Euclid: Reconstruction of Weak Lensing mass maps for non-Gaussianity studies. (arXiv:1910.03106v1 [astro-ph.CO])

Euclid: Reconstruction of Weak Lensing mass maps for non-Gaussianity studies. (arXiv:1910.03106v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Pires_S/0/1/0/all/0/1">S. Pires</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vandenbussche_V/0/1/0/all/0/1">V. Vandenbussche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kansal_V/0/1/0/all/0/1">V. Kansal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bender_R/0/1/0/all/0/1">R. Bender</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonino_D/0/1/0/all/0/1">D. Bonino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boucaud_A/0/1/0/all/0/1">A. Boucaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brinchmann_J/0/1/0/all/0/1">J. Brinchmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capobianco_V/0/1/0/all/0/1">V. Capobianco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">J. Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castellano_M/0/1/0/all/0/1">M. Castellano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cavuoti_S/0/1/0/all/0/1">S. Cavuoti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cledassou_R/0/1/0/all/0/1">R. Cl&#xe9;dassou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Congedo_G/0/1/0/all/0/1">G. Congedo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conversi_L/0/1/0/all/0/1">L. Conversi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Corcione_L/0/1/0/all/0/1">L. Corcione</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dubath_F/0/1/0/all/0/1">F. Dubath</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frailis_M/0/1/0/all/0/1">M. Frailis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franceschi_E/0/1/0/all/0/1">E. Franceschi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fumana_M/0/1/0/all/0/1">M. Fumana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grupp_F/0/1/0/all/0/1">F. Grupp</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hormuth_F/0/1/0/all/0/1">F. Hormuth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kermiche_S/0/1/0/all/0/1">S. Kermiche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohley_R/0/1/0/all/0/1">R. Kohley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kubik_B/0/1/0/all/0/1">B. Kubik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kunz_M/0/1/0/all/0/1">M. Kunz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ligori_S/0/1/0/all/0/1">S. Ligori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lilje_P/0/1/0/all/0/1">P.B. Lilje</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lloro_I/0/1/0/all/0/1">I. Lloro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maiorano_E/0/1/0/all/0/1">E. Maiorano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marggraf_O/0/1/0/all/0/1">O. Marggraf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Massey_R/0/1/0/all/0/1">R. Massey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meylan_G/0/1/0/all/0/1">G. Meylan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padilla_C/0/1/0/all/0/1">C. Padilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paltani_S/0/1/0/all/0/1">S. Paltani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pasian_F/0/1/0/all/0/1">F. Pasian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poncet_M/0/1/0/all/0/1">M. Poncet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raison_F/0/1/0/all/0/1">F. Raison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rhodes_J/0/1/0/all/0/1">J. Rhodes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roncarelli_M/0/1/0/all/0/1">M. Roncarelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saglia_R/0/1/0/all/0/1">R. Saglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_P/0/1/0/all/0/1">P. Schneider</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Secroun_A/0/1/0/all/0/1">A. Secroun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serrano_S/0/1/0/all/0/1">S. Serrano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tereno_I/0/1/0/all/0/1">I. Tereno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toledo_Moreo_R/0/1/0/all/0/1">R. Toledo-Moreo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Y/0/1/0/all/0/1">Y. Wang</a>

Weak lensing has proven to be an efficient method to constrain models of
structure formation and reveal the nature of dark energy. So far, most weak
lensing studies have focused on the shear field that can be measured directly
from the ellipticity of background galaxies. However, within the context of
forthcoming full-sky weak lensing surveys such as Euclid, convergence maps
offer an important advantage over shear fields in terms of cosmological
exploitation. While carrying the same information, the lensing signal is more
compressed in the convergence maps than in the shear field, simplifying
otherwise computationally expensive analyses, for instance non-Gaussianity
studies. However, the inversion of the non-local shear field requires accurate
control of systematic effects due to holes in the data field, field borders,
noise and the fact that the shear is not a direct observable (reduced shear).
In this paper, we present the two mass inversion methods that are being
included in the official Euclid data processing pipeline: the standard Kaiser &
Squires method (KS) and a new mass inversion method (KS+) that aims to reduce
the information loss during the mass inversion. This new method is based on the
KS methodology and includes corrections for mass mapping systematic effects.
The results of the KS+ method are compared to the original implementation of
the KS method in its simplest form, using the Euclid Flagship mock galaxy
catalogue. In particular, we estimate the quality of the reconstruction by
comparing the two-point correlation functions, third- and fourth-order moments
obtained from shear and convergence maps, and we analyse each systematic effect
independently and simultaneously. We show that the KS+ method reduces
substantially the errors on the two-point correlation function and moments
compared to the KS method. In particular, we show…

Weak lensing has proven to be an efficient method to constrain models of
structure formation and reveal the nature of dark energy. So far, most weak
lensing studies have focused on the shear field that can be measured directly
from the ellipticity of background galaxies. However, within the context of
forthcoming full-sky weak lensing surveys such as Euclid, convergence maps
offer an important advantage over shear fields in terms of cosmological
exploitation. While carrying the same information, the lensing signal is more
compressed in the convergence maps than in the shear field, simplifying
otherwise computationally expensive analyses, for instance non-Gaussianity
studies. However, the inversion of the non-local shear field requires accurate
control of systematic effects due to holes in the data field, field borders,
noise and the fact that the shear is not a direct observable (reduced shear).
In this paper, we present the two mass inversion methods that are being
included in the official Euclid data processing pipeline: the standard Kaiser &
Squires method (KS) and a new mass inversion method (KS+) that aims to reduce
the information loss during the mass inversion. This new method is based on the
KS methodology and includes corrections for mass mapping systematic effects.
The results of the KS+ method are compared to the original implementation of
the KS method in its simplest form, using the Euclid Flagship mock galaxy
catalogue. In particular, we estimate the quality of the reconstruction by
comparing the two-point correlation functions, third- and fourth-order moments
obtained from shear and convergence maps, and we analyse each systematic effect
independently and simultaneously. We show that the KS+ method reduces
substantially the errors on the two-point correlation function and moments
compared to the KS method. In particular, we show…

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