Accurate mass and velocity functions of dark matter haloes

Comparat, Johan; Prada, Francisco; Yepes, Gustavo; Klypin, Anatoly

doi:10.1093/mnras/stx1183

Cited by 50 publications

(63 citation statements)

References 72 publications

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“…N-body simulations provide information on the evolution and spatial distribution of dark-matter halos within cosmological volumes. The abundance-matching (Klypin et al 2016;Comparat et al 2017) at a snapshot redshift z = 0.75. It shows the positions of particles (e.g.…”

Section: Methodsmentioning

confidence: 99%

“…The MultiDark-Planck 2 (MDPL2) simulations have a bigger box size, 1000 h −1 Mpc on the side, and a mass resolution of 1.51 × 10 9 h −1 M . Details on the SMDPL and MDPL2 simulations can be found in Klypin et al (2016) and Comparat et al (2017). The Rockstar halo finder (Behroozi et al 2013a) has been applied to the SMDPL and MDPL2 simulations to identify halos and flag those (sub-halos) that lie within the virial radius of a more massive host-halo.…”

Section: N-body Simulationsmentioning

confidence: 99%

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Exploring the halo occupation of AGN using dark-matter cosmological simulations

Georgakakis

Comparat

Merloni

et al. 2018

Monthly Notices of the Royal Astronomical Society

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A semi-empirical model is presented that describes the distribution of Active Galactic Nuclei (AGN) on the cosmic web. It populates dark-matter halos in N-body simulations (MultiDark) with galaxy stellar masses using empirical relations based on abundance matching techniques, and then paints accretion events on these galaxies using stateof-the-art measurements of the AGN occupation of galaxies. The explicit assumption is that the large-scale distribution of AGN is independent of the physics of blackhole fueling. The model is shown to be consistent with current measurements of the two-point correlation function of AGN samples. It is then used to make inferences on the halo occupation of the AGN population. Mock AGN are found in halos with a broad distribution of masses with a mode of ≈ 10 12 h −1 M and a tail extending to cluster-size halos. The clustering properties of the model AGN depend only weakly on accretion luminosity and redshift. The fraction of satellite AGN in the model increases steeply toward more massive halos, in contrast with some recent observational results. This discrepancy, if confirmed, could point to a dependence of the halo occupation of AGN on the physics of black-hole fueling.

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Section: Methodsmentioning

confidence: 99%

Section: N-body Simulationsmentioning

confidence: 99%

Exploring the halo occupation of AGN using dark-matter cosmological simulations

Georgakakis

Comparat

Merloni

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…(51) is clearly the same integral without Q, and the 1σ variance is computed as σ Q = Q 2 − Q 2 . To compute the formation rate one needs the halo mass function, i.e., the co-moving number density of halo per halo mass bin, as provided by state-of-the-art N-body simulations; we adopt the determination by Tinker et al (2008; see also Watson et al 2013;Bocquet et al 2016;Comparat et al 2017Comparat et al , 2019. Since we are mainly concerned with the properties of ETGs residing at the center of halos, we actually exploit the galaxy halo mass function, i.e., the mass function of halos hosting one individual galaxy (though the difference with respect to the halo mass function emerge only for z 1 and M H several 10 13 M ).…”

Section: Average Over Formation Redshiftmentioning

confidence: 99%

New Analytic Solutions for Galaxy Evolution: Gas, Stars, Metals, and Dust in Local ETGs and Their High-z Star-forming Progenitors

