Age problem in the holographic dark energy model

Abstract

In this note, we test the original holographic dark energy model with some old high redshift objects. The main idea is very simple: the universe cannot be younger than its constituents. We find that the original holographic dark energy model can be ruled out, unless a lower Hubble constant is taken.

Impacts of different SNLS3 light-curve fitters on cosmological consequences of interacting dark energy models

“…In other words, the existence of the old quasar APM 08279+5255 still can not be explained in the frame of IDE model. This result is consistent with the conclusions of previous studies Alcaniz et al (2003), Wei & Zhang (2007), , Wang et al ( , 2010, Yan et al (2015). In addition, the 2σ regions of t(z) given by different LCF almost overlap, showing that the impacts of different SNLS3 LCF can not be distinguished by using the age data of OHRO.…”

“…For instance, the 3.5 Gyr old galaxy LBDS 53W091 at redshift z = 1.55 (Dunlop et al 1996), the 4.0 Gyr old galaxy LBDS 53W069 at redshift z = 1.43 (Dunlop 1999), and the old quasar APM 08279+5255, whose age is estimated to be 2.0 Gyr, at redshift z = 3.91 Hasinger et al (2002). In the literature, the age data of these three OHRO (i.e., t 1.43 ≡ t(z = 1.43) = 4.0 Gyr, t 1.55 ≡ t(z = 1.55) = 3.5 Gyr and t 3.91 ≡ t(z = 3.91) = 2.0 Gyr) have been extensively used to test various cosmological models (see e.g., Alcaniz et al 2003;Wei & Zhang 2007;Wang et al 2010;Yan et al 2015). In the present work, we will use these three age data points to test the wCDM model and the three IDE models.…”

Constraints on Dark Energy From Baryon Acoustic Peak and Galaxy Cluster Gas Mass Measurements

“…Comparison of constraints from different tests can help uncover unknown systematic effects, and combinations of constraints from different tests can better discriminate between models. Other observational tests under recent discussion include the angular size of radio sources and quasars as a function of redshift (see, e.g., Chen & Ratra 2003a;Podariu et al 2003;Daly et al 2007;Santos & Lima 2008), strong gravitational lensing (see, e.g., Lee & Ng 2007;Oguri et al 2008;Zhang et al 2009;Zhu & Sereno 2008), weak gravitational lensing (see, e.g., Takada & Bridle 2007;Fu et al 2008;Doré et al 2007;La Vacca & Colombo 2008), measurements of the Hubble parameter as a function of redshift (see, e.g., Samushia & Ratra 2006;Lazkoz & Majerotto 2007;Wei & Zhang 2008;Szydłowski et al 2008), large-scale structure baryon acoustic oscillation (BAO) peak measurements (see, e.g., Xia et al 2007;Lima et al 2007;Sapone & Amendola 2007) and galaxy cluster gas mass fraction versus redshift data (see, e.g., Allen et al 2004;Sen 2008). For recent reviews of the observational constraints on dark energy, see, e.g., Kurek & Szydłowsky (2008) and Wang (2007).…”

Self-Interacting Holographic Dark Energy

“…We obtain that T z (z) > T obj (z) at z = 3.62, 1.55, 1.43, 1.175 but T z (z) < T obj (z) at z = 3.91, so the old quasar APM 08279+5255 cannot be accommodated as the others old objects. Perhaps, the age crisis at high redshift in the case of dark energy holographic models [140] 75, we obtain that the deceleration parameter vanishes at z acc = 0.78, so the universe enters the accelerated phase earlier than the ΛCDM model. Regarding the effective equation of state, it stays in the range −1 < ω(z) < 0 for z ≥ 0, more precisely, ω(z) starts as non relativistic cold matter, decreases rapidly around z = 2 and then ends with the asymptotic value ω s = −0.95.…”

“…[127], [135]- [141,142], and references therein. The age problem within the context of holographic dark energy model was explored in [140] and [143][144][145]. In this section, we would like to consider the age problem for the SIHDE model with linear interaction.…”