  Hot corinos are of great interest due to their richness in interstellar
complex organic molecules (COMs) and the consequent potential prebiotic
connection to solar-like planetary systems. Recent surveys have reported an
increasing number of hot corino detections in Class 0/I protostars; however,
the relationships between their physical properties and the hot-corino
signatures remain elusive. In this study, our objective is to establish a
general picture of the detectability of the hot corinos by identifying the
origin of the hot-corino signatures in the sample of young stellar objects
(YSOs) obtained from the Atacama Large Millimeter/submillimeter Array Survey of
Orion Planck Galactic Cold Clumps (ALMASOP) project. We apply spectral energy
distribution (SED) modeling to our sample and identify the physical parameters
of the modeled YSOs directly, linking the detection of hot-corino signatures to
the envelope properties of the YSOs. Imaging simulations of the methanol
emission further support this scenario. We, therefore, posit that the observed
COM emission originates from the warm inner envelopes of the sample YSOs, based
on both the warm region size and the envelope density profile. The former is
governed by the source luminosity and is additionally affected by the disk and
cavity properties, while the latter is related to the evolutionary stages. This
scenario provides a framework for detecting hot-corino signatures toward
luminous Class 0 YSOs, with fewer detections observed toward similarly luminous
Class I sources.
