The Cost of Living

Amendola, Nicola

doi:10.1093/acprof:oso/9780199944590.003.0015

Cited by 5 publications

(3 citation statements)

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“…whose integrals are 1/N . In this work we shall take σ(z) = 0.05 (1 + z), coherently with Euclid expectations (Amendola et al (2013), see also Casarini et al (2011)); the distributions D r , when normalized to unity, are then dubbed δ r . They are used to define the window functions…”

Section: Tomographic Windowsmentioning

confidence: 99%

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SAMPLE VARIANCE INN-BODY SIMULATIONS AND IMPACT ON TOMOGRAPHIC SHEAR PREDICTIONS

Casarini

Piattella

Bonometto

et al. 2015

ApJ

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We study the effects of sample variance in N-body simulations as a function of the size of the simulation box, namely in connection with predictions on tomographic shear spectra. We make use of a set of eight ΛCDM simulations in boxes of 128, 256, and 512 h Mpc 1 -a side, for a total of 24, differing just by the initial seeds. Among the simulations with 128 and 512 h Mpc 1 -a side, we suitably select those closest and farthest from average. Numerical and linear spectra P k z , ( ) are suitably connected at low k to evaluate the effects of sample variance on shear spectra C ℓ ij ( ) for 5 or 10 tomographic bands. We find that shear spectra obtained by using 128 h Mpc 1 -simulations can vary up to 25%, just because of the seed. The sample variance lowers to 3.3% when using 512 h 1 -Mpc. These percentages could however slightly vary if other sets of the same number of realizations were considered. Accordingly, in order to match the 1% precision expected for the data, if still using eight boxes, we require a size of 1300 -h 1700 Mpc 1 -for them.

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Section: Tomographic Windowsmentioning

confidence: 99%

“…It is therefore hardly surprising that a number of experiments have been planned -4as, e.g., BOSS 1 , PanStarrs 2 , HETDEX 3 , DES 4 , LSST 5 , KIDS 6 WFIRST 7 , and Euclid 8 (Amendola et al 2013), aiming to scan a large area of the sky, seeking fresh information on weak lensing.…”

Section: Introductionmentioning

confidence: 99%

SAMPLE VARIANCE INN-BODY SIMULATIONS AND IMPACT ON TOMOGRAPHIC SHEAR PREDICTIONS

Casarini

Piattella

Bonometto

et al. 2015

ApJ

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“…At cosmological level, they can produce an EOS for the dark energy (in the form of a scalar-field) which can vary in cosmic time, unlike the cosmological constant Λ. This variation will be tested in the forthcoming years by numerous projects [17][18][19][20] which will help to validate or rule out a simple ΛCDM model. Since STT are a generalization of the famous Brans-Dicke theory, these theories predict small variations of the effective gravitational coupling G eff , which can be further tested observationally.…”

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confidence: 99%

On the formation of "supermassive" neutron stars and dynamical transition to spontaneous scalarization

Degollado,

Salgado,

Alcubierre

2020

Preprint

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It is well known that neutron stars can undergo a phase transition under a certain class of Scalar Tensor Theories of gravity (STT's) where a new order parameter, the scalar charge, appears within the star. This is the well known phenomenon of spontaneous scalarization (SC) discovered by Damour and Esposito-Farèse in 1993. Under such mechanism neutron stars can afford in principle a maximum mass larger than in general relativity (GR) for a given equation of state without taking into account additional observational constraints (e.g. binary systems). This opens the possibility that neutron stars might be formed with masses as large as ∼ 2M⊙ without the need of stiff, or more exotic, equations of state for the nuclear matter. Thus, STT's through SC may account for compact objects with large masses observed recently in the sky in the form of pulsars (PSR J0348+0432 with M = 2.01M±0.04⊙ observed in 2013, PSR J1614-2230 with M = 1.97 ± 0.04M⊙ observed in 2010 or J0740+6620 M = 2.14 +0.10 −0.09 M⊙ observed in 2019). However, we argue that even if that was possible such maximum mass models within STT cannot be formed solely from the dynamic transition of an initial "isolated" unscalarized neutron star whose mass cannot exceed the maximum mass in GR. This is because SC, being an energetic-preferred configuration, produces a final static star with a mass lower that the initial one with a fixed baryon mass. The mass difference between the initial and final configurations is radiated away in the form of a scalar-field. Thus, maximum mass models of scalarized neutron stars, if present in nature, must have formed by a different process, perhaps of cosmological origin or by the subsequent accretion of additional scalar charge and mass.

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The politics of quantification: The General Confederation of Italian Industry and the cost-of-living index in the late 1920s

Favero,

Gaspari

2024

Business History

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The Cost of Living

Cited by 5 publications

References 0 publications

SAMPLE VARIANCE INN-BODY SIMULATIONS AND IMPACT ON TOMOGRAPHIC SHEAR PREDICTIONS

SAMPLE VARIANCE INN-BODY SIMULATIONS AND IMPACT ON TOMOGRAPHIC SHEAR PREDICTIONS

On the formation of "supermassive" neutron stars and dynamical transition to spontaneous scalarization

The politics of quantification: The General Confederation of Italian Industry and the cost-of-living index in the late 1920s

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