KiDS+VIKING-450: Cosmic shear tomography with optical and infrared data

Hildebrandt, Hendrik; Köhlinger, F.; Busch, Jan Luca van den; Joachimi, Benjamin; Heymans, Catherine; Kannawadi, Arun; Wright, Angus H.; Asgari, Marika; Blake, Chris; Hoekstra, Henk; Joudaki, Shahab; Kuijken, Konrad; Miller, L.; Morrison, C. B.; Tröster, Tilman; Amon, A.; Archidiacono, Maria; Brieden, Samuel; Choi, A.; Jong, J. T. A. de; Erben, T.; Giblin, Benjamin; Mead, Alexander; Peacock, J. A.; Radovich, M.; Schneider, Peter; Sifón, Cristobál; Tewes, M.

doi:10.1051/0004-6361/201834878

Cited by 376 publications

(460 citation statements)

References 129 publications

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“…[73,97]; and in our model, increasing ∆N eff comes at the price of introducing DM-DR interaction effects not favoured by the data. In any case we see that the ETHOS n = 4 model offers no clear opportunities to accommodate the high value of H 0 [24] and/or the low value of σ 8 hinted by some datasets [25][26][27].…”

Section: Ethos N = 4 Modelmentioning

confidence: 99%

Constraining Dark Matter-Dark Radiation interactions with CMB, BAO, and Lyman-α

Archidiacono

Hooper

Murgia

et al. 2019

J. Cosmol. Astropart. Phys.

132

168

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Several interesting Dark Matter (DM) models invoke a dark sector leading to two types of relic particles, possibly interacting with each other: non-relativistic DM, and relativistic Dark Radiation (DR). These models have interesting consequences for cosmological observables, and could in principle solve problems like the small-scale cold DM crisis, Hubble tension, and/or low σ 8 value. Their cosmological behaviour is captured by the ETHOS parametrisation, which includes a DR-DM scattering rate scaling like a power-law of the temperature, T n . Scenarios with n = 0, 2, or 4 can easily be realised in concrete dark sector set-ups. Here we update constraints on these three scenarios using recent CMB, BAO, and high-resolution Lyman-α data. We introduce a new Lyman-α likelihood that is applicable to a wide range of cosmological models with a suppression of the matter power spectrum on small scales. For n = 2 and 4, we find that Lyman-α data strengthen the CMB+BAO bounds on the DM-DR interaction rate by many orders of magnitude. However, models offering a possible solution to the missing satellite problem are still compatible with our new bounds. For n = 0, high-resolution Lyman-α data bring no stronger constraints on the interaction rate than CMB+BAO data, except for extremely small values of the DR density. Using CMB+BAO data and a theory-motivated prior on the minimal density of DR, we find that the n = 0 model can reduce the Hubble tension from 4.1σ to 2.7σ, while simultaneously accommodating smaller values of the σ 8 and S 8 parameters hinted by cosmic shear data.

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Section: Ethos N = 4 Modelmentioning

confidence: 99%

Constraining Dark Matter-Dark Radiation interactions with CMB, BAO, and Lyman-α

Archidiacono

Hooper

Murgia

et al. 2019

J. Cosmol. Astropart. Phys.

132

168

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“…Hildebrandt et al 2012;Hoyle et al 2018;Tanaka et al 2018), or (3) direct calibration using spectroscopic redshift training samples (see e.g. Lima et al 2008;Hildebrandt et al 2017Hildebrandt et al , 2020Buchs et al 2019;Wright et al 2020). More recently, however, steps have been taken towards constructing a fourth, hybrid category which leverages both cross-correlation and direct calibration (Rau et al 2019;Sánchez & Bernstein 2018;Alarcon et al 2019).…”

Section: Introductionmentioning

confidence: 99%

KiDS+VIKING-450: Improved cosmological parameter constraints from redshift calibration with self-organising maps

