Star formation rate as a function of M_★ (top) and sSFR (SFR divided by stellar mass, bottom) for the whole sample. Line emitters and non-emitting galaxies are indicated with filled and unfilled markers, respectively. Downward triangles mark those sources affected by FIR upper limits. For the plot on the left, contours correspond to the number density of galaxies from the SDSS database and those obtained by Renzini & Peng (2015) at values of 1.2 × 10⁵ (inner), 7.0 × 10⁴ (middle), and 2.0 × 10⁴ (outer). These contours reveal the position of the star formation MS for local galaxies. Green stars represent the PAH luminous galaxies at z ∼ 1 sample from Lin et al. (2024). The plot on the right shows the different positions of the star formation MS given by Schreiber et al. (2015) and Whitaker et al. (2014). For each MS, we differentiate the mass range used by each author from the extrapolation by plotting the latter with a discontinuous line.