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1. Benchmarking Quantum Convolutional Neural Networks for Signal Classification in Simulated Gamma-Ray Burst Detection

Author

Farsian, Farida, Parmiggiani, Nicolò, Rizzo, Alessandro, Panebianco, Gabriele, Bulgarelli, Andrea, Schillirò, Francesco, Burigana, Carlo, Cardone, Vincenzo, Cappelli, Luca, Meneghetti, Massimo, Murante, Giuseppe, Sarracino, Giuseppe, Scaramella, Roberto, Testa, Vincenzo, and Trombetti, Tiziana

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Computer Science - Artificial Intelligence, Quantum Physics
Abstract

This study evaluates the use of Quantum Convolutional Neural Networks (QCNNs) for identifying signals resembling Gamma-Ray Bursts (GRBs) within simulated astrophysical datasets in the form of light curves. The task addressed here focuses on distinguishing GRB-like signals from background noise in simulated Cherenkov Telescope Array Observatory (CTAO) data, the next-generation astrophysical observatory for very high-energy gamma-ray science. QCNNs, a quantum counterpart of classical Convolutional Neural Networks (CNNs), leverage quantum principles to process and analyze high-dimensional data efficiently. We implemented a hybrid quantum-classical machine learning technique using the Qiskit framework, with the QCNNs trained on a quantum simulator. Several QCNN architectures were tested, employing different encoding methods such as Data Reuploading and Amplitude encoding. Key findings include that QCNNs achieved accuracy comparable to classical CNNs, often surpassing 90\%, while using fewer parameters, potentially leading to more efficient models in terms of computational resources. A benchmark study further examined how hyperparameters like the number of qubits and encoding methods affected performance, with more qubits and advanced encoding methods generally enhancing accuracy but increasing complexity. QCNNs showed robust performance on time-series datasets, successfully detecting GRB signals with high precision. The research is a pioneering effort in applying QCNNs to astrophysics, offering insights into their potential and limitations. This work sets the stage for future investigations to fully realize the advantages of QCNNs in astrophysical data analysis., Comment: 9 pages, Accepted for publication in 33rd Euromicro/IEEE International Conference on Parallel, Distributed and Network-Based Processing (PDP 2025)

Published
2025

2. VST-SMASH: the VST Survey of Mass Assembly and Structural Hierarchy

Author

Tortora, Crescenzo, Ragusa, Rossella, Gatto, Massimiliano, Spavone, Marilena, Hunt, Leslie, Ripepi, Vincenzo, Dall'Ora, Massimo, Abdurro'uf, Annibali, Francesca, Baes, Maarten, Belfiore, Francesco Michel Concetto, Bellucco, Nicola, Bolzonella, Micol, Cantiello, Michele, Dimauro, Paola, Kluge, Mathias, Lelli, Federico, Napolitano, Nicola R., Nucita, Achille, Radovich, Mario, Scaramella, Roberto, Schinnerer, Eva, Testa, Vincenzo, and Unni, Aiswarya

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The VLT Survey Telescope Survey of Mass Assembly and Structural Hierarchy (VST-SMASH) aims to detect tidal features and remnants around very nearby galaxies, a unique and essential diagnostic of the hierarchical nature of galaxy formation. Leveraging optimal sky conditions at ESO's Paranal Observatory, combined with the VST's multi-band optical filters, VST-SMASH aims to be the definitive survey of stellar streams and tidal remnants in the Local Volume, targeting a low surface-brightness limit of $\mu \sim$ 30 mag arcsec$^{-2}$ in the g and r bands, and $\mu \sim$ 28 mag arcsec$^{-2}$ in the i band, in a volume-limited sample of local galaxies within 11 Mpc and the Euclid footprint., Comment: 4 pages, 2 figures, 1 table, published in the ESO Messenger 193

Published
2024

3. Higher order statistics of shear field: a machine learning approach

Author

Parroni, Carolina, Tollet, Edouard, Cardone, Vincenzo F., Maoli, Roberto, and Scaramella, Roberto

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The unprecedented amount and the excellent quality of lensing data that the upcoming ground- and space-based surveys will produce represent a great opportunity to shed light on the questions that still remain unanswered concerning our universe and the validity of the standard $\Lambda$CDM cosmological model. Therefore, it is important to develop new techniques that can exploit the huge quantity of data that future observations will give us access to in the most effective way possible. For this reason, we decided to investigate the development of a new method to treat weak lensing higher order statistics, which are known to break degeneracy among cosmological parameters thanks to their capability of probing the non-Gaussian properties of the shear field. In particular, the proposed method directly applies to the observed quantity, i.e., the noisy galaxy ellipticity. We produced simulated lensing maps with different sets of cosmological parameters and used them to measure higher order moments, Minkowski functionals, Betti numbers, and other statistics related to graph theory. This allowed us to construct datasets with different size, precision, and smoothing. We then applied several machine learning algorithms to determine which method best predicts the actual cosmological parameters associated with each simulation. The best model resulted to be simple multidimensional linear regression. We used this model to compare the results coming from the different datasets and found out that we can measure with good accuracy the majority of the parameters that we considered. We also investigated the relation between each higher order estimator and the different cosmological parameters for several signal-to-noise thresholds and redshifts bins. Given the promising results, we consider this approach as a valuable resource, worth of further development.

Published
2020
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4. Going deep with Minkowski functionals of convergence maps

Author

Parroni, Carolina, Cardone, Vincenzo F., Maoli, Roberto, and Scaramella, Roberto

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Stage IV lensing surveys promise to make available an unprecedented amount of excellent data which will represent a huge leap in terms of both quantity and quality. This will open the way to the use of novel tools, which go beyond the standard second order statistics probing the high order properties of the convergence field. We discuss the use of Minkowski Functionals (MFs) as complementary probes to increase the lensing Figure of Merit (FoM), for a survey made out of a wide total area $A_{\rm{tot}}$ imaged at a limiting magnitude $\rm{mag_{W}}$ containing a subset of area $A_{\rm{deep}}$ where observations are pushed to a deeper limiting magnitude $\rm{mag_{D}}$. We present an updated procedure to match the theoretically predicted MFs to the measured ones, taking into account the impact of map reconstruction from noisy shear data. We validate this renewed method against simulated data sets with different source redshift distributions and total number density, setting these quantities in accordance with the depth of the survey. We can then rely on a Fisher matrix analysis to forecast the improvement in the FoM due to the joint use of shear tomography and MFs under different assumptions on $(A_{\rm{tot}},\,A_{\rm{deep}},\,\rm{mag_{D}})$, and the prior on the MFs nuisance parameters. It turns out that MFs can provide a valuable help in increasing the FoM of the lensing survey, provided the nuisance parameters are known with a non negligible precision. What is actually more interesting is the possibility to compensate for the loss of FoM due to a cut in the multipole range probed by shear tomography, which makes the results more robust against uncertainties in the modeling of nonlinearities. This makes MFs a promising tool to both increase the FoM and make the constraints on the cosmological parameters less affected by theoretical systematic effects.

Published
2019
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5. Minkowski Functionals of Convergence Maps and the Lensing Figure of Merit

Author

Vicinanza, Martina, Cardone, Vincenzo F., Maoli, Roberto, Scaramella, Roberto, Er, Xinzhong, and Tereno, Ismael

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Minkowski functionals (MFs) quantify the topological properties of a given field probing its departure from Gaussianity. We investigate their use on lensing convergence maps in order to see whether they can provide further insights on the underlying cosmology with respect to the standard second-order statistics, i.e., cosmic shear tomography. To this end, we first present a method to match theoretical predictions with measured MFs taking care of the shape noise, imperfections in the map reconstruction, and inaccurate description of the nonlinearities in the matter power spectrum and bispectrum. We validate this method against simulated maps reconstructed from shear fields generated by the MICE simulation. We then perform a Fisher matrix analysis to forecast the accuracy on cosmological parameters from a joint MFs and shear tomography analysis. It turns out that MFs are indeed helpful to break the $\Omega_{\rm m}$--$\sigma_8$ degeneracy thus generating a sort of chain reaction leading to an overall increase of the Figure of Merit., Comment: 16 pages, 5 figures. Matches published version in PRD

Published
2019
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6. Increasing the Lensing Figure of Merit through Higher Order Convergence Moments

Author

Vicinanza, Martina, Cardone, Vincenzo F., Maoli, Roberto, Scaramella, Roberto, and Er, Xinzhong

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The unprecedented quality, the increased dataset, and the wide area of ongoing and near future weak lensing surveys allows to move beyond the standard two points statistics thus making worthwhile to investigate higher order probes. As an interesting step towards this direction, we expolore the use of higher order moments (HOM) of the convergence field as a way to increase the lensing Figure of Merit (FoM). To this end, we rely on simulated convergence to first show that HOM can be measured and calibrated so that it is indeed possible to predict them for a given cosmological model provided suitable nuisance parameters are introduced and then marginalized over. We then forecast the accuracy on cosmological parameters from the use of HOM alone and in combination with standard shear power spectra tomography. It turns out that HOM allow to break some common degeneracies thus significantly boosting the overall FoM. We also qualitatively discuss possible systematics and how they can be dealt with., Comment: 25 pages, 5 figures, This paper extends and replaces arXiv:1606.03892. It matches PRD accepted version after minor changes

Published
2018
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7. Calibration of colour gradient bias in shear measurement using HST/CANDELS data

Author

Er, Xinzhong, Hoekstra, Henk, Schrabback, Tim, Cardone, Vincenzo F., Scaramella, Roberto, Maoli, Roberto, Vicinanza, Martina, Gillis, Bryan, and Rhodes, Jason

