  Planetary nebulae (PNe) are excellent tracers of the metal-poor haloes of
nearby early-type galaxies. They are commonly used to trace spatial
distribution and kinematics of the halo and intracluster light at distances of
up to 100 Mpcs. The results on the early-type galaxy M105 in the Leo I group
represent a benchmark for the quantitative analysis of halo and intragroup
light. Since the Leo I group lies at just a 10 Mpc distance, it is at the ideal
location to compare results from resolved stellar populations with the
homogeneous constraints over a much larger field of view from the PN
populations. In M105, we have -- for the first time -- established a direct
link between the presence of a metal-poor halo as traced by resolved red-giant
branch stars and a PN population with a high specific frequency
($\alpha$-parameter). This confirms our inferences that the high
$\alpha$-parameter PN population in the outer halo of M49 in the Virgo Cluster
traces the metal-poor halo and intra-group light.
