scholarly journals Probing the cluster pressure profile with thermal Sunyaev–Zeldovich effect and weak lensing cross-correlation

2020 ◽  
Vol 500 (2) ◽  
pp. 1806-1816
Author(s):  
Yin-Zhe Ma ◽  
Yan Gong ◽  
Tilman Tröster ◽  
Ludovic Van Waerbeke
Keyword(s):  
Gravitational Lensing ◽  
Cross Correlation ◽  
Pressure Profile ◽  
Shape Index ◽  
Weak Lensing ◽  
Recent Measurement ◽  
Pressure Profiles ◽  
Best Fitting ◽  
The Cross ◽  
Cluster Sequence

ABSTRACT We confront the universal pressure profile (UPP) proposed. with the recent measurement of the cross-correlation function of the thermal Sunyaev–Zeldovich (tSZ) effect from Planck and weak gravitational lensing measurement from the Red Cluster Sequence Lensing Survey. By using the halo model, we calculate the prediction of ξy−κ (lensing convergence and Compton-y parameter) and $\xi ^{y-\gamma _{\rm t}}$ (lensing shear and Compton-y parameter) and fit the UPP parameters by using the observational data. We find consistent UPP parameters when fixing the cosmology to either WMAP 9-yr or Planck 2018 best-fitting values. The best constrained parameter is the pressure profile concentration c500 = r500/rs, for which we find $c_{500} = 2.68^{+1.46}_{-0.96}$ (WMAP-9) and $c_{500} = 1.91^{+1.07}_{-0.65}$ (Planck-2018) for the $\xi ^{y-\gamma _t}$ estimator. The shape index for the intermediate radius region α parameter is constrained to $\alpha =1.75^{+1.29}_{-0.77}$ and $\alpha = 1.65^{+0.74}_{-0.5}$ for WMAP-9 and Planck-2018 cosmologies, respectively. Propagating the uncertainties of the UPP parameters to pressure profiles results in a factor of 3 uncertainty in the shape and magnitude. Further investigation shows that most of the signal of the cross-correlation comes from the low-redshift, inner halo profile (r ≤ rvir/2) with halo mass in the range of 1014–$10^{15}{\, {\rm M}_{\odot }}$, suggesting that this is the major regime that constitutes the cross-correlation signal between weak lensing and tSZ.

scholarly journals First measurement of the cross-correlation between CMB weak lensing and X-ray emission

2019 ◽  
Vol 625 ◽  
pp. L4 ◽  
Author(s):  
G. Hurier ◽  
P. Singh ◽  
C. Hernández-Monteagudo
Keyword(s):  
Cross Correlation ◽  
Power Spectra ◽  
Galaxy Cluster ◽  
Weak Lensing ◽  
X Rays ◽  
Satellite Mission ◽  
Local Universe ◽  
Best Fitting ◽  
The Cross ◽  
Hydrodynamical Simulations

Since the publication of the results of the Planck satellite mission in 2013, the local and early Universes have been considered to be in tension in respect of the determination of amplitude of the matter density spatial fluctuations (σ8) and the amount of matter present in the Universe (Ωm). This tension can be seen as a lack of massive galaxy clusters in the local Universe compared to the prediction inferred from Planck cosmic microwave background (CMB) best-fitting cosmology. In the present analysis we perform the first detection of the cross-correlation between X-rays and CMB weak lensing at 9.1σ. We next combine thermal Sunyaev–Zel’dovich effect, X-rays, and weak-lensing angular auto- and cross-correlation power spectra to determine the galaxy cluster hydrostatic mass bias. We derive (1 − bH) = 0.71 ± 0.07. Considering these constraints, we observe that estimations of σ8 in the local Universe are consistent with Planck CMB best-fitting cosmology. However, these results are in clear tension with the output of hydrodynamical simulations that favor (1 − bH)> 0.8.

scholarly journals SuperCLASS – III. Weak lensing from radio and optical observations in Data Release 1

2020 ◽  
Vol 495 (2) ◽  
pp. 1737-1759 ◽  
Author(s):  
Ian Harrison ◽  
Michael L Brown ◽  
Ben Tunbridge ◽  
Daniel B Thomas ◽  
Tom Hillier ◽  
...  
Keyword(s):  
Gravitational Lensing ◽  
Cross Correlation ◽  
Optical Observations ◽  
Optical Data ◽  
Weak Lensing ◽  
Data Set ◽  
Radio Data ◽  
Data Release ◽  
First Results ◽  
Radio Wavelength

