Cosmology and fundamental physics with the Euclid satellite

Amendola, Luca; Appleby, Stephen; Avgoustidis, Anastasios; Bacon, David; Baker, Tessa; Baldi, Marco; Bartolo, N.; Blanchard, Alain; Bonvin, Camille; Borgani, S.; Branchini, E.; Burrage, Clare; Camera, Stefano; Carbone, C.; Casarini, Luciano; Cropper, Mark; Rham, Claudia de; Dietrich, J. P.; Porto, C. Di; Durrer, Ruth; Ealet, A.; Ferreira, Pedro G.; Finelli⋆, F.; García-Bellido, J.; Giannantonio, T.; Guzzo, L.; Heavens, Alan; Heisenberg, Lavinia; Heymans, Catherine; Hoekstra, Henk; Hollenstein, Lukas; Holmes, Rory; Hwang, Zhiqi; Jahnke, K.; Kitching, Thomas D.; Koivisto, Tomi S.; Kunz, M.; Vacca, G. La; Linder, Eric V.; March, M.; Marra, Valerio; Martins, C. J. A. P.; Majerotto, Elisabetta; Markovic, K.; Marsh, David J. E.; Marulli, F.; Massey, Richard; Mellier, Y.; Montanari, Francesco; Mota, David F.; Nunes, Nelson J.; Percival, Will J.; Pettorino, V.; Porciani, Cristiano; Quercellini, Claudia; Read, Justin I.; Rinaldi, Massimiliano; Sapone, Domenico; Sawicki, Ignacy; Scaramella, R.; Skordis, Constantinos; Simpson, Fergus; Taylor, Andy; Thomas, Shaun A.; Trotta, Roberto; Verde, Licia; Vernizzi, Filippo; Vollmer, Adrian; Wang, Yun; Weller, J.; Złośnik, Tom

doi:10.1007/s41114-017-0010-3

Cited by 964 publications

(914 citation statements)

References 1,264 publications

(1,711 reference statements)

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“…The redshift depth will be up to z ∼ 2 for galaxy clustering and up to z ∼ 3 for cosmic shear. The combination of the galaxy power spectrum measured with Euclid and primary CMB from Planck is expected to give σ ( m ν ) = 0.04 eV; if instead the weak lensing dataset produced by Euclid is considered in combination with primary CMB, we expect σ ( m ν ) = 0.05 eV [133]. Both combinations provide a ∼ 1σ evidence in the minimal mass scenario.…”

Section: Future Lss Surveys: Desi Euclid Lsst Wfirstmentioning

confidence: 96%

“…These constraints are also summarized in Table 2 for the reader's convenience. Planck CMB+LSST-shear c 30 [36] Planck+Euclid-FS 40 [133] Stage-III CMB (ACTPol)+WFIRST BAO+FS 30 [38] Stage-III CMB+WFIRST+Euclid+LSST 8 [38] a The combination assumes a Gaussian prior on τ = 0.06 ± 0.01 roughly corresponding to the new estimate from Aghanim et al [43]. b The combination assumes σ (τ ) = 0.002 and noise level of 2.5µK · arcmin.…”

Section: Constraints On M ν From Future Surveysmentioning

confidence: 99%

“…Both combinations provide a ∼ 1σ evidence in the minimal mass scenario. Some authors have also pointed out that weak lensing data as measured by Euclid could discriminate between the two neutrino hierarchies if the true value of m ν is small enough (i.e., far enough from the degenerate region of the neutrino mass spectrum), see [133] and references therein 16 .…”

Section: Future Lss Surveys: Desi Euclid Lsst Wfirstmentioning

confidence: 99%

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Status of Neutrino Properties and Future Prospects—Cosmological and Astrophysical Constraints

2018

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Cosmological observations are a powerful probe of neutrino properties, and in particular of their mass. In this review, we first discuss the role of neutrinos in shaping the cosmological evolution at both the background and perturbation level, and describe their effects on cosmological observables such as the cosmic microwave background and the distribution of matter at large scale. We then present the state of the art concerning the constraints on neutrino masses from those observables, and also review the prospects for future experiments. We also briefly discuss the prospects for determining the neutrino hierarchy from cosmology, the complementarity with laboratory experiments, and the constraints on neutrino properties beyond their mass.

