A numerical twist on the observational spin parameter, ${\lambda }_R$

Abstract

A primary goal of integral field spectroscopic (IFS) surveys is to provide a statistical census of galaxies classified by their internal kinematics. As a result, the observational spin parameter, ${\lambda }_R$, has become one of the most popular methods of quantifying the relative importance of velocity dispersion and rotation in supporting a galaxy's inner structure. The goal of this paper is to examine the relationship between the observationally deduced ${\lambda }_R$ and one of the most commonly used theoretical spin parameters in the literature, the Bullock et al. (2001) ${\lambda }^{\prime }$. Using a set of $N$-body realisations of galaxies from which we construct mock IFS observations, we measure ${\lambda }_R$ as an observer would, incorporating the effects of beam smearing and seeing conditions. Assuming parameters typical of current IFS surveys, we confirm that there are strong positive correlations between ${\lambda }_R$ and measurement radius, and strong negative correlations between ${\lambda }_R$ and size of the PSF, for late-type galaxies; these biases can be reduced using a recently proposed empirical correction. Once observational biases are corrected for, we find that ${\lambda }_R$ provides a good approximation to $\sim \sqrt{3}/2{\lambda }^{\prime }({\mathrm{R}}_{\mathrm{eff}})$, where ${\lambda }^{\prime }$ is evaluated for the galactic stellar component within 1 R${}_{\mathrm{eff}}$.

Accepted for publication in MNRAS. 15 pages, 14 figures

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