Fig 2 - uploaded by Luigi Toffolatti
Content may be subject to copyright.
Stacked scaled image (size is 10 R 500 on a side) using a logarithmic stretch in y. Individual maps are rescaled by Φ i before averaging, and then multiplied by Φ i. The black and white circles mark the loci of 1 and 3 × R 500 , respectively.
Source publication
Taking advantage of the all-sky coverage and broad frequency range of the Planck satellite, we study the Sunyaev-Zeldovich (SZ) and pressure profiles of 62 nearby massive clusters detected at high significance in the 14-month nominal survey. Careful reconstruction of the SZ signal
indicates that most clusters are individually detected at least out...
Context in source publication
Context 1
... comparison shows a first order agreement between the Planck measurements and the ex- pected SZ profiles derived from X-ray constraints assuming a GNFW pressure profile shape. Figure 2 presents the stacked average image of the 62 clusters of our ESZ-XMM sample, plotted on a logarithmic scale. Before averaging, each individual SZ map was normalised identically to the profiles (see Eq. (12)) and randomly rotated by 0 • , 90 • , 180 • or 270 • . ...
Similar publications
We present VLA Low-band Ionosphere and Transient Experiment (VLITE) 338 MHz observations of the galaxy cluster CL 0838+1948. We combine the VLITE data with Giant Metrewave Radio Telescope 610 MHz observations and survey data. The central galaxy hosts a 250 kpc source whose emission is dominated by two large lobes at low frequencies. At higher frequ...
It is evident that considerable information exists in astronomical data below the threshold for the detection of individual sources (perhaps set for a ‘5σ’ total detection, or for isophotal detection thresholds of ‘2σ’ above the sky background), and that such information, if descriptive of an underlying population of objects characterized by a rela...
Cosmological MHD simulations of galaxy cluster formation show a significant amplification of seed magnetic fields. We developed a novel method to decompose cluster magnetized turbulence into modes and showed that the fraction of the fast mode is fairly large, around one-fourth in terms of energy. This is larger than that was estimated before, which...
This paper is the first in a series, presenting a new galaxy cluster finder based on a three-dimensional Voronoi Tesselation plus a maximum likelihood estimator, followed by gapping-filtering in radial velocity(VoML+G). The scientific aim of the series is a reassessment of the diversity of optical clusters in the local universe. A mock galaxy datab...
Merging galaxy clusters have been touted as one of the best probes for constraining self-interacting dark matter, but few simulations exist to back up this claim. We simulate equal mass mergers of 10$^{15}$ M$_\odot$ halos, like the El Gordo and Sausage clusters, with cosmologically-motivated halo and merger parameters, and with velocity-independen...
Citations
... Russell et al. 2008), or from the thermal Sunyaev-Zel'dovich effect (e.g. Collaboration et al. 2013). A magnetic field strength can then be calculated by assuming a plasma , which we denote pl , defined (in Gaussian units) as ...
... We thank an anonymous referee for a constructive and helpful report. J Software: We gratefully acknowledge the use of the following software packages: astropy (Astropy Collaboration et al. 2013Collaboration et al. , 2018, matplotlib (Hunter 2007), numba (Lam et al. 2015), scipy (Virtanen et al. 2020), pandas (Mckinney 2010; Pandas Development Team 2020), OpenMPI (Gabriel et al. 2004) and (Arnaud 1996). This paper includes results from ALP version 1.0 (Matthews 2021), but versions 1.1 and later should be used to access the Fourier scheme and more complete documentation. ...
