Extending empirical constraints on the SZ–mass scaling relation to higher redshifts via HST weak lensing measurements of nine clusters from the SPT-SZ survey at <i>z</i> ≳ 1

Zohren, H.; Schrabback, T.; Bocquet, S.; Sommer, Martin W.; Raihan, F.; Hernandez-Martin, B.; Marggraf, O.; Ansarinejad, Behzad; Bayliss, M.; Bleem, Lindsey; Erben, T.; Hoekstra, Henk; Floyd, Benjamin; Gladders, Michael D.; Kleinebreil, F.; McDonald, Michael; Schirmer, M.; Scognamiglio, D.; Sharon, Keren; Wright, Angus H.

doi:10.1051/0004-6361/202142991

Cited by 8 publications

(2 citation statements)

References 120 publications

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“…Source selection is a critical step in weak lensing because only the background galaxies carry the weak-lensing signal. In many studies of galaxy clusters, the background galaxies are selected from their color and magnitude (for example Zohren et al 2022). However, SMACSJ0723 has extensive multi-band photometry that enables the measurement of photometric redshift (photo-z).…”

Section: Source Selectionmentioning

confidence: 99%

The First Weak-lensing Analysis with the James Webb Space Telescope: SMACS J0723.3–7327

Finner

Faisst

Chary

et al. 2023

ApJ

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Utilizing the James Webb Space Telescope Early Release NIRCam Observations, we perform a weak-lensing analysis of the massive galaxy cluster SMACS J0723.3–7327 (z = 0.39). We investigate the spatial variation of the point-spread function (PSF) from the stars in the mosaic image. Our measurements show that the PSF for both modules has very small spatial and temporal variation with average complex ellipticity components of e 1 = 0.007 ± 0.001 and e 2 = 0.029 ± 0.001 in the observed north-up reference frame. We create PSF models through a principal component analysis of the stars and show that they properly account for the ellipticity of the PSF with residual shapes of e 1 = (0.3 ± 3.5) × 10−4 and e 2 = (1.8 ± 4.0) × 10−4. We select background galaxies by their photometric redshift and measure galaxy shapes by model fitting. Our weak-lensing source catalog achieves ∼215 galaxies arcmin−2. We map the convergence field of SMACSJ0723 and detect the cluster with a peak significance of 12.2σ. The mass distribution is found to elongate in the east–west direction with an extension to the northeast edge of the field of view where a candidate substructure is found in the Chandra X-ray imaging. We fit the tangential shear with a Navarro–Frenk–White model and estimate the mass of the cluster to be M 500 = 7.9 ± 1.1 × 1014 M ⊙ (M 200 = 11.4 ± 1.5 × 1014 M ⊙), which agrees with existing mass estimates. Combining the multiwavelength evidence from literature with our weak-lensing analysis, we hypothesize that SMACSJ0723 is observed near first pericenter passage and we identify candidate radio relics.

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Section: Source Selectionmentioning

confidence: 99%

The First Weak-lensing Analysis with the James Webb Space Telescope: SMACS J0723.3–7327

Finner

Faisst

Chary

et al. 2023

ApJ

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“…Applegate et al 2016;Schrabback et al 2018;Grandis et al 2019;Sommer et al 2022) and are self-consistently accounted for in the cluster scaling relation and cosmology analyses (e.g. Dietrich et al 2019;Bocquet et al 2019;Schrabback et al 2021;Chiu et al 2022;Zohren et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Euclid preparation

Giocoli,

Meneghetti,

Rasia

et al. 2024

A&A

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The photometric catalogue of galaxy clusters extracted from ESA Euclid data is expected to be very competitive for cosmological studies. Using dedicated hydrodynamical simulations, we present systematic analyses simulating the expected weak-lensing profiles from clusters in a variety of dynamic states and for a wide range of redshifts. In order to derive cluster masses, we use a model consistent with the implementation within the Euclid Consortium of the dedicated processing function and find that when we jointly model the mass and concentration parameter of the Navarro–Frenk–White halo profile, the weak-lensing masses tend to be biased low by 5–10% on average with respect to the true mass, up to z = 0.5. For a fixed value for the concentration c200 = 3, the mass bias is decreases to lower than 5%, up to z = 0.7, along with the relative uncertainty. Simulating the weak-lensing signal by projecting along the directions of the axes of the moment of inertia tensor ellipsoid, we find that orientation matters: when clusters are oriented along the major axis, the lensing signal is boosted, and the recovered weak-lensing mass is correspondingly overestimated. Typically, the weak-lensing mass bias of individual clusters is modulated by the weak-lensing signal-to-noise ratio, which is related to the redshift evolution of the number of galaxies used for weak-lensing measurements: the negative mass bias tends to be stronger toward higher redshifts. However, when we use a fixed value of the concentration parameter, the redshift evolution trend is reduced. These results provide a solid basis for the weak-lensing mass calibration required by the cosmological application of future cluster surveys from Euclid and Rubin.

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The SRG/eROSITA All-Sky Survey

Grandis,

Ghirardini,

Bocquet

et al. 2024

A&A

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Number counts of galaxy clusters across redshift are a powerful cosmological probe if a precise and accurate reconstruction of the underlying mass distribution is performed -- a challenge called mass calibration. With the advent of wide and deep photometric surveys, weak gravitational lensing (WL) by clusters has become the method of choice for this measurement. We measured and validated the WL signature in the shape of galaxies observed in the first three years of the Dark Energy Survey (DES Y3) caused by galaxy clusters and groups selected in the first all-sky survey performed by SRG (Spectrum Roentgen Gamma)/eROSITA (eRASS1). These data were then used to determine the scaling between the X-ray photon count rate of the clusters and their halo mass and redshift. We empirically determined the degree of cluster member contamination in our background source sample. The individual cluster shear profiles were then analyzed with a Bayesian population model that self-consistently accounts for the lens sample selection and contamination and includes marginalization over a host of instrumental and astrophysical systematics. To quantify the accuracy of the mass extraction of that model, we performed mass measurements on mock cluster catalogs with realistic synthetic shear profiles. This allowed us to establish that hydrodynamical modeling uncertainties at low lens redshifts ($z<0.6$) are the dominant systematic limitation. At high lens redshift, the uncertainties of the sources' photometric redshift calibration dominate. With regard to the X-ray count rate to halo mass relation, we determined its amplitude, its mass trend, the redshift evolution of the mass trend, the deviation from self-similar redshift evolution, and the intrinsic scatter around this relation. The mass calibration analysis performed here sets the stage for a joint analysis with the number counts of eRASS1 clusters to constrain a host of cosmological parameters. We demonstrate that WL mass calibration of galaxy clusters can be performed successfully with source galaxies whose calibration was performed primarily for cosmic shear experiments, opening the way for the cluster cosmological exploitation of future optical and NIR surveys like Euclid and LSST.

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Extending empirical constraints on the SZ–mass scaling relation to higher redshifts via HST weak lensing measurements of nine clusters from the SPT-SZ survey at z ≳ 1

Cited by 8 publications

References 120 publications

The First Weak-lensing Analysis with the James Webb Space Telescope: SMACS J0723.3–7327

The First Weak-lensing Analysis with the James Webb Space Telescope: SMACS J0723.3–7327

Euclid preparation

The SRG/eROSITA All-Sky Survey

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