Matter Content of the Universe  

In General > s.a. astronomy; early universe; matter.
* 1995: The dogma is b 0.05, dm 0.95, cc = 0.
* 1998: M Turner & D Schramm predict 5% ordinary matter, based on deuterium abundance.
* 1999: "Matter" consists of ordinary matter/radiation ( 0.2), dark matter, and dark energy (possibly a cosmological constant).
* 2000: Cold dark matter from new cmb data; Favored values m 0.4 0.1, b = 0.02 h–2, 0.001 < nu < 0.1, cc 0.7.
* 2001: New DASI and Boomerang cmb data; Favored values b = 0.05, dm = 0.30, de = 0.65 (p < 0).
* 2002: 2dF galaxy redshift survey and cmb, m = 1 – cc = 0.30; Using KamLAND data, nu 0.070 h–2.
* 2003: WMAP data give b = 0.04, dm = 0.23, de = 0.73; SDSS data, b = 0.05, dm = 0.25, de = 0.70.
* 2003: CDM provides best fit to data, with tot = 1.02 0.02.
* Critical density: At the present time, crit = 6 H atoms/m3 = 10–26 kg/m3; Notice that cc = c2/3H02.
* Entropy: The entropy of the universe is low but increasing.
@ Matter content: Melott PRP(90); Persic & Salucci MNRAS(92)ap/05 [baryons]; Bahcall ap/96 [large-scale structure]; White ap/96-in [large z]; Dolgov ap/02-in, ap/02-in [antimatter]; Krauss & Scherrer PRD(07)ap [radiation cannot become dominant again].
@ Density: Coles & Ellis Nat(94)aug, 97; Bahcall & Fan PNAS(98)ap; Krauss hp/98-in [cosmological constant]; Bahcall PS(00)ap/99-in [galaxy clusters]; Roos & Harun-or-Rashid ap/00, ap/00 [flatness]; Turner ApJL(02)ap/01; Schindler ap/01-in [m]; Waterhouse & Zibin a0804 [variation of ].

Magnetic Fields > s.a. astronomical phenomena.
* Theoretically: A universal magnetic field has been proposed as a way of avoiding the initial singularity in some cases; It also favors formation of structure in the universe.
* And observation: There seem to be Mpc-scale, 10–7–10–5-G magnetic fields in all galaxies and clusters, possibly arising from differential rotation and helical turbulence, but their origin is not totally clear; Search for a universal magnetic field so far has been inconclusive, and it does not seem to be favorred by many.
@ General: Enqvist IJMPD(98)ap, Carroll & Field ap/98-in, Field & Carroll PRD(00)ap/98 [primordial]; Hogan ap/00 [from recombination]; Gasperini PRD(01)ap/00 [seeds, theory]; Tsagas gq/01-in [coupling to geometry]; Clarkson et al CQG(03)ap/02 [from cmb]; Shukla PS(05) [origin]; de Gouveia Dal Pino ap/06-in.
@ Galactic and intergalactic: Anchordoqui & Goldberg PRD(02)hp/01 [extragalactic, local]; Kronberg PT(02)dec; Giovannini IJMPD(04)ap/03 [th, review]; Dar & De Rújula PRD(05)ap [theory]; > s.a. astronomical objects.
@ Early universe: Davidson PLB(96); Grasso & Rubinstein PRP(01).
@ UMF: in Olivo-Melchiorri & Melchiorri RNC(85) & refs.

Types of Matter > s.a. dark matter; electroweak theory; inflationary scenarios; quantum field theory in curved spacetime; topological defects.
* Components: Ordinary "baryonic" matter, dark matter, "dark energy" (possibly a cosmological constant).
* Cosmic IR background: One motivation to study it is to learn more about population III stars, whole light is now mostly IR.
@ Reviews: Dine ht/01-in; Durrer ap/02-in; Fukugita & Peebles ApJ(04)ap [energy inventory].
@ Repulsive matter: Cornish & Starkman ap/98; > s.a. dark energy.
@ Mirror matter: Foot PLB(99)ap [stars?], PLB(99)ap [planets?]; Mohapatra & Teplitz PLB(99)ap [MACHOs?]; Foot & Mitra APP(03)ap/02 [Solar System]; Foot & Silagadze IJMPD(05) [supernovas and GRB's]; Ciarcelluti IJMPD(05), IJMPD(05).
@ Cosmic IR background: news pn(98)jan; Biller et al PRL(98) [limits]; Kashlinsky PRP(05)ap/04; Fernandez & Komatsu ApJ(06)ap/05 [near IR]; Lagache et al ap/05-in [sources]; Kashlinsky et al ApJL(07)ap/06 [sources].
@ Cosmic 21-cm background: Cooray PRD(06) [and e scattering]; Kleban et al JCAP(07)ht, Wyithe & Loeb a0708-MNRAS [fluctuations]; Loeb JCAP(08)-a0801 [validity of classical treatment]; Metcalf a0801-in [gravitational lensing]; Pritchard & Loeb a0802-PRD [evolution]; Pen et al a0802-MNRAS [detection of structure]; > s.a. observational cosmology; perturbations.
@ Other diffuse background: Henry ap/99; Lagache et al ASS(99)ap [sub-mm]; > s.a. cmb; gamma rays; gravitons; neutrinos.

Matter Distribution > s.a. galaxy distribution; perturbations; relativistic cosmology; quantum cosmology.
* Idea: Luminous matter has a roughly fractal distribution up to 15–20 Mpc, while radiation is much more homogeneous and isotropic; They are distributed approximately the same way at galaxy cluster scales, and are possibly homogeneous on larger, super-horizon scales; We don't know why.
* Fluctuations: There is a spectrum of density fluctuations (Zel'dovich spectrum?); No consensus on origin.
@ Clustering, large-scale stucture: Governato et al Nat(98)ap [seeds]; Guzzo ap/99-in; Einasto ap/00-in; Sylos Labini & Pietronero ap/01-in [complexity]; Gott et al ApJ(05)ap/03 [complete map]; Hwang & Noh ap/05 [validity of Newtonian modeling].
@ Homogeneity: Gaite et al ApJL(99)ap/98 [matter, vs fractal]; Dautcourt ap/99 [constraints]; Lahav ap/99-in, ap/00-in; Trodden & Vachaspati MPLA(99)gq [problem].
@ Case against homogeneity: Clarkson & Barrett CQG(99)ap, Barrett & Clarkson CQG(00)ap/99; Clarkson ap/00-PhD.
@ Statistical methods: Kerscher ap/99-in; Shandarin ap/04-in; Gabrielli et al 05; > s.a. cmb.
@ Skewness: Amendola & Quercellini PRL(04)ap [and the equivalence principle].
@ Related topics: Durrer & Sylos Labini ap/98/A&AL, Gawiser ap/00-PhD [and cmb]; > s.a. fractals.

Observational Missions
* Past: COBE (Cosmic Background Explorer), launched in 1989, reported the first anisotropy in 1992.
* Present and future: WMAP (Wilkinson Microwave Anisotropy Probe) launched in 2001, reported results in 2003 and 2006; ESA's Planck, scheduled for launch in 2009.

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