The large-scale environment from cosmological simulations – I. The baryonic cosmic web

Cui, Weiguang; Knebe, Alexander; Yepes, Gustavo; Yang, Xiaohu; Borgani, S.; Kang, Xi; Power, Chris; Staveley‐Smith, L.

doi:10.1093/mnras/stx2323

Cited by 42 publications

(45 citation statements)

References 80 publications

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“…The large-scale environmentof the whole simulation box has been classified into knots, filaments, sheets, and voids using two algorithms: VWEB, which uses a velocity-shear-tensor, and PWEB , which uses a tidal-tensor (Cui et al (2018(Cui et al ( , 2019. These algorithms are described in Section 2.2, and their resolution and threshold setting are further discussed in Appendix Section B.…”

Section: E T H O D Smentioning

confidence: 99%

“…Here, we apply two algorithms, VWEB and PWEB , to classify the largescale environmentof the whole simulation box into knots, filaments, sheets, and voids (Cui et al 2018(Cui et al , 2019.…”

Section: The Cosmic Webmentioning

confidence: 99%

“…Many methods have been developed to classify/identify these cosmological structures, and we refer the reader to Libeskind et al (2018) for a detailed description. Here, we measure the large-scale environment of the dark matter simulation using two algorithms, one that uses a shear tensor, VWEB , and the other a tidal one, PWEB (Cui et al 2018(Cui et al , 2019. Both methods use the eigenvalues of the Hessian matrix for the indicator field (velocity and potential, respectively) to spatially separate out these structures.…”

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confidence: 99%

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Do model emission line galaxies live in filaments at z ∼ 1?

González-Pérez

Cui

Contreras

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Current and future cosmological surveys are targeting star-forming galaxies at z∼ 1 with nebular emission lines. We use a state-of-the-art semi-analytical model of galaxy formation and evolution to explore the large scale environment of star-forming emission line galaxies (ELGs). Model ELGs are selected such that they can be compared directly with the DEEP2, VVDS, eBOSS-SGC and DESI surveys. The large scale environment of the ELGs is classified using velocity-shear-tensor and tidal-tensor algorithms. Half of the model ELGs live in filaments and about a third in sheets. Model ELGs which reside in knots have the largest satellite fractions. We find that the shape of the mean halo occupation distribution of model ELGs varies widely for different large scale environments. To interpret our results, we also study fixed number density samples of ELGs and galaxies selected using simpler criteria, with single cuts in stellar mass, star formation rate and $\left[\rm O\, {\, \small II}\right]$ luminosity. The fixed number density ELG selection produces samples that are close to L$\left[\rm O\, {\, \small II}\right]$ and SFR selected samples for densities above 10−4.2h3Mpc−3. ELGs with an extra cut in stellar mass applied to fix their number density, present differences in sheets and knots with respect to the other samples. ELGs, SFR and L$\left[\rm O\, {\, \small II}\right]$ selected samples with equal number density have similar large scale bias but their clustering below separations of 1h−1Mpc is different.

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Section: E T H O D Smentioning

confidence: 99%

“…Here, we apply two algorithms, VWEB and PWEB , to classify the largescale environmentof the whole simulation box into knots, filaments, sheets, and voids (Cui et al 2018(Cui et al , 2019.…”

Section: The Cosmic Webmentioning

confidence: 99%

mentioning

confidence: 99%

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Do model emission line galaxies live in filaments at z ∼ 1?

González-Pérez

Cui

Contreras

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Over the last two decades, the analysis of cosmological hydrodynamical simulations has shown that a large fraction of these "missing baryons" 1 may reside in a shockheated phase of the IGM with gas densities ρ 50ρcritΩ b and temperatures 10 5 K < T < 10 7 K (Cen & Ostriker 1999;Davé et al 1999;Cen et al 2001;Davé et al 2001;Kang et al 2005;Cen & Ostriker 2006;Davé & Oppenheimer 2007); such a phase is usually denominated Warm-Hot Intergalactic Medium (WHIM). Based on these results from simulations, a variety of methods to directly detect the missing baryons has been proposed in the literature, e.g., via future radio surveys (Araya-Melo et al 2012;Vazza et al 2016;Horii et al 2017;Cui et al 2018), UV spectroscopy (Oppenheimer & Davé 2009;Bertone et al 2010;Tepper-García et al 2011;Nelson et al 2018c) and X-ray spectroscopy (Phillips et al 2001;Yoshikawa et al 2003;Viel et al 2005;Branchini et al 2009;Takei et al 2011;Kaastra et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Baryons in the Cosmic Web of IllustrisTNG – I: gas in knots, filaments, sheets, and voids

