The DESI One-Percent survey: exploring the Halo Occupation Distribution of Emission Line Galaxies with AbacusSummit simulations

Rocher, Antoine; Ruhlmann-Kleider, Vanina; Burtin, Etienne; Yuan, Sihan; de Mattia, Arnaud; Ross, Ashley J.; Aguilar, Jessica; Ahlen, Steven; Alam, Shadab; Bianchi, Davide; Brooks, David; Cole, Shaun; Dawson, Kyle; de la Macorra, Axel; Doel, Peter; Eisenstein, Daniel J.; Fanning, Kevin; Forero-Romero, Jaime E.; Garrison, Lehman H.; Gontcho A Gontcho, Satya; Gonzalez-Perez, Violeta; Guy, Julien; Hadzhiyska, Boryana; Hahn, ChangHoon; Honscheid, Klaus; Kisner, Theodore; Landriau, Martin; Lasker, James; E. Levi, Michael; Manera, Marc; Meisner, Aaron; Miquel, Ramon; Moustakas, John; Mueller, Eva-Maria; Newman, Jeffrey A.; Nie, Jundan; Percival, Will J.; Poppett, Claire; Qin, Fei; Rossi, Graziano; Samushia, Lado; Sanchez, Eusebio; Schlegel, David; Schubnell, Michael; Seo, Hee-Jong; Tarlé, Gregory; Vargas-Magaña, Mariana; Weaver, Benjamin A.; Yu, Jiaxi; Zhang, Hanyu; Zheng, Zheng; Zhou, Zhimin; Zou, Hu

doi:10.1088/1475-7516/2023/10/016

Cited by 8 publications

(8 citation statements)

References 59 publications

(100 reference statements)

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“…In this paper, we apply a halo mass cut M = 11.7 to the DARK SAGE catalog to remove the halos that are below the simulation resolution. The halo mass range of DARK SAGE can cover the halo mass range of DESI M ä [12, 14.5] (Wang et al 2022;Rocher et al 2023;Yuan et al 2023). In addition, as discussed in Section 2 of Q22, the halo mass range of DARK SAGE can also cover WALLABY.…”

Section: The Dark Sage Simulationmentioning

confidence: 99%

The Galaxy Number Density Profile of Halos

Qin,

Parkinson,

Stevens

et al. 2023

ApJ

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More precise measurements of galaxy clustering will be provided by the next generation of galaxy surveys, such as DESI, WALLABY, and the Square Kilometre Array. To utilize this information to improve our understanding of the Universe, we need to accurately model the distribution of galaxies in their host dark matter halos. In this work, we present a new galaxy number density profile of halos, which makes predictions for the positions of galaxies in the host halo, different to the widely adopted Navarro–Frenk–White (NFW) profile, since galaxies tend to be found more in the outskirts of halos (nearer the virial radius) than an NFW profile. The parameterized galaxy number density profile model of halos is fit and tested using the Dark Sage semi-analytic model of galaxy formation. We find that our galaxy number density profile model of halos can accurately reproduce the halo occupation distribution and galaxy two-point correlation function of the Dark Sage simulation. We also derive the analytic expressions for the circular velocity and gravitational potential energy for this profile model. We use the SDSS Data Release 10 galaxy group catalog to validate this galaxy number density profile model of halos. Compared to the NFW profile, we find that our model more accurately predicts the positions of galaxies in their host halo and the galaxy two-point correlation function.

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Section: The Dark Sage Simulationmentioning

confidence: 99%

The Galaxy Number Density Profile of Halos

Qin,

Parkinson,

Stevens

et al. 2023

ApJ

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“…Utilizing the highly complete ELG sample in the One-Percent Survey, a series of analyses have shown a strong clustering signal of ELGs within the scale of ∼0.5 Mpc h −1 (Gao et al 2023;Rocher et al 2023). In fact, the prominent clustering of ELGs has also been found in the surveys prior to DESI.…”

Section: Introductionmentioning

confidence: 99%

“…There are also several parallel studies focusing on the connection between galaxies and halos in the DESI One-Percent Survey (Prada et al 2023;Rocher et al 2023;Yu et al 2024;Yuan et al 2023aYuan et al , 2023b.…”

