Satellite group infall into the Milky Way: Exploring the Crater-Leo case with new HST proper motions

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Table 5.

Pericentre (r_peri), apocentre (r_apo), and eccentricity (e) derived from Gaia DR2 proper motions from Fritz et al. (2018).

Object	r_peri (kpc)	r_apo (kpc)	e
Leo II	$67_{- 52}^{+ 154}$ $67^{+154}_{-52}$	$248_{- 26}^{+ 613}$ $248^{+613}_{-26}$	$0 . 67_{- 0.39}^{+ 0.26}$ $0.67^{+0.26}_{-0.39}$
Leo IV	$153_{- 87}^{+ 8}$ $153^{+8}_{-87}$	$26071_{- 25908}^{+ 46619}$ $26071^{+46619}_{-25908}$	$0 . 989_{- 0.56}^{+ 0.007}$ $0.989^{+0.007}_{-0.56}$
Leo V	$168_{- 104}^{+ 12}$ $168^{+12}_{-104}$	$27704_{- 27495}^{+ 45671}$ $27704^{+45671}_{-27495}$	$0 . 988_{- 0.46}^{+ 0.007}$ $0.988^{+0.007}_{-0.46}$
Crater 1	$81_{- 70}^{+ 65}$ $81^{+65}_{-70}$	$159_{- 16}^{+ 7932}$ $159^{+7932}_{-16}$	$0 . 68_{- 0.43}^{+ 0.3}$ $0.68^{+0.3}_{-0.43}$

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