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Accurate shape measurements are essential to infer cosmological parameters from large area weak gravitational lensing studies. The compact diffraction-limited point-spread function (PSF) in space-based observations is greatly beneficial, but its chromaticity for a broad band observation can lead to new subtle effects that could hitherto be ignored: the PSF of a galaxy is no longer uniquely defined and spatial variations in the colours of galaxies result in biases in the inferred lensing signal. Taking Euclid as a reference, we show that this colourgradient bias (CG bias) can be quantified with high accuracy using available multi-colour Hubble Space Telescope (HST) data. In particular we study how noise in the HST observations might impact such measurements and find this to be negligible. We determine the CG bias using HST observations in the F606W and F814W filters and observe a correlation with the colour, in line with expectations, whereas the dependence with redshift is weak. The biases for individual galaxies are generally well below 1%, which may be reduced further using morphological information from the Euclid data. Our results demonstrate that CG bias should not be ignored, but it is possible to determine its amplitude with sufficient precision, so that it will not significantly bias the weak lensing measurements using Euclid data., Comment: 13 pages, 14 figures, MNRAS accepted, comments welcome

Published
2017
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8. The Euclid mission design

Author

Racca, Giuseppe D, Laureijs, Rene, Stagnaro, Luca, Salvignol, Jean Christophe, Alvarez, Jose Lorenzo, Criado, Gonzalo Saavedra, Venancio, Luis Gaspar, Short, Alex, Strada, Paolo, Boenke, Tobias, Colombo, Cyril, Calvi, Adriano, Maiorano, Elena, Piersanti, Osvaldo, Prezelus, Sylvain, Rosato, Pierluigi, Pinel, Jacques, Rozemeijer, Hans, Lesna, Valentina, Musi, Paolo, Sias, Marco, Anselmi, Alberto, Cazaubiel, Vincent, Vaillon, Ludovic, Mellier, Yannick, Amiaux, Jerome, Berthe, Michel, Sauvage, Marc, Azzollini, Ruyman, Cropper, Mark, Pottinger, Sabrina, Jahnke, Knud, Ealet, Anne, Maciaszek, Thierry, Pasian, Fabio, Zacchei, Andrea, Scaramella, Roberto, Hoar, John, Kohley, Ralf, Vavrek, Roland, Rudolph, Andreas, and Schmidt, Micha

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Euclid is a space-based optical/near-infrared survey mission of the European Space Agency (ESA) to investigate the nature of dark energy, dark matter and gravity by observing the geometry of the Universe and on the formation of structures over cosmological timescales. Euclid will use two probes of the signature of dark matter and energy: Weak gravitational Lensing, which requires the measurement of the shape and photometric redshifts of distant galaxies, and Galaxy Clustering, based on the measurement of the 3-dimensional distribution of galaxies through their spectroscopic redshifts. The mission is scheduled for launch in 2020 and is designed for 6 years of nominal survey operations. The Euclid Spacecraft is composed of a Service Module and a Payload Module. The Service Module comprises all the conventional spacecraft subsystems, the instruments warm electronics units, the sun shield and the solar arrays. In particular the Service Module provides the extremely challenging pointing accuracy required by the scientific objectives. The Payload Module consists of a 1.2 m three-mirror Korsch type telescope and of two instruments, the visible imager and the near-infrared spectro-photometer, both covering a large common field-of-view enabling to survey more than 35% of the entire sky. All sensor data are downlinked using K-band transmission and processed by a dedicated ground segment for science data processing. The Euclid data and catalogues will be made available to the public at the ESA Science Data Centre., Comment: 23 pages, 19 figures, Presented at the SPIE Astronomical Telescopes and Instrumentation conference in Edinburgh, Scotland, United Kingdom, 6 June 1 July 2016

Published
2016
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9. Improving lensing cluster mass estimate with flexion

Author

Cardone, Vincenzo F., Vicinanza, Martina, Er, Xinzhong, Maoli, Roberto, and Scaramella, Roberto

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Gravitational lensing has long been considered as a valuable tool to determine the total mass of galaxy clusters. The shear profile as inferred from the statistics of ellipticity of background galaxies allows to probe the cluster intermediate and outer regions thus determining the virial mass estimate. However, the mass sheet degeneracy and the need for a large number of background galaxies motivate the search for alternative tracers which can break the degeneracy among model parameters and hence improve the accuracy of the mass estimate. Lensing flexion, i.e. the third derivative of the lensing potential, has been suggested as a good answer to the above quest since it probes the details of the mass profile. We investigate here whether this is indeed the case considering jointly using weak lensing, magnification and flexion. We use a Fisher matrix analysis to forecast the relative improvement in the mass accuracy for different assumptions on the shear and flexion signal - to - noise (S/N) ratio also varying the cluster mass, redshift, and ellipticity. It turns out that the error on the cluster mass may be reduced up to a factor 2 for reasonable values of the flexion S/N ratio. As a general result, we get that the improvement in mass accuracy is larger for more flattened haloes, but extracting general trends is a difficult because of the many parameters at play. We nevertheless find that flexion is as efficient as magnification to increase the accuracy in both mass and concentration determination., Comment: 11 pages, 3 figures, accepted for publication on MNRAS

Published
2016
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10. Large-scale retrospective relative spectro-photometric self-calibration in space

Author

Markovic, Katarina, Percival, Will J., Scodeggio, Marco, Ealet, Anne, Wachter, Stefanie, Garilli, Bianca, Guzzo, Luigi, Scaramella, Roberto, Maiorano, Elisabetta, and Amiaux, Jerome

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We consider the application of relative self-calibration using overlap regions to spectroscopic galaxy surveys that use slit-less spectroscopy. This method is based on that developed for the SDSS by Padmanabhan at al. (2008) in that we consider jointly fitting and marginalising over calibrator brightness, rather than treating these as free parameters. However, we separate the calibration of the detector-to-detector from the full-focal-plane exposure-to-exposure calibration. To demonstrate how the calibration procedure will work, we simulate the procedure for a potential implementation of the spectroscopic component of the wide Euclid survey. We study the change of coverage and the determination of relative multiplicative errors in flux measurements for different dithering configurations. We use the new method to study the case where the flat-field across each exposure or detector is measured precisely and only exposure-to-exposure or detector-to-detector variation in the flux error remains. We consider several base dither patterns and find that they strongly influence the ability to calibrate, using this methodology. To enable self-calibration, it is important that the survey strategy connects different observations with at least a minimum amount of overlap, and we propose an "S"-pattern for dithering that fulfills this requirement. The final survey strategy adopted by Euclid will have to optimise for a number of different science goals and requirements. The large-scale calibration of the spectroscopic galaxy survey is clearly cosmologically crucial, but is not the only one., Comment: 23 pages, 19 figures, Accepted for publication in MNRAS, 2017

Published
2016
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11. Cosmology and Fundamental Physics with the Euclid Satellite

Author

Amendola, Luca, Appleby, Stephen, Avgoustidis, Anastasios, Bacon, David, Baker, Tessa, Baldi, Marco, Bartolo, Nicola, Blanchard, Alain, Bonvin, Camille, Borgani, Stefano, Branchini, Enzo, Burrage, Clare, Camera, Stefano, Carbone, Carmelita, Casarini, Luciano, Cropper, Mark, de Rham, Claudia, Dietrich, Joerg P., Di Porto, Cinzia, Durrer, Ruth, Ealet, Anne, Ferreira, Pedro G., Finelli, Fabio, Garcia-Bellido, Juan, Giannantonio, Tommaso, Guzzo, Luigi, Heavens, Alan, Heisenberg, Lavinia, Heymans, Catherine, Hoekstra, Henk, Hollenstein, Lukas, Holmes, Rory, Horst, Ole, Hwang, Zhiqi, Jahnke, Knud, Kitching, Thomas D., Koivisto, Tomi, Kunz, Martin, La Vacca, Giuseppe, Linder, Eric, March, Marisa, Marra, Valerio, Martins, Carlos, Majerotto, Elisabetta, Markovic, Dida, Marsh, David, Marulli, Federico, Massey, Richard, Mellier, Yannick, Montanari, Francesco, Mota, David F., Nunes, Nelson J., Percival, Will, Pettorino, Valeria, Porciani, Cristiano, Quercellini, Claudia, Read, Justin, Rinaldi, Massimiliano, Sapone, Domenico, Sawicki, Ignacy, Scaramella, Roberto, Skordis, Constantinos, Simpson, Fergus, Taylor, Andy, Thomas, Shaun, Trotta, Roberto, Verde, Licia, Vernizzi, Filippo, Vollmer, Adrian, Wang, Yun, Weller, Jochen, and Zlosnik, Tom

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Euclid is a European Space Agency medium class mission selected for launch in 2020 within the Cosmic Vision 2015 2025 program. The main goal of Euclid is to understand the origin of the accelerated expansion of the universe. Euclid will explore the expansion history of the universe and the evolution of cosmic structures by measuring shapes and redshifts of galaxies as well as the distribution of clusters of galaxies over a large fraction of the sky. Although the main driver for Euclid is the nature of dark energy, Euclid science covers a vast range of topics, from cosmology to galaxy evolution to planetary research. In this review we focus on cosmology and fundamental physics, with a strong emphasis on science beyond the current standard models. We discuss five broad topics: dark energy and modified gravity, dark matter, initial conditions, basic assumptions and questions of methodology in the data analysis. This review has been planned and carried out within Euclid's Theory Working Group and is meant to provide a guide to the scientific themes that will underlie the activity of the group during the preparation of the Euclid mission., Comment: This article provides an update of arXiv:1206.1225, with different authors. Forecasts are not updated in this version

