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Euclid preparation: I. The Euclid Wide Survey

(2021)

Authors:

R Scaramella, J Amiaux, Y Mellier, C Burigana, CS Carvalho, J-C Cuillandre, A Da Silva, A Derosa, J Dinis, E Maiorano, M Maris, I Tereno, R Laureijs, T Boenke, G Buenadicha, X Dupac, LM Gaspar Venancio, P Gómez-Álvarez, J Hoar, J Lorenzo Alvarez, GD Racca, G Saavedra-Criado, J Schwartz, R Vavrek, M Schirmer, H Aussel, R Azzollini, VF Cardone, M Cropper, A Ealet, B Garilli, W Gillard, BR Granett, L Guzzo, H Hoekstra, K Jahnke, T Kitching, M Meneghetti, L Miller, R Nakajima, SM Niemi, F Pasian, WJ Percival, M Sauvage, M Scodeggio, S Wachter, A Zacchei, N Aghanim, A Amara, T Auphan, N Auricchio, S Awan, A Balestra, R Bender, C Bodendorf, D Bonino, E Branchini, S Brau-Nogue, M Brescia, GP Candini, V Capobianco, C Carbone, RG Carlberg, J Carretero, R Casas, FJ Castander, M Castellano, S Cavuoti, A Cimatti, R Cledassou, G Congedo, CJ Conselice, L Conversi, Y Copin, L Corcione, A Costille, F Courbin, H Degaudenzi, M Douspis, F Dubath, CAJ Duncan, S Dusini, S Farrens, S Ferriol, P Fosalba, N Fourmanoit, M Frailis, E Franceschi, P Franzetti, M Fumana, B Gillis, C Giocoli, A Grazian, F Grupp, SVH Haugan, W Holmes, F Hormuth, P Hudelot, S Kermiche, A Kiessling, M Kilbinger, R Kohley, B Kubik, M Kümmel, M Kunz, H Kurki-Suonio, S Ligori, PB Lilje, I Lloro, O Mansutti, O Marggraf, K Markovic, F Marulli, R Massey, S Maurogordato, M Melchior, E Merlin, G Meylan, JJ Mohr, M Moresco, B Morin, L Moscardini, E Munari, RC Nichol, C Padilla, S Paltani, J Peacock, K Pedersen, V Pettorino, S Pires, M Poncet, L Popa, L Pozzetti, F Raison, R Rebolo, J Rhodes, H-W Rix, M Roncarelli, E Rossetti, R Saglia, P Schneider, T Schrabback, A Secroun, G Seidel, S Serrano, C Sirignano, G Sirri, J Skottfelt, L Stanco, JL Starck, P Tallada-Crespí, D Tavagnacco, AN Taylor, HI Teplitz, R Toledo-Moreo, F Torradeflot, M Trifoglio, EA Valentijn, L Valenziano, GA Verdoes Kleijn, Y Wang, N Welikala, J Weller, M Wetzstein, G Zamorani, J Zoubian, S Andreon, M Baldi, S Bardelli, A Boucaud, S Camera, G Fabbian, R Farinelli, J Graciá-Carpio, D Maino, E Medinaceli, S Mei, C Neissner, G Polenta, A Renzi, E Romelli, C Rosset, F Sureau, M Tenti, T Vassallo, E Zucca, C Baccigalupi, A Balaguera-Antolínez, P Battaglia, A Biviano, S Borgani, E Bozzo, R Cabanac, A Cappi, S Casas, G Castignani, C Colodro-Conde, J Coupon, HM Courtois, J Cuby, S de la Torre, S Desai, D Di Ferdinando, H Dole, M Fabricius, M Farina, PG Ferreira, F Finelli, P Flose-Reimberg, S Fotopoulou, S Galeotta, K Ganga, G Gozaliasl, IM Hook, E Keihanen, CC Kirkpatrick, P Liebing, V Lindholm, G Mainetti, M Martinelli, N Martinet, M Maturi, HJ McCracken, RB Metcalf, G Morgante, J Nightingale, A Nucita, L Patrizii, D Potter, G Riccio, AG Sánchez, D Sapone, JA Schewtschenko, M Schultheis, V Scottez, R Teyssier, I Tutusaus, J Valiviita, M Viel, W Vriend, L Whittaker
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Euclidpreparation

Astronomy & Astrophysics EDP Sciences 655 (2021) A44-A44

Authors:

A Pocino, I Tutusaus, FJ Castander, P Fosalba, M Crocce, A Porredon, S Camera, V Cardone, S Casas, T Kitching, F Lacasa, M Martinelli, A Pourtsidou, Z Sakr, S Andreon, N Auricchio, C Baccigalupi, A Balaguera-Antolínez, M Baldi, A Balestra, S Bardelli, R Bender, A Biviano, C Bodendorf, D Bonino

