KiDS+GAMA: Intrinsic alignment model constraints for current and future weak lensing cosmology

Johnston, Harry; Georgiou, Christos; Joachimi, Benjamin; Hoekstra, Henk; Chisari, Nora Elisa; Farrow, Daniel J.; Fortuna, Maria Cristina; Heymans, Catherine; Joudaki, Shahab; Kuijken, Konrad; Wright, Angus H.

doi:10.1051/0004-6361/201834714

Cited by 89 publications

(144 citation statements)

References 91 publications

(148 reference statements)

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“…Our n s values are fully consistent with Planck Collaboration et al (2018) results. In addition, our joint constraints on A IA = 0.05 +0.40 −0.44 , are consistent with the direct measurements of Johnston et al (2019), who reported A IA = 1.06 +0.47 −0.46 with a 1.6σ difference. Here we have used a joint model with a single free parameter for the intrinsic alignment of galaxies.…”

Section: Appendix A: Covariance Of Cosebissupporting

confidence: 90%

KiDS+VIKING-450 and DES-Y1 combined: Mitigating baryon feedback uncertainty with COSEBIs

Asgari

Tröster

Heymans

et al. 2020

A&A

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We present cosmological constraints from a joint cosmic shear analysis of the Kilo-Degree Survey (KV450) and the Dark Energy Survey (DES-Y1), conducted using Complete Orthogonal Sets of E/B-Integrals (COSEBIs). With COSEBIs we isolate any B-modes which have a non-cosmic shear origin and demonstrate the robustness of our cosmological E-mode analysis as no significant Bmodes are detected. We highlight how COSEBIs are fairly insensitive to the amplitude of the non-linear matter power spectrum at high k-scales, mitigating the uncertain impact of baryon feedback in our analysis. COSEBIs, therefore, allow us to utilise additional small-scale information, improving the DES-Y1 joint constraints on S 8 = σ 8 (Ω m /0.3) 0.5 and Ω m by 20%. Adopting a flat ΛCDM model we find S 8 = 0.755 +0.019 −0.021 , which is in 3.2σ tension with the Planck Legacy analysis of the cosmic microwave background.

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Section: Appendix A: Covariance Of Cosebissupporting

confidence: 90%

KiDS+VIKING-450 and DES-Y1 combined: Mitigating baryon feedback uncertainty with COSEBIs

Asgari

Tröster

Heymans

et al. 2020

A&A

Self Cite

137

130

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“…Here, only helicityzero operators (q = 0) contribute, appearing in kernel forms tr K (3) and Y (0) * 2 .K (3) . As we saw earlier, the reason why only q = 0 terms contribute to (13) term is the coupling of linear with third order perturbations. Given that at linear order only scalar (q = 0) contributions exist, statistical isotropy ensures only q = 0 components survive also in all (13) terms.…”

Section: Bias Degeneracies and Renormalisation Of The One-loop Power mentioning

confidence: 70%

“…We proceed to investigate the (13) contributions to the one-loop power spectra. Here, as discussed earlier, only the q = 0 part contributes and thus we have the density/size and shape auto-and cross-correlations P αβ(0) 00 (13) = 2b…”

Section: One-loop Power Spectrummentioning

confidence: 99%

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An EFT description of galaxy intrinsic alignments

Vlah

Chisari

Schmidt

2020

J. Cosmol. Astropart. Phys.

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146

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We present a general perturbative effective field theory (EFT) description of galaxy shape correlations, which are commonly known as intrinsic alignments. This rigorous approach extends current analytical modelling strategies in that it only relies on the equivalence principle. We present our results in terms of three-dimensional statistics for two-and three-point functions of both galaxy shapes and number counts. In case of the two-point function, we recover the well-known linear alignment result at leading order, but also present the full next-to-leading order expressions. In case of the three-point function we present leading order results for all the auto-and cross-correlations of galaxy shapes and densities. We use a spherical tensor basis to decompose the tensor perturbations in different helicity modes, which allows us to make use of isotropy and parity properties in the correlators. Combined with the results on projection presented in a forthcoming companion paper, our framework is directly applicable to accounting for intrinsic alignment contamination in weak lensing surveys, and to extracting cosmological information from intrinsic alignments. 42A.1 Two-point functions 44 A.2 Three-point functions 47 B Fields in Fourier space 50 B.1 Bias expansion and renormalisation of the one-loop power spectrum 55 B.2 Degeneracy of the bias operators 62 B.3 Bias expansion of the tree-level bispectrum 63 C Bias renormalisation for tensor fields 65 1 Explicitly, we writewhere the Dirac delta function ensures the total momentum conservation, and is a consequence of the statistical translation invariance.

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“…This effect is likely more prominent in redder galaxies, indicating that member galaxies in cluster regimes will be more affected by the IA (e.g. see Singh et al 2015;Samuroff et al 2018;Hikage et al 2019;Johnston et al 2019, for recent observational studies). Unfortunately, it is still difficult to include the IA effect in our halo-model approach in a selfconsistent way.…”

Section: Intrinsic Alignment In Cluster-sized Halosmentioning

confidence: 99%

Probing cosmology and cluster astrophysics with multiwavelength surveys – I. Correlation statistics

Shirasaki

Lau

Nagai

2019

Monthly Notices of the Royal Astronomical Society

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Upcoming multi-wavelength astronomical surveys will soon discover all massive galaxy clusters and provide unprecedented constraints on cosmology and cluster astrophysics. In this paper, we investigate the constraining power of the multi-band cluster surveys, through a joint analysis of three observables associated with clusters of galaxies, including thermal Sunyaev-Zel'dovich (tSZ) effect in cosmic microwave background (CMB), X-ray emission of ionized gas, and gravitational weak lensing effect of background galaxies by the cluster's gravitational potential. We develop a theoretical framework to predict and interpret two-point correlation statistics among the three observables using a semi-analytic model of intracluster medium (ICM) and halo-based approach. In this work, we show that the auto-and cross-angular power spectra in tSZ, X-ray and lensing statistics from upcoming missions (eROSITA, CMB-S4, and LSST) can help break the degeneracy between cosmology and ICM physics. These correlation statistics are less sensitive to selection biases, and are able to probe ICM physics in distant, faint and small clusters that are otherwise difficult to be detected individually. We show that the correlation statistics are able to provide cosmological constraints comparable to the conventional cluster abundance measurements, while constraining cluster astrophysics at the same time. Our results indicate that the correlation statistics can significantly enhance the scientific returns of upcoming multi-wavelength cluster surveys.

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KiDS+GAMA: Intrinsic alignment model constraints for current and future weak lensing cosmology

Cited by 89 publications

References 91 publications

KiDS+VIKING-450 and DES-Y1 combined: Mitigating baryon feedback uncertainty with COSEBIs

KiDS+VIKING-450 and DES-Y1 combined: Mitigating baryon feedback uncertainty with COSEBIs

An EFT description of galaxy intrinsic alignments

Probing cosmology and cluster astrophysics with multiwavelength surveys – I. Correlation statistics

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