Spectroscopic Analysis of Milky Way Outer Halo Satellites: Aquarius II and Boötes II

In this paper we present a chemical and kinematic analysis of two ultra-faint dwarf galaxies (UFDs), Aquarius II (Aqu~II) \text{Bo\"{o}tes II} (Boo~II), using Magellan/IMACS spectroscopy. We the largest sample member stars for Boo~II (12), red-giant-branch members with metallicity measurements Aqu~II (8). both UFDs, over 80\% targets selected based on $Gaia$ proper motions turned out to be spectroscopic members. order maximize accuracy stellar measurements, remove identified binary RR Lyrae variables. For measure systemic velocity $-65.3 \pm 1.8$ km s$^{-1}$ [Fe/H] = $-2.57^{+0.17}_{-0.17}$. When compared previous these values display $\sim 6$ difference in radial decrease 0.27 dex metallicity. Similarly Boo~II, $-130.4^{+1.4}_{-1.1}$ s$^{-1}$, more than 10 different from literature, almost 1 smaller at $-2.71^{+0.11}_{-0.10}$, dispersion 3 times $\sigma_{v_{\rm hel}} 2.9^{+1.6}_{-1.2}$ s$^{-1}$. Additionally, derive motion parameters model orbits UFDs. Finally, highlight extremely dark matter dominated nature compute J-factor aid searches annihilation. Despite small size close proximity it is an intermediate target indirect detection annihilation due its low corresponding density.