WebPhoton decoupling is closely related to recombination, which occurred about 378,000 years after the Big Bang (at a redshift of z = 1100 ), when the universe was a hot opaque … Webtime of matter-radiation equality, 143 y Sunyaev Zel dovich y-parameter, 470 iid, independent and identically distributed, 547, 548, 692 z eq redshift of matter-radiation equality, 143 abundances light elements, 182 acceleration, 417 af ne parameters, 324 age cosmic, 433 look-back time, 139, 140 Universe, 38, 118, 120, 139

2. Astrophysical constants 1 - Particle Data Group

WebOnce nearly all the charged particles were bound in neutral atoms, the photons no longer interacted with them and were free to propagate for the next 13.8 billion years; we currently detect those photons redshifted by a factor 1090 down to 2.725 K as the Cosmic Microwave Background Radiation ( CMB) filling today's universe. Webmatter and radiation will have the same density, ρm= ρr. This epoch is called matter-radiation equality. We’ll need to calculate it next since it determines the expansion … b built uk

cosmology - Redshift of mass-dominant universe - Physics

Webclosely related to the horizon size at matter-radiation equality for a large variety of flat ΛCDM models. Using large-volume cosmological simulations, we also show that the … Webmass of the horizon at the redshift of matter-radiation equality z eq 23000 (for mh ¼ 0:127; Spergel et al. 2007). The rela- ... PBHs are particularly interesting because, after the redshift of matter-radiation equivalence, each PBH seeds the growth of a dark halo that, over time, becomes considerably more massive ... Webthe radiation density drops faster than the dark-matter density. At a redshift zeq ∼ 3400 the equality of radia-tion and matter densities occurs. This is the beginning of the matter-dominated epoch and, after this moment, dark matter drives the expansion. During most of its life, the Universe made use of this matter dominance to b bumble