The MOSDEF Survey: Implications of the Lack of Evolution in the Dust
  Attenuation-Mass Relation to z~2
  We investigate the relationship between dust attenuation and stellar mass
($M_*$) in star-forming galaxies over cosmic time. For this analysis, we
compare measurements from the MOSFIRE Deep Evolution Field (MOSDEF) survey at
$z\sim2.3$ and the Sloan Digital Sky Survey (SDSS) at $z\sim0$, augmenting the
latter optical dataset with both UV Galaxy Evolution Explorer (GALEX) and
mid-infrared Wide-field Infrared Survey Explorer (WISE) photometry from the
GALEX-SDSS-WISE Catalog. We quantify dust attenuation using both spectroscopic
measurements of H$\alpha$ and H$\beta$ emission lines, and photometric
measurements of the rest-UV stellar continuum. The H$\alpha$/H$\beta$ ratio is
used to determine the magnitude of attenuation at the wavelength of H$\alpha$,
$A_{{\rm H}\alpha}$. Rest-UV colors and spectral-energy-distribution fitting
are used to estimate $A_{1600}$, the magnitude of attenuation at a rest
wavelength of 1600\AA. As in previous work, we find a lack of significant
evolution in the relation between dust attenuation and $M_*$ over the redshift
range $z\sim0$ to $z\sim2.3$. Folding in the latest estimates of the evolution
of $M_{{\rm dust}}$, $({M_{{\rm dust}}}/{M_{{\rm gas}}})$, and gas surface
density at fixed $M_*$, we find that the expected $M_{{\rm dust}}$ and dust
mass surface density are both significantly higher at $z\sim2.3$ than at
$z\sim0$. These differences appear at odds with the lack of evolution in dust
attenuation. To explain the striking constancy in attenuation vs. $M_*$, it is
essential to determine the relationship between metallicity and $({M_{{\rm
dust}}}/{M_{{\rm gas}}})$, the dust mass absorption coefficient, and dust
geometry, and the evolution of these relations and quantities from $z\sim0$ to
$z\sim2.3$.
