  At any given epoch, the Extragalactic Background Light (EBL) carries imprints
of integrated star formation activities in the universe till that epoch. On the
other hand, in order to estimate the EBL, when direct observations are not
possible, one requires an accurate estimation of the star formation rate
density (SFRD) and the dust attenuation ($A_\nu$) in galaxies. Here, we present
a 'progressive fitting method' that determines global average SFRD($z$) and
$A_\nu(z)$ for any given extinction curve by using the available
multi-wavelength multi-epoch galaxy luminosity function measurements. Using the
available observations, we determine the best fitted combinations of SFRD($z$)
and $A_\nu(z)$, in a simple fitting form, up to $z\sim8$ for five well known
extinction curves. We find, irrespective of the extinction curve used, the $z$
at which the SFRD($z$) peaks is higher than the $z$ above which $A_\nu(z)$
begins to decline. For each case, we compute the EBL from ultra-violet to the
far-infrared and optical depth ($\tau_\gamma$) encountered by the high energy
$\gamma$-rays due to pair production upon collisions with these EBL photons. We
compare these with measurements of the local EBL, $\gamma$-ray horizon and
$\tau_\gamma$ measurements using Fermi-LAT. All these and the comparison of
independent SFRD($z$) and $A_\nu(z)$ measurements from the literature with our
predictions favor the extinction curve similar to that of Large Magellanic
Cloud Supershell.
