Halo mass definition and multiplicity function

Juan, Enric; Salvador-Solé, E.; Domènech, Guillem; Manrique, Alberto

doi:10.1093/mnras/stu187

Cited by 13 publications

(21 citation statements)

References 38 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…AMIGA follows this growth in a well-contrasted analytic manner with no free parameters (Salvador-Solé et al 1998, 2007Raig et al 2001). This allows us to accurately calculate, at any given moment, their abundance (Juan et al 2014a(Juan et al , 2014b and inner structure and kinematics (Salvador-Solé et al 2012a, which in turn sets the structure and temperature of their hot gas (Solanes et al 2005). The amount and metallicity of such a hot gas and the properties of the central galaxy and its satellites are monitored in AMIGA from the individual halo aggregation history.…”

Section: Luminous Sourcesmentioning

confidence: 99%

CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

Salvador-Solé

Manrique

Guzmán

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

We combine observational data on a dozen independent cosmic properties at high-z with the information on reionization drawn from the spectra of distant luminous sources and the cosmic microwave background (CMB) to constrain the interconnected evolution of galaxies and the intergalactic medium since the dark ages. The only acceptable solutions are concentrated in two narrow sets. In one of them reionization proceeds in two phases: a first one driven by Population III stars, completed atz 10, and after a short recombination period a second one driven by normal galaxies, completed atz 6. In the other set both kinds of sources work in parallel until full reionization atz 6. The best solution with double reionization gives excellent fits to all the observed cosmic histories, but the CMB optical depth is 3σ larger than the recent estimate from the Planck data. Alternatively, the best solution with single reionization gives less good fits to the observed star formation rate density and cold gas mass density histories, but the CMB optical depth is consistent with that estimate. We make several predictions, testable with future observations, that should discriminate between the two reionization scenarios. As a byproduct our models provide a natural explanation to some characteristic features of the cosmic properties at high-z, as well as to the origin of globular clusters.

show abstract

Section: Luminous Sourcesmentioning

confidence: 99%

CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

Salvador-Solé

Manrique

Guzmán

et al. 2016

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…As shown in Juan et al (2014b), the FoF mass with linking length b = 0.2, FoF(0.2), is equivalent to the SO mass with overdensity ∆ vir relative to the mean cosmic density, SO(∆ vir ). This explains that the halo multiplicity function for FoF(0.2) is privileged (Q iii) in the sense that it has a roughly universal shape in top-hat filtering (Juan et al 2014b). 2006) analytic fit to the nearly universal multiplicity function of simulated halos (blue dotted line) for FoF(b=2) halo masses.…”

Section: Halo Mf and Abundance Of Non-nested Peaksmentioning

confidence: 99%

Culminating the peak CUSP to descry the dark side of halos

Salvador-Solé,

Manrique

2021

Preprint

Self Cite

View full text Add to dashboard Cite

The ConflUent System of Peak trajectories (CUSP) is a rigorous formalism in the framework of the peak theory that allows one to derive from first principles and with no free parameters the typical halo properties from the statistics of peaks in the filtered Gaussian random field of density perturbations. The predicted halo mass function, spherically averaged density, velocity dispersion, velocity anisotropy, ellipticity, prolateness and potential profiles, as well as the abundance and number density profiles of accreted and stripped subhalos and diffuse dark matter accurately recover the results of cosmological N -body simulations. CUSP is thus a powerful tool for the calculation, in any desired hierarchical cosmology with Gaussian perturbations, of halo properties beyond the mass, redshift and radial ranges covered by simulations. More importantly, CUSP unravels the origin of the characteristic features of those properties. In the present Paper we culminate its construction. We show that all halo properties but those related with subhalo stripping are independent of the assembly history of those objects, and that the Gaussian is the only smoothing window able to find the finite collapsing patches while properly accounting for the entropy increase produced in major mergers.

show abstract

“…Thus, following the collapse and virialization of those seeds, with well-known properties according to Gaussian statistics, one can accurately derive from first principles and with no single free parameter the properties of virialized haloes. 2 The halo properties so derived, namely the MF (Juan et al 2014b ) In the series of three paper initiated here, we extend the application of CUSP to the study of halo substructure. Specifically, here we relate the amount of diffuse dark matter (dDM) present at any given time in the inter-halo medium with the free-streaming mass or halo resolution mass in the real Universe or the cosmological simulation, respectively, and establish the link between subhaloes and their seeds in the initial density field.…”

mentioning

confidence: 99%

An accurate comprehensive approach to substructure – I. Accreted subhaloes

Salvador-Solé

Manrique

Botella

2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

This is the first of a series of three Papers devoted to the study of halo substructure in hierarchical cosmologies by means of the CUSP formalism. In the present Paper we derive the properties of subhaloes and diffuse dark matter (dDM) accreted onto haloes and their progenitors. Specifically, we relate the dDM present at any time in the inter-halo medium of the real Universe or a cosmological simulation with the corresponding free-streaming mass or the halo resolution mass, respectively, and establish the link between subhaloes and their seeds in the initial density field. By monitoring the collapse and virialisation of haloes, we derive from first principles and with no single free parameter the abundance and radial distribution of dDM and subhaloes accreted onto them. Our predictions are in excellent agreement with the results of simulations, but for the predicted fraction of accreted dDM, which is larger than reported in previous works as they only count the dDM accreted onto the final halo, not onto its progenitors. The derivation pursued here clarifies the origin of some key features of substructure. Overall, our results demonstrate that CUSP is a powerful tool for understanding halo substructure and extending the results of simulations to haloes with arbitrary masses, redshifts and formation times in any hierarchical cosmology endowed with random Gaussian density perturbations.

show abstract

Halo mass definition and multiplicity function

Cited by 13 publications

References 38 publications

CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

Culminating the peak CUSP to descry the dark side of halos

An accurate comprehensive approach to substructure – I. Accreted subhaloes

Contact Info

Product

Resources

About