Section: Introductionmentioning

confidence: 99%

“…ELGs are mainly late-type galaxies with significant ongoing star-forming activity, and thus their galaxy-halo connection may differ from that of normal galaxies. Several studies on the halo occupation distribution (HOD; Geach et al 2012;Contreras et al 2013;Alam et al 2020;Avila et al 2020;Okumura et al 2021;Zhai et al 2021;Yuan et al 2022a;Rocher et al 2023), conditional stellar mass function (CSMF; Guo et al 2019), subhalo abundance matching (SHAM; Favole et al 2016Favole et al , 2017Gao et al 2022Gao et al , 2023Lin et al 2023;Prada et al 2023;Yu et al 2024), semi-analytical model (Gonzalez-Perez et al 2018, and hydrodynamical simulation (Hadzhiyska et al 2021(Hadzhiyska et al , 2023a(Hadzhiyska et al , 2023bYuan et al 2022b) suggest that ELGs tend to reside in host halos with masses ∼10 12 M e h −1 and the overall satellite fraction of ELGs is less than 20%. Due to various parameterized assumptions and target selections of ELGs in different surveys with specific color cuts and photometric depths, the ELG-halo connection models vary widely.…”

Section: Introductionmentioning

confidence: 99%

“…This strong clustering is therefore considered as evidence for the one-halo conformity effect of ELGs. Meanwhile, Rocher et al (2023) combined a conformity model with different HODs to recover the ELG auto correlations down to small scales of ∼0.04 Mpc h −1 . In this model, satellite ELGs can only exist in halos where the central galaxy is an ELG.…”

Section: Introductionmentioning

confidence: 99%

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The DESI One-Percent Survey: A Concise Model for the Galactic Conformity of Emission-line Galaxies

Gao,

Jing,

et al. 2024

ApJ

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Galactic conformity is the phenomenon whereby a galaxy of a certain physical property is correlated with its neighbors of the same property, implying a possible causal relationship. The observed auto correlations of emission-line galaxies (ELGs) from the highly complete DESI One-Percent Survey exhibit a strong clustering signal on small scales, providing clear evidence for the conformity effect of ELGs. Building upon the original subhalo abundance-matching (SHAM) method developed by Gao et al., we propose a concise conformity model to improve the ELG–halo connection. In this model, the number of satellite ELGs is boosted by a factor of ∼5 in the halos whose central galaxies are ELGs. We show that the mean ELG satellite number in such central halos is still smaller than 1 and that the model does not significantly increase the overall satellite fraction. With this model, we can well recover the ELG auto correlations to the smallest scales explored with the current data (i.e., r p > 0.03 Mpc h −1 in real space and at s > 0.3 Mpc h −1 in redshift space), while the cross correlations between luminous red galaxies and ELGs are nearly unchanged. Although our SHAM model has only eight parameters, we further verify that it can accurately describe the ELG clustering in the entire redshift range from z = 0.8 to 1.6. We therefore expect that this method can be used to generate high-quality ELG lightcone mocks for DESI.

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Fast forward modelling of galaxy spatial and statistical distributions

Berner,

Refregier,

Moser

et al. 2024

J. Cosmol. Astropart. Phys.

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A forward modelling approach provides simple, fast and realistic simulations of galaxy surveys, without a complex underlying model. For this purpose, galaxy clustering needs to be simulated accurately, both for the usage of clustering as its own probe and to control systematics. We present a forward model to simulate galaxy surveys, where we extend the Ultra-Fast Image Generator to include galaxy clustering. We use the distribution functions of the galaxy properties, derived from a forward model adjusted to observations. This population model jointly describes the luminosity functions, sizes, ellipticities, SEDs and apparent magnitudes. To simulate the positions of galaxies, we then use a two-parameter relation between galaxies and halos with Subhalo Abundance Matching (SHAM). We simulate the halos and subhalos using the fast PINOCCHIO code, and a method to extract the surviving subhalos from the merger history. Our simulations contain a red and a blue galaxy population, for which we build a SHAM model based on star formation quenching. For central galaxies, mass quenching is controlled with the parameter Mlimit, with blue galaxies residing in smaller halos. For satellite galaxies, environmental quenching is implemented with the parameter tquench, where blue galaxies occupy only recently merged subhalos. We build and test our model by comparing to imaging data from the Dark Energy Survey Year 1. To ensure completeness in our simulations, we consider the brightest galaxies with i < 20. We find statistical agreement between our simulations and the data for two-point correlation functions on medium to large scales. Our model provides constraints on the two SHAM parameters Mlimit and tquench and offers great prospects for the quick generation of galaxy mock catalogues, optimized to agree with observations.

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The DESI One-Percent survey: exploring the Halo Occupation Distribution of Emission Line Galaxies with AbacusSummit simulations

Cited by 8 publications

References 59 publications

The Galaxy Number Density Profile of Halos

The Galaxy Number Density Profile of Halos

The DESI One-Percent Survey: A Concise Model for the Galactic Conformity of Emission-line Galaxies

Fast forward modelling of galaxy spatial and statistical distributions

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