Kavli Affiliate: Mark Vogelsberger
| First 5 Authors: , , , ,
| Summary:
The splashback radius $R_rm sp$ is a boundary of a halo that separates
infalling and accreted matter. This results in a steep drop in the density
profile at $R_rm st$, which is a commonly adopted proxy for $R_rm sp$.
Observationally, $R_rm st$ can be measured through fitting the projected
galaxy number density profile of the halo, but there has been some discrepancy
between the observed and expected $R_rm st$. Therefore, we investigate
whether the projection of the density profile onto the plane of the sky could
lead to any systematic bias in determining $R_rm st$, by studying the true
3-dimensional and projected halo density profiles from the IllustrisTNG
simulation. We investigate a range of projection lengths, and find that
$R^p_rm st$ obtained from projected profiles is close to the true $R^*_rm
st$, but has a slight decreasing trend with increasing projection length. We
also quantify the prominence of the splashback feature and find how the feature
shape changes with projection length.
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