A recipe for galaxy formation

Cole, Shaun; Aragón-Salamanca, Alfonso; Frenk, Carlos S.; Navarro, Julio F.; Zepf, Stephen E.

doi:10.1093/mnras/271.4.781

Cited by 829 publications

(992 citation statements)

References 23 publications

Supporting

Mentioning

958

Contrasting

Unclassified

Order By: Relevance

“…SNfb is thought to be responsible for the relatively flat galaxy stellar mass and luminosity functions compared to the steeply rising halo mass function predicted by N -body simulations for ΛCDM (e.g. Jenkins et al 2001;Tinker et al 2008;Kauffmann et al 1993;Cole et al 1994). On the smallest scales, SNfb, in conjunction with photoionisation of gas in the early Universe, can explain the small number of faint satellite galaxies seen around galaxies like the Milky Way in this model (Efstathiou 1992;Benson et al 2003;Sawala et al 2015).…”

Section: A Galactic "Tug-of-war"mentioning

confidence: 99%

Reionization in sterile neutrino cosmologies

Bose¹,

Frenk²,

Hou³

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe investigate the process of reionisation in a model in which the dark matter is a warm elementary particle such as a sterile neutrino. We focus on models that are consistent with the dark matter decay interpretation of the recently detected line at 3.5 keV in the X-ray spectra of galaxies and clusters. In warm dark matter models the primordial spectrum of density perturbations has a cut-off on the scale of dwarf galaxies. Structure formation therefore begins later than in the standard cold dark matter (CDM) model and very few objects form below the cut-off mass scale. To calculate the number of ionising photons, we use the Durham semianalytic model of galaxy formation, GALFORM. We find that even the most extreme 7 keV sterile neutrino we consider is able to reionise the Universe early enough to be compatible with the bounds on the epoch of reionisation from Planck. This, perhaps surprising, result arises from the rapid build-up of high redshift galaxies in the sterile neutrino models which is also reflected in a faster evolution of their far-UV luminosity function between 10 > z > 7 than in CDM. The dominant sources of ionising photons are systematically more massive in the sterile neutrino models than in CDM. As a consistency check on the models, we calculate the present-day luminosity function of satellites of Milky Way-like galaxies. When the satellites recently discovered in the DES survey are taken into account, strong constraints are placed on viable sterile neutrino models.

show abstract

Section: A Galactic "Tug-of-war"mentioning

confidence: 99%

Reionization in sterile neutrino cosmologies

Bose¹,

Frenk²,

Hou³

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…2 (White & Frenk 1991;Lacey & Silk 1991;Cole et al 1994). We build merger trees for 800 z = 4 galaxies equally spaced in log M h between 10 8−13 M using the modified binary merger tree algorithm with accretion presented in Parkinson et al (2008).…”

Section: Merger Tree Physicsmentioning

confidence: 99%

Essential physics of early galaxy formation

Dayal

Ferrara

Dunlop

et al. 2014

Monthly Notices of the Royal Astronomical Society

152

209

View full text Add to dashboard Cite

We present a theoretical model embedding the essential physics of early galaxy formation (z 5 − 12) based on the single premise that any galaxy can form stars with a maximal limiting efficiency that provides enough energy to expel all the remaining gas, quenching further star formation. This simple idea is implemented into a merger-tree based semi-analytical model that utilises two mass and redshiftindependent parameters to capture the key physics of supernova feedback in ejecting gas from low-mass halos, and tracks the resulting impact on the subsequent growth of more massive systems via halo mergers and gas accretion. Our model shows that: (i) the smallest halos (halo mass M h 10 10 M ) build up their gas mass by accretion from the intergalactic medium; (ii) the bulk of the gas powering star formation in larger halos (M h 10 11.5 M ) is brought in by merging progenitors; (iii) the faint-end UV luminosity function slope evolves according to α = −1.75 log z − 0.52. In addition, (iv) the stellar mass-to-light ratio is well fit by the functional form log M * = −0.38M U V − 0.13 z + 2.4, which we use to build the evolving stellar mass function to compare to observations. We end with a census of the cosmic stellar mass density (SMD) across galaxies with UV magnitudes over the range −23 M U V −11 spanning redshifts 5 < z < 12: (v) while currently detected LBGs contain ≈ 50% (10%) of the total SMD at z = 5 (8), the JWST will detect up to 25% of the SMD at z 9.5.

show abstract

“…Semi-analytic modelling is a particular simulation method which is optimized to connect the observed properties of the galaxy population -abundances, scaling relations, clustering and their evolution with redshift -to the astrophysical processes that drive the formation and evolution of individual galaxies (e.g. White 1989;Cole 1991;Lacey & Silk 1991;White & Frenk 1991;Cole et al 1994;Somerville & Primack 1999;Hatton et al 2003;Kang et al 2005;Lu et al 2011;Benson 2012). Simple phenomenological descriptions of the relevant processes are needed, each typically involving uncertain efficiency and scaling parameters.…”

Section: Introductionmentioning

confidence: 99%

Galaxy formation in the Planck cosmology – I. Matching the observed evolution of star formation rates, colours and stellar masses

Henriques

White

Thomas

et al. 2015

Monthly Notices of the Royal Astronomical Society

580

747

View full text Add to dashboard Cite

We have updated the Munich galaxy formation model to the Planck first-year cosmology, while modifying the treatment of baryonic processes to reproduce recent data on the abundance and passive fractions of galaxies from z = 3 down to z = 0. Matching these more extensive and more precise observational results requires us to delay the reincorporation of wind ejecta, to lower the surface density threshold for turning cold gas into stars, to eliminate ram-pressure stripping in haloes less massive than ∼ 10 14 M ⊙ , and to modify our model for radio mode feedback. These changes cure the most obvious failings of our previous models, namely the overly early formation of low-mass galaxies and the overly large fraction of them that are passive at late times. The new model is calibrated to reproduce the observed evolution both of the stellar mass function and of the distribution of star formation rate at each stellar mass. Massive galaxies (log M * / M ⊙ 11.0) assemble most of their mass before z = 1 and are predominantly old and passive at z = 0, while lower mass galaxies assemble later and, for log M * / M ⊙ 9.5, are still predominantly blue and star forming at z = 0. This phenomenological but physically based model allows the observations to be interpreted in terms of the efficiency of the various processes that control the formation and evolution of galaxies as a function of their stellar mass, gas content, environment and time.

show abstract

A recipe for galaxy formation

Cited by 829 publications

References 23 publications

Reionization in sterile neutrino cosmologies

Reionization in sterile neutrino cosmologies

Essential physics of early galaxy formation

Galaxy formation in the Planck cosmology – I. Matching the observed evolution of star formation rates, colours and stellar masses

Contact Info

Product

Resources

About