Scaling Evolution of Universal Dark Matter Halo Density Profiles

Raig, A.; González-Casado, Guillermo; Salvador-Solé, E.

doi:10.1086/311737

Cited by 20 publications

(17 citation statements)

References 15 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…SSM found that, given an effective value of Δ m of about , the empirical mass–density relation shown by haloes in high‐resolution N ‐body simulations of distinct hierarchical cosmologies (Navarro, Frenk & White 1997, hereafter NFW) is naturally reproduced under the assumption proposed by NFW that the characteristic density of haloes is proportional to the critical density of the universe at the time of their formation. Raig, González‐Casado & Salvador‐Solé (1998, hereafter RGS) subsequently showed that the mass–density relation is, in this case, not only consistent with but actually implied by the MPS model. To prove this, RGS assumed haloes endowed with a universal density profile à la NFW.…”

Section: Introductionsupporting

confidence: 66%

Testing the modified Press-Schechter model against N-body simulations

Raig¹,

González-Casado²,

Salvador-Solé³

2001

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

A modified version of the extended Press -Schechter model for the growth of dark-matter haloes was introduced in two previous papers, with the aim of explaining the mass -density relation shown by haloes in high-resolution cosmological simulations. In this model, major mergers are well separated from accretion, thereby allowing a natural definition of halo formation and destruction. This makes it possible to derive analytic expressions for halo formation and destruction rates, the mass accretion rate and the probability distribution functions of halo formation times and progenitor masses. The stochastic merger histories of haloes can be readily derived and easily incorporated into semi-analytical models of galaxy formation, thus avoiding the usual problems encountered in the construction of Monte Carlo merger trees from the original extended Press -Schechter formalism. Here we show that the predictions of the modified Press -Schechter model are in good agreement with the results of N-body simulations for several scale-free cosmologies.

show abstract

Section: Introductionsupporting

confidence: 66%

Testing the modified Press-Schechter model against N-body simulations

Raig¹,

González-Casado²,

Salvador-Solé³

2001

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…where ρ c and r s are, respectively, the halo characteristic density and scale radius. Salvador-Solé, Solanes, & Manrique (1998; see also Raig, González-Casado, & Salvador-Solé 1998) developed a consistent analytic description of the hierarchical evolution of DM halos that provides an excellent fit to Nbody simulations (Raig, González-Casado, & Salvador-Solé 2001). This framework for structure formation incorporates in the well-known extended Press-Schechter formalism (Lacey & Cole 1993) a pre-established phenomenological threshold ∆ m setting the fractional mass increase that separates the two basic mass aggregation regimes of dark halos: minor mergers or accretion, where these objects grow inside-out through the continuous aggregation of small clumps that do not disturb their internal structure 3 , and major merger events, in which the progenitor halos are fully disrupted giving rise to the formation of a new bound system.…”

Section: The Dark Halo Evolution Modelmentioning

confidence: 99%

Implications of Halo Inside‐Out Growth for the X‐Ray Properties of Nearby Galaxy Systems within the Preheating Scenario

Solanes

Manrique

González-Casado

et al. 2005

ApJ

View full text Add to dashboard Cite

We present an entirely analytic model for a preheated, polytropic intergalactic medium in hydrostatic equilibrium within a NFW dark halo potential in which the evolution of the halo structure between major merger events proceeds inside-out by accretion. This model is used to explain, within a standard ΛCDM cosmogony, the observed X-ray properties of nearby relaxed, non-cooling flow groups and clusters of galaxies. We find that our preferred solution to the equilibrium equations produces scaling relations in excellent agreement with observations, while simultaneously accounting for the typical structural characteristics of the distribution of the diffuse baryons. In the class of preheating models, ours stands out because it offers a unified description of the intrahalo medium for galaxy systems with total masses above ∼ 2 × 10 13 M ⊙ , does not produce baryonic configurations with large isentropic cores, and reproduces faithfully the observed behavior of the gas entropy at large radii. All this is achieved with a moderate level of energy injection of about half a keV, which can be easily accommodated within the limits of the total energy released by the most commonly invoked feedback mechanisms, as well as with a polytropic index of 1.2, consistent with both many observational determinations and predictions from high-resolution gas-dynamical simulations of non-cooling flow clusters. More interestingly, our scheme offers a physical motivation for the adoption of this specific value of the polytropic index, as it is the one that best ensures the conservation after halo virialization of the balance between the total specific energies of the gas and dark matter components for the full range of masses investigated.

show abstract

“…3 3 These are actually formulae for fast mass gain and can include accretion. Analytic formulae differentiating between major mergers and accretion have been found by Raig, Gonzalez‐Casado & Salvador‐Sole (1998), Salvador‐Sole, Solanes & Manrique (1998) and Andreu, Gonzalez‐Casado & Salvador‐Sole (2001). …”

mentioning

confidence: 92%

“…These are actually formulae for fast mass gain and can include accretion. Analytic formulae differentiating between major mergers and accretion have been found byRaig, Gonzalez-Casado & Salvador-Sole (1998), Salvador-Sole, Solanes & Manrique (1998) andAndreu, Gonzalez-Casado & Salvador-Sole (2001).4 If the m 0 halo has come from an m i halo, all of its mass was not previously in the m i halo, only m i /m 0 of its mass. But the quantity wanted here is the full mass of haloes which have had mergers, i.e.…”

mentioning

confidence: 93%

Source mergers and bubble growth during reionization

Cohn

Chang

2007

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The recently introduced models of reionization bubbles based on extended Press–Schechter theory (by Furlanetto, Hernquist & Zaldarriaga) are generalized to include mergers of ionization sources. Sources with a recent major merger are taken to have enhanced photon production due to star formation, and accretion on to a central black hole if a black hole is present. This produces a scatter in the number of ionized photons corresponding to a halo of a given mass and a change in photon production over time for any given halo mass. By extending previous methods, photon production histories, bubble distributions and ionization histories are computed for several different parameter and recombination assumptions. The resulting distributions interpolate between previously calculated limiting cases.

show abstract

Scaling Evolution of Universal Dark Matter Halo Density Profiles

Cited by 20 publications

References 15 publications

Testing the modified Press-Schechter model against N-body simulations

Testing the modified Press-Schechter model against N-body simulations

Implications of Halo Inside‐Out Growth for the X‐Ray Properties of Nearby Galaxy Systems within the Preheating Scenario

Source mergers and bubble growth during reionization

Contact Info

Product

Resources

About