Published
2016
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12. Euclid & SKA Synergies

Author

Kitching, Thomas D., Bacon, David, Brown, Michael L., Bull, Philip, McEwen, Jason D., Oguri, Masamune, Scaramella, Roberto, Takahashi, Keitaro, Wu, Kinwah, and Yamauchi, Daisuke

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Over the past few years two of the largest and highest fidelity experiments conceived have been approved for construction: Euclid is an ESA M-Class mission that will map three-quarters of the extra galactic sky with Hubble Space Telescope resolution optical and NIR imaging, and NIR spectroscopy, its scientific aims (amongst others) are to create a map of the dark Universe and to determine the nature of dark energy. The Square Kilometre Array (SKA) has similar scientific aims (and others) using radio wavelength observations. The two experiments are synergistic in several respects, both through the scientific objectives and through the control of systematic effects. SKA Phase-1 and Euclid will be commissioned on similar timescales offering an exciting opportunity to exploit synergies between these facilities., Comment: This article is part of the 'SKA Synergies Chapter, Advancing Astrophysics with the SKA (AASKA14) Conference, Giardini Naxos (Italy), June 9th-13th 2014'

Published
2015

13. SKA synergy with Microwave Background studies

Author

Burigana, Carlo, Alexander, Paul, Baccigalupi, Carlo, Barbosa, Domingos, Blanchard, Alain, De Rosa, Adriano, de Zotti, Gianfranco, Finelli, Fabio, Gruppuso, Alessandro, Jones, Michael, Matarrese, Sabino, Melchiorri, Alessandro, Molinari, Diego, Negrello, Mattia, Paoletti, Daniela, Perrotta, Francesca, Scaramella, Roberto, and Trombetti, Tiziana

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The extremely high sensitivity and resolution of the Square Kilometre Array (SKA) will be useful for addressing a wide set of themes relevant for cosmology, in synergy with current and future cosmic microwave background (CMB) projects. Many of these themes also have a link with future optical-IR and X-ray observations. We discuss the scientific perspectives for these goals, the instrumental requirements and the observational and data analysis approaches, and identify several topics that are important for cosmology and astrophysics at different cosmic epochs., Comment: 16 pages, 3 figures. Approved as Chapter in "Advancing Astrophysics with the Square Kilometre Array", June 8-13, 2014, Giardini Naxos, Italy. Submission: August 22, 2014; in revised form: December 23, 2014; approval notification: January 12, 2015. In press on Proceedings of Science (PoS)

Published
2015

14. On the shear estimation bias induced by the spatial variation of colour across galaxy profiles

Author

Semboloni, Elisabetta, Hoekstra, Henk, Huang, Zhuoyi, Cardone, Vincenzo, Cropper, Mark, Joachimi, Benjamin, Kitching, Thomas, Kuijken, Konrad, Lombardi, Marco, Maoli, Roberto, Mellier, Yannick, Miller, Lance, Rhodes, Jason, Scaramella, Roberto, Schrabback, Tim, and Velander, Malin

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The spatial variation of the colour of a galaxy may introduce a bias in the measurement of its shape if the PSF profile depends on wavelength. We study how this bias depends on the properties of the PSF and the galaxies themselves. The bias depends on the scales used to estimate the shape, which may be used to optimise methods to reduce the bias. Here we develop a general approach to quantify the bias. Although applicable to any weak lensing survey, we focus on the implications for the ESA Euclid mission. Based on our study of synthetic galaxies we find that the bias is a few times 10^-3 for a typical galaxy observed by Euclid. Consequently, it cannot be neglected and needs to be accounted for. We demonstrate how one can do so using spatially resolved observations of galaxies in two filters. We show that HST observations in the F606W and F814W filters allow us to model and reduce the bias by an order of magnitude, sufficient to meet Euclid's scientific requirements. The precision of the correction is ultimately determined by the number of galaxies for which spatially-resolved observations in at least two filters are available. We use results from the Millennium Simulation to demonstrate that archival HST data will be sufficient for the tomographic cosmic shear analysis with the Euclid dataset., Comment: MNRAS submitted, 18 pages, 13 Figures

Published
2012
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15. Defining a weak lensing experiment in space

Author

Cropper, Mark, Hoekstra, Henk, Kitching, Thomas, Massey, Richard, Amiaux, Jerome, Miller, Lance, Mellier, Yannick, Rhodes, Jason, Rowe, Barnaby, Pires, Sandrine, Saxton, Curtis, and Scaramella, Roberto

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This paper describes the definition of a typical next-generation space-based weak gravitational lensing experiment. We first adopt a set of top-level science requirements from the literature, based on the scale and depth of the galaxy sample, and the avoidance of systematic effects in the measurements which would bias the derived shear values. We then identify and categorise the contributing factors to the systematic effects, combining them with the correct weighting, in such a way as to fit within the top-level requirements. We present techniques which permit the performance to be evaluated and explore the limits at which the contributing factors can be managed. Besides the modelling biases resulting from the use of weighted moments, the main contributing factors are the reconstruction of the instrument point spread function (PSF), which is derived from the stellar images on the image, and the correction of the charge transfer inefficiency (CTI) in the CCD detectors caused by radiation damage., Comment: 26 pages, 12 figures. Version 2 contains changes from the refereeing with a useful clarification of points in section 2.2, leading to an added section 2.3, while section 3.1 has been slightly expanded. There are no changes to the results. Other minor edits have been made, and the author list slightly amended. Accepted by MNRAS. See companion (theory) paper Massey et al (2013) MNRAS, 429, 661

Published
2012
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16. Origins of weak lensing systematics, and requirements on future instrumentation (or knowledge of instrumentation)

Author

Massey, Richard, Hoekstra, Henk, Kitching, Thomas, Rhodes, Jason, Cropper, Mark, Amiaux, Jerome, Harvey, David, Mellier, Yannick, Meneghetti, Massimo, Miller, Lance, Paulin-Henriksson, Stephane, Pires, Sandrine, Scaramella, Roberto, and Schrabback, Tim

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The first half of this paper explores the origin of systematic biases in the measurement of weak gravitational lensing. Compared to previous work, we expand the investigation of PSF instability and fold in for the first time the effects of non-idealities in electronic imaging detectors and imperfect galaxy shape measurement algorithms. Together, these now explain the additive A(l) and multiplicative M(l) systematics typically reported in current lensing measurements. We find that overall performance is driven by a product of a telescope/camera's *absolute performance*, and our *knowledge about its performance*. The second half of this paper propagates any residual shear measurement biases through to their effect on cosmological parameter constraints. Fully exploiting the statistical power of Stage IV weak lensing surveys will require additive biases A<1.8e-12 and multiplicative biases M<4.0e-3. These can be allocated between individual budgets in hardware, calibration data and software, using results from the first half of the paper. If instrumentation is stable and well-calibrated, we find extant shear measurement software from GREAT10 already meet requirements on galaxies detected at S/N=40. Averaging over a population of galaxies with a realistic distribution of sizes, it also meets requirements for a 2D cosmic shear analysis from space. If used on fainter galaxies or for 3D cosmic shear tomography, existing algorithms would need calibration on simulations to avoid introducing bias at a level similar to the statistical error. Requirements on hardware and calibration data are discussed in more detail in a companion paper. Our analysis is intentionally general, but is specifically being used to drive the hardware and ground segment performance budget for the design of the European Space Agency's recently-selected Euclid mission., Comment: 19 pages, 5 figures. Submitted to MNRAS. See companion (implementation) paper Cropper et al

Published
2012
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17. Cosmology and fundamental physics with the Euclid satellite

Author

Amendola, Luca, Appleby, Stephen, Bacon, David, Baker, Tessa, Baldi, Marco, Bartolo, Nicola, Blanchard, Alain, Bonvin, Camille, Borgani, Stefano, Branchini, Enzo, Burrage, Clare, Camera, Stefano, Carbone, Carmelita, Casarini, Luciano, Cropper, Mark, deRham, Claudia, di Porto, Cinzia, Ealet, Anne, Ferreira, Pedro G., Finelli, Fabio, Garcia-Bellido, Juan, Giannantonio, Tommaso, Guzzo, Luigi, Heavens, Alan, Heisenberg, Lavinia, Heymans, Catherine, Hoekstra, Henk, Hollenstein, Lukas, Holmes, Rory, Horst, Ole, Jahnke, Knud, Kitching, Thomas D., Koivisto, Tomi, Kunz, Martin, La Vacca, Giuseppe, March, Marisa, Majerotto, Elisabetta, Markovic, Katarina, Marsh, David, Marulli, Federico, Massey, Richard, Mellier, Yannick, Mota, David F., Nunes, Nelson, Percival, Will, Pettorino, Valeria, Porciani, Cristiano, Quercellini, Claudia, Read, Justin, Rinaldi, Massimiliano, Sapone, Domenico, Scaramella, Roberto, Skordis, Constantinos, Simpson, Fergus, Taylor, Andy, Thomas, Shaun, Trotta, Roberto, Verde, Licia, Vernizzi, Filippo, Vollmer, Adrian, Wang, Yun, Weller, Jochen, and Zlosnik, Tom

