1212.4157 (Giulia Despali et al.)

Ellipsoidal halo finders and implications for models of triaxial halo formation    [PDF]

Giulia Despali, Giuseppe Tormen, Ravi K. Sheth

We describe an algorithm for identifying ellipsoidal haloes in numerical simulations, and quantify how the resulting estimates of halo mass and shape differ with respect to spherical halo finders. Haloes become more prolate when fit with ellipsoids, the difference being most pronounced for the more aspherical objects. Although the ellipsoidal mass is systematically larger, this is typically by less than 10% for most of the haloes. However, even this small difference in mass corresponds to a significant difference in shape from the spherical counterpart. We quantify these effects on the initial mass and deformation tensors, on which most models of triaxial collapse are based. By studying the properties of protohaloes in the initial conditions, we find that models in which protohaloes are identified in Lagrangian space by three positive eigenvalues of the deformation tensor are tenable only at the masses well-above M_*. The overdensity $\delta$ within almost any protohalo is larger than the critical value associated with spherical collapse; this is in good qualitative agreement with models which identify haloes requiring that collapse have occured along all three principal axes, each axis having turned around from the universal expansion at a different time. On average, delta increases as mass M decreases, scaling as delta_c(1 + 0.2sigma) with rms scatter 0.2sigma(M). The mean ellipticity e and prolateness p of the deformation tensor both increase as M decreases (e*delta/sigma =0.4, rms_e = 0.14; p*delta/sigma = 0, rms_p=0.15). [Abridged]

View original: http://arxiv.org/abs/1212.4157