  Jupiter Trojans (JTs) librate about the Lagrangian stationary centers L4 and
L5 associated with this planet on a typically small-eccentricity and
moderate-inclination heliocentric orbits. The physical and orbital properties
of JTs provide important clues about the dynamical evolution of the giant
planets in the early Solar System, as well as populations of planetesimals in
their source regions. Here we use decade long observations from the Catalina
Sky Survey (station G96) to determine the bias-corrected orbital and magnitude
distributions of JTs. We distinguish the background JT population, filling
smoothly the long-term stable orbital zone about L4 and L5 points, and
collisional families. We find that the cumulative magnitude distribution of JTs
(the background population in our case) has a steep slope for $H\leq 9$,
followed with a moderately shallow slope till $H\simeq 14.5$, beyond which the
distribution becomes even shallower. At $H=15$ we find a local power-law
exponent $0.38\pm 0.01$. We confirm the asymmetry between the magnitude limited
background populations in L4 and L5 clouds characterized by a ratio $1.45\pm
0.05$ for $H<15$. Our analysis suggests an asymmetry in the inclination
distribution of JTs, with the L4 population being tighter and the L5 population
being broader. We also provide a new catalog of the synthetic proper elements
for JTs with an updated identification of statistically robust families (9 at
L4, and 4 at L5). The previously known Ennomos family is found to consist of
two, overlapping Deiphobus and Ennomos families.
