Appropriating Egypt for the Ara Pacis Augustae*

A Review on the Scalar Field/Bose-Einstein Condensate Dark Matter Model

“…Over the past few decades, theories concerning the stability of galaxies ( [108,9]) indicated that most of the mass in our Universe is dark (i.e., it does not emits or absorbs light [90,116]), therefore resulting unobservable by telescopes. The suggestion that "dark matter" may form a large fraction of the density in the Universe was raised by Zwicky in 1937.…”

“…The observed flatness of the galactic rotation curved indicating the presence of dark matter halos around galaxies [108]. Summed to these evidences are the observations of the cosmic microwave background (CMB) anisotropies ( [112,57]) combined with large-scale structure and type Ia supernova luminosity data ( [100,101,102,97]) which all together constrain the cosmological parameters also finding once more that visible matter contributes only about 4% of the energy density of the Universe, gravitational lensing [99] and X-ray spectra ( [69,37,116,36,87]) in elliptical galaxies, and the high velocity dispersion and gas temperature in clusters of galaxies ( [116,74]), all of them leading to a picture in which galaxies are composed of a luminous galactic disk surrounded by a galactic halo of dark matter. Also the relative contribution of the dark matter component is usually specified in terms of the mass-to-light ratio, M/L; which reflects the total amount of mass relative to the total light within a given scale.…”

The Mass‐to‐Light Function: Antibias and \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{emp

“…In this method, the average ratio of the observed mass to light of the largest possible systems is used; assuming it is a fair sample, it can then be multiplied by the total luminosity density of the universe to yield the universal mass density. When the method is applied to rich clusters of galaxies -the largest virilized systems for which a mass has been reliably determined -the total mass density of the universe adds up to only Ω ≃ 0.2 (where Ω is the mass density in units of the critical density) (Zwicky 1957, Abell 1965, Ostriker, Peebles & Yahil 1974, Bahcall 1977, Faber & Gallagher 1979, Trimble 1987, Peebles 1993, Bahcall, Lubin & Dorman 1995, Carlberg et al 1996, 1997, and references therein). A fundamental assumption in this determination, however, is that the mass-to-light ratio (M/L) of clusters is a fair representation of the universal value.…”

“…Observations of galaxies, groups and clusters of galaxies suggest that M/L increases as a function of scale up to scales of hundreds of kiloparsecs (Schwarzschild 1954, Rubin & Ford 1970, Roberts & Rots 1973, Ostriker et al 1974, Einasto et al 1974, Davis et al 1980, Trimble 1987, Gramann 1990, Zaritzky et al 1993, Fischer et al 1999, but then flattens out and remains approximately constant on larger scales (Bahcall, Lubin & Dorman 1995). In the modern context we normally interpret this fact as indicating that luminous galaxies are more concentrated in peak density regions than the dark matter because baryons are dissipational.…”

Faint Blue Objects on the Hubble Deep Field North and South as Possible Nearby Old Halo White Dwarfs

“…Using data derived from the deepest and finest angular resolution images of the universe yet acquired by astronomers at optical wavelengths using the Hubble Space Telescope (HST) in two postage-stamp sections of the sky (Williams et al 1996a,b), plus simple geometrical and scaling arguments, we demonstrate that the faint blue population of point-source objects detected on those two fields (Méndez et al 1996) could actually be ancient halo white dwarfs at distances closer than about 2 kpc from the Sun. This finding has profound implications, as the mass density of the detected objects would account for about half of the missing dark matter in the Milky-Way (Bahcall and Soneira 1980), thus solving one of the most controversial issues of modern astrophysics (Trimble 1987, Ashman 1992.…”