First detection of stacked X-ray emission from cosmic web filaments

Tanimura, Hidehiko; Aghanim, N.; Kolodzig, Alexander; Douspis, M.; Malavasi, Nicola

doi:10.1051/0004-6361/202038521

Cited by 65 publications

(44 citation statements)

References 49 publications

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“…We note here that the predicted X-ray in the simulations is sensitive to the assumed metallicity (here the metallicity is 0.3 of solar) as well as the exact energy range (the energy range used in the simulations is 0.3-2 keV rather than the 0.1-2.4 keV band of ROSAT). The average X-ray surface brightness found here from the real LRG pairs is ∼4-10 times higher than that reported by Tanimura et al (2020), who also stacked on the RASS data. Tanimura et al (2020) used more ROSAT channels, a different sample of filaments to stack, and a slightly different method of analysis all of which could explain the discrepancy.…”

Section: Cosmological Simulationscontrasting

confidence: 74%

“…The average X-ray surface brightness found here from the real LRG pairs is ∼4-10 times higher than that reported by Tanimura et al (2020), who also stacked on the RASS data. Tanimura et al (2020) used more ROSAT channels, a different sample of filaments to stack, and a slightly different method of analysis all of which could explain the discrepancy.…”

Section: Cosmological Simulationscontrasting

confidence: 74%

“…There have been few direct detections of hot gas filaments in the X-ray (Werner et al 2008;Eckert et al 2015), as well as a recent E-mail: tessa.vernstrom@csiro.au detection via stacking (Tanimura et al 2020). The most recent direct detection from Reiprich et al (2021) used the extended ROentgen Survey with an Imaging Telescope Array (eROSITA) telescope to measure a 15 Mpc long X-ray filament between two clusters.…”

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confidence: 99%

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Discovery of magnetic fields along stacked cosmic filaments as revealed by radio and X-ray emission

Vernstrom

Heald

Vazza

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Diffuse filaments connect galaxy clusters to form the cosmic web. Detecting these filaments could yield information on the magnetic field strength, cosmic ray population and temperature of intercluster gas, yet, the faint and large-scale nature of these bridges makes direct detections very challenging. Using multiple independent all-sky radio and X-ray maps we stack pairs of luminous red galaxies as tracers for cluster pairs. For the first time, we detect an average surface brightness between the clusters from synchrotron (radio) and thermal (X-ray) emission with ≳ 5σ significance, on physical scales larger than observed to date (≥3 Mpc). We obtain a synchrotron spectral index of α ≃ −1.0 and estimates of the average magnetic field strength of 30 ≤ B ≤ 60 nG, derived from both equipartition and Inverse Compton arguments, implying a 5 to 15 per cent degree of field regularity when compared with Faraday rotation measure estimates. While the X-ray detection is inline with predictions, the average radio signal comes out higher than predicted by cosmological simulations and dark matter annihilation and decay models. This discovery demonstrates that there are connective structures between mass concentrations that are significantly magnetised, and the presence of sufficient cosmic rays to produce detectable synchrotron radiation.

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Section: Cosmological Simulationscontrasting

confidence: 74%

Section: Cosmological Simulationscontrasting

confidence: 74%

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confidence: 99%

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Discovery of magnetic fields along stacked cosmic filaments as revealed by radio and X-ray emission

Vernstrom

Heald

Vazza

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…4.3). Although there have been very recent fruitful attempts at a first detection of this barely visible baryonic component (Macquart et al 2020;Tanimura et al 2020), there exist no accurate measurements of its distribution around isolated galaxies. However, we can safely continue as long as all estimates of g bar (in the measurements, models and simulations) are based on the same components (in our case: stars + cold gas).…”

Section: The Rar Of Kids Compared To Mg Theoriesmentioning

confidence: 99%

The weak lensing radial acceleration relation: Constraining modified gravity and cold dark matter theories with KiDS-1000