Pantoni

Lapi

Massardi

et al. 2019

ApJ

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We present a set of new analytic solutions aimed at self-consistently describing the spatially-averaged time evolution of the gas, stellar, metal, and dust content in an individual starforming galaxy hosted within a dark halo of given mass and formation redshift. Then, as an application, we show that our solutions, when coupled to specific prescriptions for parameter setting (inspired by in-situ galaxy-black hole coevolution scenarios) and merger rates (based on numerical simulations), can be exploited to reproduce the main statistical relationships followed by early-type galaxies and by their high-redshift starforming progenitors. Our analytic solutions allow to easily disentangle the diverse role of the main physical processes regulating galaxy formation, to quickly explore the related parameter space, and to make transparent predictions on spatially-averaged quantities. As such, our analytic solutions may provide a basis for improving the (subgrid) physical recipes presently implemented in theoretical approaches and numerical simulations, and can offer a benchmark for interpreting and forecasting current and future broadband observations of high-redshift starforming galaxies.2 PANTONI ET AL. evolution of the gas, stellar, metal, and dust content in an individual starforming galaxy hosted within a dark halo of given mass and formation redshift. Our basic framework pictures a galaxy as an open, one-zone system comprising three interlinked mass components: a reservoir of warm gas subject to cooling and condensation toward the central regions; cold gas fed by infall and depleted by star formation and stellar feedback (type-II supernovae [SNe] and stellar winds); stellar mass, partially restituted to the cold phase by stars during their evolution. Remarkably, the corresponding analytic solutions for the metal enrichment history of the cold gas and stellar mass are self-consistently derived using as input the solutions for the evolution of the mass components; the metal equations includes effects of feedback, astration, instantaneous production during star formation, and delayed production by type-Ia SNe, possibly following a specified delay time distribution. Finally, the dust mass evolution takes into account the formation of grain cores associated to star formation, and of the grain mantles due to accretion onto pre-existing cores; astration of dust by star formation and stellar feedback, and spallation by SN shockwaves are also included.We then apply our analytic solutions to describe the formation of spheroids/early-type galaxies (ETGs) and the evolution of their starforming progenitors. To this purpose, we couple our solutions to two additional ingredients: (i) specific prescriptions for parameter setting, inspired by in-situ galaxy-black hole coevolution scenarios of ETG formation; (ii) estimates of the halo and stellar mass growth by mergers, computed on the basis of the merger rates from state-of-the-art numerical simulations. We then derive and confront with available data a bunch of fundamental spatially-...

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“…The set of eROSITA mocks is made public here 1 2 N-BODY DATA We use the halo catalogues of the MDPL2 simulation 2 (Planck cosmology, 3840 3 particles of mass 2.2 × 10 9 M , 1475.5 Mpc on the side, Klypin et al 2016) post-processed with the rockstar merger trees software (Behroozi et al 2013). The halo mass function is correct to a few percent down to halo masses of M vir ∼ 10 11 M (Comparat et al 2017). In this analysis, we consider distinct haloes more massive than 2 × 10 11 M .…”

Section: Introductionmentioning

confidence: 99%

Active galactic nuclei and their large-scale structure: an eROSITA mock catalogue

Comparat

Merloni

Salvato

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In the context of the upcoming SRG/eROSITA survey, we present an N-body simulation-based mock catalogue for X-ray selected AGN samples. The model reproduces the observed hard X-ray AGN luminosity function (XLF) and the soft X-ray logN-logS from redshift 0 to 6. The XLF is reproduced to within ±5% and the logN-logS to within ±20%. We develop a joint X-ray -optical extinction and classification model. We adopt a set of empirical spectral energy distributions to predict observed magnitudes in the UV, optical and NIR. With the latest eROSITA all sky survey sensitivity model, we create a high-fidelity full-sky mock catalogue of X-ray AGN. It predicts their distributions in right ascension, declination, redshift and fluxes. Using empirical medium resolution optical spectral templates and an exposure time calculator, we find that 1.1×10 6 (4×10 5 ) fiber-hours are needed to follow-up spectroscopically from the ground the detected X-ray AGN with an optical magnitude 21 < r < 22.8 (22.8 < r < 25) with a 4-m (8-m) class multi-object spectroscopic facility. We find that future clustering studies will measure the AGN bias to the percent level at redshift z < 1.2 and should discriminate possible scenarios of galaxy-AGN co-evolution. We predict the accuracy to which the baryon acoustic oscillation standard ruler will be measured using X-ray AGN: better than 3% for AGN between redshift 0.5 to 3 and better than 1% using the Lyα forest of X-ray QSOs discovered between redshift 2 and 3. eROSITA will provide an outstanding set of targets for future galaxy evolution and cosmological studies.

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Accurate mass and velocity functions of dark matter haloes

Cited by 50 publications

References 72 publications

Exploring the halo occupation of AGN using dark-matter cosmological simulations

Exploring the halo occupation of AGN using dark-matter cosmological simulations

New Analytic Solutions for Galaxy Evolution: Gas, Stars, Metals, and Dust in Local ETGs and Their High-z Star-forming Progenitors

Active galactic nuclei and their large-scale structure: an eROSITA mock catalogue

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