14 results on '"Kitching, T. D."'
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2. Cosmic shear bias and calibration in dark energy studies.
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Taylor, A N and Kitching, T D
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DARK energy , *SHEAR (Mechanics) , *GRAVITY , *POWER spectra , *PARAMETER estimation - Abstract
With the advent of large-scale weak lensing surveys there is a need to understand how realistic, scale-dependent systematics bias cosmic shear and dark energy measurements, and how they can be removed. Here, we show how spatially varying image distortions are convolved with the shear field, mixing convergence E and B modes, and bias the observed shear power spectrum. In practise, many of these biases can be removed by calibration to data or simulations. The uncertainty in this calibration is marginalized over, and we calculate how this propagates into parameter estimation and degrades the dark energy Figure-of-Merit. We find that noise-like biases affect dark energy measurements the most, while spikes in the bias power have the least impact. We argue that, in order to remove systematic biases in cosmic shear surveys and maintain statistical power, effort should be put into improving the accuracy of the bias calibration rather than minimizing the size of the bias. In general, this appears to be a weaker condition for bias removal. We also investigate how to minimize the size of the calibration set for a fixed reduction in the Figure-of-Merit. Our results can be used to correctly model the effect of biases and calibration on a cosmic shear survey, assess their impact on the measurement of modified gravity and dark energy models, and to optimize survey and calibration requirements. [ABSTRACT FROM AUTHOR]
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- 2018
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3. Cosmology and fundamental physics with the Euclid satellite
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Amendola, L., Appleby, S., Bacon, D., Baker, T., Baldi, M., Bartolo, N., Blanchard, A., Bonvin, C., Borgani, S., Branchini, E., Burrage, C., Camera, S., Carbone, C., Casarini, L., Cropper, M., de Rham, C., Di Porto, C., Ealet, A., Ferreira, P. G., Finelli, F., García-Bellido, J., Giannantonio, T., Guzzo, L., Heavens, A., Heisenberg, L., Heymans, C., Hoekstra, H., Hollenstein, L., Holmes, R., Horst, O., Jahnke, K., Kitching, T. D., Koivisto, T., Kunz, M., La Vacca, G., March, M., Majerotto, E., Markovic, K., Marsh, D., Marulli, F., Massey, R., Mellier, Y., Mota, D. F., Nunes, N. J., Percival, W., Pettorino, V., Porciani, C., Quercellini, C., Read, J., Rinaldi, M., Sapone, D., Scaramella, R., Skordis, C., Simpson, F., Taylor, A., Thomas, S., Trotta, R., Verde, L., Vernizzi, F., Vollmer, A., Wang, Y., Weller, J., Zlosnik, T., Skordis, C. [0000-0001-5873-4259], 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), 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), Université Paris-Sud - Paris 11 (UP11), 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), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Amendola, Luca, Appleby, Stephen, Avgoustidis, Anastasio, 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, Jörg P., Di Porto, Cinzia, Durrer, Ruth, Ealet, Anne, Ferreira, Pedro G., Finelli, Fabio, García-Bellido, Juan, Giannantonio, Tommaso, Guzzo, Luigi, Heavens, Alan, Heisenberg, Lavinia, Heymans, Catherine, Hoekstra, Henk, Hollenstein, Luka, Holmes, Rory, Hwang, Zhiqi, Jahnke, Knud, Kitching, Thomas D., Koivisto, Tomi, Kunz, Martin, La Vacca, Giuseppe, Linder, Eric, March, Marisa, Marra, Valerio, Martins, Carlo, 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, Constantino, Simpson, Fergu, Taylor, Andy, Thomas, Shaun, Trotta, Roberto, Verde, Licia, Vernizzi, Filippo, Vollmer, Adrian, Wang, Yun, Weller, Jochen, Zlosnik, Tom, Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de Physique des Particules de Marseille ( CPPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Aix Marseille Université ( AMU ), Université Paris-Sud - Paris 11 ( UP11 ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Institut de Physique Théorique - UMR CNRS 3681 ( IPHT ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), 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), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Luca, Amendola, Stephen, Appleby, David, Bacon, Tessa, Baker, Marco, Baldi, Nicola, Bartolo, Alain, Blanchard, Camille, Bonvin, Enzo, Branchini, Clare, Burrage, Stefano, Camera, Carmelita, Carbone, Luciano, Casarini, Mark, Cropper, Claudia de, Rham, Cinzia Di, Porto, Anne, Ealet, Pedro G., Ferreira, Fabio, Finelli, Juan García, Bellido, Tommaso, Giannantonio, Luigi, Guzzo, Alan, Heaven, Lavinia, Heisenberg, Catherine, Heyman, Henk, Hoekstra, Lukas, Hollenstein, Rory, Holme, Ole, Horst, Knud, Jahnke, Thomas D., Kitching, Tomi, Koivisto, Martin, Kunz, Giuseppe La, Vacca, Marisa, March, Elisabetta, Majerotto, Katarina, Markovic, David, Marsh, Federico, Marulli, Richard, Massey, Yannick, Mellier, David