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Accretion rates ($\dot{M}$) of young stars show a strong correlation withobject mass ($M$); however, extension of the $\dot{M}-M$ relation into thesubstellar regime is less certain. Here, we present the Comprehensive Archiveof Substellar and Planetary Accretion Rates (CASPAR), the largest to-datecompilation of substellar accretion diagnostics. CASPAR includes: 658 stars,130 brown dwarfs, and 10 bound planetary mass companions. In this work, weinvestigate the contribution of methodological systematics to scatter in the$\dot{M}-M$ relation, and compare brown dwarfs to stars. In our analysis, werederive all quantities using self-consistent models, distances, and empiricalline flux to accretion luminosity scaling relations to reduce methodologicalsystematics. This treatment decreases the original $1\sigma$ scatter in the$\log \dot{M}-\log M$ relation by $\sim17$%, suggesting that it makes only asmall contribution to the dispersion. CASPAR rederived values are best fit by$\dot{M}\propto M^{2.02\pm0.06}$ from 10~$M_\mathrm{J}$ to 2~$M_\odot$,confirming previous results. However, we argue that the brown dwarf and stellarpopulations are better described separately and by accounting for both mass andage. Therefore, we derive separate age-dependent $\dot{M}-M$ relations forthese regions, and find a steepening in the brown dwarf $\dot{M}-M$ slope withage. Within this mass regime, the scatter decreases from 1.36 dex to 0.94 dex,a change of $\sim$44%. This result highlights the significant role thatevolution plays in the overall spread of accretion rates, and suggests thatbrown dwarfs evolve faster than stars, potentially as a result of differentaccretion mechanisms.

The Comprehensive Archive of Substellar and Planetary Accretion Rates