KiDS+VIKING-450 and DES-Y1 combined: Cosmology with cosmic shear


S Joudaki, H Hildebrandt, D Traykova, N Chisari, C Heymans, A Kannawadi, K Kuijken, A Wright, M Asgari, T Erben, H Hoekstra, B Joachimi, L Miller, T Tröster, JLVD Busch

We present a combined tomographic weak gravitational lensing analysis of the Kilo Degree Survey (KV450) and the Dark Energy Survey (DES-Y1). We homogenize the analysis of these two public cosmic shear datasets by adopting consistent priors and modeling of nonlinear scales, and determine new redshift distributions for DES-Y1 based on deep public spectroscopic surveys. Adopting these revised redshifts results in a $0.8 \sigma$ reduction in the DES-inferred value for $S_8$. The combined KV450 + DES-Y1 constraint on $S_8 = 0.762^{+0.025}_{-0.024}$ is in tension with the Planck 2018 constraint from the cosmic microwave background at the level of $2.5\sigma$. This result highlights the importance of developing methods to provide accurate redshift calibration for current and future weak lensing surveys.

Euclid preparation: VI. Verifying the Performance of Cosmic Shear Experiments


H Aussel, I Conti, N Auricchio, M Baldi, S Bardelli, A Biviano, D Bonino, E Borsato, E Bozzo, E Branchini, S Brau-Nogue, M Brescia, J Brinchmann, C Burigana, S Camera, V Capobianco, C Carbone, J Carretero, F Castander, M Castellano, S Cavuoti, R Cledassou, C Colodro-Conde, G Congedo, C Conselice

Our aim is to quantify the impact of systematic effects on the inference of cosmological parameters from cosmic shear. We present an end-to-end approach that introduces sources of bias in a modelled weak lensing survey on a galaxy-by-galaxy level. Residual biases are propagated through a pipeline from galaxy properties (one end) through to cosmic shear power spectra and cosmological parameter estimates (the other end), to quantify how imperfect knowledge of the pipeline changes the maximum likelihood values of dark energy parameters. We quantify the impact of an imperfect correction for charge transfer inefficiency (CTI) and modelling uncertainties of the point spread function (PSF) for Euclid, and find that the biases introduced can be corrected to acceptable levels.

GAMA+KiDS: Alignment of galaxies in galaxy groups and its dependence on galaxy scale

Astronomy & Astrophysics EDP Sciences (0)

C Georgiou, NE Chisari, MC Fortuna, H Hoekstra, K Kuijken, B Joachimi, M Vakili, M Bilicki, A Dvornik, T Erben, B Giblin, C Heymans, NR Napolitano, H Shan

The fourth data release of the Kilo-Degree Survey: ugri imaging and nine-band optical-IR photometry over 1000 square degrees


K Kuijken, C Heymans, A Dvornik, H Hildebrandt, JTAD Jong, AH Wright, T Erben, M Bilicki, B Giblin, H-Y Shan, F Getman, A Grado, H Hoekstra, LANCE Miller, N Napolitano, M Paolilo, M Radovich, P Schneider, W Sutherland, M Tewes, C Tortora, EA Valentijn, GAV Kleijn

