PINOCCHIO and the hierarchical build-up of dark matter haloes

Taffoni, Giuliano; Monaco, Pierluigi; Theuns, Tom

doi:10.1046/j.1365-8711.2002.05441.x

Cited by 48 publications

(61 citation statements)

References 53 publications

(98 reference statements)

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“…(16) should give the fraction of all mass in virialized objects; however, erfc(0) = 1 so that Eq. (16) states that only half of the mass density of the universe is contained in virialized objects. Press & Schechter noted this as a problem associated with not counting underdense regions in the integral Eq.…”

Section: The Press-schechter Mass Functionmentioning

confidence: 99%

“…This is the publicly-available PINOCCHIO code developed by P. Monaco and collaborators [14,15,16] , [85]. (A similar tool that can be used to generate mock catalogs of halos rapidly is PTHalos developed by Scoccimarro and Sheth [83,84]) The great value of the PINOCCHIO code is that it is considerably less computationally expensive than a cosmological N-body simulation but predicts halo properties and formation histories that are in better agreement with N-body results relative to the simple excursion set approach (for a recent example see Ref.…”

Section: E the Pinocchio Algorithmmentioning

confidence: 99%

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The Excursion Set Theory of Halo Mass Functions, Halo Clustering, and Halo Growth

Zentner

2007

Int. J. Mod. Phys. D

239

261

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I review the excursion set theory with particular attention toward applications to cold dark matter halo formation and growth, halo abundance, and halo clustering.After a brief introduction to notation and conventions, I begin by recounting the heuristic argument leading to the mass function of bound objects given by Press & Schechter. I then review the more formal derivation of the Press-Schechter halo mass function that makes use of excursion sets of the density field. The excursion set formalism is powerful and can be applied to numerous other problems. I review the excursion set formalism for describing both halo clustering and bias and the properties of void regions. As one of the most enduring legacies of the excursion set approach and one of its most common applications, I spend considerable time reviewing the excursion set theory of halo growth. This section of the review culminates with the description of two Monte Carlo methods for generating ensembles of halo mass accretion histories. In the last section, I emphasize that the standard excursion set approach is the result of several simplifying assumptions. Dropping these assumptions can lead to more faithful predictions and open excursion set theory to new applications. One such assumption is that the height of the barriers that define collapsed objects is a constant function of scale. I illustrate the implementation of the excursion set approach for barriers of arbitrary shape. One such application is the now well-known improvement of the excursion set mass function derived from * National Science Foundation Fellow 2 the "moving" barrier for ellipsoidal collapse. I also emphasize that the statement that halo accretion histories are independent of halo environment in the excursion set approach is not a general prediction of the theory. It is a simplifying assumption.I review the method for constructing correlated random walks of the density field in the more general case. I construct a simple toy model to illustrate that excursion set theory (with a constant barrier height) makes a simple and general prediction for the relation between halo accretion histories and the large-scale environments of halos:regions of high density preferentially contain late-forming halos and conversely for regions of low density. I conclude with a brief discussion of the importance of this prediction relative to recent numerical studies of the environmental dependence of halo properties.

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Section: The Press-schechter Mass Functionmentioning

confidence: 99%

Section: E the Pinocchio Algorithmmentioning

confidence: 99%

The Excursion Set Theory of Halo Mass Functions, Halo Clustering, and Halo Growth

Zentner

2007

Int. J. Mod. Phys. D

239

261

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“…Coles & Jones (1991) and Cole et al (2005) used the log-normal model to generate mock catalogues; Chuang et al (2015) used an approach based on the Zel'dovich approximation to create mock catalogues that can accurately reproduce the one-point, two-point, and three-point statistics; Scoccimarro & Sheth (2002) and Manera et al (2013) used the 2LPT formalism to create matter density fields from which halo catalogues were extracted (PTHalos). de la Torre & Peacock (2013) instead used a method based on the sampling of the mass function to create halos under the limit resolution of the halos; Tassev et al (2013Tassev et al ( , 2015 used a method based on Lagrangian Perturbation Theory (LPT) and similar methods were used by (Monaco et al 2002a,b;Taffoni et al 2002;Monaco et al 2013). A compilation of some of the fast methods for generating mock catalogues can be found in Chuang et al (2014).…”

Section: Introductionmentioning

confidence: 99%

The importance of the cosmic web and halo substructure for power spectra

Pace

Manera

Bacon

et al. 2015

Mon. Not. R. Astron. Soc.

