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Showing 1 to 4 of 4 for “"halo-mass-function"”.

  1. Simulations of dark energy cosmologies

    … such as the growth of large scale structure, the halo mass function and baryonic acoustic oscillations. We study the power spectrum in redshift space in $\Lambda$CDM and quintessence dark energy models and test predictions for the form of the redshift space distortions. An improved model for the …

    durham Repository record for Simulations of dark energy cosmologies (opens in a new tab)

  2. GALAXY-HALO CONNECTION AND CLUSTERING IN THE PRESENCE OF DYNAMICAL DARK ENERGY AND MASSIVE NEUTRINOS

    … of the connection between dark matter subhaloes and galaxies, and the analysis of the galaxy cluster mass function and clustering, in cosmologies alternative to the standard LCDM model. To this aim a large set of cosmological N-body simulations has been used, the so-called “Dark Energy and …

    milano Repository record for GALAXY-HALO CONNECTION AND CLUSTERING IN THE PRESENCE OF DYNAMICAL DARK ENERGY AND MASSIVE NEUTRINOS (opens in a new tab)

  3. The Role of Baryons and Neutrinos in the Evolution of Large-Scale Structure

    … is the effect of the cosmic background of massive neutrinos. As these remain relativistic to relatively late times, they will free-stream out of overdensities, altering the formation of large-scale structure (LSS). If this effect can be accurately modelled, it presents an independent method …

    liverpool-jm Repository record for The Role of Baryons and Neutrinos in the Evolution of Large-Scale Structure (opens in a new tab)

  4. Cosmology with Velocity Dispersion based Counts of Groups and the Effect of AGN Feedback on Host Galaxy Morphology

    … problem is systematic errors in the absolute halo mass calibration in cluster studies, which is required to convert the standard theoretical prediction (the halo mass function) into counts as a function of the observable (e.g., X-ray luminosity, Sunyaev-Zel'dovich flux, optical richness). Here …

    liverpool-jm Repository record for Cosmology with Velocity Dispersion based Counts of Groups and the Effect of AGN Feedback on Host Galaxy Morphology (opens in a new tab)