  Cumulative optical and infrared emission from galaxies accumulated over
cosmological time scales, the extragalactic background light (EBL), could be
probed by complementary techniques of direct observations and source counting
in the visible and infrared as well as via its imprint on the signal of distant
active galactic nuclei in gamma rays. We compare the visible and infrared
measurements with the gamma-ray constraints and study if the discrepancies of
the measurements with different methods could be due to the presence of
features in the EBL spectrum that are localised in the micron wavelength range.
We combined data on time-averaged spectra of selected blazars that were
obtained by Fermi and ground-based gamma-ray telescopes. We also modelled the
effect of absorption on EBL while allowing for the existence of a previously
unaccounted spectral feature. We show that a previously reported 'excess' in
EBL flux in the $\sim 1$~micron wavelength range is consistent with gamma-ray
measurements, that is, if the excess has the form of a narrow feature of the
width $\delta \lambda < \lambda$ and an overall flux of up to 15 nW/(m$^2$ sr)
above the 'minimal' EBL, which is estimated from the visible and infrared
source counts. Such 'bump-like' spectral features could originate, for example,
from decaying dark-matter particles, or either axions or peculiar astrophysical
processes in the course of star-formation history. We discuss the possibilities
for the search of spectral features in the EBL with the Cherenkov Telescope
Array (CTA).