F., Mota, Nelson J., Nune, Will, Percival, Valeria, Pettorino, Cristiano, Porciani, Claudia, Quercellini, Justin, Read, Massimiliano, Rinaldi, Domenico, Sapone, Roberto, Scaramella, Constantinos, Skordi, Fergus, Simpson, Andy, Taylor, Shaun, Thoma, Roberto, Trotta, Licia, Verde, Filippo, Vernizzi, Adrian, Vollmer, Yun, Wang, Jochen, Weller, Tom, Zlosnik, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Luca Amendola, Stephen Appleby, David Bacon, Tessa Baker, Marco Baldi, Nicola Bartolo, Alain Blanchard, Camille Bonvin, Stefano Borgani, Enzo Branchini, Clare Burrage, Stefano Camera, Carmelita Carbone, Luciano Casarini, Mark Cropper, Claudia de Rham, Cinzia Di Porto, Anne Ealet, Pedro G. Ferreira, Fabio Finelli, Juan García-Bellido, Tommaso Giannantonio, Luigi Guzzo, Alan Heaven, Lavinia Heisenberg, Catherine Heyman, Henk Hoekstra, Lukas Hollenstein, Rory Holme, Ole Horst, Knud Jahnke, Thomas D. Kitching, Tomi Koivisto, Martin Kunz, Giuseppe La Vacca, Marisa March, Elisabetta Majerotto, Katarina Markovic, David Marsh, Federico Marulli, Richard Massey, Yannick Mellier, David F. Mota, Nelson J. Nune, Will Percival, Valeria Pettorino, Cristiano Porciani, Claudia Quercellini, Justin Read, Massimiliano Rinaldi, Domenico Sapone, Roberto Scaramella, Constantinos Skordi, Fergus Simpson, Andy Taylor, Shaun Thoma, Roberto Trotta, Licia Verde, Filippo Vernizzi, Adrian Vollmer, Yun Wang, Jochen Weller, Tom Zlosnik, Dietrich, Jörg P, Ferreira, Pedro G, Kitching, Thomas D, Mota, David F, Nunes, Nelson J, Amendola, L, Appleby, S, Bacon, D, Baker, T, Baldi, M, Bartolo, N, Blanchard, A, Bonvin, C, Borgani, S, Branchini, E, Burrage, C, Camera, S, Carbone, C, Casarini, L, Cropper, M, de Rham, C, Di Porto, C, Ealet, A, Ferreira, P, Finelli, F, García Bellido, J, Giannantonio, T, Guzzo, L, Heavens, A, Heisenberg, L, Heymans, C, Hoekstra, H, Hollenstein, L, Holmes, R, Horst, O, Jahnke, K, Kitching, T, Koivisto, T, Kunz, M, LA VACCA, G, March, M, Majerotto, E, Markovic, K, Marsh, D, Marulli, F, Massey, R, Mellier, Y, Mota, D, Nunes, N, Percival, W, Pettorino, V, Porciani, C, Quercellini, C, Read, J, Rinaldi, M, Sapone, D, Scaramella, R, Skordis, C, Simpson, F, Taylor, A, Thomas, S, Trotta, R, Verde, L, Vernizzi, F, Vollmer, A, Wang, Y, Weller, J, Zlosnik, T, Science and Technology Facilities Council (STFC), Imperial College Trust, Science and Technology Facilities Council, Avgoustidis, A, Dietrich, J, Durrer, R, Garcia-Bellido, J, Hwang, Z, La Vacca, G, Linder, E, Marra, V, Martins, C, Markovic, D, Montanari, F, Sawicki, I, Ferreira Pedro, G., Horst, Ole, Kitching Thomas, D., Markovic, Katarina, Mota David, F., Nunes, Nelson, and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)
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Cosmology ,Dark energy ,Galaxy evolution ,Physics and Astronomy (miscellaneous) ,cosmological model ,Cold dark matter ,[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,gravitation: model ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Review Article ,Astrophysics ,01 natural sciences ,7. Clean energy ,General Relativity and Quantum Cosmology ,High Energy Physics - Phenomenology (hep-ph) ,GALAXY REDSHIFT SURVEY ,3-POINT CORRELATION-FUNCTION ,Cosmology and Extragalactic Astrophysic [Astrophysics] ,010303 astronomy & astrophysics ,Physics ,COSMIC cancer database ,galaxy: redshift ,PHYSICS, PARTICLES & FIELDS ,Mathematics::History and Overview ,formation ,Astrophysics::Instrumentation and Methods for Astrophysics ,hep-ph ,EQUATION-OF-STATE ,Nuclear & Particles Physics ,High Energy Physics - Phenomenology ,Physical Sciences ,astro-ph.CO ,galaxy: cluster ,NONLINEAR STRUCTURE FORMATION ,history ,expansion: acceleration ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Cosmic Vision ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,gr-qc ,Dark matter ,satellite ,FOS: Physical sciences ,General Relativity and Quantum Cosmology (gr-qc) ,Astrophysics::Cosmology and Extragalactic Astrophysics ,lcsh:Atomic physics. Constitution and properties of matter ,PRIMORDIAL NON-GAUSSIANITY ,dark matter ,Metric expansion of space ,GENERALIZED CHAPLYGIN-GAS ,[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO] ,FIS/05 - ASTRONOMIA E ASTROFISICA ,Settore FIS/05 - Astronomia e Astrofisica ,LARGE-SCALE STRUCTURE ,0103 physical sciences ,Galaxy formation and evolution ,High Energy Physics: Phenomenology ,FUTURE REDSHIFT SURVEYS ,structure ,Euclid Theory Working Group ,Science & Technology ,DIGITAL-SKY-SURVEY ,010308 nuclear & particles physics ,Astrophysics: Cosmology and Extragalactic Astrophysics ,Astronomy ,N-BODY SIMULATIONS ,MICROWAVE-ANISOTROPY-PROBE ,Phenomenology [High Energy Physics] ,Galaxy ,boundary condition ,lcsh:QC170-197 ,COLD DARK-MATTER ,0201 Astronomical And Space Sciences ,cosmology ,dark energy ,galaxy evolution ,LENSING MASS RECONSTRUCTION ,13. Climate action ,[PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] - 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
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- 2013
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4. Path-integral evidence.