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In this work we study the relevance of the cosmic web and substructures on the matter and lensing power spectra measured from halo mock catalogues extracted from the N-body simulations. Since N-body simulations are computationally expensive, it is common to use faster methods that approximate the dark matter field as a set of halos. In this approximation, we replace mass concentrations in N-body simulations by a spherically symmetric Navarro-FrenkWhite halo density profile. We also consider the full mass field as the sum of two distinct fields: dark matter halos (M > 9 × 10 12 M ⊙ /h) and particles not included into halos. Mock halos reproduce well the matter power spectrum, but underestimate the lensing power spectrum on large and small scales. For sources at z s = 1 the lensing power spectrum is underestimated by up to 40% at ℓ ≈ 10 4 with respect to the simulated halos. The large scale effect can be alleviated by combining the mock catalogue with the dark matter distribution outside the halos. In addition, to evaluate the contribution of substructures we have smeared out the intra-halo substructures in a N-body simulation while keeping the halo density profiles unchanged. For the matter power spectrum the effect of this smoothing is only of the order of 5%, but for lensing substructures are much more important: for ℓ ≈ 10 4 the internal structures contribute 30% of the total spectrum. These findings have important implications in the way mock catalogues have to be created, suggesting that some approximate methods currently used for galaxy surveys will be inadequate for future weak lensing surveys.

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“…3 N-body simulations, the 100 Mpc/h run used by Monaco et al (2002b) and Taffoni et al (2002), and the 250 Mpc/h presented by Fontanot et al (2003). In both cases we run  with a single grid, and on the same initial conditions as the simulations.…”

Section: Appendix B: Pinocchio Accuracy In Recovering Peculiar Velocimentioning

confidence: 99%

“…In Sect. 2 we decompose the velocity field of DM halos into streaming, gradient and random components, and show how to estimate such velocity components on DM halo catalogues generated with the  code (Monaco et al 2002). In Sect.…”

Section: Introductionmentioning

confidence: 99%

Tracing large-scale structure at high redshift with Lyman-α emitters: the effect of peculiar velocities

Monaco¹,

Møller

Fynbo

et al. 2005

A&A

Self Cite

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Abstract.We investigate the effect of peculiar velocities on the redshift space distribution of z > ∼ 2 galaxies, and we focus in particular on Lyα emitters. We generate catalogues of dark matter (DM) halos and identify emitters with halos of the same co-moving space density (M(Lyα emitters) ≈ 3 × 10 11 M ). We decompose the peculiar velocity field of halos into streaming, gradient and random components, and compute and analyse these as a function of scale. Streaming velocities are determined by fluctuations on very large scales, strongly affected by sample variance, but have a modest impact on the interpretation of observations. Gradient velocities are the most important as they distort structures in redshift space, changing the thickness and orientation of sheets and filaments. Random velocities are typically below or of the same order as the typical observational uncertainty on the redshift. We discuss the importance of these effects for the interpretation of data on the large-scale structure as traced by Lyα emitters (or similar kinds of astrophysical high-redshift objects), focusing on the induced errors in the viewing angles of filaments. We compare our predictions of velocity patterns for Lyα emitters to observations and find that redshift clumping of Lyα emitters, as reported for instance in the fields of high-redshift radio galaxies, does not allow to infer whether an observed field is sampling an early galaxy overdensity.

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PINOCCHIO and the hierarchical build-up of dark matter haloes

Cited by 48 publications

References 53 publications

The Excursion Set Theory of Halo Mass Functions, Halo Clustering, and Halo Growth

The Excursion Set Theory of Halo Mass Functions, Halo Clustering, and Halo Growth

The importance of the cosmic web and halo substructure for power spectra

Tracing large-scale structure at high redshift with Lyman-α emitters: the effect of peculiar velocities

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