  A substantial number of super-Earths have been discovered, and atmospheres of
transiting super-Earths have also been observed by transmission spectroscopy.
Several lines of observational evidence indicate that most super-Earths do not
possess massive H$_2$/He atmospheres. However, accretion and retention of less
massive atmospheres on super-Earths challenge planet formation theory. We
consider the following three mechanisms: (i) envelope heating by pebble
accretion, (ii) mass loss during giant impacts, and (iii) atmospheric loss by
stellar X-ray and EUV photoevaporation. We investigate whether these mechanisms
influence the amount of the atmospheres that form around super-Earths. We
develop a code combining an N-body simulation of pebble-driven planetary
formation and an atmospheric evolution simulation. We demonstrate that the
observed orbital properties of super-Earths are well reproduced by the results
of our simulations. However, (i) heating by pebble accretion ceases prior to
disk dispersal, (ii) the frequency of giant impact events is too low to sculpt
massive atmospheres, and (iii) many super-Earths having H$_2$/He atmospheres of
$\gtrsim 10$ wt% survive against stellar irradiations for 1 Gyr. Therefore, it
is likely that other mechanisms such as suppression of gas accretion are
required to explain less massive atmospheres ($\lesssim 10$ wt%) of
super-Earths.
