  The ultraviolet continuum traces young stars while the near-infrared unveils
older stellar populations and dust-obscured regions. Balmer emission lines
provide insights on gas properties and young stellar objects but are highly
affected by dust attenuation. The near-infrared Paschen lines suffer less dust
attenuation and can be used to measure star formation rates (SFRs) in
star-forming regions obscured by dust clouds. We select 13 sources between
redshifts 1 and 3 observed with HST, JWST/NIRCam and NIRSpec based on the
availability of at least one Balmer and one Paschen line with S/N > 5. With a
newly-developed version of CIGALE, we fit their hydrogen line equivalent widths
(EWs) and photometric data. We assess the impacts of the removal of
spectroscopic data by comparing the quality of the fits of the
spectro-photometric data to those with photometric data only. We compare the
single (BC03) vs binary (BPASS) stellar populations models in the fitting
process of spectro-photometric data. We derive the differential attenuation and
explore different attenuation recipes by fitting spectro-photometric data with
BC03. For each stellar model and for each input dataset (with and without EWs),
we quantify the deviation on the SFRs and stellar masses from the "standard"
choice. On average, the SFRs are overestimated and the stellar masses are
underestimated when EWs are not included as input data. We find a major
contribution of the H${\alpha}$ emission line to the broadband photometric
measurements of our sources, and a trend of increasing contribution with
specific SFR. Using the BPASS models has a significant impact on the derived
SFRs and stellar masses. We show that a flexible attenuation recipe provides
more accurate estimates of the dust attenuation parameters, especially the
differential attenuation which agrees with the original value of Charlot & Fall
(2000).
