The Cosmic Energy Inventory

By M. Fukugita. 2004

458 citations recorded by the source corpus.

We present an inventory of the cosmic mean densities of energy associated with all the known states of matter and radiation at the present epoch. The observational and theoretical bases for the inventory have become rich enough to allow estimates with observational support for the densities of energy in some 40 forms. The result is a global portrait of the effects of the physical processes of cosmic evolution.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/43579a0c832fe71ede84990e58b2960fb6a01843

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In Astronomy and Astrophysics

Citations in the corpus

Cool Gas in High-Redshift Galaxies (2013, background): “The most important feature of our current understanding of the field is that star and galaxy formation is inefficient: only ∼5% of all baryons (i.e. atoms of all kind) are in stars and dark stellar remnants at redshift zero (e.g., Fukugita & Peebles 2004).”
A LARGER ESTIMATE OF THE ENTROPY OF THE UNIVERSE (2009, methodology): “003 (Fukugita & Peebles 2004), and by using the range of speciﬁc entropies for ISM and IGM components, we ﬁnd The uncertainties in Equations (9) and (11) are dominated by uncertainties in the mass weighting of the speciﬁc entropies, but also include uncertainties in Ω ∗ , Ω gas and the volume of…”
CMB-S4 Science Case, Reference Design, and Project Plan (2019, unknown): “, [380, 381]).”
Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions (2011, background): “on inventory of the Universe, ∼ 30% of the baryons produced during big bang nucleosynthesis (BBN) are missing (Figure 40), and presumably reside in some as yet undetected (dark) form. It is estimated [161, 422] that the observed baryons in clusters only account for about 4% of those produced during ”
Mass, metal, and energy feedback in cosmological simulations (2007, background): “Fukugita & Peebles (2004) estimate a 〈Zb〉(z = 0) ∼ 0.68Z⊙ for all metals including those in remnants, which exceeds the metals not locked up (i.e. the ones we track) by a factor of a few.”
THE BARYON CENSUS IN A MULTIPHASE INTERGALACTIC MEDIUM: 30% OF THE BARYONS MAY STILL BE MISSING (2011, background): “Following the discussion of Fukugita & Peebles (2004), which augments the H I measurements by the expected accompanying cold He I and H2, we plot the total cold gas mass in Figure 9 as 1.7±0.4% of the baryons.”
A semi-analytic model for the co-evolution of galaxies, black holes and active galactic nuclei (2008, background): “…(warm/hot diffuse gas and hot gas in haloes) dominate the baryon budget at all redshifts, in agreement with observational constraints at low redshift (e.g. Fukugita & Peebles 2004) and the predictions of numerical hydrodynamic simulations (Bertone, Schaye & Dolag 2008, and references therein).”
The morgana model for the rise of galaxies and active nuclei (2006, methodology): “Following Fukugita & Peebles (2004), the H I and molecular gas densities at z = 0 C© 2007 The Authors.”
THE SPACE MOTION OF LEO I: THE MASS OF THE MILKY WAY'S DARK MATTER HALO (2012, background): “…Mvir,MW = 5 × 1011 M , then essentially all of those baryons are accounted for by observed stars and gas in and around the Galaxy; if Mvir,MW = 2.5×1012 M , then a large majority of the MW’s baryons are missing (Fukugita & Peebles 2004; Anderson & Bregman 2010; Gupta et al. 2012; Fang et al. 2013).”
DO HOT HALOS AROUND GALAXIES CONTAIN THE MISSING BARYONS? (2010, background): “But studies that attempt to count baryons in the low-redshift universe (Fukugita et al. 1998; Fukugita & Peebles 2004; Nicastro et al. 2005a) find that only about a tenth of this figure is observed in stars and cool gas in galaxies, while another third of Ωb is divided between the hot plasma in the…”
The Search for the Missing Baryons at Low Redshift (2007, background): “Fukugita & Peebles (2004) assigns uncertainties to these choices, leading to uncertainties of about 25% for the stellar content.”
THE EVOLUTION OF GALAXY NUMBER DENSITY AT z < 8 AND ITS IMPLICATIONS (2016, background): “For example, it is of astronomical interest to calculate how many stars are in our Galaxy, how many planets are surrounding these stars (Fressin et al. 2013), the total mass density of the universe (e.g., Fukugita & Peebles 2004), amongst other absolutes in the universe’s properties.”
Reconciling the local galaxy population with damped Lyman α cross-sections and metal abundances (2005, methodology): “Kulkarni & Fall (200 ) and Fukugita & Peebles (2004) applied similar techniques, but integrated over the optical luminosity function and found values of Z̄ ≈ 0.8Z⊙ andZ̄ = 0.83 ± 0.25Z⊙.”
Galaxy groups and clouds in the local (z∼ 0.01) Universe (2010, background): “The horizontal dotted line captures the ratio M/LK = 97 M⊙/L⊙, Galaxy groups in the Local universe 13 which corresponds to K-luminosity density jK = 4.28 10 8 L⊙ Mpc −3 (Jones et al. 2006) assuming Hubble constant H0 = 73 km s −1 Mpc−1 and the cosmic parameter of matter density Ωm = 0.28 in the stan”
A census of metals and baryons in stars in the local universe (2007, background): “…5.219 +1.606 −1.428 This work 8.40+6.04−1.96 6.18 +4.44 −1.44 1 8.96 6.58 2 4.62 ± 1.08 3.4 ± 0.8 3 6.57 4.83 4 3.4 2.5 5 4.2–6.4 3.09–4.7 6 8.7–13.3 6.3–9.7 7 Observational estimates of metal mass density in stars are from: (1) Pagel (2002), (2) Dunne et al. (2003), (3) Fukugita & Peebles (2004).”
Simulations of Cosmic Chemical Enrichment (2006, background): “Journal compilation C© 2007 RAS, MNRAS 376, 1465–1479 Downloaded from https://academic.oup.com/mnras/article-abstract/376/4/1465/1013918 by guest on 30 July 2018 25 per cent of baryons turn into stars, which is too large compared with observational estimates (e.g. Fukugita & Peebles 2004).”
Herschel-ATLAS: rapid evolution of dust in galaxies over the last 5 billion years (2010, background): “Fukugita & Peebles (2004) estimated a theoretical value of dust = 2.5 × 10−6 today based on the estimated density of cold gas, the metallicity-weighted LF of galaxies and a dust to metals ratio of 0.2.”