## Non-linear dynamics and mass function of cosmic structures## I. Analytical results
^{1} Laboratoire d'Astrophysique Extragalactique et de
Cosmologie, Observatoire de Paris-Meudon, F-92195 Meudon Cedex,
France^{2} CEA, DSM/DAPNIA/Service d'Astrophysique CE-SACLAY,
F-91191 Gif-sur-Yvette, France
We investigate some modifications to the Press & Schechter (1974) (PS) prescription resulting from shear and tidal effects. These modifications rely on more realistic treatments of the collapse process than the standard approach based on the spherical model. First, we show that the mass function resulting from a new approximate Lagrangian dynamic (Audit & Alimi 1996), contains more objects at high mass, than the classical PS mass function and is well fitted by a PS-like function with a threshold density of . However, such a Lagrangian description can underestimate the epoch of structure formation since it defines it as the collapse of the first principal axis. We therefore suggest some analytical prescriptions, for computing the collapse time along the second and third principal axes, and we deduce the corresponding mass functions. The collapse along the third axis is delayed by the shear and the number of objects of high mass then decreases. Finally, we show that the shear also strongly affects the formation of low-mass halos. This dynamical effect implies a modification of the low-mass slope of the mass function and allows the reproduction of the observed luminosity function of field galaxies. In a companion paper, we present results of numerical simulations which complete this work.
## Contents- 1. Introduction
- 2. Mass functions from Lagrangian dynamics
- 3. Beyond Lagrangian models
- 4. Conclusion
- Appendix A
- Appendix A: collapse epoch using our dynamical model
- Appendix B: computation of the low-mass behavior of the mass function for the third axis collapse
- References
© European Southern Observatory (ESO) 1997 Online publication: April 28, 1998 |