ABSTRACT We describe the first results on weak gravitational lensing from the SuperCLASS survey: the first survey specifically designed to measure the weak lensing effect in radio-wavelength data, both alone and in cross-correlation with optical data. We analyse $1.53 \, \mathrm{deg}^2$ of optical data from the Subaru telescope and $0.26 \, \mathrm{deg}^2$ of radio data from the e-MERLIN and VLA telescopes (the DR1 data set). Using standard methodologies on the optical data only we make a significant (10σ) detection of the weak lensing signal (a shear power spectrum) due to the massive supercluster of galaxies in the targeted region. For the radio data we develop a new method to measure the shapes of galaxies from the interferometric data, and we construct a simulation pipeline to validate this method. We then apply this analysis to our radio observations, treating the e-MERLIN and VLA data independently. We achieve source densities of $0.5 \,$ arcmin−2 in the VLA data and $0.06 \,$ arcmin−2 in the e-MERLIN data, numbers which prove too small to allow a detection of a weak lensing signal in either the radio data alone or in cross-correlation with the optical data. Finally, we show preliminary results from a visibility-plane combination of the data from e-MERLIN and VLA which will be used for the forthcoming full SuperCLASS data release. This approach to data combination is expected to enhance both the number density of weak lensing sources available, and the fidelity with which their shapes can be measured.

scholarly journals A gravitational lensing detection of filamentary structures connecting luminous red galaxies

2020 ◽  
Vol 633 ◽  
pp. A89 ◽  
Author(s):  
Qianli Xia ◽  
Naomi Robertson ◽  
Catherine Heymans ◽  
Alexandra Amon ◽  
Marika Asgari ◽  
...  
Keyword(s):  
Gravitational Lensing ◽  
Critical Density ◽  
Average Density ◽  
Sloan Digital Sky Survey ◽  
Weak Lensing ◽  
Luminous Red Galaxies ◽  
Sky Survey ◽  
Combining Data ◽  
Red Galaxies ◽  
Cluster Sequence

We present a weak lensing detection of filamentary structures in the cosmic web, combining data from the Kilo-Degree Survey, the Red Cluster Sequence Lensing Survey, and the Canada-France-Hawaii Telescope Lensing Survey. The line connecting luminous red galaxies with a separation of 3 − 5 h−1 Mpc was chosen as a proxy for the location of filaments. We measured the average weak lensing shear around ∼11 000 candidate filaments selected in this way from the Sloan Digital Sky Survey. After nulling the shear induced by the dark matter haloes around each galaxy, we reported a 3.4σ detection of an anisotropic shear signal from the matter that connects them. Adopting a filament density profile, motivated from N-body simulations, the average density at the centre of these filamentary structures was found to be 15 ± 4 times the critical density.

scholarly journals RCSLenS: testing gravitational physics through the cross-correlation of weak lensing and large-scale structure

2015 ◽  
Vol 456 (3) ◽  
pp. 2806-2828 ◽  
Author(s):  
Chris Blake ◽  
Shahab Joudaki ◽  
Catherine Heymans ◽  
Ami Choi ◽  
Thomas Erben ◽  
...  
Keyword(s):  
Large Scale ◽  
Cross Correlation ◽  
Large Scale Structure ◽  
Scale Structure ◽  
Weak Lensing ◽  
The Cross

The cross-correlation of the Lyman-α forest and weak lensing of CMB: a new cosmological tool

2010 ◽  
Author(s):  
Alberto Vallinotto ◽  
Jean-Michel Alimi ◽  
André Fuözfa
Keyword(s):  
Cross Correlation ◽  
Weak Lensing ◽  
The Cross

scholarly journals ON the Cross-Correlation of Galaxies with UVX Objects and QSOS

1984 ◽  
Vol 78 ◽  
pp. 467-472
Author(s):  
B.J. Boyle ◽  
T. Shanks ◽  
R. Fong
Keyword(s):  
Cross Correlation ◽  
Ultra Violet ◽  
Recent Measurement ◽  
Clusters Of Galaxies ◽  
Tentative Evidence ◽  
The Cross

Recent measurement of UK Schmidt plates have yielded interesting results on the cross-correlation of galaxies with QSOs and ultra-violet excess (UVX) objects. We find that in all Schmidt fields so far analysed there appears to be a significant anti-correlation (at angular scales less than 5') between the positions of galaxies and QSOs and between the positions of galaxies and UVX objects. This anti-correlation appears to be restricted to those galaxies that are found in clusters. These observations can very naturally be explained using a model in which dust within clusters of galaxies obscures the QSOs lying at cosmological distances behind them. This hypothesis may be further corroborated by tentative evidence that the UVX objects and the QSOs appear to be reddened close to clusters of galaxies.

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