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Kitching, T. D. and Taylor, A. N.
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BAYESIAN analysis , *ASTRONOMICAL perturbation , *GAUSSIAN distribution , *COSMOLOGICAL constant , *DARK energy , *DARK matter - Abstract
Here we present a Bayesian formalism for the goodness of fit that is the evidence for a fixed functional form over the evidence for all functions that are a general perturbation about this form. This is done under the assumption that the statistical properties of the data can be modelled by a multivariate Gaussian distribution. We use this to show how one can optimize an experiment to find evidence for a fixed function over perturbations about this function. We apply this formalism to an illustrative problem of measuring perturbations in the dark energy equation of state about a cosmological constant. [ABSTRACT FROM AUTHOR]
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- 2015
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5. 3D weak gravitational lensing of the CMB and galaxies.
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Kitching, T. D., Heavens, A. F., and Das, S.
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GRAVITATIONAL lenses , *POWER spectra , *POLARIZATION (Nuclear physics) , *DARK energy , *NEUTRINO mass - Abstract
In this paper, we present a power spectrum formalism that combines the full 3D information from the galaxy ellipticity field, with information from the cosmic microwave background (CMB). We include in this approach galaxy cosmic shear and galaxy intrinsic alignments, CMB deflection, CMB temperature, and CMB polarization data; including the interdatum power spectra between all quantities. We apply this to forecasting cosmological parameter errors for CMB and imaging surveys and show that the additional covariance between the CMB and ellipticity measurements can improve dark energy equation of state measurements by 30 per cent. We present predictions for Euclid-like, Planck, ACTPoL, and CoRE-like experiments and show that the combination of cosmic shear and the CMB, from Euclid-like and CoRE-like experiments, could in principle measure the sum of neutrino masses with an error of 0.003 eV, and the dark energy equation of state with an error on w0 of less than 0.02. [ABSTRACT FROM AUTHOR]
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- 2015
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6. 3D cosmic shear: cosmology from CFHTLenS.
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Kitching, T. D., Heavens, A. F., Alsing, J., Erben, T., Heymans, C., Hildebrandt, H., Hoekstra, H., Jaffe, A., Kiessling, A., Mellier, Y., Miller, L., van Waerbeke, L., Benjamin, J., Coupon, J., Fu, L., Hudson, M. J., Kilbinger, M., Kuijken, K., Rowe, B. T. P., and Schrabback, T.
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METAPHYSICAL cosmology , *SPHERICAL harmonics , *REDSHIFT , *ANISOTROPY , *TOMOGRAPHY , *DARK energy - Abstract
This paper presents the first application of 3D cosmic shear to a wide-field weak lensing survey. 3D cosmic shear is a technique that analyses weak lensing in three dimensions using a spherical harmonic approach, and does not bin data in the redshift direction. This is applied to CFHTLenS, a 154 square degree imaging survey with a median redshift of 0.7 and an effective number density of 11 galaxies per square arcminute usable for weak lensing. To account for survey masks we apply a 3D pseudo-Cℓ approach on weak lensing data, and to avoid uncertainties in the highly non-linear regime, we separately analyse radial wavenumbers k ≤ 1.5 and 5.0 h Mpc−1, and angular wavenumbers ℓ ≈ 400–5000. We show how one can recover 2D and tomographic power spectra from the full 3D cosmic shear power spectra and present a measurement of the 2D cosmic shear power spectrum, and measurements of a set of 2-bin and 6-bin cosmic shear tomographic power spectra; in doing so we find that using the 3D power in the calculation of such 2D and tomographic power spectra from data naturally accounts for a minimum scale in the matter power spectrum. We use 3D cosmic shear to constrain cosmologies with parameters ΩM, ΩB, σ8, h , ns, w0 and wa. For a non-evolving dark energy equation of state, and assuming a flat cosmology, lensing combined with Wilkinson Microwave Anisotropy Probe 7 results in h = 0.78 ± 0.12, ΩM = 0.252 ± 0.079, σ8 = 0.88 ± 0.23 and w = −1.16 ± 0.38 using only scales k ≤ 1.5 h Mpc−1. We also present results of lensing combined with first year Planck results, where we find no tension with the results from this analysis, but we also find no significant improvement over the Planck results alone. We find evidence of a suppression of power compared to Lambda cold dark matter (LCDM) on small scales 1.5 < k ≤ 5.0 h Mpc−1 in the lensing data, which is consistent with predictions of the effect of baryonic feedback on the matter power spectrum. [ABSTRACT FROM AUTHOR]
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- 2014
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7. The impact of galaxy colour gradients on cosmic shear measurement.
