The cosmic web of the Local Universe: cosmic variance, matter content
  and its relation to galaxy morphology
  We present, for the first time, a Local Universe (LU) characterization using
high precision constrained $N$-body simulations based on self-consistent
phase-space reconstructions of the large-scale structure in the Two-Micron
All-Sky Galaxy Redshift Survey. We analyse whether we live in a special cosmic
web environment by estimating cosmic variance from a set of unconstrained
$\Lambda$CDM simulations as a function of distance to random observers. By
computing volume and mass filling fractions for voids, sheets, filaments and
knots, we find that the LU displays a typical scatter of about $1\sigma$ at
scales $r>15\,h^{-1}\,{\rm Mpc}$, in agreement with $\Lambda$CDM, converging to
a fair unbiased sample when considering spheres of about $60\,h^{-1}\,{\rm
Mpc}$ radius. Additionally, we compute the matter density profile of the LU and
found a reasonable agreement with the estimates of Karachentsev (2012) only
when considering the contribution of dark haloes. This indicates that
observational estimates may be biased towards low density values. As a first
application of our reconstruction, we investigate the likelihood of different
galaxy morphological types to inhabit certain cosmic web environments. In
particular, we find that, irrespective of the method used to define the web,
either based on the density or the peculiar velocity field, elliptical galaxies
show a clear tendency to preferentially reside in clusters as opposed to voids
(up to a level of $5.3\sigma$ and $9.8\sigma$ respectively) and conversely for
spiral galaxies (up to a level of $5.6\sigma$ and $5.4\sigma$ respectively).
These findings are compatible with previous works, albeit at higher confidence
levels.