Axion-like particles (ALPs) are a well-motivated extension to the standard model of particle physics, and X-ray observations of cluster-hosted AGN currently place the most stringent constraints on the ALP coupling to electromagnetism, $g_{a \gamma}$, for very light ALPs ($m_a\lesssim10^{-11}$ eV). We revisit limits obtained by Reynolds et al. (2020) using Chandra X-ray grating spectroscopy of NGC 1275, the central AGN in the Perseus cluster, examining the impact of the X-ray spectral model and magnetic field model. We also present a new publicly available code, ALPro, which we use to solve the ALP propagation problem. We discuss evidence for turbulent magnetic fields in Perseus and show that it can be important to resolve the magnetic field structure on scales below the coherence length. We re-analyse the NGC 1275 X-ray spectra using an improved data reduction and baseline spectral model. We find the limits are insensitive to whether a partially covering absorber is used in the fits. At low $m_a$ ($m_a\lesssim10^{-13}$ eV), we find marginally weaker limits on $g_{a \gamma}$ (by $0.1-0.3$ dex) with different magnetic field models, compared to Model B from Reynolds et al. (2020). A Gaussian random field (GRF) model designed to mimic $\sim50$ kpc scale coherent structures also results in only slightly weaker limits. We conclude that the existing Model B limits are robust assuming that $\beta_{\rm pl}\approx100$, and are insensitive to whether cell-based or GRF methods are used. However, astrophysical uncertainties regarding the strength and structure of cluster magnetic fields persist, motivating high sensitivity RM observations and tighter constraints on the radial profile of $\beta_{\rm pl}$.
... Here, σ T is the cross-section for Thomson scattering (see [85,86] for more details). The X-COP sample contains 12 low-redshift (0.04 < z < 0.1) massive galaxy clusters for which hydrostatic mass profiles, corrected for a non-thermal contribution to intracluster medium pressure [87], was recovered with an unprecedented accuracy (relative median error of 3% at R 500 and 6% at R 200 (see detailed discussion in [81]). ...
The idea of massive graviton plays a fundamental role in modern physics as a landmark of most scenarios related to modified gravity theories. Limits on graviton mass can be obtained through different methods, using all the capabilities of multi-messenger astronomy available today. In this paper, we consider some emerging opportunities. In particular, modified relativistic dispersion relations of massive gravitons may lead to changes in the travel time of gravitational waves (GWs) emitted from distant astrophysical objects. Strong gravitational lensing of signals from a carefully selected class of extra-galactic sources such as compact object binaries (actually, binary neutron stars) is predicted to play an important role in this context. Comparing time delays between images of the lensed GW signal and its electromagnetic (EM) counterpart may be a new model-independent strategy (proposed by us in X.-L. Fan et al, 2017), which is especially promising in light of the fruitful observing runs of interferometric GW detectors, resulting in numerous GW signals. In addition to this direct, kinematic method, one can use an indirect, static method. In this approach, the non-zero graviton mass would modify estimates of the total cluster mass via a Yukawa term, influencing the Newtonian potential. In A. Piórkowska-Kurpas et al, 2022, using the X-COP galaxy cluster sample, we obtained mg<(4.99−6.79)×10−29 eV (at 95% C.L.), which is one of the best available constraints.
... We adopt the best-fit values obtained from the analysis of the stacked pressure profile of Planck tSZ clusters, [50]. We also fix the parameter α A10 p ¼ 0.12 as obtained by Arnaud et al. [49] in their x-ray sample analysis. ...
Hot, ionized gas leaves an imprint on the cosmic microwave background via the thermal Sunyaev Zel'dovich (tSZ) effect. The cross-correlation of gravitational lensing (which traces the projected mass) with the tSZ effect (which traces the projected gas pressure) is a powerful probe of the thermal state of ionized baryons throughout the Universe, and is sensitive to effects such as baryonic feedback. In a companion paper (Gatti et al. 2021), we present tomographic measurements and validation tests of the cross-correlation between galaxy shear measurements from the first three years of observations of the Dark Energy Survey, and tSZ measurements from a combination of Atacama Cosmology Telescope and Planck observations. In this work, we use the same measurements to constrain models for the pressure profiles of halos across a wide range of halo mass and redshift. We find evidence for reduced pressure in low mass halos, consistent with predictions for the effects of feedback from active galactic nuclei. We infer the hydrostatic mass bias (B≡M500c/MSZ) from our measurements, finding B=1.8±0.1 when adopting the Planck-preferred cosmological parameters. We additionally find that our measurements are consistent with a non-zero redshift evolution of B, with the correct sign and sufficient magnitude to explain the mass bias necessary to reconcile cluster count measurements with the Planck-preferred cosmology. Our analysis introduces a model for the impact of intrinsic alignments (IA) of galaxy shapes on the shear-tSZ correlation. We show that IA can have a significant impact on these correlations at current noise levels.
