  Accretion signatures from bound brown dwarf and protoplanetary companions
provide evidence for ongoing planet formation, and accreting substellar objects
have enabled new avenues to study the astrophysical mechanisms controlling
formation and accretion processes. Delorme 1 (AB)b, a ~30-45 Myr circumbinary
planetary mass companion, was recently discovered to exhibit strong H$\alpha$
emission. This suggests ongoing accretion from a circumplanetary disk, somewhat
surprising given canonical gas disk dispersal timescales of 5-10 Myr. Here, we
present the first NIR detection of accretion from the companion in Pa$\beta$,
Pa$\gamma$, and Br$\gamma$ emission lines from SOAR/TripleSpec 4.1, confirming
and further informing its accreting nature. The companion shows strong line
emission, with $L_{line} \approx 1-6 \times 10^{-8}~L_\odot$ across lines and
epochs, while the binary host system shows no NIR hydrogen line emission
($L_{line} <0.32-11\times10^{-7}\ L_\odot$). Observed NIR hydrogen line ratios
are more consistent with a planetary accretion shock than with local line
excitation models commonly used to interpret stellar magnetospheric accretion.
Using planetary accretion shock models, we derive mass accretion rate estimates
of $\dot{M}_{\mathrm{pla}}\sim3$-$4\times 10^{-8}\ M_\mathrm{J}$ yr$^{-1}$,
somewhat higher than expected under the standard star formation paradigm.
Delorme 1 (AB)b's high accretion rate is perhaps more consistent with formation
via disk fragmentation. Delorme 1 (AB)b is the first protoplanet candidate with
clear (S/N$\sim$5) NIR hydrogen line emission.
