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We investigate the non-adiabatic effect of time-dependent deformations in theMilky Way (MW) halo potential on stellar streams. Specifically, we consider theMW's response to the infall of the Large Magellanic Cloud (LMC) and how thisimpacts our ability to recover the spherically averaged MW mass profile fromobservation using stream actions. Previously, action clustering methods haveonly been applied to static or adiabatic MW systems to constrain the propertiesof the host system. We use a time-evolving MW--LMC simulation described bybasis function expansions. We find that for streams with realisticobservational uncertainties on shorter orbital periods and without closeencounters with the LMC, e.g. GD-1, the radial action distribution issufficiently clustered to locally recover the MW mass profile across the streamradial range within a 2 sigma confidence interval determined using a Fisherinformation approach. For streams with longer orbital periods and closeencounters with the LMC, e.g. Orphan-Chenab (OC), the radial actiondistribution disperses as the MW halo has deformed non-adiabatically. Hence,for OC streams generated in potentials that include a MW halo with anydeformations, action clustering methods will fail to recover the mass profilewithin a 2 sigma uncertainty. Finally, we investigate whether the clustering ofstream energies can provide similar constraints. Surprisingly, we find forOC-like streams, the recovered spherically averaged mass profiles demonstrateless sensitivity to the time-dependent deformations in the potential.

Action and energy clustering of stellar streams in deforming Milky Way dark matter haloes