Spectral Evidence of Solar Neighborhood Analogs in CALIFA Galaxies
  We introduce a novel non-parametric method to find solar neighborhood analogs
(SNAs) in extragalactic IFS surveys. The main ansatz is that the physical
properties of the solar neighborhood (SN) should be encoded in its optical
stellar spectrum. We assume that our best estimate of such spectrum is the one
extracted from the analysis performed by the Code for Stellar properties
Heuristic Assignment (\textsc{CoSHA}) from the MaStar stellar library. It
follows that finding SNAs in other galaxies consist in matching, in a $\chi^2$
sense, the SN reference spectrum across the optical extent of the observed
galaxies. We apply this procedure to a selection of CALIFA galaxies, by
requiring a close to face-on projection, relative isolation and non-AGN. We
explore how the local and global properties of the SNAs (stellar age,
metallicity, dust extinction, mass-to-light ratio, stellar surface mass and
star-formation densities and galactocentric distance) and their corresponding
host galaxies (morphological type, total stellar mass, star-formation rate,
effective radius) compare with those of the SN and the Milky Way (MW). We find
that SNAs are located preferentially in S(B)a~--~S(B)c galaxies, in a ring-like
structure, which radii seems to scale with the galaxy size. Despite the known
sources of systematics and errors, {most} properties present a considerable
agreement with the literature on the SN. We conclude that the solar
neighborhood is relatively common in our sample of SNAs. Our results warrants a
systematic exploration of correlations among the physical properties of the
SNAs and their host galaxies. We reckon that our method should inform current
models of the galactic habitable zone in our MW and other galaxies.
