The assembly bias of emission-line galaxies

Jiménez, Esteban; Padilla, Nelson; Contreras, Sergio; Zehavi, Idit; Baugh, C. M.; Orsi, Álvaro

doi:10.1093/mnras/stab1819

Cited by 9 publications

(3 citation statements)

References 92 publications

(118 reference statements)

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“…at the level of 𝑏 1 etc.) as reported in Jiménez et al (2021) for instance. This being said, one should remain cautious and avoid taking these results as definitive until a thorough study based on different galaxy formation models (we vary some of the GALACTI-CUS parameters in section §3.3) and merger trees probing a wider range of halo mass and redshift is carried out.…”

Section: Galaxies Selected By H𝛼 Luminositysupporting

confidence: 59%

Non-Gaussian assembly bias from a semi-analytic galaxy formation model

Marinucci¹,

Desjacques²,

Benson³

2023

Preprint

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We use 𝑧 = 1 mock galaxy catalogues produced with the semi-analytic code GALACTICUS to study the dependence of the non-Gaussian bias parameter 𝑏 𝜙 on the mass assembly history of the host halos. We generate large sets of merger trees and measure the non-Gaussian assembly bias Δ𝑏 𝜙 for galaxies selected by color magnitude and emission line luminosities. For galaxies selected by 𝑔 − 𝑟 color, we find a large assembly bias consistent with the analysis of Barreira et al. (2020) based on hydro-dynamical simulations of galaxy formation. This effect arises from the fact that a larger value of the normalization amplitude 𝜎 8 implies a faster mass assembly (at fixed halo mass) and, therefore, older and redder galaxies. On the contrary, for galaxies selected by their H𝛼 luminosity, we do not detect a significant assembly bias, at least at 𝑧 = 1 and in the halo mass range 3 × 10 10 < 𝑀 < 10 12 𝑀 considered here. This is presumably due to the fact that emission line strengths are mainly sensitive to the instantaneous star formation rate, which appears to depend weakly on 𝜎 8 at 𝑧 = 1. This indicates that the non-Gaussian assembly bias should be less of a concern for future emission line galaxy surveys.We also investigate, for the first time, the sensitivity of the non-Gaussian assembly bias to a change in the parameters of the galaxy formation model that control the AGN and stellar feedback as well as the star formation rate. When these parameters change within a factor of two from their fiducial value, they induce variations up to order unity in the measured Δ𝑏 𝜙 , but the overall trends with color or luminosity remain the same. However, since these results may be sensitive to the choice of galaxy formation model, it will be prudent to extend this analysis to other semi-analytic models in addition to halo mass and redshift.

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Section: Galaxies Selected By H𝛼 Luminositysupporting

confidence: 59%

Non-Gaussian assembly bias from a semi-analytic galaxy formation model

Marinucci¹,

Desjacques²,

Benson³

2023

Preprint

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“…Some works have studied this using hydrodynamical simulations, and have reported a detection of assembly bias in the simulated galaxy density field as well [45][46][47]. These results have led to several recent efforts to incorporate it in semi-analytical models such as (decorated) HOD and abundance matching techniques 1 [35,45,[48][49][50][51][52][53][54][55][56][57][58]. On the observational front, however, the detection of assembly bias in observational data remains more debated: despite a number of studies claiming a detection (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…On the observational front, however, the detection of assembly bias in observational data remains more debated: despite a number of studies claiming a detection (e.g. [48,55,[59][60][61][62][63][64][65][66]), reanalyses and other independent investigations using similar galaxy samples have returned no clear evidence of assembly bias in observations (e.g. [67][68][69][70][71][72][73][74][75]).…”

Section: Introductionmentioning

confidence: 99%

Assembly bias in quadratic bias parameters of dark matter halos from forward modeling

Lazeyras

2021

J. Cosmol. Astropart. Phys.

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We use the forward modeling approach to galaxy clustering combined with the likelihood from the effective-field theory of large-scale structure to measure assembly bias, i.e. the dependence of halo bias on properties beyond the total mass, in the linear (b1) and second order bias parameters (b2 and bK 2) of dark matter halos in N-body simulations. This is the first time that assembly bias in the tidal bias parameter bK 2 is measured. We focus on three standard halo properties: the concentration c, spin λ, and sphericity s, for which we find an assembly bias signal in bK 2 that is opposite to that in b1. Specifically, at fixed mass, halos that get more (less) positively biased in b1, get less (more) negatively biased in bK 2. We also investigate the impact of assembly bias on the b2(b1) and bK 2(b1) relations, and find that while the b2(b1) relation stays roughly unchanged, assembly bias strongly impacts the bK 2(b1) relation. This impact likely extends also to the corresponding relation for galaxies, which motivates future studies to design better priors on bK 2(b1) for use in cosmological constraints from galaxy clustering data.

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The MillenniumTNG Project: the large-scale clustering of galaxies

Bose

Hadzhiyska

Barrera

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Modern redshift surveys are tasked with mapping out the galaxy distribution over enormous distance scales. Existing hydrodynamical simulations, however, do not reach the volumes needed to match upcoming surveys. We present results for the clustering of galaxies using a new, large volume hydrodynamical simulation as part of the MillenniumTNG (MTNG) project. With a computational volume that is ≈15 times larger than the next largest such simulation currently available, we show that MTNG is able to accurately reproduce the observed clustering of galaxies as a function of stellar mass. When separated by colour, there are some discrepancies with respect to the observed population, which can be attributed to the quenching of satellite galaxies in our model. We combine MTNG galaxies with those generated using a semi-analytic model to emulate the sample selection of luminous red galaxies (LRGs) and emission-line galaxies (ELGs) and show that, although the bias of these populations is approximately (but not exactly) constant on scales larger than ≈10 Mpc, there is significant scale-dependent bias on smaller scales. The amplitude of this effect varies between the two galaxy types and between the semi-analytic model and MTNG. We show that this is related to the distribution of haloes hosting LRGs and ELGs. Using mock SDSS-like catalogues generated on MTNG lightcones, we demonstrate the existence of prominent baryonic acoustic features in the large-scale galaxy clustering. We also demonstrate the presence of realistic redshift space distortions in our mocks, finding excellent agreement with the multipoles of the redshift-space clustering measured in SDSS data.

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The assembly bias of emission-line galaxies

Cited by 9 publications

References 92 publications

Non-Gaussian assembly bias from a semi-analytic galaxy formation model

Non-Gaussian assembly bias from a semi-analytic galaxy formation model

Assembly bias in quadratic bias parameters of dark matter halos from forward modeling

The MillenniumTNG Project: the large-scale clustering of galaxies

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