The Kilo-Degree Survey (KiDS) is an ongoing optical wide-field imaging survey with the OmegaCAM camera at the VLT Survey Telescope, specifically designed for measuring weak gravitational lensing by galaxies and large-scale structure. When completed it will consist of 1350 square degrees imaged in four filters (ugri). Here we present the fourth public data release which more than doubles the area of sky covered by data release 3. We also include aperture-matched ZYJHKs photometry from our partner VIKING survey on the VISTA telescope in the photometry catalogue. We illustrate the data quality and describe the catalogue content. Two dedicated pipelines are used for the production of the optical data. The Astro-WISE information system is used for the production of co-added images in the four survey bands, while a separate reduction of the r-band images using the theli pipeline is used to provide a source catalogue suitable for the core weak lensing science case. All data have been re-reduced for this data release using the latest versions of the pipelines. The VIKING photometry is obtained as forced photometry on the theli sources, using a re-reduction of the VIKING data that starts from the VISTA pawprints. Modifications to the pipelines with respect to earlier releases are described in detail. The photometry is calibrated to the Gaia DR2 G band using stellar locus regression. In this data release a total of 1006 square-degree survey tiles with stacked ugri images are made available, accompanied by weight maps, masks, and single-band source lists. We also provide a multi-band catalogue based on r-band detections, including homogenized photometry and photometric redshifts, for the whole dataset. Mean limiting magnitudes (5 sigma in a 2" aperture) are 24.23, 25.12, 25.02, 23.68 in ugri, respectively, and the mean r-band seeing is 0.70".

Weak lensing in the Horizon-AGN simulation lightcone. Small scale baryonic effects


C Gouin, R Gavazzi, C Pichon, Y Dubois, C Laigle, NE Chisari, S Codis, JULIEN Devriendt, S Peirani

Context. Accurate model predictions including the physics of baryons are required to make the most of the upcoming large cosmological surveys devoted to gravitational lensing. The advent of hydrodynamical cosmological simulations enables such predictions on sufficiently sizeable volumes. Aims. Lensing quantities (deflection, shear, convergence) and their statistics (convergence power spectrum, shear correlation functions, galaxy-galaxy lensing) are computed in the past lightcone built in the Horizon-AGN hydrodynamical cosmological simulation, which implements our best knowledge on baryonic physics at the galaxy scale in order to mimic galaxy populations over cosmic time. Methods. Lensing quantities are generated over a one square degree field of view by performing multiple-lens plane ray-tracing through the lightcone, taking full advantage of the 1 kpc resolution and splitting the line of sight over 500 planes all the way to redshift z~7. Two methods are explored (standard projection of particles with adaptive smoothing, and integration of the acceleration field) to assert a good implementation. The focus is on small scales where baryons matter most. Results. Standard cosmic shear statistics are impacted at the 10% level by the baryonic component for angular scales below a few arcmin. The galaxy-galaxy lensing signal, or galaxy-shear correlation function, is consistent with measurements for the redshift z~0.5 massive galaxy population. At higher redshift z>1, the impact of magnification bias on this correlation is relevant for separations greater than 1 Mpc. Conclusions. This work is pivotal for all current and upcoming weak lensing surveys and represents a first step towards building a full end-to-end generation of lensed mock images from large cosmological hydrodynamical simulations.

Modelling baryonic feedback for survey cosmology

Open Journal of Astrophysics (0)

NE Chisari, AJ Mead, S Joudaki, P Ferreira, A Schneider, J Mohr, T Tröster, D Alonso, IG McCarthy, S Martin-Alvarez, J Devriendt, A Slyz, MPV Daalen

Observational cosmology in the next decade will rely on probes of the distribution of matter in the redshift range between $0<z<3$ to elucidate the nature of dark matter and dark energy. In this redshift range, galaxy formation is known to have a significant impact on observables such as two-point correlations of galaxy shapes and positions, altering their amplitude and scale dependence beyond the expected statistical uncertainty of upcoming experiments at separations under 10 Mpc. Successful extraction of information in such a regime thus requires, at the very least, unbiased models for the impact of galaxy formation on the matter distribution, and can benefit from complementary observational priors. This work reviews the current state of the art in the modelling of baryons for cosmology, from numerical methods to approximate analytical prescriptions, and makes recommendations for studies in the next decade, including a discussion of potential probe combinations that can help constrain the role of baryons in cosmological studies. We focus, in particular, on the modelling of the matter power spectrum, $P(k,z)$, as a function of scale and redshift, and of the observables derived from this quantity. This work is the result of a workshop held at the University of Oxford in November of 2018.