Abstract:

Photometric redshifts (photo-zs) are one of the main ingredients in the analysis of cosmological probes. Their accuracy particularly affects the results of the analyses of galaxy clustering with photometrically selected galaxies (GCph) and weak lensing. In the next decade, space missions such as Euclid will collect precise and accurate photometric measurements for millions of galaxies. These data should be complemented with upcoming ground-based observations to derive precise and accurate photo-zs. In this article we explore how the tomographic redshift binning and depth of ground-based observations will affect the cosmological constraints expected from the Euclid mission. We focus on GCph and extend the study to include galaxy-galaxy lensing (GGL). We add a layer of complexity to the analysis by simulating several realistic photo-z distributions based on the Euclid Consortium Flagship simulation and using a machine learning photo-z algorithm. We then use the Fisher matrix formalism together with these galaxy samples to study the cosmological constraining power as a function of redshift binning, survey depth, and photo-z accuracy. We find that bins with an equal width in redshift provide a higher figure of merit (FoM) than equipopulated bins and that increasing the number of redshift bins from ten to 13 improves the FoM by 35% and 15% for GCph and its combination with GGL, respectively. For GCph, an increase in the survey depth provides a higher FoM. However, when we include faint galaxies beyond the limit of the spectroscopic training data, the resulting FoM decreases because of the spurious photo-zs. When combining GCph and GGL, the number density of the sample, which is set by the survey depth, is the main factor driving the variations in the FoM. Adding galaxies at faint magnitudes and high redshift increases the FoM, even when they are beyond the spectroscopic limit, since the number density increase compensates for the photo-z degradation in this case. We conclude that there is more information that can be extracted beyond the nominal ten tomographic redshift bins of Euclid and that we should be cautious when adding faint galaxies into our sample since they can degrade the cosmological constraints
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Model-independent constraints on clustering and growth of cosmic structures from BOSS DR12 galaxies in harmonic space

ArXiv preprint. 14 pages, 8 figures, 3 tables

Authors:

Konstantinos Tanidis, Stefano Camera

Abstract:

We present a new, model-independent measurement of the clustering amplitude of galaxies and the growth of cosmic large-scale structures from the Baryon Oscillation Spectroscopic Survey (BOSS) 12th data release (DR12). This is achieved by generalising harmonic-space power spectra for galaxy clustering to measure separately the magnitudes of the density and of the redshift-space distortion terms, which are respectively related to the clustering amplitude, bσ8(z), and the growth, fσ8(z). We adopt a tomographic approach with 15 redshift bins in the range z∈[0.15,0.67]. We restrict our analysis to strictly linear scales, implementing a redshift-dependent maximum multipole for each of the tomographic bins. Thus, we obtain 30 data points in total, 15 for each of the quantities bσ8(z) and fσ8(z). The measurements do not appear to suffer from any apparent systematic effect and show excellent agreement with the theoretical prediction from a concordance cosmology as from the Planck satellite. Our results also agree with previous analyses by the BOSS collaboration. Although each single datum has, in general, a larger error bar than that obtained in configuration- or Fourier-space analyses, our study provides the community with a larger number of tomographic data points that allow for a complementary tracking in redshift of the evolution of fundamental cosmological quantities.
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Euclid preparation: IX. EuclidEmulator2 – power spectrum emulation with massive neutrinos and self-consistent dark energy perturbations

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 505:2 (2021) 2840-2869

Authors:

