363 research outputs found
Non-linear shrinkage estimation of large-scale structure covariance
In many astrophysical settings, covariance matrices of large data sets have to be determined empirically from a finite number of mock realizations. The resulting noise degrades inference and precludes it completely if there are fewer realizations than data points. This work applies a recently proposed non-linear shrinkage estimator of covariance to a realistic example from large-scale structure cosmology. After optimizing its performance for the usage in likelihood expressions, the shrinkage estimator yields subdominant bias and variance comparable to that of the standard estimator with a factor of ∼50 less realizations. This is achieved without any prior information on the properties of the data or the structure of the covariance matrix, at a negligible computational cost
Relations between three-point configuration space shear and convergence statistics
With the growing interest in and ability of using weak lensing studies to
probe the non-Gaussian properties of the matter density field, there is an
increasing need for the study of suitable statistical measures, e.g. shear
three-point statistics. In this paper we establish the relations between the
three-point configuration space shear and convergence statistics, which are an
important missing link between different weak lensing three-point statistics
and provide an alternative way of relating observation and theory. The method
we use also allows us to derive the relations between other two- and
three-point correlation functions. We show the consistency of the relations
obtained with already established results and demonstrate how they can be
evaluated numerically. As a direct application, we use these relations to
formulate the condition for E/B-mode decomposition of lensing three-point
statistics, which is the basis for constructing new three-point statistics
which allow for exact E/B-mode separation. Our work applies also to other
two-dimensional polarization fields such as that of the Cosmic Microwave
Background.Comment: 17 pages, 5 figures, submitted to A&
Euclid - an ESA Medium Class Mission
Euclid is an ESA Medium Class mission in the Cosmic Visions program
to be launched in 2020. With its 1.2 m telescope, Euclid is going to survey 15, 000 deg2
of extragalactic sky in a broad optical band with outstanding image quality fit for weak
gravitational lensing measurements. It will also provide near-infrared slitless spectroscopy
of more than 107
emission-line galaxies with the main goal of measuring
galaxy clustering. Imaging in three near-infrared bands by Euclid will be complemented
by ground-based follow-up in optical bands to supply high-quality photometric redshift
estimates out to z = 2. In combination, its primary cosmological science drivers, weak
gravitational lensing and galaxy clustering, will yield unprecedented constraints on the
properties of dark matter and dark energy, as well as the validity of Einstein gravity on
large scales. Euclid’s rich datasets will facilitate further cosmological probes such as
statistics of galaxy clusters or the study of galactic dark matter haloes, and a vast array
of legacy science. In the following a brief overview on the Euclid mission and its key
science is provided
Characterising improvements in photometric redshift probability density functions with galaxy morphology
In this work, we studied the impact of galaxy morphology on photometric redshift (photo-z) probability density functions (PDFs). By including galaxy morphological parameters like the radius, axis-ratio, surface brightness and the Sérsic index in addition to the ugriz broadbands as input parameters, we used the machine learning photo-z algorithm ANNZ2 to train and test on galaxies from the Canada-France-Hawaii Telescope Stripe-82 (CS82) Survey. Metrics like the continuous ranked probability score (CRPS), probability integral transform (PIT), Bayesian odds parameter, and even the width and height of the PDFs were evaluated, and the results were compared when different number of input parameters were used during the training process. We find improvements in the CRPS and width of the PDFs when galaxy morphology has been added to the training, and the improvement is larger especially when the number of broadband magnitudes are lacking
Intrinsic alignment of redMaPPer clusters: cluster shape-matter density correlation
We measure the alignment of the shapes of galaxy clusters, as traced by their satellite distributions, with the matter density field using the public redMaPPer catalogue based on Sloan Digital Sky Survey–Data Release 8 (SDSS-DR8), which contains 26 111 clusters up to z ∼ 0.6. The clusters are split into nine redshift and richness samples; in each of them, we detect a positive alignment, showing that clusters point towards density peaks. We interpret the measurements within the tidal alignment paradigm, allowing for a richness and redshift dependence. The intrinsic alignment (IA) amplitude at the pivot redshift z = 0.3 and pivot richness λ = 30 is
AgenIA=12.6+1.5−1.2
AIAgen=12.6−1.2+1.5
. We obtain tentative evidence that the signal increases towards higher richness and lower redshift. Our measurements agree well with results of maxBCG clusters and with dark-matter-only simulations. Comparing our results to the IA measurements of luminous red galaxies, we find that the IA amplitude of galaxy clusters forms a smooth extension towards higher mass. This suggests that these systems share a common alignment mechanism, which can be exploited to improve our physical understanding of IA
Self-calibration of weak lensing systematic effects using combined two- and three-point statistics
We investigate the prospects for using the weak lensing bispectrum alongside the power spectrum to control systematic uncertainties in a Euclid-like survey. Three systematic effects are considered: the intrinsic alignment of galaxies, uncertainties in the means of tomographic redshift distributions, and multiplicative bias in the measurement of the shear signal. We find that the bispectrum is very effective in mitigating these systematic errors. Varying all three systematics simultaneously, a joint power spectrum and bispectrum analysis reduces the area of credible regions for the cosmological parameters Ω_{m} and σ_{8} by a factor of 90 and for the two parameters of a time-varying dark energy equation of state by a factor of almost 20, compared with the baseline approach of using the power spectrum alone and of imposing priors consistent with the accuracy requirements specified for Euclid. We also demonstrate that including the bispectrum self-calibrates all three systematic effects to the stringent levels required by the forthcoming generation of weak lensing surveys, thereby reducing the need for external calibration data
Cross correlation surveys with the Square Kilometre Array
By the time that the first phase of the Square Kilometre Array is deployed it
will be able to perform state of the art Large Scale Structure (LSS) as well as
Weak Gravitational Lensing (WGL) measurements of the distribution of matter in
the Universe. In this chapter we concentrate on the synergies that result from
cross-correlating these different SKA data products as well as external
correlation with the weak lensing measurements available from CMB missions. We
show that the Dark Energy figures of merit obtained individually from WGL/LSS
measurements and their independent combination is significantly increased when
their full cross-correlations are taken into account. This is due to the
increased knowledge of galaxy bias as a function of redshift as well as the
extra information from the different cosmological dependences of the
cross-correlations. We show that the cross-correlation between a spectroscopic
LSS sample and a weak lensing sample with photometric redshifts can calibrate
these same photometric redshifts, and their scatter, to high accuracy by
modelling them as nuisance parameters and fitting them simultaneously
cosmology. Finally we show that Modified Gravity parameters are greatly
constrained by this cross-correlations because weak lensing and redshift space
distortions (from the LSS survey) break strong degeneracies in common
parameterisations of modified gravity.Comment: 12 pages, 3 figures. This article is part of the 'Cosmology Chapter,
Advancing Astrophysics with the SKA (AASKA14) Conference, Giardini Naxos
(Italy), June 9th-13th 2014
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