The impact of baryons on the matter power spectrum from the Horizon-AGN cosmological hydrodynamical simulation


NE Chisari, MLA Richardson, J Devriendt, Y Dubois, A Schneider, AMCL Brun, RS Beckmann, S Peirani, A Slyz, C Pichon

Accurate cosmology from upcoming weak lensing surveys relies on knowledge of the total matter power spectrum at percent level at scales $k &lt; 10$ $h$/Mpc, for which modelling the impact of baryonic physics is crucial. We compare measurements of the total matter power spectrum from the Horizon cosmological hydrodynamical simulations: a dark matter-only run, one with full baryonic physics, and another lacking Active Galactic Nuclei (AGN) feedback. Baryons cause a suppression of power at $k\simeq 10$ $h/$Mpc of $&lt;15\%$ at $z=0$, and an enhancement of a factor of a few at smaller scales due to the more efficient cooling and star formation. The results are sensitive to the presence of the highest mass haloes in the simulation and the distribution of dark matter is also impacted up to a few percent. The redshift evolution of the effect is non-monotonic throughout $z=0-5$ due to an interplay between AGN feedback and gas pressure, and the growth of structure. We investigate the effectiveness of the "baryonic correction model" proposed by Schneider &amp; Teyssier (2015) in describing our results. We require a different redshift evolution and propose an alternative fitting function with $4$ free parameters that reproduces our results within $5\%$. Compared to other simulations, we find the impact of baryonic processes on the total matter power spectrum to be smaller at $z=0$. Nevertheless, our results also suggest that AGN feedback is not strong enough in the simulation. Total matter power spectra from the Horizon simulations are made publicly available at

Cosmological Simulations for Combined-Probe Analyses: Covariance and Neighbour-Exclusion Bias


J Harnois-Deraps, A Amon, A Choi, V Demchenko, C Heymans, A Kannawadi, R Nakajima, E Sirks, LV Waerbeke, Y-C Cai, B Giblin, H Hildebrandt, H Hoekstra, L Miller, T Troester

We present a public suite of weak lensing mock data, extending the Scinet Light Cone Simulations (SLICS) to simulate cross-correlation analyses with different cosmological probes. These mocks include KiDS-450- and LSST-like lensing data, cosmic microwave background lensing maps and simulated spectroscopic surveys that emulate the GAMA, BOSS and 2dFLenS galaxy surveys. With 817 independent realisations, our mocks are optimised for combined-probe covariance estimation, which we illustrate for the case of a joint measurement involving cosmic shear, galaxy-galaxy lensing and galaxy clustering from KiDS-450 and BOSS data. With their high spatial resolution, the SLICS are also optimal for predicting the signal for novel lensing estimators, for the validation of analysis pipelines, and for testing a range of systematic effects such as the impact of neighbour-exclusion bias on the measured tomographic cosmic shear signal. For surveys like KiDS and DES, where the rejection of neighbouring galaxies occurs within ~2 arcseconds, we show that the measured cosmic shear signal will be biased low, but by less than a percent on the angular scales that are typically used in cosmic shear analyses. The amplitude of the neighbour-exclusion bias doubles in deeper, LSST-like data. The simulation products described in this paper are made available at

Redshift and luminosity evolution of the intrinsic alignments of galaxies in Horizon-AGN

ArXiv (0)

NE Chisari, C Laigle, S Codis, Y Dubois, J Devriendt, L Miller, K Benabed, A Slyz, R Gavazzi, C Pichon

