Causality, randomness, and the microwave background

(1995)

Authors:

Andreas Albrecht, David Coulson, Pedro Ferreira, Joao Magueijo

Causality, randomness, and the microwave background

ArXiv astro-ph/9505030 (1995)

Authors:

Andreas Albrecht, David Coulson, Pedro Ferreira, Joao Magueijo

Abstract:

Fluctuations in the cosmic microwave background (CMB) temperature are being studied with ever increasing precision. Two competing types of theories might describe the origins of these fluctuations: ``inflation'' and ``defects''. Here we show how the differences between these two scenarios can give rise to striking signatures in the microwave fluctuations on small scales, assuming a standard recombination history. These should enable high resolution measurements of CMB anisotropies to distinguish between these two broad classes of theories, independent of the precise details of each.

AN IMAGING K-BAND SURVEY - II: THE REDSHIFT SURVEY AND GALAXY EVOLUTION IN THE INFRARED

ArXiv astro-ph/9502094 (1995)

Authors:

Karl Glazebrook, JA Peacock, L Miller, CA Collins

Abstract:

We present a redshift survey of 124 galaxies, from an imaging $K$-band survey complete to $K\simeq 17.3$. The optical-to-infrared colours are consistent with the range expected from synthetic galaxy spectra, although there are some cases of very red nuclei. Our data show no evidence for evolution of the $K$-band luminosity function at $z<0.5$, and the results are well described by a Schechter function with $M_K^*=-22.75\pm0.13+5\log_{10}h$ and $\phi^*=0.026\pm0.003 h^3 {\rm Mpc^{-3}}$. This is a somewhat higher normalization than has been found by previous workers, and it removes much of the excess in faint $K$ and $B$ counts with respect to a no-evolution model. However, we do find evidence for evolution at $z>0.5$: $M_K^*$ is approximately 0.75 mag. brighter at $z=1$. This luminosity evolution is balanced by a reduced normalization at high redshift. The overall evolution is thus opposite to that expected in simple merger-dominated models.

COSMIC STRINGS IN AN OPEN UNIVERSE WITH BARYONIC AND NONBARYONIC DARK-MATTER

PHYSICAL REVIEW LETTERS 74:18 (1995) 3522-3525

Cosmic Strings in an Open Universe with Baryonic and Non-Baryonic Dark Matter

ArXiv astro-ph/9410032 (1994)

Abstract:

We study the effects of cosmic strings on structure formation in open universes. We calculate the power spectrum of density perturbations for two class of models: one in which all the dark matter is non baryonic (CDM) and one in which it is all baryonic (BDM). Our results are compared to the 1 in 6 IRAS QDOT power spectrum. The best candidates are then used to estimate $\mu$, the energy per unit length of the string network. Some comments are made on mechanisms by which structures are formed in the two theories.