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Voigt, L. M., Bridle, S. L., Amara, A., Cropper, M., Kitching, T. D., Massey, R., Rhodes, J., and Schrabback, T.
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GALAXIES ,SHEAR (Mechanics) ,CONSTRAINTS (Physics) ,DARK energy ,ATMOSPHERE ,WAVELENGTHS ,SIGNAL-to-noise ratio - Abstract
ABSTRACT Cosmic shear has been identified as the method with the most potential to constrain dark energy. To capitalize on this potential, it is necessary to measure galaxy shapes with great accuracy, which in turn requires a detailed model for the image blurring by the telescope and atmosphere, the point spread function (PSF). In general, the PSF varies with wavelength and therefore the PSF integrated over an observing filter depends on the spectrum of the object. For a typical galaxy the spectrum varies across the galaxy image, thus the PSF depends on the position within the image. We estimate the bias on the shear due to such colour gradients by modelling galaxies using two co-centred, co-elliptical Sérsic profiles, each with a different spectrum. We estimate the effect of ignoring colour gradients and find the shear bias from a single galaxy can be very large depending on the properties of the galaxy. We find that halving the filter width reduces the shear bias by a factor of about 5. We show that, to the first order, tomographic cosmic shear two point statistics depend on the mean shear bias over the galaxy population at a given redshift. For a single broad filter, and averaging over a small galaxy catalogue from Simard et al., we find a mean shear bias which is subdominant to the predicted statistical errors for future cosmic shear surveys. However, the true mean shear bias may exceed the statistical errors, depending on how accurately the catalogue represents the observed distribution of galaxies in the cosmic shear survey. We then investigate the bias on the shear for two-filter imaging and find that the bias is reduced by at least an order of magnitude. Lastly, we find that it is possible to calibrate galaxies for which colour gradients were ignored using two-filter imaging of a fair sample of noisy galaxies, if the galaxy model is known. For a signal-to-noise ratio of 25 the number of galaxies required in each tomographic redshift bin is of the order of 10
4 . [ABSTRACT FROM AUTHOR]- Published
- 2012
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8. On mitigation of the uncertainty in non-linear matter clustering for cosmic shear tomography.
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Kitching, T. D. and Taylor, A. N.
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MATTER , *POWER spectra , *BARYONS , *PHYSICAL cosmology , *TOMOGRAPHY , *DARK energy , *NONLINEAR theories - Abstract
ABSTRACT We present a new method that deals with the uncertainty in matter clustering in cosmic shear power spectrum analysis that arises mainly due to poorly understood non-linear baryonic processes on small scales. We show that the majority of information about new physics contained in the shear power comes from these small scales. Removing these non-linear scales from a cosmic shear analysis results in 50 per cent cut in the accuracy of measurements of dark energy parameters, marginalizing over all other parameters. In this paper we propose a method to recover the information on small scales by allowing cosmic shear surveys to measure the non-linear matter power spectrum themselves and marginalize over all possible power spectra using path integrals. Information is still recoverable in these non-linear regimes from the geometric part of weak lensing. In this self-calibration regime we recover 90 per cent of the information on dark energy. Including an informative prior, we find that the non-linear matter power spectrum needs to be accurately known to 1 per cent down to k= 50 h−1 Mpc, or a scale of 120 kpc, to recover 99 per cent of the dark energy information. This presents a significant theoretical challenge to understand baryonic effects on the scale of galaxy haloes. [ABSTRACT FROM AUTHOR]
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- 2011
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9. Figures of merit for testing standard models: application to dark energy experiments in cosmology.
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Amara, A. and Kitching, T. D.
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DARK energy , *METAPHYSICAL cosmology , *PHYSICS experiments , *MATHEMATICAL statistics , *GAUSSIAN processes , *MATHEMATICAL optimization , *SUPERNOVAE - Abstract
Given a standard model to test, an experiment can be designed to (i) measure the standard model parameters, (ii) extend the standard model or (iii) look for evidence of deviations from the standard model. To measure (or extend) the standard model, the Fisher matrix is widely used in cosmology to predict expected parameter errors for future surveys under Gaussian assumptions. In this paper, we present a framework that can be used to design experiments that will maximize the chance of finding a deviation from the standard model. Using a simple illustrative example, discussed in Appendix A, we show that the optimal experimental configuration can depend dramatically on the optimization approach chosen. We also show some simple cosmology calculations, where we study baryonic acoustic oscillation and supernovae surveys. In doing so, we also show how external data, such as the positions of the cosmic microwave background peak measured by Wilkinson Microwave Anisotropy Probe, and theory priors can be included in the analysis. In the cosmological cases that we have studied (Dark Energy Task Force Stage III), we find that the three optimization approaches yield similar results, which is reassuring and indicates that the choice of optimal experiment is fairly robust at this level. However, this may not be the case as we move to more ambitious future surveys. [ABSTRACT FROM AUTHOR]
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- 2011
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10. Path integral marginalization for cosmology: scale-dependent galaxy bias and intrinsic alignments.