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology
Abstract

Euclid is a European Space Agency medium class mission selected for launch in 2019 within the Cosmic Vision 2015-2025 programme. The main goal of Euclid is to understand the origin of the accelerated expansion of the Universe. Euclid will explore the expansion history of the Universe and the evolution of cosmic structures by measuring shapes and redshifts of galaxies as well as the distribution of clusters of galaxies over a large fraction of the sky. Although the main driver for Euclid is the nature of dark energy, Euclid science covers a vast range of topics, from cosmology to galaxy evolution to planetary research. In this review we focus on cosmology and fundamental physics, with a strong emphasis on science beyond the current standard models. We discuss five broad topics: dark energy and modified gravity, dark matter, initial conditions, basic assumptions and questions of methodology in the data analysis. This review has been planned and carried out within Euclid's Theory Working Group and is meant to provide a guide to the scientific themes that will underlie the activity of the group during the preparation of the Euclid mission., Comment: 236 pages, minor edits to match the journal version 2013

Published
2012
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18. Testing the distance duality relation with present and future data

Author

Cardone, Vincenzo F., Spiro, Susanna, Hook, Isobel, and Scaramella, Roberto

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The assumptions that "light propagates along null geodesics of the spacetime metric" and "the number of photons is conserved along the light path" lead to the distance duality relation (DDR), $\eta = D_L(z) (1 + z)^{-2}/D_A(z) = 1$, with $D_L(z)$ and $D_A(z)$ the luminosity and angular diameter distances to a source at redshift $z$. In order to test the DDR, we follow the usual strategy comparing the angular diameter distances of a set of clusters, inferred from X - ray and radio data, with the luminosity distance at the same cluster redshift using the local regression technique to estimate $D_L(z)$ from Type Ia Supernovae (SNeIa) Hubble diagram. In order to both strengthen the constraints on the DDR and get rid of the systematics related to the unknown cluster geometry, we also investigate the possibility to use Baryon Acoustic Oscillations (BAO) to infer $D_A(z)$ from future BAO surveys. As a test case, we consider the proposed Euclid mission investigating the precision can be afforded on $\eta(z)$ from the expected SNeIa and BAO data. We find that the combination of BAO and the local regression coupled allows to reduce the errors on $\eta_a = d\eta/dz|_{z = 0}$ by a factor two if one $\eta_0 = \eta(z = 0) = 1$ is forced and future data are used. On the other hand, although the statistical error on $\eta_0$ is not significantly reduced, the constraints on this quantity will be nevertheless ameliorated thanks to the reduce impact of systematics., Comment: 10 pages, 1 figure, 1 table, accepted for publication on Physical Review D

Published
2012
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19. Constraining the ages of the fireballs in the wake of the dIrr galaxy VCC1217 / IC3418

Author

Fumagalli, Mattia, Gavazzi, Giuseppe, Scaramella, Roberto, and Franzetti, Paolo

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A complex of Halpha emitting blobs with strong FUV excess is associated to the dIrr galaxy VCC1217 / IC3418 (Hester et al. 2010), and extends up to 17 Kpc in the South-East direction. These outstanding features can be morphologically divided into diffuse filaments and compact knots, where most of the star formation activity traced by Halpha takes place. We investigate the properties of the galaxy and the blobs using a multiwavelength approach in order to constrain their origin. We collect publicly available data in UV and Halpha and observe the scene in the optical U,g,r,i bands with LBT. The photometric data allows to evaluate the star formation rate and to perform a SED fitting separately of the galaxy and the blobs in order to constrain their stellar population age. Moreover we analyze the color and luminosity profile of the galaxy and its spectrum to investigate its recent interaction with the Virgo cluster. Our analysis confirms that the most plausible mechanism for the formation of the blobs is ram pressure stripping by the Virgo cluster IGM. The galaxy colors, luminosity profile and SED are consistent with a sudden gas depletion in the last few hundred Myr. The SED fitting of the blobs constrains their ages in < 400 Myr., Comment: 10 pages, 11 figures, accepted for publication in Astronomy and Astrophysics

Published
2010
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20. Constraining Modified Gravity with Euclid

Author

Martinelli, Matteo, Calabrese, Erminia, De Bernardis, Francesco, Melchiorri, Alessandro, Pagano, Luca, and Scaramella, Roberto

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics, High Energy Physics - Phenomenology
Abstract

Future proposed satellite missions as Euclid can offer the opportunity to test general relativity on cosmic scales through mapping of the galaxy weak lensing signal. In this paper we forecast the ability of these experiments to constrain modified gravity scenarios as those predicted by scalar-tensor and $f(R)$ theories. We found that Euclid will improve constraints expected from the PLANCK satellite on these modified gravity models by two orders of magnitude. We discuss parameter degeneracies and the possible biases introduced by modified gravity.

Published
2010
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22. The VST - VLT Survey Telescope

Author

Arnaboldi, Magda, Capaccioli, Massimo, Mancini, Dario, Scaramella, Roberto, Sedmak, Giorgio, Kurz, Richard, Bergeron, Jacqueline, editor, and Renzini, Alvio, editor

Published
2000
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24. Euclid preparation - XVII. Cosmic Dawn Survey: Spitzer Space Telescope observations of the Euclid deep fields and calibration fields

Author

Euclid Collaboration, Moneti, A., McCracken, H. J., Shuntov, M., Kauffmann, O. B., Capak, P., Davidzon, I., Ilbert, O., Scarlata, C., Toft, S., Weaver, J., Pires, S., Poncet, M., Popa, L., POZZETTI, Lucia, Raison, F., Rebolo, R., Rhodes, J., Rix, H., Roncarelli, M., Rossetti, E., Chary, R., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespí, P., Taylor, A. N., Cuby, J., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., ANDREON, Stefano, BARDELLI, Sandro, Faisst, A. L., Camera, S., Graciá-Carpio, J., Medinaceli, E., Mei, S., Polenta, G., Romelli, Erik, Sureau, F., Tenti, M., Vassallo, T., ZACCHEI, Andrea, Masters, D. C., ZUCCA, Elena, Baccigalupi, C., Balaguera-Antolínez, A., Bernardeau, F., BIVIANO, ANDREA, BOLZONELLA, MICOL, Bozzo, E., BURIGANA, CARLO, Cabanac, R., CAPPI, Alberto, McPartland, C., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Di Ferdinando, D., FARINA, Maria, FINELLI, FABIO, Flose-Reimberg, P., Mobasher, B., Fotopoulou, S., GALEOTTA, Samuele, Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I., Joachimi, B., Kansal, V., Keihanen, E., Sanders, D. B., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., MORGANTE, GIANLUCA, SCARAMELLA, Roberto, Morisset, N., Nucita, A., Patrizii, L., Potter, D., Renzi, A., RICCIO, GIUSEPPE, Sánchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Stern, D., Scottez, V., SEFUSATTI, Emiliano, Teyssier, R., Tubio, O., Tutusaus, I., Valiviita, J., VIEL, MATTEO, Hildebrandt, H., Szapudi, I., Teplitz, H., Zalesky, L., Amara, A., AURICCHIO, NATALIA, Bodendorf, C., BONINO, Donata, Branchini, Enzo, Brau-Nogue, S., BRESCIA, Massimo, Brinchmann, J., Capobianco, Vito, CARBONE, Carmelita, Carretero, J., Castander, F. J., CASTELLANO, MARCO, CAVUOTI, STEFANO, Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., CORCIONE, Leonardo, Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., FRAILIS, Marco, FRANCESCHI, ENRICO, FUMANA, Marco, GARILLI, BIANCA MARIA ROSA, Gillis, B., GIOCOLI, Carlo, Granett, B. R., GRAZIAN, Andrea, Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kümmel, M., Kunz, M., Kurki-Suonio, H., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., MAIORANO, Elisabetta, MANSUTTI, Oriana, Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., MENEGHETTI, MASSIMO, MERLIN, Emiliano, Meylan, G., Moresco, M., Moscardini, L., Munari, Emiliano, Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Euclid Collaboration, Moneti, A., Mccracken, H. J., Shuntov, M., Kauffmann, O. B., Capak, P., Davidzon, I., Ilbert, O., Scarlata, C., Toft, S., Weaver, J., Chary, R., Cuby, J., Faisst, A. L., Masters, D. C., Mcpartland, C., Mobasher, B., Sanders, D. B., Scaramella, R., Stern, D., Szapudi, I., Teplitz, H., Zalesky, L., Amara, A., Auricchio, N., Bodendorf, C., Bonino, D., Branchini, E., Brau-Nogue, S., Brescia, M., Brinchmann, J., Capobianco, V., Carbone, C., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Garilli, B., Gillis, B., Giocoli, C., Granett, B. R., Grazian, A., Grupp, F., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., K??mmel, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Mansutti, O., Marggraf, O., Markovic, K., Marulli, F., Massey, R., Maurogordato, S., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Rix, H., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Cresp??, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Andreon, S., Bardelli, S., Camera, S., Graci??-Carpio, J., Medinaceli, E., Mei, S., Polenta, G., Romelli, E., Sureau, F., Tenti, M., Vassallo, T., Zacchei, A., Zucca, E., Baccigalupi, C., Balaguera-Antol??nez, A., Bernardeau, F., Biviano, A., Bolzonella, M., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Di Ferdinando, D., Farina, M., Finelli, F., Flose-Reimberg, P., Fotopoulou, S., Galeotta, S., Ganga, K., Garcia-Bellido, J., Gaztanaga, E., Gozaliasl, G., Hook, I., Joachimi, B., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Maoli, R., Martinelli, M., Martinet, N., Maturi, M., Metcalf, R. B., Morgante, G., Morisset, N., Nucita, A., Patrizii, L., Potter, D., Renzi, A., Riccio, G., S??nchez, A. G., Sapone, D., Schirmer, M., Schultheis, M., Scottez, V., Sefusatti, E., Teyssier, R., Tubio, O., Tutusaus, I., Valiviita, J., Viel, M., Hildebrandt, H., Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, UAM. Departamento de Física Teórica, Moneti A., Mccracken H.J., Shuntov M., Kauffmann O.B., Capak P., Davidzon I., Ilbert O., Scarlata C., Toft S., Weaver J., Chary R., Cuby J., Faisst A.L., Masters D.C., Mcpartland C., Mobasher B., Sanders D.B., Scaramella R., Stern D., Szapudi I., Teplitz H., Zalesky L., Amara A., Auricchio N., Bodendorf C., Bonino D., Branchini E., Brau-Nogue S., Brescia M., Brinchmann J., Capobianco V., Carbone C., Carretero J., Castander F.J., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Costille A., Cropper M., Da Silva A., Degaudenzi H., Douspis M., Dubath F., Duncan C.A.J., Dupac X., Dusini S., Farrens S., Ferriol S., Fosalba P., Frailis M., Franceschi E., Fumana M., Garilli B., Gillis B., Giocoli C., Granett B.R., Grazian A., Grupp F., Haugan S.V.H., Hoekstra H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kermiche S., Kiessling A., Kilbinger M., Kitching T., Kohley R., Kummel M., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maiorano E., Mansutti O., Marggraf O., Markovic K., Marulli F., Massey R., Maurogordato S., Meneghetti M., Merlin E., Meylan G., Moresco M., Moscardini L., Munari E., Niemi S.M., Padilla C., Paltani S., Pasian F., Pedersen K., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Rebolo R., Rhodes J., Rix H., Roncarelli M., Rossetti E., Saglia R., Schneider P., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Tallada-Crespi P., Taylor A.N., Tereno I., Toledo-Moreo R., Torradeflot F., Wang Y., Welikala N., Weller J., Zamorani G., Zoubian J., Andreon S., Bardelli S., Camera S., Gracia-Carpio J., Medinaceli E., Mei S., Polenta G., Romelli E., Sureau F., Tenti M., Vassallo T., Zacchei A., Zucca E., Baccigalupi C., Balaguera-Antolinez A., Bernardeau F., Biviano A., Bolzonella M., Bozzo E., Burigana C., Cabanac R., Cappi A., Carvalho C.S., Casas S., Castignani G., Colodro-Conde C., Coupon J., Courtois H.M., Di Ferdinando D., Farina M., Finelli F., Flose-Reimberg P., Fotopoulou S., Galeotta S., Ganga K., Garcia-Bellido J., Gaztanaga E., Gozaliasl G., Hook I., Joachimi B., Kansal V., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Maoli R., Martinelli M., Martinet N., Maturi M., Metcalf R.B., Morgante G., Morisset N., Nucita A., Patrizii L., Potter D., Renzi A., Riccio G., Sanchez A.G., Sapone D., Schirmer M., Schultheis M., Scottez V., Sefusatti E., Teyssier R., Tubio O., Tutusaus I., Valiviita J., Viel M., Hildebrandt H., Kummel, M., Tallada-Crespi, P., Gracia-Carpio, J., Balaguera-Antolinez, A., and Sanchez, A. G.