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Section: Future Lss Surveys: Desi Euclid Lsst Wfirstmentioning

confidence: 96%

Section: Constraints On M ν From Future Surveysmentioning

confidence: 99%

Section: Future Lss Surveys: Desi Euclid Lsst Wfirstmentioning

confidence: 99%

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Status of Neutrino Properties and Future Prospects—Cosmological and Astrophysical Constraints

2018

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“…The second category approach is by modified general relativity including Horndeski's types such as galileons, chameleons, Brans-Dicke, symmetrons, and other possibilities. In the third strategy, based on a thermodynamics point of view, phenomenological exotic fluids are supposed for an alternative dark energy model [4][5][6][7][8].…”

Section: Introductionmentioning

confidence: 99%

“…From observational points of view, ongoing and upcoming generation of ground-based and space-based surveys classified in various stages ranging from I to IV, one can refer to background and perturbations of observables [5,45]. Subsequently, we will rely on the state-of-the-art observational data sets such as supernova type Ia (SNIa), gamma ray bursts (GRBs), baryonic acoustic oscillation (BAO) and CMB evolution based on background dynamics to examine the consistency of our model.…”

Section: Introductionmentioning

confidence: 99%

Non-minimal derivative coupling scalar field and bulk viscous dark energy

2017

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Inspired by thermodynamical dissipative phenomena, we consider bulk viscosity for dark fluid in a spatially flat two-component Universe. Our viscous dark energy model represents phantom-crossing which avoids bigrip singularity. We propose a non-minimal derivative coupling scalar field with zero potential leading to accelerated expansion of the Universe in the framework of bulk viscous dark energy model. In this approach, the coupling constant, κ, is related to viscosity coefficient, γ , and the present dark energy density, Ω 0 DE . This coupling is bounded as. We implement recent observational data sets including a joint light-curve analysis (JLA) for SNIa, gamma ray bursts (GRBs) for most luminous astrophysical objects at high redshifts, baryon acoustic oscillations (BAO) from different surveys, Hubble parameter from HST project, Planck CMB power spectrum and lensing to constrain model free parameters. The joint analysis of JLA + GRBs + BAO + HST shows that Ω 0 DE = 0.696 ± 0.010, γ = 0.1404 ± 0.0014 and H 0 = 68.1 ± 1.3. Planck TT observation provides γ = 0.32 +0.31 −0.26 in the 68% confidence limit for the viscosity coefficient. The cosmographic distance ratio indicates that current observed data prefer to increase bulk viscosity. The competition between phantom and quintessence behavior of the viscous dark energy model can accommodate cosmological old objects reported as a sign of age crisis in the ΛCDM model. Finally, tension in the Hubble parameter is alleviated in this model. a

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The isolated elliptical galaxy NGC 5812–MOND or dark matter?

Richtler,

Salinas,

Lane

et al. 2023

Astron Nachr

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There exist isolated elliptical galaxies, whose dynamics can be modeled without resorting to dark matter or MOND, for example, NGC 7507. Such objects lack understanding within the current framework of galaxy formation. The isolated elliptical NGC 5812 is another object to investigate a possible role of isolation. We use globular clusters (GCs) and the galaxy light itself as dynamical tracers to constrain its mass profile. We employ Gemini/GMOS mask spectroscopy, apply the GMOS reduction procedures provided within IRAF, measure GC velocities by cross correlation methods and extract the line‐of‐sight kinematics of galaxy spectra using the tool pPXF. We identify 28 GCs with an outermost galactocentric distance of 20 kpc, for which velocities could be obtained. Furthermore, 16 spectra of the integrated galaxy light out to 6 kpc have been used to model the central kinematics. These spectra provide evidence for a disturbed velocity field, which is plausible given the disturbed morphology of the galaxy. We construct spherical Jeans models for the galaxy light and apply tracer mass estimators for the globular clusters. With the assumptions inherent to the mass estimators, MOND is compatible with the mass out to 20 kpc. However, a dark matter free galaxy is not excluded, given the uncertainties related to a possible nonsphericity and a possible nonequilibrium state. We find one globular cluster with an estimated mass of , the first Ultra Compact Dwarf in an isolated elliptical. We put NGC 5812 into the general context of dark matter or alternative ideas in elliptical galaxies. The case for a MONDian phenomenology also among early‐type galaxies has become so strong that deviating cases appear astrophysically more interesting than agreements. The baryonic Tully Fisher relation (BTFR) as predicted by MOND is observed in some samples of early‐type galaxies, in others not. However, in cases of galaxies that deviate from the MONDian prediction, data quality and data completeness are often problematic.

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Cosmology and fundamental physics with the Euclid satellite

Cited by 964 publications

References 1,264 publications

Status of Neutrino Properties and Future Prospects—Cosmological and Astrophysical Constraints

Status of Neutrino Properties and Future Prospects—Cosmological and Astrophysical Constraints

Non-minimal derivative coupling scalar field and bulk viscous dark energy

The isolated elliptical galaxy NGC 5812–MOND or dark matter?

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