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Kitching, T. D. and Taylor, A. N.
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METAPHYSICAL cosmology , *MAXIMUM likelihood statistics , *GAUSSIAN distribution , *DARK energy , *PARAMETER estimation , *REDSHIFT - Abstract
ABSTRACT We present a path integral likelihood formalism that extends parametrized likelihood analyses to include continuous functions. The method finds the maximum-likelihood point in function-space, and marginalizes over all possible functions, under the assumption of a Gaussian-distributed function-space. We apply our method to the problem of removing unknown systematic functions in two topical problems for dark energy research: scale-dependent galaxy bias in redshift surveys and galaxy intrinsic alignments in cosmic shear surveys. We find that scale-dependent galaxy bias will degrade information on cosmological parameters unless the fractional variance in the bias function is known to 10 per cent. Measuring and removing intrinsic alignments from cosmic shear surveys with a flat prior can reduce the dark energy figure of merit by 20 per cent, however provided that the scale and redshift dependence is known to better than 10 per cent with a Gaussian prior, the dark energy figure of merit can be enhanced by a factor of 2 with no extra assumptions. [ABSTRACT FROM AUTHOR]
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- 2011
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11. Weak lensing forecasts for dark energy, neutrinos and initial conditions.
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Debono, I., Rassat, A., Réfrégier, A., Amara, A., and Kitching, T. D.
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GRAVITATIONAL lenses ,MICROLENSING (Astrophysics) ,COSMOLOGICAL constant ,DARK energy ,NEUTRINOS ,LEPTONS (Nuclear physics) - Abstract
Weak gravitational lensing provides a sensitive probe of cosmology by measuring the mass distribution and the geometry of the low-redshift Universe. We show how an all-sky weak lensing tomographic survey can jointly constrain different sets of cosmological parameters describing dark energy, massive neutrinos (hot dark matter) and the primordial power spectrum. In order to put all sectors on an equal footing, we introduce a new parameter β, the second-order running spectral index. Using the Fisher matrix formalism with and without cosmic microwave background (CMB) priors, we examine how the constraints vary as the parameter set is enlarged. We find that weak lensing with CMB priors provides robust constraints on dark energy parameters and can simultaneously provide strong constraints on all three sectors. We find that the dark energy sector is largely insensitive to the inclusion of the other cosmological sectors. Implications for the planning of future surveys are discussed. [ABSTRACT FROM AUTHOR]
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- 2010
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12. Fisher matrix decomposition for dark energy prediction.
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Kitching, T. D. and Amara, A.
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DARK energy , *ASTROPHYSICS , *TOMOGRAPHY , *EIGENFUNCTIONS , *REDSHIFT , *NUMERICAL solutions to boundary value problems - Abstract
Within the context of constraining an expansion of the dark energy equation of state we show that the eigendecomposition of Fisher matrices is sensitive to both the maximum order of the expansion and the basis set choice. We investigate the Fisher matrix formalism in the case that a particular function is expanded in some basis set. As an example we show results for an all-sky weak lensing tomographic experiment. We show that the set of eigenfunctions is not unique and that the best constrained functions are only reproduced accurately at very higher order , a top-hat basis set requires an even higher order. We show that the common approach used for finding the marginalized eigenfunction errors is sensitive to the choice of parameters and priors. The eigendecomposition of Fisher matrices is a potentially useful tool that can be used to determine the predicted accuracy with which an experiment could constrain . It also allows for the reconstruction of the redshift sensitivity of the experiment to changes in . However, the technique is sensitive to both the order and the basis set choice. Publicly available code is available as part oficosmo at . [ABSTRACT FROM AUTHOR]
- Published
- 2009
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13. Euclid: The reduced shear approximation and magnification bias for Stage IV cosmic shear experiments
- Author
