The lives of high-redshift mergers

McCavana, Tom; Micic, M.; Lewis, Geraint F.; Sinha, Manodeep; Sharma, Sanjib; Holley‐Bockelmann, Kelly; Bland-Hawthorn, Joss

doi:10.1111/j.1365-2966.2012.21202.x

Cited by 24 publications

(29 citation statements)

References 47 publications

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“…Satellite galaxies are those associated with each dark matter branch merging with the main progenitor. When galaxies become satellites in larger haloes, they are assigned a dynamical friction time-scale for final coalescence with the central galaxy taken from McCavana et al (2012). They are also assigned all the mass and structural properties of a central galaxy in a typical halo, within the Monte Carlo catalog, of the same mass at the time of infall.…”

Section: Methodsmentioning

confidence: 99%

AVOIDING PROGENITOR BIAS: THE STRUCTURAL AND MASS EVOLUTION OF BRIGHTEST GROUP AND CLUSTER GALAXIES IN HIERARCHICAL MODELS SINCEz≲ 1

Shankar

Buchan

Rettura

et al. 2015

ApJ

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The mass and structural evolution of massive galaxies is one of the hottest topics in galaxy formation. This is because it may reveal invaluable insights into the still debated evolutionary processes governing the growth and assembly of spheroids. However, direct comparison between models and observations is usually prevented by the so-called progenitor bias, i.e., new galaxies entering the observational selection at later epochs, thus eluding a precise study of how pre-existing galaxies actually evolve in size. To limit this effect, we here gather data on high-redshift brightest group and cluster galaxies, evolve their (mean) host halo masses down to z = 0 along their main progenitors, and assign as their "descendants" local Sloan Digital Sky Survey central galaxies matched in host halo mass. At face value, the comparison between high redshift and local data suggests a noticeable increase in stellar mass of a factor of 2 since z ∼ 1, and of 2.5 in mean effective radius. We then compare the inferred stellar mass and size growth with those predicted by hierarchical models for central galaxies, selected at high redshifts to closely match the halo and stellar mass bins as in the data. Only hierarchical models characterized by very limited satellite stellar stripping and parabolic orbits are capable of broadly reproducing the stellar mass and size increase of a factor of ∼2-4 observed in cluster galaxies since z ∼ 1. The predicted, average (major) merger rate since z ∼ 1 is in good agreement with the latest observational estimates.

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Section: Methodsmentioning

confidence: 99%

AVOIDING PROGENITOR BIAS: THE STRUCTURAL AND MASS EVOLUTION OF BRIGHTEST GROUP AND CLUSTER GALAXIES IN HIERARCHICAL MODELS SINCEz≲ 1

Shankar

Buchan

Rettura

et al. 2015

ApJ

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“…where A=0.9, B=1.0, C=0.6, D=0.1 (McCavana et al 2012). The factor τ dyn is given by (Jiang & van den Bosch 2016),…”

Section: Subhalo Merging Timescalementioning

confidence: 99%

A statistical semi-empirical model: satellite galaxies in groups and clusters

Grylls

Shankar

Zanisi

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present STEEL a STatistical sEmi-Empirical modeL designed to probe the distribution of satellite galaxies in groups and clusters. Our fast statistical methodology relies on tracing the abundances of central and satellite haloes via their mass functions at all cosmic epochs with virtually no limitation on cosmic volume and mass resolution. From mean halo accretion histories and subhalo mass functions the satellite mass function is progressively built in time via abundance matching techniques constrained by number densities of centrals in the local Universe. By enforcing dynamical merging timescales as predicted by high-resolution N-body simulations, we obtain satellite distributions as a function of stellar mass and halo mass consistent with current data. We show that stellar stripping, star formation, and quenching play all a secondary role in setting the number densities of massive satellites above M * 3 × 10 10 M . We further show that observed star formation rates used in our empirical model over predict low-mass satellites below M * 3 × 10 10 M , whereas, star formation rates derived from a continuity equation approach yield the correct abundances similar to previous results for centrals.

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“…Compared with the main result using the merger timescale model J08 (Figure 7), there is a ∼ 25% change in the amplitude of δξ ∆s . Hong et al (2016) also considered four alternative models for the calculation of merger timescale: 1) the LC93 model (Lacey & Cole 1993) based on analytic calculation, 2) the B08 (Boylan-Kolchin et al 2008) and 3) the V13 (Villalobos et al 2013) models based on isolated simulations, and 4) the M12 model (McCavana et al 2012) based on cosmological simulation. Among the five merger timescale models, J08 model produces mock galaxies having properties and 2pCF best agree with the observational data (Hong et al 2016); the LC93 model, having the shortest merger timescale among the five models, produces galaxies with properties and 2pCF most deviated from the observations.…”

Section: Ock Galaxies F or Systematic Correctionmentioning

confidence: 99%

Cosmological Constraints From the Redshift Dependence of the Alcock–paczynski Effect: Application to the SDSS-Iii Boss Dr12 Galaxies

Park

Sabiu

et al. 2016

ApJ

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We apply the methodology developed in Li et al. ( , 2015 to BOSS DR12 galaxies and derive cosmological constraints from the redshift dependence of the Alcock-Paczynski (AP) effect. The apparent anisotropy in the distribution of observed galaxies arise from two main sources, the redshiftspace distortion (RSD) effect due to the galaxy peculiar velocities, and the geometric distortion when incorrect cosmological models are assumed for transforming redshift to comoving distance, known as the AP effect. Anisotropies produced by the RSD effect are, although large, maintaining a nearly uniform magnitude over a large range of redshift, while the degree of anisotropies from the AP effect varies with redshift by much larger magnitude. We split the DR12 galaxies into six redshift bins, measure the 2-point correlation function in each bin, and assess the redshift evolution of anisotropies. We obtain constraints of Ω m = 0.290±0.053, w = −1.07±0.15, which are comparable with the current constraints from other cosmological probes such as type Ia supernovae, cosmic microwave background, and baryon acoustic oscillation (BAO). Combining these cosmological probes with our method yield tight constraints of Ω m = 0.301 ± 0.006, w = −1.054 ± 0.025. Our method is complementary to the other large scale structure probes like BAO and topology. We expect this technique will play an important role in deriving cosmological constraints from large scale structure surveys. Subject headings: large-scale structure of Universe -dark energy -cosmological parameters

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The lives of high-redshift mergers

Cited by 24 publications

References 47 publications

AVOIDING PROGENITOR BIAS: THE STRUCTURAL AND MASS EVOLUTION OF BRIGHTEST GROUP AND CLUSTER GALAXIES IN HIERARCHICAL MODELS SINCEz≲ 1

AVOIDING PROGENITOR BIAS: THE STRUCTURAL AND MASS EVOLUTION OF BRIGHTEST GROUP AND CLUSTER GALAXIES IN HIERARCHICAL MODELS SINCEz≲ 1

A statistical semi-empirical model: satellite galaxies in groups and clusters

Cosmological Constraints From the Redshift Dependence of the Alcock–paczynski Effect: Application to the SDSS-Iii Boss Dr12 Galaxies

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