Top: fractional Hα (left) and He I λ5877 (right) luminosity of Delorme 1 (AB)b (filled green circle) shown with respective values from the CASPAR sample of young stars, brown dwarfs, and planets (‘BD’, ‘Pl’), sample of active field M-dwarfs from Stelzer et al. (2013b) and Bochanski et al. (2007), and sample of Class III non-accretors from Manara et al. (2013). The available Hα measurement for the target with MUSE is shown as the filled green square. The dashed red line (shaded region denotes error bars) shows the mean activity index for Hα (Stelzer et al. 2013a) and He I (this work). The blue lines denote the median measurements for CASPAR stars (dotted) and brown dwarfs, planets (dashed). Bottom: accretion luminosity of Delorme 1 (AB)b measured from UV excess, He I lines, and Hα, along with Class III sources from Manara et al. (2013) and CASPAR accretors. Also shown are low-mass Class II accretors (unfilled teal crosses) and non-accretors (black dots, with upper limits as downward arrows) from Almendros-Abad et al. (2024) and a sample of accreting YSOs from seven star-forming regions from Manara et al. (2023) (pink crosses). T_eff—L_acc,noise relation from Manara et al. (2013) is shown as the dashed red curve, and the L_acc,noise from Venuti et al. (2019) at 20 M_Jup is shown as the dashed black line. FAM25 and AMI21 denotes L_line-L_acc scaling relations from Fiorellino et al. (2025) and Aoyama et al. (2021) respectively, and L_acc derived from MUSE epoch is denoted as the brown triangle. In all the panels, measurements from the primary are denoted as a yellow star and fall very close to the measurements from non-accretors.