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F. Pasian, Stefano Cavuoti, Felix Hormuth, Giulio Fabbian, A. C. Deshpande, V. F. Cardone, Natalia Auricchio, Julien Zoubian, G. Polenta, Simona Mei, Ole Marggraf, Ivan Lloro, E. Franceschi, Leonardo Corcione, Martin Kunz, Peter Schneider, Valeria Pettorino, Carmelita Carbone, J. Carretero, Rafael Toledo-Moreo, A. Secroun, S. Kermiche, Stéphane Paltani, Frank Grupp, Sandrine Pires, H. Israel, Florent Sureau, Z. Sakr, Peter Taylor, Mauro Roncarelli, G. Meylan, G. Sirri, S. Casas, F. Lacasa, Massimo Meneghetti, Lauro Moscardini, M. Poncet, Massimo Brescia, P. B. Lilje, Roberto P. Saglia, C. Bodendorf, G. Congedo, I. Tutusaus, A. N. Taylor, B. Kubik, Domenico Sapone, Bianca Garilli, F. Dubath, V. Capobianco, S. Dusini, Cristobal Padilla, Mark Cropper, Ismael Tereno, Martin Kilbinger, Thomas D. Kitching, Sebastiano Ligori, F. Raison, R. Cledassou, D. Bonino, Eugenio Maiorano, M. Fumana, Jean-Luc Starck, Yu Wang, Marco Castellano, Henk Hoekstra, Stefano Camera, Santiago Serrano, Richard Massey, Knud Jahnke, Jason Rhodes, L. Conversi, Luca Valenziano, 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 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 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), Istituto Nazionale di Astrofisica (INAF), Centre National d'Études Spatiales [Toulouse] (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), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-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'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), Euclid Consortium, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), 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), PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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 Paris Cité (UPCité), 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), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Royal Society (UK), National Aeronautics and Space Administration (US), Science and Technology Facilities Council (UK), California Institute of Technology, European Commission, Academy of Finland, Agenzia Spaziale Italiana, Belgian Science Policy Office, Canadian Euclid Consortium, Centre National D'Etudes Spatiales (France), German Centre for Air and Space Travel, Danish Space Research Institute, Fundação para a Ciência e a Tecnologia (Portugal), Ministerio de Economía y Competitividad (España), Netherlands Research School for Astronomy, Romanian Space Agency, State Secretariat for Education, Research and Innovation (Switzerland), Norwegian Space Agency, UK Space Agency, 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 Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Deshpande, A. C., Kitching, T. D., Cardone, V. F., Taylor, P. L., Casas, S., Camera, S., Carbone, C., Kilbinger, M., Pettorino, V., Sakr, Z., Sapone, D., Tutusaus, I., Auricchio, N., Bodendorf, C., Bonino, D., Brescia, M., Capobianco, V., Carretero, J., Castellano, M., Cavuoti, S., Cledassou, R., Congedo, G., Conversi, L., Corcione, L., Cropper, M., Dubath, F., Dusini, S., Fabbian, G., Franceschi, E., Fumana, M., Garilli, B., Grupp, F., Hoekstra, H., Hormuth, F., Israel, H., Jahnke, K., Kermiche, S., Kubik, B., Kunz, M., Lacasa, F., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Marggraf, O., Massey, R., Mei, S., Meneghetti, M., Meylan, G., Moscardini, L., Padilla, C., Paltani, S., Pasian, F., Pires, S., Polenta, G., Poncet, M., Raison, F., Rhodes, J., Roncarelli, M., Saglia, R., Schneider, P., Secroun, A., Serrano, S., Sirri, G., Starck, J. L., Sureau, F., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Valenziano, L., Wang, Y., Zoubian, J., Deshpande A.C., Kitching T.D., Cardone V.F., Taylor P.L., Casas S., Camera S., Carbone C., Kilbinger M., Pettorino V., Sakr Z., Sapone D., Tutusaus I., Auricchio N., Bodendorf C., Bonino D., Brescia M., Capobianco V., Carretero J., Castellano M., Cavuoti S., Cledassou R., Congedo G., Conversi L., Corcione L., Cropper M., Dubath F., Dusini S., Fabbian G., Franceschi E., Fumana M., Garilli B., Grupp F., Hoekstra H., Hormuth F., Israel H., Jahnke K., Kermiche S., Kubik B., Kunz M., Lacasa F., Ligori S., Lilje P.B., Lloro I., Maiorano E., Marggraf O., Massey R., Mei S., Meneghetti M., Meylan G., Moscardini L., Padilla C., Paltani S., Pasian F., Pires S., Polenta G., Poncet M., Raison F., Rhodes J., Roncarelli M., Saglia R., Schneider P., Secroun A., Serrano S., Sirri G., Starck J.L., Sureau F., Taylor A.N., Tereno I., Toledo-Moreo R., Valenziano L., Wang Y., and Zoubian J.
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,weak ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,methods: analytical ,gravitational lensing: weak ,0103 physical sciences ,Statistical physics ,observations [Cosmology] ,dark energy ,010303 astronomy & astrophysics ,Weak gravitational lensing ,Physics ,COSMIC cancer database ,010308 nuclear & particles physics ,Cosmology: Observations ,Gravitational lensing: weak ,Methods: Analytical ,Spectral density ,Astronomy and Astrophysics ,Covariance ,Galaxy ,matter ,Analytical [Methods] ,Shear (geology) ,Cosmology: Observation ,Space and Planetary Science ,statistics ,cosmology: observations ,Log-normal distribution ,astro-ph.CO ,weak [Gravitational lensing] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,constraints ,Order of magnitude ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Stage IV weak lensing experiments will offer more than an order of magnitude leap in precision. We must therefore ensure that our analyses remain accurate in this new era. Accordingly, previously ignored systematic effects must be addressed. In this work, we evaluate the impact of the reduced shear approximation and magnification bias, on the information obtained from the angular power spectrum. To first-order, the statistics of reduced shear, a combination of shear and convergence, are taken to be equal to those of shear. However, this approximation can induce a