  The star formation rate (SFR) is a crucial astrophysical tracer for
understanding the formation and evolution of galaxies, determining the
interaction between interstellar medium properties and star formation. The
mainstream approach to study the stellar content in galaxies relies on pure
stellar population synthesis models. However, these methods fail to account for
the contamination of SFR caused by nebular gas radiation. Recent studies have
indicated that neglecting nebular radiation contamination appears to be
non-negligible in galaxies with intense star-forming activities and at
relatively high redshifts, potentially leading to overestimation of stellar
masses. However, there is currently limited targeted research, particularly
regarding galaxies at higher redshifts (z < 0.5). In this investigation, we
employ the BPT diagram to select a sample of 2575 star-formation galaxies (SFG)
from the SDSS-DR18 dataset, all within specified signal-to-noise ratio (S/N)
ranges. Using the spectroscopic fitting tool FADO, which is capable of
excluding nebular radiation contributions in spectral fitting, we conduct a
tentative investigation of the SFR of star-forming galaxies in SDSS- DR18 with
redshifts z < 0.5. Our results show that 45% of the samples show
H{\alpha}{\lambda}6563 obtained from FADO fitting to be smaller than that
derived solely from the pure stellar population synthesis model qsofitmore,
particularly pronounced between redshifts 0.2 and 0.4. We find that the
contribution of nebulae is significant and exhibits an evolutionary trend with
redshift. We anticipate that by combining optical and near-infrared spectral
data, the influence of nebulae may become more prominent in star-forming
galaxies at higher redshifts.