Intrinsic galaxy shape and angular momentum alignments can arise in cosmological large-scale structure due to tidal interactions or galaxy formation processes. Cosmological hydrodynamical simulations have recently come of age as a tool to study these alignments and their contamination to weak gravitational lensing. We probe the redshift and luminosity evolution of intrinsic alignments in Horizon-AGN between z=0 and z=3 for galaxies with an r-band absolute magnitude of <-20. Alignments transition from being radial at low redshifts and high luminosities, dominated by the contribution of ellipticals, to being tangential at high redshift and low luminosities, where discs dominate the signal. This cannot be explained by the evolution of the fraction of ellipticals and discs alone: intrinsic evolution in the amplitude of alignments is necessary. The alignment amplitude of elliptical galaxies alone is smaller in amplitude by a factor of ~2, but has similar luminosity and redshift evolution as in current observations and in the nonlinear tidal alignment model at projected separations of > 1 Mpc. Alignments of discs are null in projection and consistent with current low redshift observations. The combination of the two populations yields an overall amplitude a factor of ~4 lower than observed alignments of luminous red galaxies with a steeper luminosity dependence. The restriction on accurate galaxy shapes implies that the galaxy population in the simulation is complete only to an r-band absolute magnitude of <-20. Higher resolution simulations will be necessary to avoid extrapolation of the intrinsic alignment predictions to the range of luminosities probed by future surveys.


The Astrophysical Journal IOP Publishing 807 (0) 22-22

S Miyazaki, M Oguri, T Hamana, M Tanaka, L Miller, Y Utsumi, Y Komiyama, H Furusawa, J Sakurai, S Kawanomoto, F Nakata, F Uraguchi, M Koike, D Tomono, R Lupton, JE Gunn, H Karoji, H Aihara, H Murayama, M Takada

The impact of high spatial frequency atmospheric distortions on weak lensing measurements

ArXiv (0)

C Heymans, B Rowe, H Hoekstra, L Miller, T Erben, T Kitching, LV Waerbeke

High precision cosmology with weak gravitational lensing requires a precise measure of the Point Spread Function across the imaging data where the accuracy to which high spatial frequency variation can be modelled is limited by the stellar number density across the field. We analyse dense stellar fields imaged at the Canada-France-Hawaii Telescope to quantify the degree of high spatial frequency variation in ground-based imaging Point Spread Functions and compare our results to models of atmospheric turbulence. The data shows an anisotropic turbulence pattern with an orientation independent of the wind direction and wind speed. We find the amplitude of the high spatial frequencies to decrease with increasing exposure time as $t^{-1/2}$, and find a negligibly small atmospheric contribution to the Point Spread Function ellipticity variation for exposure times $t>180$ seconds. For future surveys analysing shorter exposure data, this anisotropic turbulence will need to be taken into account as the amplitude of the correlated atmospheric distortions becomes comparable to a cosmological lensing signal on scales less than $\sim 10$ arcminutes. This effect could be mitigated, however, by correlating galaxy shear measured on exposures imaged with a time separation greater than 50 seconds, for which we find the spatial turbulence patterns to be uncorrelated.

Euclid Definition Study Report

ArXiv (0)