bias in the cosmological parameters that can no longer be neglected. A separate bias arises from the statistics of shear being altered by the preferential selection of galaxies and the dilution of their surface densities, in high-magnification regions. The corrections for these systematic effects take similar forms, allowing them to be treated together. We calculated the impact of neglecting these effects on the cosmological parameters that would be determined from Euclid, using cosmic shear tomography. To do so, we employed the Fisher matrix formalism, and included the impact of the super-sample covariance. We also demonstrate how the reduced shear correction can be calculated using a lognormal field forward modelling approach. These effects cause significant biases in Omega_m, sigma_8, n_s, Omega_DE, w_0, and w_a of -0.53 sigma, 0.43 sigma, -0.34 sigma, 1.36 sigma, -0.68 sigma, and 1.21 sigma, respectively. We then show that these lensing biases interact with another systematic: the intrinsic alignment of galaxies. Accordingly, we develop the formalism for an intrinsic alignment-enhanced lensing bias correction. Applying this to Euclid, we find that the additional terms introduced by this correction are sub-dominant., Comment: 16 pages, 6 figures, submitted to Astronomy & Astrophysics on 16/12/2019, accepted on 04/03/2020. SSC Fisher procedure corrected
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- 2020
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14. Euclid: Impact of non-linear and baryonic feedback prescriptions on cosmological parameter estimation from weak lensing cosmic shear
- Author
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Andrea Zacchei, E. Franceschi, Hannu Kurki-Suonio, Z. Sakr, M. Martinelli, N. Welikala, Thomas D. Kitching, V. F. Cardone, Natalia Auricchio, V. Capobianco, C. J. Conselice, Peter Schneider, S. Dusini, Rafael Toledo-Moreo, Marian Douspis, Elisabetta Maiorano, A. Balestra, Enzo Branchini, A. Secroun, Martin Kunz, Henk Hoekstra, M. Kilbinger, B. Gillis, Ismael Tereno, Sebastien Clesse, Fabio Pasian, Stefano Camera, Massimo Brescia, S. Paltani, Chiara Sirignano, Jean-Luc Starck, Mauro Roncarelli, Andy Taylor, Alkistis Pourtsidou, L. Popa, R. Cledassou, L. Conversi, M. Frailis, M. Poncet, J. Carretero, G. Meylan, A. Boucaud, Jason Rhodes, G. Polenta, Luca Valenziano, B. Morin, Ole Marggraf, S. Serrano, Sebastiano Ligori, F. Dubath, Lauro Moscardini, Yu Wang, Marco Castellano, Roberto P. Saglia, F. Grupp, Stefano Cavuoti, F. Sureau, Richard Massey, Knud Jahnke, K. Pedersen, Domenico Sapone, W. A. Holmes, I. Lloro, Luigi Guzzo, F. Raison, Luciano Casarini, K. Markovic, Alina Kiessling, Emanuel Rossetti, C. Padilla, Julien Zoubian, T. Vassallo, Edwin A. Valentijn, G. Sirri, Pablo Fosalba, M. Archidiacono, Anne Costille, S. Pires, Andrea Cimatti, Giulio Fabbian, David F. Mota, Leonardo Corcione, Massimo Meneghetti, P. B. Lilje, S. Casas, Isaac Tutusaus, G. Congedo, Valeria Pettorino, Felix Hormuth, Carmelita Carbone, S. Niemi, S. Ilić, S. Kermiche, Carlo Giocoli, 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), 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), 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), Centre National d'Études Spatiales [Toulouse] (CNES), 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 d'astrophysique spatiale (IAS), 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), 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), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Euclid, Ministerio de Ciencia, Innovación y Universidades (España), La Caixa, European Commission, Canadian Euclid Consortium, Astronomy, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Martinelli, M., Tutusaus, I., Archidiacono, M., Camera, S., Cardone, V. F., Clesse, S., Casas, S., Casarini, L., Mota, D. F., Hoekstra, H., Carbone, C., Ilic, S., Kitching, T. D., Pettorino, V., Pourtsidou, A., Sakr, Z., Sapone, D., Auricchio, N., Balestra, A., Boucaud, A., Branchini, E., Brescia, M., Capobianco, V., Carretero, J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conselice, C., Conversi, L., Corcione, L., Costille, A., Douspis, M., Dubath, F., Dusini, S., Fabbian, G., Fosalba, P., Frailis, M., Franceschi, E., Gillis, B., Giocoli, C., Grupp, F., Guzzo, L., Holmes, W., Hormuth, F., Jahnke, K., Kermiche, S., Kiessling, A., Kilbinger, M., Kunz, M., Kurki-Suonio, H., Ligori, S., Lilje, P. B., Lloro, I., Maiorano, E., Marggraf, O., Markovic, K., Massey, R., Meneghetti, M., Meylan, G., Morin, B., Moscardini, L., Niemi, S., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pires, S., Polenta, G., Poncet, M., Popa, L., Raison, F., Rhodes, J., Roncarelli, M., Rossetti, E., Saglia, R., Schneider, P., Secroun, A., Serrano, S., Sirignano, C., Sirri, G., Starck, J. -L., Sureau, F., Taylor, A. N., Tereno, I., Toledo-Moreo, R., Valentijn, E. A., Valenziano, L., Vassallo, T., Wang, Y., Welikala, N., Zacchei, A., Zoubian, J., Martinelli M., Tutusaus I., Archidiacono M., Camera S., Cardone V.F., Clesse S., Casas S., Casarini L., Mota D.F., Hoekstra H., Carbone C., Ilic S., Kitching T.D., Pettorino V., Pourtsidou A., Sakr Z., Sapone D., Auricchio N., Balestra A., Boucaud A., Branchini E., Brescia M., Capobianco V., Carretero J., Castellano M., Cavuoti S., Cimatti A., Cledassou R., Congedo G., Conselice C., Conversi L., Corcione L., Costille A., Douspis M., Dubath F., Dusini S., Fabbian G., Fosalba P., Frailis M., Franceschi E., Gillis B., Giocoli C., Grupp F., Guzzo L., Holmes W., Hormuth F., Jahnke K., Kermiche S., Kiessling A., Kilbinger M., Kunz M., Kurki-Suonio H., Ligori S., Lilje P.B., Lloro I., Maiorano E., Marggraf O., Markovic K., Massey R., Meneghetti M., Meylan G., Morin B., Moscardini L., Niemi S., Padilla C., Paltani S., Pasian F., Pedersen K., Pires S., Polenta G., Poncet M., Popa L., Raison F., Rhodes J., Roncarelli M., Rossetti E., Saglia R., Schneider P., Secroun A., Serrano S., Sirignano C., Sirri G., Starck J.