Martizzi

Vogelsberger

Artale

et al. 2019

Monthly Notices of the Royal Astronomical Society

172

167

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We analyze the IllustrisTNG simulations to study the mass, volume fraction and phase distribution of gaseous baryons embedded in the knots, filaments, sheets and voids of the Cosmic Web from redshift z = 8 to redshift z = 0. We find that filaments host more starforming gas than knots, and that filaments also have a higher relative mass fraction of gas in this phase than knots. We also show that the cool, diffuse Intergalactic Medium (IGM; T < 10 5 K, n H < 10 −4 (1 + z) cm −3 ) and the Warm-Hot Intergalactic Medium (WHIM; 10 5 K < T < 10 7 K, n H < 10 −4 (1 + z) cm −3 ) constitute ∼ 39% and ∼ 46% of the baryons at redshift z = 0, respectively. Our results indicate that the WHIM may constitute the largest reservoir of missing baryons at redshift z = 0. Using our Cosmic Web classification, we predict the WHIM to be the dominant baryon mass contribution in filaments and knots at redshift z = 0, but not in sheets and voids where the cool, diffuse IGM dominates. We also characterise the evolution of WHIM and IGM from redshift z = 4 to redshift z = 0, and find that the mass fraction of WHIM in filaments and knots evolves only by a factor ∼ 2 from redshift z = 0 to z = 1, but declines faster at higher redshift. The WHIM only occupies 4 − 11% of the volume at redshift 0 z 1. We predict the existence of a significant number of currently undetected OVII and NeIX absorption systems in cosmic filaments which could be detected by future X-ray telescopes like Athena.

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“…where λ th is a free threshold parameter Libeskind et al 2012Libeskind et al , 2013. Following the discussion of Carlesi et al (2014); Cui et al (2018Cui et al ( , 2019, we set λ th = 0.1, which presents better agreement to the visualised density field. Our mock galaxies are then placed onto the same grid checking for the web classification of the cell they lie in.…”

Section: A the Vweb Methodsmentioning

confidence: 99%

A semi-analytical perspective on massive galaxies at z ∼ 0.55

Stoppacher

Prada

Montero-Dorta

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The most massive and luminous galaxies in the Universe serve as powerful probes to study the formation of structure, the assembly of mass, and cosmology. However, their detailed formation and evolution is still barely understood. Here we extract a sample of massive mock galaxies from the semi-analytical model of galaxy formation (SAM) Galacticus from the MultiDark-Galaxies, by replicating the CMASS photometric selection from the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS). The comparison of the Galacticus CMASSmock with BOSS-CMASS data allows us to explore different aspects of the massive galaxy population at 0.5 < z < 0.6, including the galaxy-halo connection and the galaxy clustering. We find good agreement between our modelled galaxies and observations regarding the galaxyhalo connection, but our CMASS-mock over-estimates the clustering amplitude of the 2-point correlation function, due to a smaller number density compared to BOSS, a lack of blue objects, and a small intrinsic scatter in stellar mass at fixed halo mass of < 0.1 dex. To alleviate this problem, we construct an alternative mock catalogue mimicking the CMASS colour-magnitude distribution by randomly down-sampling the SAM catalogue. This CMASS-mock reproduces the clustering of CMASS galaxies within 1σ and shows some environmental dependency of star formation properties that could be connected to the quenching of star formation and the assembly bias.

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The large-scale environment from cosmological simulations – I. The baryonic cosmic web

Cited by 42 publications

References 80 publications

Do model emission line galaxies live in filaments at z ∼ 1?

Do model emission line galaxies live in filaments at z ∼ 1?

Baryons in the Cosmic Web of IllustrisTNG – I: gas in knots, filaments, sheets, and voids

A semi-analytical perspective on massive galaxies at z ∼ 0.55

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