  The extragalactic background light (EBL) contains all the radiation emitted
by nuclear and accretion processes in stars and compact objects since the epoch
of recombination. Measuring the EBL density directly is challenging, especially
in the near- to far-infrared waveband, mainly due to the zodiacal light
foreground. Instead, gamma-ray astronomy offers the possibility to indirectly
set limits on the EBL by studying the effects of gamma-ray absorption in the
very high energy (VHE:$>$100 GeV) spectra of distant blazars. The High Altitude
Water Cherenkov gamma ray observatory (HAWC) is one of the few instruments
sensitive to gamma rays with energies above 10 TeV. This offers the opportunity
to probe the EBL in the near/mid IR region: $\lambda$ = 1 $\mu$m - 100 $\mu$m.
In this study, we fit physically motivated emission models to Fermi Large Area
Telescope (LAT) GeV data to extrapolate the intrinsic TeV spectra of blazars.
We then simulate a large number of absorbed spectra for different randomly
generated EBL model shapes and calculate Bayesian credible bands in the EBL
intensity space by comparing and testing the agreement between the absorbed
spectra and HAWC extragalactic observations of two blazars. The resulting bands
are in agreement with current EBL lower and upper limits, showing a downward
trend towards higher wavelength values $\lambda>10\, \mu$m also observed in
previous measurements.