R Laureijs, J Amiaux, S Arduini, J-L Auguères, J Brinchmann, R Cole, M Cropper, C Dabin, L Duvet, A Ealet, B Garilli, P Gondoin, L Guzzo, J Hoar, H Hoekstra, R Holmes, T Kitching, T Maciaszek, Y Mellier, F Pasian, W Percival, J Rhodes, GS Criado, M Sauvage, R Scaramella, L Valenziano, S Warren, R Bender, F Castander, A Cimatti, OL Fèvre, H Kurki-Suonio, M Levi, P Lilje, G Meylan, R Nichol, K Pedersen, V Popa, RR Lopez, H-W Rix, H Rottgering, W Zeilinger, F Grupp, P Hudelot, R Massey, M Meneghetti, L Miller, S Paltani, S Paulin-Henriksson, S Pires, C Saxton, T Schrabback, G Seidel, J Walsh, N Aghanim, L Amendola, J Bartlett, C Baccigalupi, J-P Beaulieu, K Benabed, J-G Cuby, D Elbaz, P Fosalba, G Gavazzi, A Helmi, I Hook, M Irwin, J-P Kneib, M Kunz, F Mannucci, L Moscardini, C Tao, R Teyssier, J Weller, G Zamorani, MRZ Osorio, O Boulade, JJ Foumond, AD Giorgio, P Guttridge, A James, M Kemp, J Martignac, A Spencer, D Walton, T Blümchen, C Bonoli, F Bortoletto, C Cerna, L Corcione, C Fabron, K Jahnke, S Ligori, F Madrid, L Martin, G Morgante, T Pamplona, E Prieto, M Riva, R Toledo, M Trifoglio, F Zerbi, F Abdalla, M Douspis, C Grenet, S Borgani, R Bouwens, F Courbin, J-M Delouis, P Dubath, A Fontana, M Frailis, A Grazian, J Koppenhöfer, O Mansutti, M Melchior, M Mignoli, J Mohr, C Neissner, K Noddle, M Poncet, M Scodeggio, S Serrano, N Shane, J-L Starck, C Surace, A Taylor, G Verdoes-Kleijn, C Vuerli, OR Williams, A Zacchei, B Altieri, IE Sanz, R Kohley, T Oosterbroek, P Astier, D Bacon, S Bardelli, C Baugh, F Bellagamba, C Benoist, D Bianchi, A Biviano, E Branchini, C Carbone, V Cardone, D Clements, S Colombi, C Conselice, G Cresci, N Deacon, J Dunlop, C Fedeli, F Fontanot, P Franzetti, C Giocoli, J Garcia-Bellido, J Gow, A Heavens, P Hewett, C Heymans, A Holland, Z Huang, O Ilbert, B Joachimi, E Jennins, E Kerins, A Kiessling, D Kirk, R Kotak, O Krause, O Lahav, FV Leeuwen, J Lesgourgues, M Lombardi, M Magliocchetti, K Maguire, E Majerotto, R Maoli, F Marulli, S Maurogordato, H McCracken, R McLure, A Melchiorri, A Merson, M Moresco, M Nonino, P Norberg, J Peacock, R Pello, M Penny, V Pettorino, CD Porto, L Pozzetti, C Quercellini, M Radovich, A Rassat, N Roche, S Ronayette, E Rossetti, B Sartoris, P Schneider, E Semboloni, S Serjeant, F Simpson, C Skordis, G Smadja, S Smartt, P Spano, S Spiro, M Sullivan, A Tilquin, R Trotta, L Verde, Y Wang, G Williger, G Zhao, J Zoubian, E Zucca

Euclid is a space-based survey mission from the European Space Agency designed to understand the origin of the Universe's accelerating expansion. It will use cosmological probes to investigate the nature of dark energy, dark matter and gravity by tracking their observational signatures on the geometry of the universe and on the cosmic history of structure formation. The mission is optimised for two independent primary cosmological probes: Weak gravitational Lensing (WL) and Baryonic Acoustic Oscillations (BAO). The Euclid payload consists of a 1.2 m Korsch telescope designed to provide a large field of view. It carries two instruments with a common field-of-view of ~0.54 deg2: the visual imager (VIS) and the near infrared instrument (NISP) which contains a slitless spectrometer and a three bands photometer. The Euclid wide survey will cover 15,000 deg2 of the extragalactic sky and is complemented by two 20 deg2 deep fields. For WL, Euclid measures the shapes of 30-40 resolved galaxies per arcmin2 in one broad visible R+I+Z band (550-920 nm). The photometric redshifts for these galaxies reach a precision of dz/(1+z) < 0.05. They are derived from three additional Euclid NIR bands (Y, J, H in the range 0.92-2.0 micron), complemented by ground based photometry in visible bands derived from public data or through engaged collaborations. The BAO are determined from a spectroscopic survey with a redshift accuracy dz/(1+z) =0.001. The slitless spectrometer, with spectral resolution ~250, predominantly detects Ha emission line galaxies. Euclid is a Medium Class mission of the ESA Cosmic Vision 2015-2025 programme, with a foreseen launch date in 2019. This report (also known as the Euclid Red Book) describes the outcome of the Phase A study.