Subjects
SAMPLE, Large-scale structure of Universe, DATA RELEASE, Formation, Surveys, observations, Dark energy, Dark matter, Galaxy: formation, Large-scale structure of Universe, Surveys [Cosmology], kosmologia, Astrophysics, Cosmology: observation, dark matter, galaksijoukot, pimeä aine, surveys, Dark energy, Dark matter, observations [Cosmology], dark energy, Observations, LEGACY SURVEY, Astrophysics of Galaxies, Física, Astronomy and Astrophysics, 115 Astronomy, Space science, EVOLUTION, Cosmology, galaksit, GALAXIES, Cosmology: observations, Galaxy: formation, Galaxy, formation [Galaxy], Space and Planetary Science, cosmology: observations, large-scale structure of Universe, pimeä energia, Cosmology and Nongalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Artículo escrito por un elevado núnmero de autores, sólo se referencian el qque aparece en primer lugar, los autores pertenecientes a la UAM y el nombre del grupo de colaboración, si lo hubiere, We present a new infrared survey covering the three Euclid deep fields and four other Euclid calibration fields using Spitzer Space Telescope's Infrared Array Camera (IRAC). We combined these new observations with all relevant IRAC archival data of these fields in order to produce the deepest possible mosaics of these regions. In total, these observations represent nearly 11 % of the total Spitzer Space Telescope mission time. The resulting mosaics cover a total of approximately 71.5 deg2 in the 3.6 and 4.5 μm bands, and approximately 21.8 deg2 in the 5.8 and 8 μm bands. They reach at least 24 AB magnitude (measured to 5σ, in a 2″​​.5 aperture) in the 3.6 μm band and up to ∼5 mag deeper in the deepest regions. The astrometry is tied to the Gaia astrometric reference system, and the typical astrometric uncertainty for sources with 16 "< "[3.6]< 19 is ≲ 0″​​.15. The photometric calibration is in excellent agreement with previous WISE measurements. We extracted source number counts from the 3.6 μm band mosaics, and they are in excellent agreement with previous measurements. Given that the Spitzer Space Telescope has now been decommissioned, these mosaics are likely to be the definitive reduction of these IRAC data. This survey therefore represents an essential first step in assembling multi-wavelength data on the Euclid deep fields, which are set to become some of the premier fields for extragalactic astronomy in the 2020s

Published
2022
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25. Euclid preparation XV. Forecasting cosmological constraints for the Euclid and CMB joint analysis