Wright

Hildebrandt

Busch

et al. 2020

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We present updated cosmological constraints for the KiDS+VIKING-450 cosmic shear data set (KV450) estimated through redshift distributions and photometric samples defined using self-organising maps (SOMs). Our fiducial analysis finds marginal posterior constraints of S8 ≡ σ8 Ωm/0.3 = 0.716−0.038+0.043, which are smaller but otherwise consistent with previous works that have applied this data set (|ΔS8| = 0.023). We analysed additional samples and redshift distributions set up in three ways: (1) by excluding certain spectroscopic surveys during redshift calibration; (2) by excluding lower-confidence spectroscopic redshifts in redshift calibration; and (3) by considering only those photometric sources which are jointly calibrated by at least three spectroscopic surveys. In all cases, the method utilised here has been proven to be robust: we find a maximal deviation from our fiducial analysis of |ΔS8| ≤ 0.011 for all samples defined and analysed using our SOM. To demonstrate the reduction in systematic biases found within our analysis, we highlight our results when performing redshift calibration without the DEEP2 spectroscopic data set. In this case, we find marginal posterior constraints of S8 = 0.707−0.042+0.046; this is a difference, with respect to the fiducial, that is both significantly smaller and in the opposite direction with regard to the equivalent shift from previous works. These results suggest that our improved cosmological parameter estimates are not sensitive to pathological misrepresentations of photometric sources by the spectroscopy used for direct redshift calibration and, therefore, that this systematic effect cannot be responsible for the observed difference between S8 estimates made with KV450 and Planck CMB probes.

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“…This discrepancy is particularly challenging given that the lensing signal obtained from the Planck angular trispectrum is consistent with the standard cosmology [1]. Furthermore, a 2σ difference in the Ω m − σ 8 plane can be inferred by comparing CMB and cosmic shear data [4] (see also [5]), where Ω m is the matter density parameter and σ 8 is the matter fluctuation amplitude on scales of 8h −1 Mpc. Currently, one of the main arguments is that such discrepancies may be an indication of new physics beyond ΛCDM, and many analyses have investigated alternative scenarios that could reconcile the data sets.…”

Section: Introductionmentioning

confidence: 99%

Looking for interactions in the cosmological dark sector

Benetti

Miranda

Borges

et al. 2019

J. Cosmol. Astropart. Phys.

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We study observational signatures of non-gravitational interactions between the dark components of the cosmic fluid, which can be either due to creation of dark particles from the expanding vacuum or an effect of the clustering of a dynamical dark energy. In particular, we analyse a class of interacting models (Λ(t)CDM), characterised by the parameter α, that behaves at background level like cold matter at early times and tends to a cosmological constant in the asymptotic future. In our analysis we consider both background and primordial perturbations evolutions of the model. We use Cosmic Microwave Background (CMB) data together with late time observations, such as the Joint Light-curve Analysis (JLA) supernovae data, the Hubble Space Telescope (HST) measurement of the local value of the Hubble-Lemaître parameter, and primordial deuterium abundance from Lyα systems to test the observational viability of the model and some of its extensions. We found that there is no preference for values of α different from zero (characterising interaction), even if there are some indications for positive values when the minimal Λ(t)CDM model is analysed. When extra degrees of freedom in the relativistic component of the cosmic fluid are considered, the data favour negative values of α, which means an energy flux from dark energy to dark matter. * When non-linear scales are included, one finds Ωm0 ≈ 0.29 [36,37].

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KiDS+VIKING-450: Cosmic shear tomography with optical and infrared data

Cited by 376 publications

References 129 publications

Constraining Dark Matter-Dark Radiation interactions with CMB, BAO, and Lyman-α

Constraining Dark Matter-Dark Radiation interactions with CMB, BAO, and Lyman-α

KiDS+VIKING-450: Improved cosmological parameter constraints from redshift calibration with self-organising maps

Looking for interactions in the cosmological dark sector

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