Bayesian Photometric Redshifts for Weak Lensing Applications

ArXiv (0)

E Edmondson, L Miller, C Wolf

The next generation of weak gravitational lensing surveys is capable of generating good measurements of cosmological parameters, provided that, amongst other requirements, adequate redshift information is available for the background galaxies that are measured. It is frequently assumed that photometric redshift techniques provide the means to achieve this. Here we compare Bayesian and frequentist approaches to photometric redshift estimation, particularly at faint magnitudes. We identify and discuss the biases that are inherent in the various methods, and describe an optimum Bayesian method for extracting redshift distributions from photometric data.

Clusters, brightest cluster galaxies and galaxy alignments


N Chisari

This thesis develops two main topics related to the study of the large-scale structure of the Universe. The first one is the intrinsic alignment of galaxies. These are correlations between the shapes and orientations of galaxies that arise mainly as a consequence of tidal forces across a large range of scales. I use the tidal alignment model to predict how the intrinsic alignment of Luminous Red Galaxies could in the future provide constraints on the Baryon Acoustic Oscillation scale, a standard ruler for measuring the expansion of the Universe. I also show that primordial signatures of inflation can translate into a non-Gaussian bias in the correlation of the intrinsic shapes of galaxies, which could be observed with future surveys. The second main topic discussed in this thesis is clusters of galaxies. I use data from the Sloan Digital Sky Survey and a public catalog of galaxy clusters to estimate the alignment of galaxies around groups and clusters of galaxies. The novelty of this work is mainly in the method for estimating the alignment signal. In photometric surveys, the redshift uncertainty is large compared to the size of a cluster, making the distinction between galaxies in the cluster and in the background very challenging. In the method developed here, each galaxy is assigned a posterior probability distribution function of its redshift to separate the alignment component from the gravitational lensing of galaxies in the background. Among the galaxies that make up a cluster, Brightest Cluster Galaxies stand out by their luminosity. I study the connection between these galaxies and other ellipticals to understand the physics of their formation. Finally, I re-develop the Adaptive Matched Filter method for finding clusters in spectroscopic and photometric surveys to include a new treatment of the distances to galaxies. Again, I model the distance to each galaxy using a redshift posterior and propose other modifications to the algorithm that will be of use to upcoming photometric surveys.

The environment of long gamma-ray burst host galaxies

Boletín de la Asociación Argentina de Astronomía 51 (0) 243-246

N Chisari, M Mayochi, L Pellizza

The study of the properties of long gamma-ray burst host galaxies and their environment could shed light onto the problem of the nature of the stellar progenitors of these high-energy phenomena. In this paper we present preliminary results of an investigation of the host environment of 8 long gamma-ray bursts, that suggest that these phenomena occur in field galaxies.

Separated flow behavior in an in-vitro rigid model of the laryngeal channel

Journal of the Acoustical Society of America 123 (0) 3577-3577

D Sciamarella, N Chisari, G Artana, L Bailly, X Pelorson

RCSLenS: Cosmic Distances from Weak Lensing

ArXiv (0)

TD Kitching, M Viola, H Hildebrandt, A Choi, T Erben, DG Gilbank, C Heymans, L Miller, R Nakajima, EV Uitert

In this paper we present results of applying the shear-ratio method to the RCSLenS data. The method takes the ratio of the mean of the weak lensing tangential shear signal about galaxy clusters, averaged over all clusters of the same redshift, in multiple background redshift bins. In taking a ratio the mass-dependency of the shear signal is cancelled-out leaving a statistic that is dependent on the geometric part of the lensing kernel only. We apply this method to 535 clusters and measure a cosmology-independent distance-redshift relation to redshifts z~1. In combination with Planck data the method lifts the degeneracies in the CMB measurements, resulting in cosmological parameter constraints of OmegaM=0.31 +/- 0.10 and w0 = -1.02 +/- 0.37, for a flat wCDM cosmology.