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We have performed H and KS band
observations of the planetary system around HR 8799 using the new AO system at the Large
Binocular Telescope and the PISCES Camera. The excellent instrument performance (Strehl
ratios up to 80% in H band) enabled the detection of the innermost
planet, HR 8799e, at H band for the first time. The
H and KS magnitudes of HR 8799e are similar
to those of planets c and d, with planet
e being slightly brighter. Therefore, HR 8799e is
likely slightly more massive than c and d. We also
explored possible orbital configurations and their orbital stability. We confirm that the
orbits of planets b, c and e are
consistent with being circular and coplanar; planet d should have either
an orbital eccentricity of about 0.1 or be non-coplanar with respect to b
and c. Planet e can not be in circular and coplanar
orbit in a 4:2:1 mean motion resonances with c and d,
while coplanar and circular orbits are allowed for a 5:2 resonance. The analysis of
dynamical stability shows that the system is highly unstable or chaotic when planetary
masses of about 5 MJ for b and
7 MJ for the other planets are adopted. Significant regions
of dynamical stability for timescales of tens of Myr are found when adopting planetary
masses of about 3.5, 5, 5, and 5 MJ for
HR 8799b, c, d, and
e respectively. These masses are below the current estimates based on
the stellar age (30 Myr) and theoretical models of substellar objects
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