Author

Euclid Collaboration, Ilić, S., Aghanim, N., Baccigalupi, C., BERMEJO CLIMENT, JOSE RAMON, Fabbian, G., Legrand, L., PAOLETTI, DANIELA, Ballardini, M., Archidiacono, M., Douspis, M., Kubik, B., Kümmel, M., Kurki-Suonio, H., Laureijs, R., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., MANSUTTI, Oriana, Marggraf, O., Marulli, F., FINELLI, FABIO, Massey, R., Maurogordato, S., MENEGHETTI, MASSIMO, MERLIN, Emiliano, Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, Emiliano, Niemi, S. M., Ganga, K., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Percival, W., Pires, S., Poncet, M., Popa, L., POZZETTI, Lucia, Raison, F., Hernández-Monteagudo, C., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., SCARAMELLA, Roberto, Schneider, P., Secroun, A., Seidel, G., Serrano, S., LATTANZI, Mario Gilberto, Sirignano, C., Starck, J. L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., VALENZIANO, LUCA, Verdoes Kleijn, G. A., Marinucci, D., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Medinaceli, E., Mei, S., Rosset, C., Sureau, F., Vassallo, T., Migliaccio, M., ZACCHEI, Andrea, ANDREON, Stefano, Balaguera-Antolínez, A., Baldi, M., BARDELLI, Sandro, BIVIANO, ANDREA, BORGANI, STEFANO, Bozzo, E., BURIGANA, CARLO, Cabanac, R., CARBONE, Carmelita, CAPPI, Alberto, Carvalho, C. S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J., de la Torre, S., Di Ferdinando, D., Dole, H., Casas, S., FARINA, Maria, Ferreira, P. G., Flose-Reimberg, P., GALEOTTA, Samuele, Gozaliasl, G., Graciá-Carpio, J., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Martinelli, M., Maino, D., Martinet, N., Maturi, M., Metcalf, R. B., MORGANTE, GIANLUCA, Neissner, C., Nightingale, J., Nucita, A. A., Potter, D., RICCIO, GIUSEPPE, Tutusaus, I., Romelli, Erik, Schirmer, M., Schultheis, M., Scottez, V., Teyssier, R., Tramacere, A., Valiviita, J., VIEL, MATTEO, Whittaker, L., ZUCCA, Elena, Natoli, P., Ntelis, P., Pagano, L., Wenzl, L., GRUPPUSO, ALESSANDRO, Kitching, T., Langer, M., Mauri, N., Patrizii, L., Renzi, A., Sirri, G., Stanco, L., Tenti, M., Vielzeuf, P., Lacasa, F., Polenta, G., Yankelevich, V., Blanchard, A., Sakr, Z., Pourtsidou, A., Camera, S., CARDONE, Vincenzo Fabrizio, Kilbinger, M., Kunz, M., Markovic, K., Pettorino, V., Sánchez, A. G., Sapone, D., Amara, A., AURICCHIO, NATALIA, Bender, R., Bodendorf, C., BONINO, Donata, Branchini, Enzo, BRESCIA, Massimo, Brinchmann, J., Capobianco, Vito, Carretero, J., Castander, F. J., CASTELLANO, MARCO, CAVUOTI, STEFANO, Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., CORCIONE, Leonardo, Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Ealet, A., Farrens, S., Fosalba, P., FRAILIS, Marco, FRANCESCHI, ENRICO, FRANZETTI, PAOLO, FUMANA, Marco, GARILLI, BIANCA MARIA ROSA, Gillard, W., Gillis, B., GIOCOLI, Carlo, GRAZIAN, Andrea, Grupp, F., Guzzo, L., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kohley, R., Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Universidad de La Laguna [Tenerife - SP] (ULL), Instituto de Astrofisica de Canarias (IAC), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), International Center for Relativistic Astrophysics (ICRA), Università degli Studi di Roma, Dipartimento di Matematica [Roma II] (DIPMAT), Università degli Studi di Roma Tor Vergata [Roma], Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National d'Études Spatiales [Toulouse] (CNES), Herschel Science Center [Madrid], European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Paris-Saclay, Université Paris Cité (UPCité), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), Centre de Calcul de l'IN2P3 (CC-IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Euclid Collaboration, Astronomy, Intelligent Systems, Ilic S., Aghanim N., Baccigalupi C., Bermejo-Climent J.R., Fabbian G., Legrand L., Paoletti D., Ballardini M., Archidiacono M., Douspis M., Finelli F., Ganga K., Hernandez-Monteagudo C., Lattanzi M., Marinucci D., Migliaccio M., Carbone C., Casas S., Martinelli M., Tutusaus I., Natoli P., Ntelis P., Pagano L., Wenzl L., Gruppuso A., Kitching T., Langer M., Mauri N., Patrizii L., Renzi A., Sirri G., Stanco L., Tenti M., Vielzeuf P., Lacasa F., Polenta G., Yankelevich V., Blanchard A., Sakr Z., Pourtsidou A., Camera S., Cardone V.F., Kilbinger M., Kunz M., Markovic K., Pettorino V., Sanchez A.G., Sapone D., Amara A., Auricchio N., Bender R., Bodendorf C., Bonino D., Branchini E., Brescia M., Brinchmann J., Capobianco V., Carretero J., Castander F.J., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Congedo G., Conselice C.J., Conversi L., Copin Y., Corcione L., Costille A., Cropper M., Da Silva A., Degaudenzi H., Dubath F., Duncan C.A.J., Dupac X., Dusini S., Ealet A., Farrens S., Fosalba P., Frailis M., Franceschi E., Franzetti P., Fumana M., Garilli B., Gillard W., Gillis B., Giocoli C., Grazian A., Grupp F., Guzzo L., Haugan S.V.H., Hoekstra H., Holmes W., Hormuth F., Hudelot P., Jahnke K., Kermiche S., Kiessling A., Kohley R., Kubik B., Kummel M., Kurki-Suonio H., Laureijs R., Ligori S., Lilje P.B., Lloro I., Mansutti O., Marggraf O., Marulli F., Massey R., Maurogordato S., Meneghetti M., Merlin E., Meylan G., Moresco M., Morin B., Moscardini L., Munari E., Niemi S.M., Padilla C., Paltani S., Pasian F., Pedersen K., Percival W., Pires S., Poncet M., Popa L., Pozzetti L., Raison F., Rebolo R., Rhodes J., Roncarelli M., Rossetti E., Saglia R., Scaramella R., Schneider P., Secroun A., Seidel G., Serrano S., Sirignano C., Starck J.L., Tallada-Crespi P., Taylor A.N., Tereno I., Toledo-Moreo R., Torradeflot F., Valentijn E.A., Valenziano L., Verdoes Kleijn G.A., Wang Y., Welikala N., Weller J., Zamorani G., Zoubian J., Medinaceli E., Mei S., Rosset C., Sureau F., Vassallo T., Zacchei A., Andreon S., Balaguera-Antolinez A., Baldi M., Bardelli S., Biviano A., Borgani S., Bozzo E., Burigana C., Cabanac R., Cappi A., Carvalho C.S., Castignani G., Colodro-Conde C., Coupon J., Courtois H.M., Cuby J., De La Torre S., Di Ferdinando D., Dole H., Farina M., Ferreira P.G., Flose-Reimberg P., Galeotta S., Gozaliasl G., Gracia-Carpio J., Keihanen E., Kirkpatrick C.C., Lindholm V., Mainetti G., Maino D., Martinet N., Maturi M., Metcalf R.B., Morgante G., Neissner C., Nightingale J., Nucita A.A., Potter D., Riccio G., Romelli E., Schirmer M., Schultheis M., Scottez V., Teyssier R., Tramacere A., Valiviita J., Viel M., Whittaker L., Zucca E., Euclid, Collaboration, Ilić, S., Aghanim, N., Baccigalupi, C., Bermejo-Climent, J. R., Fabbian, G., Legrand, L., Paoletti, D., Ballardini, M., Archidiacono, M., Douspis, M., Finelli, F., Ganga, K., Hernández-Monteagudo, C., Lattanzi, M., Marinucci, D., Migliaccio, M., Carbone, C., Casas, S., Martinelli, M., Tutusaus, I., Natoli, P., Ntelis, P., Pagano, L., Wenzl, L., Gruppuso, A., Kitching, T., Langer, M., Mauri, N., Patrizii, L., Renzi, A., Sirri, G., Stanco, L., Tenti, M., Vielzeuf, P., Lacasa, F., Polenta, G., Yankelevich, V., Blanchard, A., Sakr, Z., Pourtsidou, A., Camera, S., Cardone, V. F., Kilbinger, M., Kunz, M., Markovic, K., Pettorino, V., Sánchez, A. G., Sapone, D., Amara, A., Auricchio, N., Bender, R., Bodendorf, C., Bonino, D., Branchini, E., Brescia, M., Brinchmann, J., Capobianco, V., Carretero, J., Castander, F. J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Costille, A., Cropper, M., Da Silva, A., Degaudenzi, H., Dubath, F., Duncan, C. A. J., Dupac, X., Dusini, S., Ealet, A., Farrens, S., Fosalba, P., Frailis, M., Franceschi, E., Franzetti, P., Fumana, M., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Grazian, A., Grupp, F., Guzzo, L., Haugan, S. V. H., Hoekstra, H., Holmes, W., Hormuth, F., Hudelot, P., Jahnke, K., Kermiche, S., Kiessling, A., Kohley, R., Kubik, B., Kümmel, M., Kurki-Suonio, H., Laureijs, R., Ligori, S., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Marulli, F., Massey, R., Maurogordato, S., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Morin, B., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Percival, W., Pires, S., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Scaramella, R., Schneider, P., Secroun, A., Seidel, G., Serrano, S., Sirignano, C., Starck, J. L., Tallada-Crespí, P., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Valentijn, E. A., Valenziano, L., Verdoes Kleijn, G. A., Wang, Y., Welikala, N., Weller, J., Zamorani, G., Zoubian, J., Medinaceli, E., Mei, S., Rosset, C., Sureau, F., Vassallo, T., Zacchei, A., Andreon, S., Balaguera-Antolínez, A., Baldi, M., Bardelli, S., Biviano, A., Borgani, S., Bozzo, E., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Castignani, G., Colodro-Conde, C., Coupon, J., Courtois, H. M., Cuby, J., de la Torre, S., Di Ferdinando, D., Dole, H., Farina, M., Ferreira, P. G., Flose-Reimberg, P., Galeotta, S., Gozaliasl, G., Graciá-Carpio, J., Keihanen, E., Kirkpatrick, C. C., Lindholm, V., Mainetti, G., Maino, D., Martinet, N., Maturi, M., Metcalf, R. B., Morgante, G., Neissner, C., Nightingale, J., Nucita, A. A., Potter, D., Riccio, G., Romelli, E., Schirmer, M., Schultheis, M., Scottez, V., Teyssier, R., Tramacere, A., Valiviita, J., Viel, M., Whittaker, L., Zucca, E., Department of Physics, Research Program in Systems Oncology, Helsinki Institute of Physics, Ilic, S., Hernandez-Monteagudo, C., Sanchez, A. G., Kummel, M., Tallada-Crespi, P., Balaguera-Antolinez, A., De La Torre, S., Gracia-Carpio, J., Ili??, S., Hern??ndez-Monteagudo, C., S??nchez, A. G., K??mmel, M., Tallada-Cresp??, P., Balaguera-Antol??nez, A., and Graci??-Carpio, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, statistical [methods], FOS: Physical sciences, Astrophysics, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, Joint analysis, kosmologia, 01 natural sciences, methods, NO, pimeä aine, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], mikroaallot, Settore FIS/05 - Astronomia e Astrofisica, surveys, 0103 physical sciences, tsz, survey, 010303 astronomy & astrophysics, Physics, methods: statistical, 010308 nuclear & particles physics, Computer Science::Information Retrieval, maailmankaikkeus, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, cross-correlation, 115 Astronomy, Space science, Cosmic background radiation, Large-scale structure of Universe, Methods: statistical, Surveys, kosminen taustasäteily, Space and Planetary Science, method, large-scale structure of Universe, pimeä energia, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The combination and cross-correlation of the upcoming $Euclid$ data with cosmic microwave background (CMB) measurements is a source of great expectation since it will provide the largest lever arm of epochs, ranging from recombination to structure formation across the entire past light cone. In this work, we present forecasts for the joint analysis of $Euclid$ and CMB data on the cosmological parameters of the standard cosmological model and some of its extensions. This work expands and complements the recently published forecasts based on $Euclid$-specific probes, namely galaxy clustering, weak lensing, and their cross-correlation. With some assumptions on the specifications of current and future CMB experiments, the predicted constraints are obtained from both a standard Fisher formalism and a posterior-fitting approach based on actual CMB data. Compared to a $Euclid$-only analysis, the addition of CMB data leads to a substantial impact on constraints for all cosmological parameters of the standard $\Lambda$-cold-dark-matter model, with improvements reaching up to a factor of ten. For the parameters of extended models, which include a redshift-dependent dark energy equation of state, non-zero curvature, and a phenomenological modification of gravity, improvements can be of the order of two to three, reaching higher than ten in some cases. The results highlight the crucial importance for cosmological constraints of the combination and cross-correlation of $Euclid$ probes with CMB data., Comment: 20 pages, 8 figures, 5 tables, 1 appendix; updated to match version accepted by journal