Brouwer

Oman²,

Valentijn³

et al. 2021

A&A

130

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We present measurements of the radial gravitational acceleration around isolated galaxies, comparing the expected gravitational acceleration given the baryonic matter (gbar) with the observed gravitational acceleration (gobs), using weak lensing measurements from the fourth data release of the Kilo-Degree Survey (KiDS-1000). These measurements extend the radial acceleration relation (RAR), traditionally measured using galaxy rotation curves, by 2 decades in gobs into the low-acceleration regime beyond the outskirts of the observable galaxy. We compare our RAR measurements to the predictions of two modified gravity (MG) theories: modified Newtonian dynamics and Verlinde’s emergent gravity (EG). We find that the measured relation between gobs and gbar agrees well with the MG predictions. In addition, we find a difference of at least 6σ between the RARs of early- and late-type galaxies (split by Sérsic index and u − r colour) with the same stellar mass. Current MG theories involve a gravity modification that is independent of other galaxy properties, which would be unable to explain this behaviour, although the EG theory is still limited to spherically symmetric static mass models. The difference might be explained if only the early-type galaxies have significant (Mgas ≈ M⋆) circumgalactic gaseous haloes. The observed behaviour is also expected in Λ-cold dark matter (ΛCDM) models where the galaxy-to-halo mass relation depends on the galaxy formation history. We find that MICE, a ΛCDM simulation with hybrid halo occupation distribution modelling and abundance matching, reproduces the observed RAR but significantly differs from BAHAMAS, a hydrodynamical cosmological galaxy formation simulation. Our results are sensitive to the amount of circumgalactic gas; current observational constraints indicate that the resulting corrections are likely moderate. Measurements of the lensing RAR with future cosmological surveys (such as Euclid) will be able to further distinguish between MG and ΛCDM models if systematic uncertainties in the baryonic mass distribution around galaxies are reduced.

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“…Other claims to have detected the WHIM include possible detection of O VII lines, excess dispersion measure over our Galaxy and the host galaxy in fast rasio bursts (FRBs), and stacked X-ray emission from cosmic web filaments using the thermal Sunyaev-Zelodovich (tSZ) effect (e.g. Nicastro et al 2018;Macquart et al 2020;Tanimura et al 2020).…”

mentioning

confidence: 99%

Probing the physical properties of the intergalactic medium using gamma-ray bursts

Dalton

Morris

Fumagalli

2021

Monthly Notices of the Royal Astronomical Society

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We use Gamma-ray burst (GRB) spectra total continuum absorption to estimate the key intergalactic medium (IGM) properties of hydrogen column density ($\mathit {N}_{\mathrm{HXIGM}}$), metallicity, temperature and ionisation parameter over a redshift range of 1.6 ≤ z ≤ 6.3, using photo-ionisation (PIE) and collisional ionisation equilibrium (CIE) models for the ionised plasma. We use more realistic host metallicity, dust corrected where available, in generating the host absorption model, assuming that the host intrinsic hydrogen column density is equal to the measured ionisation corrected intrinsic neutral column from UV spectra (${\it N}_{\mathrm{H}\, \rm \small {I,IC}}$). We find that the IGM property results are similar, regardless of whether the model assumes all PIE or CIE. The $\mathit {N}_{\mathrm{HXIGM}}$ scales as (1 + z)1.0 − 1.9, with equivalent hydrogen mean density at z = 0 of $n_0 = 1.8^{+1.5}_{-1.2} \times 10^{-7}$ cm−3. The metallicity ranges from ∼0.1 Z⊙ at z ∼ 2 to ∼0.001 Z⊙ at redshift z > 4. The PIE model implies a less rapid decline in average metallicity with redshift compared to CIE. Under CIE, the temperature ranges between 5.0 < log (T/K) < 7.1. For PIE the ionisation parameter ranges between 0.1 < log (ξ) < 2.9. Using our model, we conclude that the IGM contributes substantially to the total absorption seen in GRB spectra and that this contribution rises with redshift, explaining why the hydrogen column density inferred from X-rays is substantially in excess of the intrinsic host contribution measured in UV.

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First detection of stacked X-ray emission from cosmic web filaments

Cited by 65 publications

References 49 publications

Discovery of magnetic fields along stacked cosmic filaments as revealed by radio and X-ray emission

Discovery of magnetic fields along stacked cosmic filaments as revealed by radio and X-ray emission

The weak lensing radial acceleration relation: Constraining modified gravity and cold dark matter theories with KiDS-1000

Probing the physical properties of the intergalactic medium using gamma-ray bursts

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