  (Abridged) We aim to enlarge the number of known hot corinos and carry out a
first comparative study with hot cores. The ultimate goal is to understand
whether complex organic molecules form in the gas phase or on grain surfaces,
and what the possible key parameters are. We observed millimeter rotational
transitions of HCOOH, HCOOCH3, CH3OCH3, CH3CN, and C2H5CN in a sample of
low-mass protostars with the IRAM-30m. Using the rotational diagram method
coupled with the information about the sources' structure, we calculate the
abundances of the observed molecules. To interpret these abundances, we review
the proposed formation processes of the above molecules. We report the
detection of HCOOCH3 and/or CH3CN towards NGC1333-IRAS4B and NGC1333-IRAS2A. We
find that abundance ratios of O-bearing molecules to methanol or formaldehyde
in hot corinos are comparable and about unity, and are relatively (depending on
how the ratios are determined) higher than those in hot cores and in Galactic
center clouds. So far, complex organic molecules were detected in all the hot
corinos where they were searched for, suggesting that it is a common phase for
low-mass protostars. While some evidence points to grain-surface synthesis
(either in the cold or warm-up phase) of these molecules (in particular for
HCOOH and HCOOCH3), the present data do not allow us to disregard gas-phase
formation. More observational, laboratory, and theoretical studies are required
to improve our understanding of hot corinos.