Published
2022
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26. Euclid preparation

Author

Scaramella, Roberto, Casas, Ricard, Castander, Francisco J., Fosalba, Pablo, Serrano, S., Martinelli, Matteo, Tutusaus, Isaac, Euclid Collaboration, European Space Agency, Academy of Finland, Agenzia Spaziale Italiana, European Commission, Centre National D'Etudes Spatiales (France), and Fundação para a Ciência e a Tecnologia (Portugal)

Subjects
Methods: numerical, Dark energy, Dark matter, Space vehicles, Surveys
Abstract

Euclid Collaboration: R. Scaramella et al., Euclid is a mission of the European Space Agency that is designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (the Euclid Wide Survey: EWS) in visible and near-infrared bands, covering approximately 15 000 deg2 of extragalactic sky in six years. The wide-field telescope and instruments are optimised for pristine point spread function and reduced stray light, producing very crisp images. This paper presents the building of the Euclid reference survey: the sequence of pointings of EWS, deep fields, and calibration fields, as well as spacecraft movements followed by Euclid as it operates in a step-and-stare mode from its orbit around the Lagrange point L2. Each EWS pointing has four dithered frames; we simulated the dither pattern at the pixel level to analyse the effective coverage. We used up-to-date models for the sky background to define the Euclid region-of-interest (RoI). The building of the reference survey is highly constrained from calibration cadences, spacecraft constraints, and background levels; synergies with ground-based coverage were also considered. Via purposely built software, we first generated a schedule for the calibrations and deep fields observations. On a second stage, the RoI was tiled and scheduled with EWS observations, using an algorithm optimised to prioritise the best sky areas, produce a compact coverage, and ensure thermal stability. The result is the optimised reference survey RSD_2021A, which fulfils all constraints and is a good proxy for the final solution. The current EWS covers ≈14 500 deg2. The limiting AB magnitudes (5σ point-like source) achieved in its footprint are estimated to be 26.2 (visible band IE) and 24.5 (for near infrared bands YE, JE, HE); for spectroscopy, the Hα line flux limit is 2 × 10−16 erg−1 cm−2 s−1 at 1600 nm; and for diffuse emission, the surface brightness limits are 29.8 (visible band) and 28.4 (near infrared bands) mag arcsec−2., The Euclid Consortium acknowledges the European Space Agency and a number of agencies and institutes that have supported the development of Euclid, in particular the Academy of Finland, the Agenzia Spaziale Italiana, the Belgian Science Policy, the Canadian Euclid Consortium, the Centre National d’Etudes Spatiales, the Deutsches Zentrum für Luft-und Raumfahrt, the Danish Space Research Institute, the Fundação para a Ciência e a Tecnologia, the Ministerio de Economia y Competitividad, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Romanian Space Agency, the State Secretariat for Education, Research and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid website (http://www.euclid-ec.org).

Published
2022

30. Euclid preparation

Author

Euclid Collaboration, Paykari, P., Kitching, T., Hoekstra, H., Azzollini, R., CARDONE, Vincenzo Fabrizio, Cropper, M., Duncan, C. A. J., Kannawadi, A., Miller, L., Aussel, H., Polenta, G., Pourtsidou, A., Raison, F., Renzi, A., Rhodes, J., Romelli, Erik, Roncarelli, M., Rossetti, E., Saglia, R., Sakr, Z., Conti, I. F., Sánchez, A. G., Sapone, D., SCARAMELLA, Roberto, Schneider, P., Schrabback, T., Scottez, V., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., AURICCHIO, NATALIA, Stanco, L., Starck, J. -L., Sureau, F., Tallada-Crespí, P., Taylor, A., Tenti, M., Tereno, I., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Baldi, M., VALENZIANO, LUCA, Vannier, M., Vassallo, T., Zoubian, J., ZUCCA, Elena, BARDELLI, Sandro, Biviano, A., BONINO, Donata, Borsato, E., Bozzo, E., Branchini, Enzo Franco, Brau-Nogue, S., BRESCIA, Massimo, Brinchmann, J., BURIGANA, CARLO, Camera, S., Capobianco, Vito, CARBONE, Carmelita, Carretero, J., Casas, S., Castander, F. J., CASTELLANO, MARCO, CAVUOTI, STEFANO, Charles, Y., Cledassou, R., Colodro-Conde, C., Congedo, G., Conselice, C., Conversi, L., Copin, Y., Coupon, J., Courtois, H. M., Da Silva, A., Dupac, X., Fabbian, G., Farrens, S., Ferreira, P. G., Fosalba, P., Fourmanoit, N., FRAILIS, Marco, Fumana, M., GALEOTTA, Samuele, GARILLI, BIANCA MARIA ROSA, Gillard, W., Gillis, B. R., Giocoli, C., Graciá-Carpio, J., Grupp, F., Hormuth, F., Ilić, S., Israel, H., Jahnke, K., Keihanen, E., Kermiche, S., Kilbinger, M., Kirkpatrick, C. C., Kubik, B., Kunz, M., Kurki-Suonio, H., Lacasa, F., Laureijs, R., Le Mignant, D., LIGORI, Sebastiano, Lilje, P. B., Lloro, I., Maciaszek, T., MAIORANO, Elisabetta, Marggraf, O., Markovic, K., Martinelli, M., Martinet, N., Marulli, F., Massey, R., Mauri, N., MEDINACELI VILLEGAS, EDUARDO, Mei, S., Mellier, Y., MENEGHETTI, MASSIMO, Metcalf, R. B., Moresco, M., Moscardini, L., Munari, E., Neissner, C., Nichol, R. C., Niemi, S., Nutma, T., Padilla, C., Paltani, S., PASIAN, Fabio, Pettorino, V., Pires, S., Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Queen Mary University of London (QMUL), Institut d'Estudis Espacials de Catalunya (IEEC-CSIC), and Euclid Collaboration

Subjects
Physics, COSMIC cancer database, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, gravitational lensing: weak, Shear (geology), Space and Planetary Science, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, addenda, errata
Abstract

International audience; Authors Lacasa, Martinelli, Pourtsidou, Tutusaus, were inadvertently missed from the original authorship list. This is now corrected.

Published
2020
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32. Modelling of Zodiacal Light Emission for Space Missions

Author

MARIS, Michele, SCARAMELLA, Roberto, BURIGANA, CARLO, Romelli, Erik, Amiaux, Jerome, Carvalho, Carla Sofia, Cuillandre, Jean-Charles, Cunha Da Silva, Antonio Jose, De Rosa, Adriano, Dinis, Joao, Hudelot, Patrick, Maiorano, Ettore, Tereno, Ismael, TROMBETTI, Tiziana, ITA, FRA, and PRT

Subjects
Physics::Space Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

Accurate planning of forthcoming missions requires an accurate knowledge of diffuse sources in order to optimize mission parameters and the scanning strategy. Zodiacal Light (ZL or Zody) is a well known contaminant for ground based and space-borne observations and contributes to determine the limit magnitude of a survey. Despite the physical origin of ZL is well known, predicting and modeling Zody contamination is complicated by a number of subtleties. The cloud of Interplanetary Dust Particles has a quite complex 3D structure, whose main geometrical parameters have been assessed in the last two decades, but their photometrical properties are affected by a significant level of uncertainty. The observer orbiting the Sun is moving within the cloud of IDPs, leading to an important time dependence in the perturbing signal and asking for a precise knowledge of the expected trajectory and scanning strategy of the mission. This work illustrates this problem taking the ESA Euclid mission as a case study and presenting the Zody EUclid Simulator (ZEUS) developed for this mission.

Published
2019

34. The Euclid survey planning system (Conference Presentation)

Author

Gómez-Alvarez, Pedro, Dupac, Xavier, Buenadicha, Guillermo, Vavrek, Roland, Hoar, John, Laureijs, René, Scaramella, Roberto, Dinis, Joao, Amiaux, Jerôme, Tereno, Ismael, and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)

Subjects
Planning, Euclid, Space, Survey, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Cosmology
Abstract

International audience; The Euclid mission is a cosmological survey mission to map the geometry of the Dark Universe and to understand the nature of Dark Matter and Dark Energy. Euclid will use two main probes for these purposes: Weak Lensing and Galaxy Clustering, measuring billions of galaxy shapes and millions of galaxies redshifts. Euclid will execute a wide survey covering part of the Extragalactic sky (15.000 degrees2) and three deep surveys near the ecliptic poles plus calibration fields. Mission planning is a key aspect to optimize the scientific return of the mission. There are a number of technical aspects that should be taken into account: restricted sky area at a given time due to spacecraft pointing constraints, Wide/Deep surveys and calibration interleaving, density of galaxies and stars, extinction, zodiacal light, CCD degradation, straylight, due to science payload constraints and constraints imposed by the galactic foreground components. The so-called Euclid Survey System (ESS) is the mission planning software infrastructure, developed by ESA at ESAC to support operational planning. This software has been already used to produce and evaluate several versions of the so-called reference surveys used to support other aspects of the mission. The Euclid Survey Planning System also has to interact with several actors: The scientific group in the Euclid Consortium in charge of designing the survey, the Instruments Design and Operation groups (IDTs/IOTs), ESA Operations Centre in Darmstadt (Germany), the Euclid Archive and it also needs also to produce reports which will help assessing the status of the survey and its level of scientific performance.

