SDSS-IV MaNGA: Signatures of halo assembly in kinematically misaligned
  galaxies
  We investigate the relationship of kinematically misaligned galaxies with
their large-scale environment, in the context of halo assembly bias. According
to numerical simulations, halo age at fixed halo mass is intrinsically linked
to the large-scale tidal environment created by the cosmic web. We investigate
the relationship between distances to various cosmic web features and
present-time gas accretion rate. We select a sub-sample of ~900 central
galaxies from the MaNGA survey with defined global position angles (PA; angle
at which velocity change is greatest) for their stellar and H$\alpha$ gas
components up to a minimum of 1.5 effective radii ($R_e$). We split the sample
by misalignment between the gas and stars as defined by the difference in their
PA. For each central galaxy we find its distance to nodes and filaments within
the cosmic web, and estimate the host halo's age using the central stellar mass
to total halo mass ratio $M_{*}/M_{h}$. We also construct halo occupation
distributions using a background subtraction technique for galaxy groups split
using the central galaxy's kinematic misalignment. We find, at fixed halo mass,
no statistical difference in these properties between our kinematically aligned
and misaligned galaxies. We suggest that the lack of correlation could be
indicative of cooling flows from the hot halo playing a far larger role than
`cold mode' accretion from the cosmic web or a demonstration that the spatial
extent of current large-scale integral field unit (IFU) surveys hold little
information about large-scale environment extractable through this method.
