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waynehu

Professor, Department of Astronomy and Astrophysics
University of Chicago

Group Contact CV Computing SnapShots
CMB Introduction '96   Intermediate '01   Polarization Intro '01   Cosmic Symphony '04   Polarization Primer '97   Review '02   Power Animations   Lensing   Power Prehistory   Legacy Material '96   PhD Thesis '95 Baryon Acoustic Oscillations Cosmic Shear Clusters
Transfer Function WMAP Likelihood Reionization PPF for CAMB Halo Mass Conversion Cluster Abundance
Cosmology [321] Current Topics [282] Galaxies and Universe [242] Radiative Processes [305] Research Preparation [307] GR Perturbation Theory [408] Advanced CMB [448]

Halo Mass Conversion

Wayne Hu & Andrey Kravtsov

Driver and fitting routines for converting halo mass definitions from one spherical overdensity to another assuming an NFW density profile

Inputs: original mass M&Delta and overdensity &Delta and concentration c=r&Delta /rs and the desired target overdensity &Deltanew. Overdensity may be with respect to mean or critical so long as the target definition is defined in the same way. If c < 0, a Bullock et al default in a ΛCDM cosmology with &sigma8=0.8, and the mass is assumed to be virial mass in h-1Ms. (1/14/11: I/O swap between inputing the old vs new concentration fixed pointed out by Yin Li)

Outputs: MΔnew mass at the target overdensity &Deltanew

References

[1] ''Sample Variance Considerations for Cluster Surveys,'' Hu & Kravtsov (2003) ApJ, 584, 702, astro-ph/0203169