Published
2018
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37. Cosmology and fundamental physics with the Euclid satellite

Author

Amendola, Luca, Appleby, Stephen, Avgoustidis, Anastasios, Bacon, David, Baker, Tessa, Baldi, Marco, Bartolo, Nicola, Blanchard, Alain, Bonvin, Camille, Borgani, Stefano, Branchini, Enzo, Burrage, Clare, Camera, Stefano, Carbone, Carmelita, Casarini, Luciano, Cropper, Mark, de Rham, Claudia, Dietrich, Joerg P., Di Porto, Cinzia, Durrer, Ruth, Ealet, Anne, Ferreira, Pedro G., Finelli, Fabio, Garcia-Bellido, Juan, Giannantonio, Tommaso, Guzzo, Luigi, Heavens, Alan, Heisenberg, Lavinia, Heymans, Catherine, Hoekstra, Henk, Hollenstein, Lukas, Holmes, Rory, Hwang, Zhiqi, Jahnke, Knud, Kitching, Thomas D., Koivisto, Tomi, Kunz, Martin, La Vacca, Giuseppe, Linder, Eric, March, Marisa, Marra, Valerio, Martins, Carlos, Majerotto, Elisabetta, Markovic, Dida, Marsh, David, Marulli, Federico, Massey, Richard, Mellier, Yannick, Montanari, Francesco, Mota, David F., Nunes, Nelson J., Percival, Will, Pettorino, Valeria, Porciani, Cristiano, Quercellini, Claudia, Read, Justin, Rinaldi, Massimiliano, Sapone, Domenico, Sawicki, Ignacy, Scaramella, Roberto, Skordis, Constantinos, Simpson, Fergus, Taylor, Andy, Thomas, Shaun, Trotta, Roberto, Verde, Licia, Vernizzi, Filippo, Vollmer, Adrian, Wang, Yun, Weller, Jochen, Zlosnik, Tom, Amendola, Luca, Appleby, Stephen, Avgoustidis, Anastasios, Bacon, David, Baker, Tessa, Baldi, Marco, Bartolo, Nicola, Blanchard, Alain, Bonvin, Camille, Borgani, Stefano, Branchini, Enzo, Burrage, Clare, Camera, Stefano, Carbone, Carmelita, Casarini, Luciano, Cropper, Mark, de Rham, Claudia, Dietrich, Joerg P., Di Porto, Cinzia, Durrer, Ruth, Ealet, Anne, Ferreira, Pedro G., Finelli, Fabio, Garcia-Bellido, Juan, Giannantonio, Tommaso, Guzzo, Luigi, Heavens, Alan, Heisenberg, Lavinia, Heymans, Catherine, Hoekstra, Henk, Hollenstein, Lukas, Holmes, Rory, Hwang, Zhiqi, Jahnke, Knud, Kitching, Thomas D., Koivisto, Tomi, Kunz, Martin, La Vacca, Giuseppe, Linder, Eric, March, Marisa, Marra, Valerio, Martins, Carlos, Majerotto, Elisabetta, Markovic, Dida, Marsh, David, Marulli, Federico, Massey, Richard, Mellier, Yannick, Montanari, Francesco, Mota, David F., Nunes, Nelson J., Percival, Will, Pettorino, Valeria, Porciani, Cristiano, Quercellini, Claudia, Read, Justin, Rinaldi, Massimiliano, Sapone, Domenico, Sawicki, Ignacy, Scaramella, Roberto, Skordis, Constantinos, Simpson, Fergus, Taylor, Andy, Thomas, Shaun, Trotta, Roberto, Verde, Licia, Vernizzi, Filippo, Vollmer, Adrian, Wang, Yun, Weller, Jochen, and Zlosnik, Tom

Abstract

Euclid is a European Space Agency medium-class mission selected for launch in 2020 within the cosmic vision 2015-2025 program. The main goal of Euclid is to understand the origin of the accelerated expansion of the universe. Euclid will explore the expansion history of the universe and the evolution of cosmic structures by measuring shapes and red-shifts of galaxies as well as the distribution of clusters of galaxies over a large fraction of the sky. Although the main driver for Euclid is the nature of dark energy, Euclid science covers a vast range of topics, from cosmology to galaxy evolution to planetary research. In this review we focus on cosmology and fundamental physics, with a strong emphasis on science beyond the current standard models. We discuss five broad topics: dark energy and modified gravity, dark matter, initial conditions, basic assumptions and questions of methodology in the data analysis. This review has been planned and carried out within Euclid's Theory Working Group and is meant to provide a guide to the scientific themes that will underlie the activity of the group during the preparation of the Euclid mission.

Published
2018
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40. Mission-level performance verification approach for the Euclid space mission

Author

Vavrek, Roland D., additional, Laureijs, René J., additional, Lorenzo Alvarez, Jose, additional, Amiaux, Jérôme, additional, Mellier, Yannick, additional, Azzollini, Ruyman, additional, Buenadicha, Guillermo, additional, Saavedra Criado, Gonzalo, additional, Cropper, Mark, additional, Dabin, Christophe, additional, Ealet, Anne, additional, Garilli, Bianca, additional, Gregorio, Anna, additional, Hoekstra, Henk, additional, Jahnke, Knud, additional, Kilbinger, Martin, additional, Kitching, Tom, additional, Hoar, John, additional, Percival, Will, additional, Racca, Giuseppe D., additional, Salvignol, Jean-Christophe, additional, Sauvage, Marc, additional, Scaramella, Roberto, additional, Gaspar Venancio, Luis M., additional, Wang, Yun, additional, Zacchei, Andrea, additional, and Wachter, Stefanie, additional

Published
2016
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41. The Euclid mission design

Author

Racca, Giuseppe D., additional, Laureijs, René, additional, Stagnaro, Luca, additional, Salvignol, Jean-Christophe, additional, Lorenzo Alvarez, José, additional, Saavedra Criado, Gonzalo, additional, Gaspar Venancio, Luis, additional, Short, Alex, additional, Strada, Paolo, additional, Bönke, Tobias, additional, Colombo, Cyril, additional, Calvi, Adriano, additional, Maiorano, Elena, additional, Piersanti, Osvaldo, additional, Prezelus, Sylvain, additional, Rosato, Pierluigi, additional, Pinel, Jacques, additional, Rozemeijer, Hans, additional, Lesna, Valentina, additional, Musi, Paolo, additional, Sias, Marco, additional, Anselmi, Alberto, additional, Cazaubiel, Vincent, additional, Vaillon, Ludovic, additional, Mellier, Yannick, additional, Amiaux, Jérôme, additional, Berthé, Michel, additional, Sauvage, Marc, additional, Azzollini, Ruyman, additional, Cropper, Mark, additional, Pottinger, Sabrina, additional, Jahnke, Knud, additional, Ealet, Anne, additional, Maciaszek, Thierry, additional, Pasian, Fabio, additional, Zacchei, Andrea, additional, Scaramella, Roberto, additional, Hoar, John, additional, Kohley, Ralf, additional, Vavrek, Roland, additional, Rudolph, Andreas, additional, and Schmidt, Micha, additional

Published
2016
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43. The VIMOS VLT deep survey : final public release of ~ 35 000 galaxies and active galactic nuclei covering 13 billion years of evolution

Author

Le Fèvre, Olivier, Adami, Christophe, Arnouts, Stéphane, Bardelli, Sandro, Bolzonella, Micol, Bondi, Marco, Bongiorno, Angela, Bottini, Dario, Cappi, Alberto, Cassata, Paolo, Charlot, Stéphane, Ciliegi, Paolo, Contini, Thierry, Cucciati, Olga, Torre, Sylvain de la, Foucaud, Sebastien, Franzetti, Paolo, Garilli, Bianca, Gavignaud, Isabelle, Guzzo, Luigi, Ilbert, Olivier, Iovino, Angela, Le Brun, Vincent, Lemaux, Brian, López-Sanjuan, Carlos, Maccagni, Dario, McCracken, Henry J., Marano, Bruno, Marinoni, Christian, Mazure, Alain, Mellier, Yannick, Merighi, Roberto, Merluzzi, Paolo, Moreau, Chrystel, Paltani, Stephane, Pellò, Roser, Pollo, Agnieszka, Pozzetti, Lucia, Scaramella, Roberto, Scodeggio, Marco, Tasca, Lidia, Tresse, Laurence, Vergani, Daniela, Vettolani, Giampaolo, Zamorani, Giovanni, Zanichelli, Alessandra, and Zucca, Elena

Abstract

The VIMOS VLT Deep Survey (VVDS) final and public data release offers an excellent opportunity to revisit galaxy evolution with a sample of 35 016 galaxies and active galactic nuclei covering the redshift range 0 < z < 6.7. The VVDS includes three tiered surveys, the wide, deep and ultra-deep surveys, covering up to 8.7 square degrees, and each magnitude-selected with limits i_{AB} = 22.5, 24 and 24.75 respectively. The VVDS redshifts, spectra, and all associated multi-wavelength data are available at http://cesam.lam.fr/vvds. The highlights and scientific legacy of the VVDS are summarised.

Published
2014

44. SKA synergy with Microwave Background studies

Author

Burigana, Carlo, primary, Alexander, Paul, additional, Baccigalupi, Carlo, additional, Barbosa, Domingos S., additional, Blanchard, Alain, additional, De Rosa, Adriano, additional, De Zotti, Gianfranco, additional, Finelli, Fabio, additional, Gruppuso, Alessandro, additional, Jones, M., additional, Matarrese, Sabino, additional, Melchiorri, Alessandro, additional, Molinari, Diego, additional, Negrello, Mattia, additional, Paoletti, Daniela, additional, Perrotta, Francesca, additional, Scaramella, Roberto, additional, and Trombetti, Tiziana, additional

Published
2015
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