... This also includes the distribution of different metal species within galaxies and galaxy clusters [48] and the properties of the AGN population [43,49]. Especially, the simulations well reproduce the observed pressure profiles of galaxy clusters [39,50] and x-ray scaling relations [51]. ...
The thermal Sunyaev-Zeldovich effect contains information about the thermal history of the Universe, which is observable in maps of the Compton y parameter; however, it does not contain information about the redshift of the sources. Recent papers have utilized a tomographic approach, by cross correlating the Compton y map with the locations of galaxies with known redshift in order to deproject the signal along the line of sight. In this paper, we test the validity and accuracy of this tomographic approach to probe the thermal history of the Universe. We use the state-of-the-art, cosmological, and hydrodynamical simulation, Magneticum, for which the thermal history of the Universe is a known quantity. The key ingredient is the Compton-y-weighted halo bias, by, which is computed from the halo model. We find that, at redshifts currently available, the method reproduces the correct mean thermal pressure (or the density-weighted mean temperature) with high accuracy, validating and confirming the results of previous papers. At higher redshifts (z≳2), there is significant disagreement between by from the halo model and the simulation.
... where E(z) = H(z)/H 0 and the generalized NFW profile p A10 (x) is given by: (12) We adopt the best-fit values obtained from the analysis of the stacked pressure profile of Planck tSZ clusters, P A10 = 6.41, c A10 500 = 1.81, α A10 = 1.33, β A10 = 4.13 and γ A10 = 0.31 [40]. We also fix the parameter α A10 p = 0.12 as obtained by Arnaud et al. [39] in their X-ray sample analysis. ...
Hot, ionized gas leaves an imprint on the cosmic microwave background via the thermal Sunyaev Zel'dovich (tSZ) effect. The cross-correlation of gravitational lensing (which traces the projected mass) with the tSZ effect (which traces the projected gas pressure) is a powerful probe of the thermal state of ionized baryons throughout the Universe, and is sensitive to effects such as baryonic feedback. In a companion paper (Gatti et al. 2021), we present tomographic measurements and validation tests of the cross-correlation between galaxy shear measurements from the first three years of observations of the Dark Energy Survey, and tSZ measurements from a combination of Atacama Cosmology Telescope and ${\it Planck}$ observations. In this work, we use the same measurements to constrain models for the pressure profiles of halos across a wide range of halo mass and redshift. We find evidence for reduced pressure in low mass halos, consistent with predictions for the effects of feedback from active galactic nuclei. We infer the hydrostatic mass bias ($B \equiv M_{500c}/M_{\rm SZ}$) from our measurements, finding $B = 1.8\pm0.1$ when adopting the ${\it Planck}$-preferred cosmological parameters. We additionally find that our measurements are consistent with a non-zero redshift evolution of $B$, with the correct sign and sufficient magnitude to explain the mass bias necessary to reconcile cluster count measurements with the ${\it Planck}$-preferred cosmology. Our analysis introduces a model for the impact of intrinsic alignments (IA) of galaxy shapes on the shear-tSZ correlation. We show that IA can have a significant impact on these correlations at current noise levels.
... Here, we list some of these with uncertainties and their width relative to those of the priors we employ. As mentioned by Schneider & Teyssier (2015), Ade et al. (2013) suggests η = 0.3−0.7 (30 per cent of the width of our prior) from the radial profile of the cluster gas fraction; X-ray data (Sun et al. 2009;Vikhlinin et al. 2009;Gonzalez et al. 2013) suggests β = 0.3−0.8 (20 per cent width) and M c = 0.2−2.0 × 10 14 h −1 M (26 per cent width) from the bounded gas fraction-M 500 relation. ...
