1/28, 1404.2844 Vazza F, Eckert D, Simionescu A, Br¨ uggen M, Ettori S (2013) Proper- ties of gas clumps and gas clumping factor in the intra-cluster medium. MNRAS429:799–814, DOI 10.1093/mnras/sts375, 1211.1695 Vazza F, Br¨ uggen M, Ghe...

    2013 arXiv

  2. [63]

    DOI 10.1007/$10933596 3$ Irwin KD, Lehnert KW (2004) Microwave SQUID multiplexer. Applied Physics Letters 85(11):2107, DOI 10.1063/1.1791733 Kaastra J, Finoguenov A, Nicastro F, Branchini E, Schaye J, Cappelluti N, Nevalainen J, Barcons X, Bregman J, Croston J, Dolag K, Ettori...

    2004 arXiv

  3. [133]

    Simionescu et al

    MNRAS437:1909–1917, DOI 10.1093/mnras/stt2021, 1306.6336 36 A. Simionescu et al. Moseley SH, Mather JC, McCammon D (1984) Thermal detectors as x-ray spectrometers. Journal of Applied Physics 56(5):1257–1262, DOI 10.1063/ 1.334129, URL https://doi.org/10.1063/1.334129, https://...

    1984 arXiv

  4. [223]

    A&A482(3):L29–L33, DOI 10.1051/0004-6361:200809599, 0803.2525 Werner N, Urban O, Simionescu A, Allen SW (2013) A uniform metal dis- tribution in the intergalactic medium of the Perseus cluster of galaxies. Nature502:656–658, DOI 10.1038/nature12646, 1310.7948 Yamada S, Ohashi ...

    2013 arXiv

  5. [1705]

    07897 Osmond JPF, Ponman TJ (2004) The GEMS project: X-ray analysis and statistical properties of the group sample. MNRAS350(4):1511–1535, DOI 10.1111/j.1365-2966.2004.07742.x, astro-ph/0402439 Ota N, Nagai D, Lau ET (2018) Constraining hydrostatic mass bias of galaxy clusters...

    2004

  6. [1803]

    ApJ696:1640–1656, DOI 10.1088/0004-637X/696/2/1640, 0902.3323 Morandi A, Cui W (2014) Measuring the gas clumping in Abell

    06296 Molnar SM, Hearn N, Haiman Z, Bryan G, Evrard AE, Lake G (2009) Accre- tion Shocks in Clusters of Galaxies and Their SZ Signature from Cosmolog- ical Simulations. ApJ696:1640–1656, DOI 10.1088/0004-637X/696/2/1640, 0902.3323 Morandi A, Cui W (2014) Measuring the gas clum...

    2009 arXiv

  7. [1907]

    08284 Truong N, Rasia E, Mazzotta P, Planelles S, Biffi V, Fabjan D, Beck AM, Borgani S, Dolag K, Gaspari M (2018) Cosmological hydrodynamical sim- ulations of galaxy clusters: X-ray scaling relations and their evolution. MNRAS474(3):4089–4111, DOI 10.1093/mnras/stx2927, 1607.00...

    2018 arXiv

  8. [2142]

    A&A605:A25, DOI 10.1051/0004-6361/201730555, 1705.05844 Eckert D, Ghirardini V, Ettori S, Rasia E, Biffi V, Pointecouteau E, Ros- Voyage through the Hidden Physics of the Cosmic Web 33 setti M, Molendi S, Vazza F, Gastaldello F (2019) Non-thermal pressure support in X-COP galaxy...

    2019 arXiv

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