Matter Content of the Universe  

In General > s.a. astronomy; early-universe cosmology; 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]; Holder et al a0907/ApJ [baryon-dark matter ratio fluctuations]; Ferreira & Starkmann Sci-a0911 [dark fields vs modified gravity].
@ 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 references: 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 AIP-ap/06.
@ 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); Brown PhD(06)-a0812 [primordial].
@ 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).
* 2008: Recent experiments, including PAMELA, ATIC, WMAP, and EGRET, have revealed unusually high electron-positron production in the cosmos, more so than can be explained by mechanisms such as supernova explosions or cosmic-ray collisions; This discrepancy is leading some researchers to speculate that dark matter may play a part [@ news pt(08)nov].
* 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 GRBs]; 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, Fernandez et al a0906/ApJ [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 NCB(07)-a0801-in [gravitational lensing]; Pritchard & Loeb PRD(08)-a0802 [evolution]; Pen et al a0802/MNRAS [detection of structure]; Peterson et al a0902-rp [mapping]; Khatri & Wandelt a0910-in [and fundamental physics]; > s.a. observational cosmology; perturbations.
@ Other diffuse background: Henry ap/99; Lagache et al ASS(99)ap [sub-mm]; Zhao et al PLB(09) [free-streaming gas in radiation-dominated era]; > s.a. cmb; gamma rays; gravitons; neutrinos.

Matter Distribution > s.a. galaxy distribution [including cosmic web]; 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.
* Galactic vs cosmic abundances: The Milky Way and all other galaxies are missing most of their baryons in that the ratio of the known baryonic mass to the gravitating mass (within the virial radius), is several times less than the cosmic ratio determined from WMAP.
* 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]; Bregman a0906 [galactic vs cosmic].
@ 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 PhD(99)ap/00.
@ Local void scenarios: Alexander et al a0710 [supernova and cmb data]; > s.a. theory of cosmological acceleration.
@ 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 A&AL-ap/98, Gawiser PhD(99)ap/00 [and cmb]; > s.a. fractals in physics.

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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