SFR−M_* plane for xCOLD GASS sample from Saintonge et al. (2017) with our H I absorbing galaxy marked in blue rectangle (colour-coded on the atomic gas fraction). The black dots represent H I non-detections in their sample while the grey contours represents the distribution of the SDSS galaxy population. The absorber galaxy is marked in a rectangle to represent the range of SFR derived; see Sect. 3.2 for details. The f_H I, which corresponds to the ratio between M_HI and (M_* + M_HI), for our H I absorber galaxy ranges between –1.1 and –2.1 (in logscale) for a T_spin of 1000 K and 100 K respectively. For plotting, we consider a T_spin of 1000 K. ©AAS. Reproduced with permission.