Galaxy Formation and Evolution: Frontmatter

By H. Mo, F. V. D. Bosch, Simon D. M. White. 2010

288 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geometry and Topology

View Paper: https://www.semanticscholar.org/paper/e230def1da4c0ae86323c983db1ed659dfdc2a6f

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Citations in the corpus

The Milky Way’s stellar disk (2013, methodology): “In the world of galaxies, the Milky Way is in many ways as typical as it gets: half of the Universe’s present-day stars live in galaxies that match our Milky Way in stellar mass, size, chemical abundance, etc. within factors of a few (e.g., Mo et al. 2010).”
The extragalactic background light and the gamma-ray opacity of the universe (2012, methodology): “…energy releases over cosmic history: Iν(λ0, z0) = ∫ ∞ z0 (1 + z) Lν(λ, z) 4π dL(z)2 dVc(z) δΩ (2) = ( 1 4π ) ∫ ∞ z0 Lν(λ, z) ∣ ∣ ∣ ∣ c dt dz ∣ ∣ ∣ ∣ dz where c|dt/dz| is given by (e.g. Mo et al., 2010): c ∣ ∣ ∣ ∣ dt dz ∣ ∣ ∣ ∣ = RH (1 + z)E(z) ; RH ≡ c H0 (3) E(z) ≡ [ ΩR(1 + z) 4 + Ωm(1 + z) 3 +…”
Disruption of Dark Matter Substructure: Fact or Fiction? (2017, background): “…to be significant for the most massive subhaloes, with a mass that exceeds a few percent of that of the host halo (e.g., Binney & Tremaine 2008; Mo et al. 2010), and various studies have pointed out that indeed dynamical friction makes a negligible contribution to the evolution of the ensemble…”
Dynamics for galactic archaeology (2013, background): “Nevertheless in the recent years significant progress has been made with simulations of galaxy formation and we now have a pretty good idea of how galaxies form (Mo et al., 2010).”
Early galaxy formation and its large-scale effects (2018, methodology): “ing a non-relativistic monoatomic gas such that c2 s= 5kBT 3mp ; (7) where kBis the Boltzmann constant, mpis the proton mass and T is the CMB temperature. This results in a co-moving Jeans length [84]: Jˇ0:01( bh2) 1=2 Mpc; (8) where bis the baryonic density parameter at z= 0, yielding a constant ”
Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, methodology): “This results in the ‘linear’ halo model, which has been used previously by numerous authors (e.g., Ma & Fry 2000; Seljak 2000; Scoccimarro et al. 2001; Guzik & Seljak 2002; Mandelbaum et al. 2005; Seljak et al. 2005; see also Cooray & Sheth 2002 and Mo et al. 2010).”
Chemical signatures of formation processes in the stellar populations of simulated galaxies (2011, background): “Nevertheless important open questions remain, in particular on galactic scales (Mo et al. 2010).”
UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, methodology): “Here, we adopt a crude cooling time estimate from Mo et al. (2010): tcool∼ 1.5×109 yr ( Tvir 106 K )( 10−3 cm−3 〈nH〉 )( 10−23 erg cm3 s−1 Λ(Tvir) ) (30) where nH is the average density of hydrogen atoms in the halo; we take the cooling function Λ(T ) from De Rijcke et al. (2013) for a 1/3Z gas.”