The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample

Scolnic, D.; Jones, D. O.; Rest, A.; Pan, Y.-C.; Chornock, R.; Foley, R. J.; Huber, M. E.; Keßler, R.; Narayan, Gautham; Riess, Adam G.; Rodney, S.; Berger, E.; Brout, D.; Challis, Peter; Drout, M. R.; Finkbeiner, Douglas P.; Lunnan, R.; Kirshner, R.; Sanders, Nathan; Schlafly, Edward F.; Smartt, S. J.; Stubbs, C. W.; Tonry, J.; Wood‐Vasey, W. M.; Foley, Michael; Hand, Jared; Johnson, Emily; Burgett, W. S.; Chambers, K.; Draper, P. W.; Hodapp, Klaus W.; Kaiser, N.; Kudritzki, R. P.; Magnier, E. A.; Metcalfe, N.; Bresolin, Fabio; Gáll, Erwin; Kotak, R.; McCrum, M.; Smith, K.

doi:10.3847/1538-4357/aab9bb

Cited by 2,182 publications

(2,170 citation statements)

References 135 publications

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“…First, we considered the low-redshift regime through the use of the Pantheon type Ia Supernovae (SNe Ia) catalogue (Scolnic et al 2018) and the observational Hubble data (OHD) acquired by means of the differential age method (Jimenez & Loeb 2002). We refer the readers to D'Agostino (2019) and references therein for details on both SNe Ia and OHD data sets and their respective likelihood functions.…”

Section: Low-redshift Domainmentioning

confidence: 99%

High-redshift cosmography: auxiliary variables versus Padé polynomials

Capozziello

D’Agostino

Luongo

2020

Monthly Notices of the Royal Astronomical Society

112

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Cosmography becomes non-predictive when cosmic data span beyond the red shift limit z ≃ 1. This leads to a strong convergence issue that jeopardizes its viability. In this work, we critically compare the two main solutions of the convergence problem, i.e. the y-parametrizations of the redshift and the alternatives to Taylor expansions based on Padé series. In particular, among several possibilities, we consider two widely adopted parametrizations, namely y 1 = 1 − a and y 2 = arctan(a −1 − 1), being a the scale factor of the Universe. We find that the y 2 -parametrization performs relatively better than the y 1 -parametrization over the whole redshift domain. Even though y 2 overcomes the issues of y 1 , we get that the most viable approximations of the luminosity distance d L (z) are given in terms of Padé approximations. In order to check this result by means of cosmic data, we analyze the Padé approximations up to the fifth order, and compare these series with the corresponding y-variables of the same orders. We investigate two distinct domains involving Monte Carlo analysis on the Pantheon Superovae Ia data, H(z) and shift parameter measurements. We conclude that the (2,1) Padé approximation is statistically the optimal approach to explain low and high-redshift data, together with the fifth-order y 2 -parametrization. At high redshifts, the (3,2) Padé approximation cannot be fully excluded, while the (2,2) Padé one is essentially ruled out.

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Section: Low-redshift Domainmentioning

confidence: 99%

High-redshift cosmography: auxiliary variables versus Padé polynomials

Capozziello

D’Agostino

Luongo

2020

Monthly Notices of the Royal Astronomical Society

112

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“…• Supernovae Type Ia (Pantheon): The Supernovae Type Ia (SNIa) were the first indicators for an accelerating phase of the universe. Here, we use the latest compilation of SNIa data (known as Pantheon sample) comprising 1048 data points [63].…”

Section: Observational Data and Statistical Methodsmentioning

confidence: 99%

Dark sectors with dynamical coupling

et al. 2019

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Coupled dark matter-dark energy scenarios are modeled via a dimensionless parameter ξ, which controls the strength of their interaction. While this coupling is commonly assumed to be constant, there is no underlying physical law or symmetry that forbids a time-dependent ξ parameter. The most general and complete interacting scenarios between the two dark sectors should therefore allow for such a possibility, and it is the main purpose of this study to constrain two possible and wellmotivated coupled cosmologies by means of the most recent and accurate early and late-time universe observations. We find that CMB data alone prefers ξ(z) > 0 and therefore a smaller amount of dark matter, alleviating some crucial and well-known cosmological data tensions. An objective assessment of the Bayesian evidence for the coupled models explored here shows no particular preference for the presence of a dynamical dark sector coupling. more recently, an extra encouraging aspect of these theories has improved their role as an alternative to a pure ΛCDM universe. Namely, in dark matter-dark energy coupled cosmologies the tension between local and CMB estimations of the Hubble constant H 0 could be ameliorated [43,44,45,46]. Current cosmological observations still allow for significant interactions among the two dark sectors, i.e. between dark matter and dark energy, see e.g. Refs. [47,48,49,50,51,52]. In this work we consider an interacting scenario in which vacuum interacts with pressure-less dark matter adopting the more general phenomenological viewpoint, i.e. inspecting a time-dependent coupling. Such a consideration also entails the case of a coupling parameter that remains constant in cosmic time. For our analyses we have assumed that our universe is homogeneous and isotropic, that is, its geometry is well described by the Friedmann-Lemaître-Robertson-Walker line element.The work has been organized as follows. Section 2 contains the gravitational equations within an interacting universe. In Sec. 3 we describe the observational data and the methodology used to constrain the interacting dark energy models. Section 4 presents the observational constraints on the models, including also a Bayesian evidence analysis. Finally, we draw our conclusions in Sec. 5. GRAVITATIONAL EQUATIONS OF A UNIVERSE WITH INTERACTING DARK SECTORSA homogeneous and isotropic universe is well described by the Friedmann-Lemaître-Robertson-Walker (FLRW) metric: arXiv:1906.11697v1 [astro-ph.CO]

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“…For type Ia supernova we make use of the full Pantheon sample [23] incorporating the heliocentric redshift, correcting in this way the issue previously mentioned about peculiar velocities at high redshift [24]. The Hubble parameter as a function of redshift H(z) data is obtained by cosmic chronometers and taken from the compilation made in [25].…”

Section: Observational Constraintsmentioning

confidence: 99%

“…Written in this way we have two free parameters: H 0 and the combination Γ/3H 0 . As starting point of our study we use only type Ia supernova data from the Pantheon sample [23]. In this case, the observable is the distance modulus…”

Section: A γ = Constant Modelmentioning

confidence: 99%

Challenging matter creation models in the phantom divide

et al. 2020

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We perform a study both statistical and theoretical for cosmological models of matter creation and their ability to describe effective phantom models of dark energy. Such models are beyond the ΛCDM model since the resulting cosmic expansion is not adiabatic. In fact, we show that this approach exhibits transient phantom/quintessence scenarios at present time and tends to the standard cosmological model at some stage of the cosmic evolution. We discuss some generalities of the thermodynamics properties for this type of cosmological model; we emphasize on the behavior of the temperature associated to dark matter, which keeps positive along cosmic evolution together with the entropy. The enrichment of this type of model by means of the incorporation of cosmological constant and dissipative effects in the fluid description to explore their cosmological consequences in the expansion of the universe is considered. Finally, a generalization for the matter production rate as an inhomogeneous expression of the Hubble parameter and its derivatives is discussed; as in all the cases examined, such election leads to an effective phantom/quintessence behavior.

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The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample

Cited by 2,182 publications

References 135 publications

High-redshift cosmography: auxiliary variables versus Padé polynomials

High-redshift cosmography: auxiliary variables versus Padé polynomials

Dark sectors with dynamical coupling

Challenging matter creation models in the phantom divide

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