Probing Galaxy assembly bias in BOSS galaxies using void probabilities

Walsh, Kilian; Tinker, Jeremy L.

doi:10.1093/mnras/stz1351

Cited by 39 publications

(27 citation statements)

References 70 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Lacerna, Padilla & Stasyszyn 2014;Hearin, Watson & van den Bosch 2015;Watson et al 2015;Montero-Dorta et al 2017), while others indicate that the imprint on the galaxy distribution is small (e.g. Lin et al 2016;Zu & Mandelbaum 2016;Walsh & Tinker 2019). Assessing the existence of assembly bias in the real Universe is an important task; cosmological constraints from future surveys will most likely be limited by how well we can model the observations rather than the precision of the measurements.…”

mentioning

confidence: 99%

The assembly bias of emission-line galaxies

Jiménez

Padilla

Contreras

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The next generation of spectroscopic surveys will target emission-line galaxies (ELGs) to produce constraints on cosmological parameters. We study the large scale structure traced by ELGs using a combination of a semi-analytical model of galaxy formation, a code that computes the nebular emission from H ii regions using the properties of the interstellar medium, and a large-volume, high-resolution N-body simulation. We consider fixed number density samples where galaxies are selected by either their Hα, [O iii] λ5007 or [O ii] λλ3727 − 3729 emission line luminosities. We investigate the assembly bias signatures of these samples, and compare them to those of stellar mass and SFR selected samples. Interestingly, we find that the [O iii]- and [O ii]-selected samples display scale-dependent bias on large scales and that their assembly bias signatures are also scale-dependent. Both these effects are more pronounced for lower number density samples. The [O iii] and [O ii] emitters that contribute most to the scale dependence tend to have a low gas-phase metallicity and are preferentially found in low-density regions. We also measure the baryon acoustic oscillation (BAO) feature and the β parameter related to the growth rate of overdensities. We find that the scale of the BAO peak is roughly the same for all selections and that β is scale-dependent at large scales. Our results suggest that ELG samples include environmental effects that should be modelled in order to remove potential systematic errors that could affect the estimation of cosmological parameters.

show abstract

mentioning

confidence: 99%

The assembly bias of emission-line galaxies

Jiménez

Padilla

Contreras

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Finally, although we have not addressed it here, our wellcalibrated machinery can be used to perform clustering measurements at fixed halo mass for both central and satellite galaxies separately. This type of measurements are relevant in the context of galaxy assembly bias (see, e.g., Zentner et al 2016;Miyatake et al 2016;Zu et al 2016;Lin et al 2016;Sunayama et al 2016;Montero-Dorta et al 2017;Artale et al 2018;Niemiec et al 2018;Zehavi et al 2018;Walsh & Tinker 2019;Sunayama & More 2019;Obuljen et al 2020;Montero-Dorta et al 2020a,b). The excellent classification of central and satellite galaxies that we have achieved with the SDSS can also be employed to investigate the manifestation of physical processes that drive the evolution of galaxy populations, particularly with the improved data quality of upcoming surveys.…”

Section: Discussionmentioning

confidence: 99%

“…However, a number of secondary dependencies of halo clustering have been identified in recent years (on, e.g., halo age, concentration or spin, see, e.g., Sheth & Tormen 2004;Gao et al 2005;Wechsler et al 2006;Gao & White 2007;Angulo et al 2008;Li et al 2008;Lazeyras et al 2017;Paranjape & Padmanabhan 2017;Salcedo et al 2018;Han et al 2018;Mao et al 2018; Sato-Polito 1 http://www.tng-project.org Johnson et al 2019;Ramakrishnan et al 2019;Tucci et al 2020). Whether these dependencies transmit to the galaxy population or not is still a matter of intense debate (Zentner et al 2016;Miyatake et al 2016;Zu et al 2016;Lin et al 2016;Sunayama et al 2016;Montero-Dorta et al 2017;Artale et al 2018;Niemiec et al 2018;Zehavi et al 2018;Walsh & Tinker 2019;Sunayama & More 2019;Montero-Dorta et al 2020a,b;Obuljen et al 2020;Salcedo et al 2020), but the existence of secondary halo bias adds a important element to the modelling of the halo-galaxy connection (e.g. Hearin & Watson 2013;Hearin et al 2014Hearin et al , 2016Zentner et al 2019;Wechsler & Tinker 2018;Contreras et al 2020;Xu et al 2020).…”

