Energy conditions bounds and their confrontation with supernovae data

Abstract

The energy conditions play an important role in the understanding of several properties of the Universe, including the current accelerating expansion phase and the possible existence of the so-called phantom fields. We show that the integrated bounds provided by the energy conditions on cosmological observables such as the distance modulus $\mu (z)$ and the lookback time $t_L(z)$ are not sufficient (nor necessary) to ensure the local fulfillment of the energy conditions, making explicit the limitation of these bounds in the confrontation with observational data. We recast the energy conditions as bounds on the deceleration and normalized Hubble parameters, obtaining new bounds which are necessary and sufficient for the local fulfillment of the energy conditions. A statistical confrontation, with $1\sigma -3\sigma$ confidence levels, between our bounds and supernovae data from the gold and combined samples is made for the recent past. Our analyses indicate, with $3\sigma$ confidence levels, the fulfillment of both the weak energy condition (WEC) and dominant energy condition (DEC) for $z\le 1$ and $z\lesssim 0.8$, respectively. In addition, they suggest a possible recent violation of the null energy condition (NEC) with $3\sigma$, i.e. a very recent phase of super-acceleration. Our analyses also show the possibility of violation of the strong energy condition (\textbf{SEC}) with $3\sigma$ in the recent past ($z\le 1$), but interestingly the $q(z)$-best-fit curve crosses the SEC-fulfillment divider at $z\simeq 0.67$, which is a value very close to the beginning of the epoch of cosmic acceleration predicted by the standard concordance flat $\Lambda$CDM scenario.

7 pages, 3 figures. V2: Version to appear in Phys.Rev.D, analyses extended to 1sigma, 2sigma and 3sigma confidence levels, references added, minors changes

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Cited by in corpus (3)

• How to Distinguish Dark Energy and Modified Gravity?
• Energy conditions bounds and supernovae data
• Bounding the Hubble flow in terms of the w parameter