Is the core-cusp problem a matter of perspective: Jeans Anisotropic Modeling against numerical simulations by Wenting Wang et al. on Monday 21 November

Mock member stars for 28 dwarf galaxies are constructed from the cosmological

Auriga simulation, which reflect the dynamical status of realistic stellar

tracers. The axis-symmetric Jeans Anisotropic Multi-Gaussian Expansion (JAM)

modeling is applied to 6,000 star particles for each system, to recover the

underlying matter distribution. The stellar or dark matter component

individually is poorly recovered, but the total profile is constrained more

reasonably. The mass within the half-mass radius of tracers is recovered the

tightest, and the mass between 200 and 300 pc, $M(200-300\mathrm{pc})$, is

constrained ensemble unbiasedly, with a scatter of 0.167 dex. If using 2,000

particles and only line-of-sight velocities with typical errors, the scatter in

$M(200-300\mathrm{pc})$ is increased by $\sim$50%. Quiescent Sagittarius

dSph-like systems and star-forming systems with strong outflows show distinct

features, with $M(200-300\mathrm{pc})$ mostly under-estimated for the former,

and likely over-estimated for the latter. The biases correlate with the

dynamical status, which is a result of contraction motions due to tidal effects

in quiescent systems or galactic winds in star-forming systems, driving them

out of equilibrium. After including Gaia DR3 proper motion errors, we find

proper motions can be as useful as line-of-sight velocities for nearby systems

at $<\sim$60 kpc. By extrapolating the actual density profiles and the

dynamical constraints down to scales below the resolution, we find the mass

within 150 pc can be constrained ensemble unbiasedly, with a scatter of

$\sim$0.255 dex. In the end, we show that the contraction of member stars in

nearby systems is detectable based on Gaia DR3 proper motion errors.

arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2206.12121v2