Global Attenuation in Spiral Galaxies in Optical and Infrared Bands
  The emerging light from a galaxy is under the influence of its own
interstellar medium, as well as its spatial orientation. Considering a sample
of 2,239 local spiral galaxies in optical (SDSS u, g, r, i, and z) and infrared
bands (WISE W1, W1), we study the dependency of the global intrinsic
attenuation in spiral galaxies on their morphologies, sizes, and spatial
inclinations. Reddening is minimal at the extremes of low mass and gas
depletion and maximal in galaxies that are relatively massive and metal-rich
and still retain substantial gas reserves. A principal component constructed
from observables that monitor galaxy mass, relative HI content to old stars,
and infrared surface brightness is strongly correlated with the amplitude of
obscuration. We determine both a parametric model for dust obscuration and a
non-parametric model based on the Gaussian process formalism. An average dust
attenuation curve is derived for wavelengths between 0.36 and 4.5 microns.