Euclid Collaboration, M Knabenhans, J Stadel, D Potter, J Dakin, S Hannestad, T Tram, S Marelli, A Schneider, R Teyssier, P Fosalba, S Andreon, N Auricchio, C Baccigalupi, A Balaguera-Antolínez, M Baldi, S Bardelli, P Battaglia, R Bender, A Biviano, C Bodendorf, E Bozzo, E Branchini, M Brescia, C Burigana, R Cabanac, S Camera, V Capobianco, A Cappi, C Carbone, J Carretero, CS Carvalho, R Casas, S Casas, M Castellano, G Castignani, S Cavuoti, R Cledassou, C Colodro-Conde, G Congedo, CJ Conselice, L Conversi, Y Copin, L Corcione, J Coupon, HM Courtois, A Da Silva, S de la Torre, D Di Ferdinando, CAJ Duncan, X Dupac, G Fabbian, S Farrens, PG Ferreira, F Finelli, M Frailis, E Franceschi, S Galeotta, B Garilli, C Giocoli, G Gozaliasl, J Graciá-Carpio, F Grupp, L Guzzo, W Holmes, F Hormuth, H Israel, K Jahnke, E Keihanen, S Kermiche, CC Kirkpatrick, B Kubik, M Kunz, H Kurki-Suonio, S Ligori, PB Lilje, I Lloro, D Maino, O Marggraf, K Markovic, N Martinet, F Marulli, R Massey, N Mauri, S Maurogordato, E Medinaceli, M Meneghetti, B Metcalf, G Meylan, M Moresco, B Morin, L Moscardini, E Munari, C Neissner, SM Niemi, C Padilla, S Paltani, F Pasian, L Patrizii, V Pettorino, S Pires, G Polenta, M Poncet, F Raison, A Renzi, J Rhodes, G Riccio, E Romelli, M Roncarelli, R Saglia, AG Sánchez, D Sapone, P Schneider, V Scottez, A Secroun, S Serrano, C Sirignano, G Sirri, L Stanco, F Sureau, P Tallada Crespí, AN Taylor, M Tenti, I Tereno, R Toledo-Moreo, F Torradeflot, L Valenziano, J Valiviita, T Vassallo, M Viel, Y Wang, N Welikala, L Whittaker, A Zacchei, E Zucca
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Strong detection of the CMB lensing and galaxy weak lensing cross-correlation from ACT-DR4, Planck Legacy, and KiDS-1000

Astronomy & Astrophysics EDP Sciences 649 (2021) A146-A146

Authors:

Naomi Clare Robertson, David Alonso, Joachim Harnois-Déraps, Omar Darwish, Arun Kannawadi, Alexandra Amon, Marika Asgari, Maciej Bilicki, Erminia Calabrese, Steve K Choi, Mark J Devlin, Jo Dunkley, Andrej Dvornik, Thomas Erben, Simone Ferraro, Maria Cristina Fortuna, Benjamin Giblin, Dongwon Han, Catherine Heymans, Hendrik Hildebrandt, J Colin Hill, Matt Hilton, Shuay-Pwu P Ho, Henk Hoekstra, Johannes Hubmayr, John P Hughes, Benjamin Joachimi, Shahab Joudaki, Kenda Knowles, Konrad Kuijken, Mathew S Madhavacheril, Kavilan Moodley, Lance Miller, Toshiya Namikawa, Federico Nati, Michael D Niemack, Lyman A Page, Bruce Partridge, Emmanuel Schaan, Alessandro Schillaci, Peter Schneider, Neelima Sehgal, Blake D Sherwin, Cristóbal Sifón, Suzanne T Staggs, Tilman Tröster, Alexander van Engelen, Edwin Valentijn, Edward J Wollack, Angus H Wright

Abstract:

<jats:p>We measured the cross-correlation between galaxy weak lensing data from the Kilo Degree Survey (KiDS-1000, DR4) and cosmic microwave background (CMB) lensing data from the Atacama Cosmology Telescope (ACT, DR4) and the <jats:italic>Planck</jats:italic> Legacy survey. We used two samples of source galaxies, selected with photometric redshifts, (0.1 &lt; <jats:italic>z</jats:italic><jats:sub>B</jats:sub> &lt; 1.2) and (1.2 &lt; <jats:italic>z</jats:italic><jats:sub>B</jats:sub> &lt; 2), which produce a combined detection significance of the CMB lensing and weak galaxy lensing cross-spectrum of 7.7<jats:italic>σ</jats:italic>. With the lower redshift galaxy sample, for which the cross-correlation was detected at a significance of 5.3<jats:italic>σ</jats:italic>, we present joint cosmological constraints on the matter density parameter, Ω<jats:sub>m</jats:sub>, and the matter fluctuation amplitude parameter, <jats:italic>σ</jats:italic><jats:sub>8</jats:sub>, marginalising over three nuisance parameters that model our uncertainty in the redshift and shear calibration as well as the intrinsic alignment of galaxies. We find our measurement to be consistent with the best-fitting flat ΛCDM cosmological models from both <jats:italic>Planck</jats:italic> and KiDS-1000. We demonstrate the capacity of CMB weak lensing cross-correlations to set constraints on either the redshift or shear calibration by analysing a previously unused high-redshift KiDS galaxy sample (1.2 &lt; <jats:italic>z</jats:italic><jats:sub>B</jats:sub> &lt; 2), with the cross-correlation detected at a significance of 7<jats:italic>σ</jats:italic>. This analysis provides an independent assessment for the accuracy of redshift measurements in a regime that is challenging to calibrate directly owing to known incompleteness in spectroscopic surveys.</jats:p>
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