-L., Sureau F., Taylor A.N., Tereno I., Toledo-Moreo R., Valentijn E.A., Valenziano L., Vassallo T., Wang Y., Welikala N., Zacchei A., Zoubian J., UAM.Departamento de Física Teórica, Department of Physics, and Helsinki Institute of Physics
- Subjects
Cosmological parameter ,Structure formation ,Large-scale structure of Universe ,Astrophysics - cosmology and nongalactic astrophysics ,media_common.quotation_subject ,Cosmological parameters ,Dark matter ,Cosmic microwave background ,Large-scale structure of universe ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,114 Physical sciences ,7. Clean energy ,01 natural sciences ,Large-scale structure ,symbols.namesake ,N-body ,Universe ,Gravitational lensing: weak ,Dark energy ,0103 physical sciences ,Statistical physics ,Planck ,010303 astronomy & astrophysics ,Weak gravitational lensing ,media_common ,Precision emulation ,Physics ,Galaxy formation ,massive neutrinos ,010308 nuclear & particles physics ,Computer Science::Information Retrieval ,Física ,Astronomy and Astrophysics ,115 Astronomy, Space science ,Astronomía ,Gravitational lens ,Space and Planetary Science ,astro-ph.CO ,symbols ,Sample variance ,Accurate halo-model ,weak [Gravitational lensing] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Matter power spectrum ,Hubble's law - Abstract
Martinelli, M., et al., Upcoming surveys will map the growth of large-scale structure with unprecented precision, improving our understanding of the dark sector of the Universe. Unfortunately, much of the cosmological information is encoded on small scales, where the clustering of dark matter and the effects of astrophysical feedback processes are not fully understood. This can bias the estimates of cosmological parameters, which we study here for a joint analysis of mock Euclid cosmic shear and Planck cosmic microwave background data. We use different implementations for the modelling of the signal on small scales and find that they result in significantly different predictions. Moreover, the different non-linear corrections lead to biased parameter estimates, especially when the analysis is extended into the highly non-linear regime, with the Hubble constant, H0, and the clustering amplitude, σ8, affected the most. Improvements in the modelling of non-linear scales will therefore be needed if we are to resolve the current tension with more and better data. For a given prescription for the non-linear power spectrum, using different corrections for baryon physics does not significantly impact the precision of Euclid, but neglecting these correction does lead to large biases in the cosmological parameters. In order to extract precise and unbiased constraints on cosmological parameters from Euclid cosmic shear data, it is therefore essential to improve the accuracy of the recipes that account for non-linear structure formation, as well as the modelling of the impact of astrophysical processes that redistribute the baryons., Stefano Camera acknowledges support from the Italian Ministry of Education, University and Research (Miur) through Rita Levi Mon-talcini project ‘Prometheus – Probing and Relating Observables with Multiwavelength Experiments To Help Enlightening the Universe’s Structure’, and the ‘Departments of Excellence 2018–2022’ Grant awarded by Miur (L. 232/2016). The work of SC is supported by the Belgian Fund for Research FNRS-F.R.S. I. T. acknowledges support from the Spanish Ministry of Science, Innovation and Universities through grant ESP2017-89838-C3-1-R. I. T. and T. K. acknowledge funding from the H2020 programme of the European Commission through grant 776247. AP is a UK Research and Innovation Future Leaders Fellow, grant MR/S016066/1. 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 Tecnolo-gia, the Ministerio de Economia y Competitividad, the National Aeronautics and Space Administration, 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 web site (http://www.euclid-ec.org). D. F. M. thanks the Research Council of Norway for their support, and the resources provided by UNINETT Sigma2 – the National Infrastructure for High Performance Computing and Data Storage in Norway. M. M. has received the support of a fellowship from “la Caixa” Foundation (ID 100010434), with fellowship code LCF/BQ/PI19/11690015, and the support of the Spanish Agencia Estatal de Investigacion through the grant “IFT Centro de Excelencia Severo Ochoa SEV-2016-0597”. This paper is based upon work from the COST action CA15117 (CANTATA), supported by COST (European Cooperation in Science and Technology). M. A. acknowledges the computing
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- 2021
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