Density split statistics: Joint model of counts and lensing in cells

Friedrich, Oliver; Gruen, D.; DeRose, Joseph J.; Kirk, D.; Krause, E.; McClintock, Thomas; Rykoff, E. S.; Seitz, S.; Wechsler, Risa H.; Bernstein, G. M.; Blazek, Jonathan; Chang, C.; Hilbert, Stefan; Jain, Bhuvnesh; Kovács, András; Lahav, O.; Abdalla, F. B.; Allam, S.; Annis, James; Bechtol, K.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Rosell, A. Carnero; Kind, M. Carrasco; Carretero, J.; Cunha, C. E.; D’Andrea, C. B.; Costa, L. N. da; Davis, C.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Drlica-Wagner, A.; Eifler, T. F.; Fosalba, P.; Frieman, J.; García-Bellido, J.; Gaztañaga, E.; Gerdes, D. W.; Giannantonio, T.; Gruendl, R. A.; Gschwend, J.; Gutiérrez, G.; Honscheid, K.; James, D. J.; Jarvis, Mike; Kuêhn, K.; Kuropatkin, N.; Lima, M.; March, M.; Marshall, J. L.; Melchior, P.; Menanteau, F.; Miquel, R.; Mohr, J. J.; Nord, B.; Plazas, A. A.; Sánchez, E.; Scarpine, V.; Schindler, R. H.; Schubnell, M.; Sevilla-Noarbe, I.; Sheldon, E.; Smith, M.; Soares-Santos, M.; Sobreira, F.; Suchyta, E.; Swanson, M. E. C.; Tarlè, G.; Thomas, D.; Troxel, M. A.; Vikram, V.; Weller, J.

doi:10.1103/physrevd.98.023508

Cited by 82 publications

(128 citation statements)

References 88 publications

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“…The latter conditions are not true in practice, which is why the degree and spatial distribution of masking still affects the width of PðN i Þ at fixed expectation value. Tests of likelihood runs and the masked PðNÞ in the Buzzard simulations (see Appendix E and [28]) indicate that this is not a major concern for our analysis.…”

Section: A Splitting the Sky By Densitymentioning

confidence: 99%

“…In order to describe our signal as a function of (i) cosmological parameters, (ii) parameters that connect galaxy counts to the matter (over)density, and (iii) nuisance parameters, we use the model developed and tested in Friedrich et al [28]. We only briefly summarize it here, with an emphasis on required extensions for the use on observational data, and refer the reader to that paper for details.…”

Section: Modelmentioning

confidence: 99%

“…Our data vector in this work contains two components, the modeling of which was extensively tested in Friedrich et al [28]. In Sec.…”

Section: Measured Signalsmentioning

confidence: 99%

“…Because the Universe is isotropic, we will omit the dependence onn, i.e., only consider a single line of sight. As detailed in Friedrich et al [28], the density split lensing signal can be calculated from the convergence profile around lines of sight with a fixed value of N T . This profile can be computed as…”

Section: Modelmentioning

confidence: 99%

“…Here, we use a very basic statistic, the mean tracer galaxy overdensity in our density quintiles, that was extensively tested in Friedrich et al [28]-other signals could significantly improve the constraining power in the future.…”

Section: Counts-in-cellsmentioning

confidence: 99%

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Density split statistics: Cosmological constraints from counts and lensing in cells in DES Y1 and SDSS data

Gruen¹,

Friedrich²,

Krause³

et al. 2018

Phys. Rev. D

Self Cite

107

114

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We derive cosmological constraints from the probability distribution function (PDF) of evolved large-scale matter density fluctuations. We do this by splitting lines of sight by density based on their count of tracer galaxies, and by measuring both gravitational shear around and counts-in-cells in overdense and underdense lines of sight, in Dark Energy Survey (DES) First Year and Sloan Digital Sky Survey (SDSS) data. Our analysis uses a perturbation theory model [O. Friedrich et al., Phys. Rev. D 98, 023508 (2018)] and is validated using N-body simulation realizations and log-normal mocks. It allows us to constrain cosmology, bias and stochasticity of galaxies with respect to matter density and, in addition, the skewness of the matter density field. From a Bayesian model comparison, we find that the data weakly prefer a connection of galaxies and matter that is stochastic beyond Poisson fluctuations on ≤ 20 arcmin angular smoothing scale. The two stochasticity models we fit yield DES constraints on the matter density Ω m ¼ 0.26 −0.07 for the two stochasticity models), but consistent with each other and with the 3 x 2pt results if stochasticity is at the low end of the posterior range. As an additional test of gravity, counts and lensing in cells allow to compare the skewness S 3 of the matter density PDF to its ΛCDM prediction. We find no evidence of excess skewness in any model or data set, with better than 25 per cent relative precision in the skewness estimate from DES alone.