Section: Introductionmentioning

confidence: 99%

The galaxy size–halo mass scaling relations and clustering properties of central and satellite galaxies

Rodríguez

Montero-Dorta

Angulo

et al. 2021

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

In this work, we combine size and stellar mass measurements from the Sloan Digital Sky Server (SDSS) with the group finder algorithm of Rodriguez & Merchán in order to determine the stellar and halo mass – size relations of central and satellite galaxies separately. We show that, while central and satellite galaxies display similar stellar mass – size relations, their halo mass – size relations differ significantly. As expected, more massive haloes tend to host larger central galaxies. However, the size of satellite galaxies depends only slightly on halo virial mass. We show that these results are compatible with a remarkably simple model in which the size of central and satellite galaxies scales as the cubic root of their host halo mass, with the normalization for satellites being ∼ 30 per cent smaller than that for central galaxies, which can be attributed to tidal stripping. We further check that our measurements are in excellent agreement with predictions from the IllustrisTNG hydrodynamical simulation. In the second part of this paper, we analyse how the clustering properties of central and satellite galaxies depend on their size. We demonstrate that, independently of the stellar mass threshold adopted, smaller galaxies are more tightly clustered than larger galaxies when either the entire sample or only satellites are considered. The opposite trend is observed on large scales when the size split is performed for the central galaxies alone. Our results place significant constraints for halo–galaxy connection models that link galaxy size with the properties of their hosting haloes.

show abstract

“…Despite several detection claims, galaxy assembly bias is still generally regarded as an unconfirmed hypothesis (see, e.g., Miyatake et al 2016;Lin et al 2016;Sunayama et al 2016;Zu et al 2017;Montero-Dorta et al 2017;Niemiec et al 2018;Zentner et al 2019;Walsh & Tinker 2019;Sunayama & More 2019;Obuljen et al 2019;Montero-Dorta et al 2020a;Obuljen et al 2020;Salcedo et al 2020 for more information). In the context of hydrodynamical simulations, Montero-Dorta et al (2020b) showed that the halo assembly bias signal is present in IllustrisTNG and propagates to the central galaxy population when this is split by properties such as colour or SFR.…”

Section: Introductionmentioning

confidence: 99%

On the influence of halo mass accretion history on galaxy properties and assembly bias

Montero-Dorta,

Chaves-Montero,

Artale

et al. 2021

Preprint

View full text Add to dashboard Cite

Halo assembly bias is the secondary dependence of the clustering of dark-matter haloes on their assembly histories at fixed halo mass. This established dependence is expected to manifest itself on the clustering of the galaxy population, a potential effect commonly known as galaxy assembly bias. Using the IllustrisTNG300 magnetohydrodynamical simulation, we analyse the dependence of the properties and clustering of galaxies on the shape of the specific mass accretion history of their hosting haloes (sMAH). We first show that several halo and galaxy properties strongly correlate with the slope of the sMAH (𝛽) at fixed halo mass. Namely, haloes with increasingly steeper 𝛽 increment their halo masses faster at early times, and their hosted galaxies present larger stellar-to-halo mass ratios, lose their gas faster, reach the peak of their star formation histories at higher redshift, and become quenched earlier. We also demonstrate that 𝛽 is more directly connected to these key galaxy formation properties than other broadly employed halo proxies, such as formation time. Finally, we measure the secondary dependence of galaxy clustering on 𝛽 at fixed halo mass as a function of redshift. By tracing back the evolution of individual haloes, we show that the amplitude of the galaxy assembly bias signal for the progenitors of 𝑧 = 0 galaxies increases with redshift, reaching a factor of 2 at 𝑧 = 1 for haloes of 𝑀 halo = 10 11.5 − 10 12 ℎ −1 M . The measurement of the evolution of assembly bias along the merger tree provides a new theoretical perspective to the study of secondary bias. Our findings, which show a tight relationship between halo accretion and both the clustering and some of the main observational properties of the galaxy population, have also important implications for the generation of mock catalogues for upcoming cosmological surveys.

show abstract

Probing Galaxy assembly bias in BOSS galaxies using void probabilities

Cited by 39 publications

References 70 publications

The assembly bias of emission-line galaxies

The assembly bias of emission-line galaxies

The galaxy size–halo mass scaling relations and clustering properties of central and satellite galaxies

On the influence of halo mass accretion history on galaxy properties and assembly bias

Contact Info

Product

Resources

About