In physical cosmology, the Sheth–Tormen approximation is a halo mass function. It is named after Ravi K. Sheth and Giuseppe Tormen, who proposed their function in 1999.
Background The Sheth–Tormen approximation extends the Press–Schechter formalism by assuming that halos are not necessarily spherical, but merely elliptical. The distribution of the density fluctuation is as follows: f ( σ r ) = A 2 a π [ 1 + ( σ r 2 a δ c 2 ) 0.3 ] δ c σ r exp ( − a δ c 2 2 σ r 2 ) , {\displaystyle f(\sigma _{r})=A{\sqrt {\frac {2a}{\pi }}}\left[1+\left({\frac {\sigma _{r}^{2}}{a\delta _{c}^{2}}}\right)^{0.3}\right]{\frac {\delta _{c}}{\sigma _{r}}}\exp \left(-{\frac {a\delta _{c}^{2}}{2\sigma _{r}^{2}}}\right),} where δ c = 1.686 {\displaystyle \delta _{c}=1.686} , a = 0.707 {\displaystyle a=0.707} , and A = 0.3222 {\displaystyle A=0.3222} . The parameters were empirically obtained from the five-year release of WMAP.
Discrepancies with simulations In 2010, the Bolshoi cosmological simulation predicted that the Sheth–Tormen approximation is inaccurate for the most distant objects. Specifically, the Sheth–Tormen approximation overpredicts the abundance of haloes by a factor of 10 {\displaystyle 10} for objects with a redshift z > 10 {\displaystyle z>10} , but is accurate at low redshifts.
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