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Section: A Splitting the Sky By Densitymentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

“…Our data vector in this work contains two components, the modeling of which was extensively tested in Friedrich et al [28]. In Sec.…”

Section: Measured Signalsmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

Section: Counts-in-cellsmentioning

confidence: 99%

See 3 more Smart Citations

Density split statistics: Cosmological constraints from counts and lensing in cells in DES Y1 and SDSS data

Gruen¹,

Friedrich²,

Krause³

et al. 2018

Phys. Rev. D

Self Cite

107

114

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show abstract

CFHTLenS: Galaxy bias as function of scale, stellar mass, and colour

Simon

Hilbert

2021

A&A

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Galaxy models predict a tight relation between the clustering of galaxies and dark matter on cosmological scales, but predictions differ notably in the details. We used this opportunity and tested two semi-analytic models by the Munich and Durham groups with data from the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS). For the test we measured the scale-dependent galaxy bias factor b(k) and correlation factor r(k) from linear to non-linear scales of k ≈ 10 h Mpc −1 at two redshiftsz = 0.35, 0.51 for galaxies with stellar mass between 5 × 10 9 and 3 × 10 11 h −2 70 M. Our improved gravitational lensing technique accounts for the intrinsic alignment of sources and the magnification of lens galaxies for better constraints for the galaxy-matter correlation r(k). Galaxy bias in CFHTLenS increases with k and stellar mass; it is colour-dependent, revealing the individual footprints of galaxy types. Despite a reasonable model agreement for the relative change with both scale and galaxy properties, there is a clear conflict for b(k) with no model preference: the model galaxies are too weakly clustered. This may flag a model problem at z 0.3 for all stellar masses. As in the models, however, there is a high correlation r(k) between matter and galaxy density on all scales, and galaxy bias is typically consistent with a deterministic bias on linear scales. Only our blue and low-mass galaxies of about 7 × 10 9 h −2 70 M atz = 0.51 show, contrary to the models, a weak tendency towards a stochastic bias on linear scales where r ls = 0.75 ± 0.14 (stat.) ± 0.06 (sys.). This result is of interest for cosmological probes, such as E G , that rely on a deterministic galaxy bias. We provide Monte Carlo realisations of posterior constraints for b(k) and r(k) in CFHTLenS for every galaxy sample in this paper as online material.

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An adapted filter function for density split statistics in weak lensing

Burger¹,

Schneider²,

Demchenko

et al. 2020

A&A

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Context. The density split statistics in weak gravitational lensing analyses probes the correlation between regions of different (foreground) galaxy number densities and their weak lensing signal, which is measured by the shape distortion of background galaxies. Aims. In this paper, we reconsider density split statistics, by constructing a new angular filter function that is adapted to the expected relation between the galaxy number density and shear pattern, in a way that the filter weighting the galaxy number density is matched to the filter that is used to quantify the shear signal. Methods. We used the results of numerical ray-tracing simulations, specifically through the Millennium Simulation supplemented by a galaxy distribution based on a semi-analytic model, to construct a matched pair of adapted filter functions for the galaxy density and the tangential shear signal. We compared the performance of our new filter to the previously used top-hat filter, applying both to a different and independent set of numerical simulations (SLICS, cosmo-SLICS). Results. We show that the adapted filter yields a better correlation between the total matter and the galaxy distribution. Furthermore, the adapted filter provides a larger signal-to-noise ratio to constrain the bias between the total matter and the galaxy distribution, and we show that it is, in general, a more sensitive discriminator between different cosmologies, with the exception of cosmologies with very large σ8 values. All analyses lead to the conclusion that our adapted filter should be favoured in future density split statistic works.

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Density split statistics: Joint model of counts and lensing in cells

Cited by 82 publications

References 88 publications

Density split statistics: Cosmological constraints from counts and lensing in cells in DES Y1 and SDSS data

Density split statistics: Cosmological constraints from counts and lensing in cells in DES Y1 and SDSS data

CFHTLenS: Galaxy bias as function of scale, stellar mass, and colour

An adapted filter function for density split statistics in weak lensing

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