As weak lensing surveys are becoming deeper and cover larger areas, information will be available on small angular scales down to the arcmin level. To extract this extra information, accurate modelling of baryonic effects is necessary. In this work, we adopt a baryonic correction model, which includes gas both bound inside and ejected from dark matter (DM) haloes, a central galaxy, and changes in the DM profile induced by baryons. We use this model to incorporate baryons into a large suite of DM-only N-body simulations, covering a grid of 75 cosmologies in the Ωm − σ8 parameter space. We investigate how baryons affect Gaussian and non-Gaussian weak lensing statistics and the cosmological parameter inferences from these statistics. Our results show that marginalizing over baryonic parameters degrades the constraints in Ωm − σ8 space by a factor of 2 − 5 compared to those with baryonic parameters fixed. We also find that combining the lensing power spectrum and peak counts can break the degeneracy between cosmological and baryonic parameters and mitigate the impact of the uncertainty in baryonic physics.
... To assess the impact of a change in min instead, we repeated both analysis switching from min = 10 to min = 70 and found quantitatively negligible differences. In all these cases we have employed bins logarithmically spaced in , 20 when ∈ [10, 1000] and [70,1000], and 27 when ∈ [10, 5000] and [70,5000]. The choice of binning is further discussed in appendix E. ...
... To assess the impact of a change in min instead, we repeated both analysis switching from min = 10 to min = 70 and found quantitatively negligible differences. In all these cases we have employed bins logarithmically spaced in , 20 when ∈ [10, 1000] and [70,1000], and 27 when ∈ [10, 5000] and [70,5000]. The choice of binning is further discussed in appendix E. ...
... Having made the point that the bispectrum allows us to separately fit multiple parameters, we now inquire what are the prospects considering tSZ observations combined to prior knowledge of cosmological and gas parameters. Generally, the gas parameters are fixed to the best-fit values of simulations [39], external X-Ray [40], or stacked tSZ clusters [70] measurements, and not varied throughout the analysis of cosmological parameters. On the other hand, one can also think of using the Planck primary anisotropies measure- Figure 8. Impact of degeneracies on the parameters error bars. ...
Non-Gaussian (NG) statistics of the thermal Sunyaev-Zeldovich (tSZ) effect carry significant information which is not contained in the power spectrum. Here, we perform a joint Fisher analysis of the tSZ power spectrum and bispectrum to verify how much the full bispectrum can contribute to improve parameter constraints. We go beyond similar studies of this kind in several respects: first of all, we include the complete power spectrum and bispectrum (auto- and cross-) covariance in the analysis, computing all NG contributions; furthermore we consider a multi-component foreground scenario and model the effects of component separation in the forecasts; finally, we consider an extended set of both cosmological and intra-cluster medium parameters. We show that the tSZ bispectrum is very efficient at breaking parameter degeneracies, making it able to produce even stronger cosmological constraints than the tSZ power spectrum: e.g. the standard deviation on σ8 shrinks from σPS(σ8)=0.35 to σBS(σ8)=0.065 when we consider a multi-parameter analysis. We find that this is mostly due to the different response of separate triangle types (e.g. equilateral and squeezed) to changes in model parameters. While weak, this shape dependence is clearly non-negligible for cosmological parameters, and it is even stronger, as expected, for intra-cluster medium parameters.
... This also includes the distribution of different metal species within galaxies and galaxy clusters [48] and the properties of the AGN population [43,49]. Especially the simulations well reproduce the observed pressure profiles of galaxy clusters [39,50] and X-ray scaling relations [51]. ...
The thermal Sunyaev-Zeldovich effect contains information about the thermal history of the universe, observable in maps of the Compton $y$ parameter; however, it does not contain information about the redshift of the sources. Recent papers have utilized a tomographic approach, cross-correlating the Compton $y$ map with the locations of galaxies with known redshift, in order to deproject the signal along the line of sight. In this paper, we test the validity and accuracy of this tomographic approach to probe the thermal history of the universe. We use the state-of-the-art cosmological hydrodynamical simulation, Magneticum, for which the thermal history of the universe is a known quantity. The key ingredient is the Compton-$y$-weighted halo bias, $b_y$, computed from the halo model. We find that, at redshifts currently available, the method reproduces the correct mean thermal pressure (or the density-weighted mean temperature) to high accuracy, validating and confirming the results of previous papers. At higher redshifts ($z\gtrsim 2.5$), there is significant disagreement between $b_y$ from the halo model and the simulation.
