Notes. Uncertainties for detections and upper limits for tentative and nondetections correspond to a 95%, and a 3-σ confidence interval respectively. For nondetections, we assumed that a signature should have a FWHM covering at least 10 SPIRou pixels. Mass-loss rate ($\dot{m}$) and temperature of the escape (T) were estimated with the reduced χ² maps (Fig. 7), using the model parameters in Table 5 and computed with our wrapper of p-winds (see Sec. 4). This corresponds to our model M1 (see Sec. 5.1), which provided equivalent results to our model M2. Error and upper limits estimations are detailed in Appendix F.2 for the depth and EW, and in Appendix F.3 for $\dot{m}$ and T. Constraints on $\dot{m}$ and T are reported for ≥98/2 (model M1) and 90/10 values (model M4) for the H/He ratio for comparison. The corresponding ratio is indicated in parenthesis below the relevant parameter. We were not able to derive upper limits for K2-25 b due to its extremely low S/N (see Fig. A.1), and for AU Mic b due to the overlapping of a strong stellar residual with the expected planetary He lines positions.