The observed cosmic star formation rate density has an evolution which
  resembles a {\Gamma}(a, bt) distribution and can be described successfully by
  only 2 parameters
  A debate is emerging regarding the recent inconsistent results of different
studies for the Cosmic Star Formation Rate Density (CSFRD) at high-z. We employ
UV and IR datasets to investigate the star formation rate function (SFRF) at
${\rm z \sim 0-9}$. We find that the SFRFs derived from the dust corrected
${\rm UV}$ (${\rm UV_{corr}}$) data contradict those from IR on some key issues
since they are described by different distributions (Schechter vs double-power
law), imply different physics for galaxy formation (${\rm UV_{corr}}$ data
suggest a SFR limit/strong mechanism that diminish the number density of high
star forming systems with respect IR) and compare differently with the stellar
mass density evolution obtained from SED fitting (${\rm UV_{corr}}$ is in
agreement, while IR in tension up to 0.5 dex). However, both tracers agree on a
constant CSFRD evolution at ${\rm z \sim 1-4}$ and point to a plateau instead
of a peak. In addition, using both indicators we demonstrate that the evolution
of the {\it observed} CSFRD can be described by only {\bf 2} parameters and a
function that has the form of a Gamma distribution (${\bf \Gamma(a,bt)}$). In
contrast to previous parameterizations used in the literature our framework
connects the parameters to physical properties like the star formation rate
depletion time and cosmic baryonic gas density. The build up of stellar mass
occurs in $\Gamma(a,bt)$ distributed steps and is the result of gas consumption
up to the limit that there is no eligible gas for SF at t = ${\rm \infty}$,
resulting to a final cosmic stellar mass density of $\sim 0.5 \times 10^9 \,
{\rm \frac{M_{\odot}}{Mpc^3}}$.