... Having made the point that the bispectrum allows to separately fit multiple parameters, we now inquire what are the prospects considering tSZ observations combined to prior knowledge of cosmological and gas parameters. Generally, the gas parameters are fixed to the best-fit values of simulations [64], external X-Ray [36], or stacked tSZ clusters [65] measurements, and not varied throughout the analysis of cosmological parameters. On the other hand, one can also think of using the Planck primary anisotropies measurements to set a prior on the cosmological parameters, and exploit tSZ anisotropies data to cross-check the gas parame- Notice that the power spectrum 1σ ellipses have been rescaled by a factor to fit in the same graph. ...
Non-Gaussian (NG) statistics of the thermal Sunyaev-Zeldovich (tSZ) effect carry significant information which is not contained in the power spectrum. Here, we perform a joint Fisher analysis of the tSZ power spectrum and bispectrum to verify how much the full bispectrum can contribute to improve parameter constraints. We go beyond similar studies of this kind in several respects: first of all, we include the complete power spectrum and bispectrum (auto- and cross-) covariance in the analysis, computing all NG contributions; furthermore we consider a multi-component foreground scenario and model the effects of component separation in the forecasts; finally, we consider an extended set of both cosmological and intra-cluster medium parameters. We show that the tSZ bispectrum is very efficient at breaking parameter degeneracies, making it able to produce even stronger cosmological constraints than the tSZ power spectrum: e.g. the standard deviation on $\sigma_8$ shrinks from $\sigma^\text{PS}(\sigma_8)=0.35$ to $\sigma^\text{BS}(\sigma_8)=0.065$ when we consider a multi-parameter analysis. We find that this is mostly due to the different response of separate triangle types (e.g. equilateral and squeezed) to changes in model parameters. While weak, this shape dependence is clearly non-negligible for cosmological parameters, and it is even stronger, as expected, for intra-cluster medium parameters.
... To this end, we compute P (r) over the range (0.1, 1.5)R 500 , and fit it with the universal pressure profile [46,47] given by (28) with (P 0 , α, δ, γ) fitting parameters 3 , and P 500 a redshift and mass dependent normalization which, following [48], we set as 4 The Q GR 0 (r) function entering the theoretical pressure profile in Eq.(24) depends on the values of the double -β model parameters. For later applications, it is convenient to reparameterize them as {β, r c1 , r c2 , n 01 , n 02 } −→ {β, log x c1 , log x c2 , log n 01 , log (n 02 /n 01 )} (30) with x ci = r ci /R 200 . ...
... However, we here just want to have realistic profiles for both the convergence and the pressure which is what we indeed get in this way. We use the parameters in Table I to generate the theoretical pressure profile and fit it with Eq.(28) adjusting the parameters (P 0 , α, δ) while keeping c 500 to the input value and fixing γ = 0.31 as recommended in [48]. The quality of the fit can be guessed computing ...
... We must rather compare the value of the fitting parameters to those obtained fitting real clusters. To this aim, we can rely on the values reported in [48] where the fit has been performed for the subsample of 62 clusters with SZ measurements from the early Planck data release. The median, 68 and 95% CL of the best fit parameters to the theoretical BOXSZ and observed Planck clusters are as follows Although the ranges have a good overlap, we can nevertheless note that the typical P 0 values for our sample are definitely larger than those for Planck clusters. ...
Degenerate higher-order scalar-tensor (DHOST) theories are considered the most general class of scalar-tensor theories so that any constraints on them apply to the full set of scalar-tensor models. DHOST theories modify the laws of gravity even at galaxy clusters scale hence affecting the weak lensing (WL), X-ray and Sunyaev-Zel'dovich observables. We derive the theoretical expression for the lensing convergence $\kappa$, and the pressure profile $P$, of clusters in the framework of DHOST theories, and quantify how much they deviate from their General Relativity (GR) counterparts. We argue that combined measurements of $\kappa$, $P$, and of the electron number density, $n_e$, can constrain both the cluster and DHOST theory parameters. We carry on a Fisher matrix forecasts analysis to investigate whether this is indeed the case considering different scenarios for the spatial resolution and errors on the measured quantities.
