TY - JOUR
T1 - LBT observations of the HR8799 planetary system â†
T2 - First detection of HR8799e in H band
AU - Esposito, S.
AU - Mesa, D.
AU - Skemer, A.
AU - Arcidiacono, C.
AU - Claudi, R. U.
AU - Desidera, S.
AU - Gratton, R.
AU - Mannucci, F.
AU - Marzari, F.
AU - Masciadri, E.
AU - Close, L.
AU - Hinz, P.
AU - Kulesa, C.
AU - McCarthy, D.
AU - Males, J.
AU - Agapito, G.
AU - Argomedo, J.
AU - Boutsia, K.
AU - Briguglio, R.
AU - Brusa, G.
AU - Busoni, L.
AU - Cresci, G.
AU - Fini, L.
AU - Fontana, A.
AU - Guerra, J. C.
AU - Hill, J. M.
AU - Miller, D.
AU - Paris, D.
AU - Pinna, E.
AU - Puglisi, A.
AU - Quiros-Pacheco, F.
AU - Riccardi, A.
AU - Stefanini, P.
AU - Testa, V.
AU - Xompero, M.
AU - Woodward, C.
PY - 2012
Y1 - 2012
N2 - We have performed H and KS band observations of the planetary system around HR8799 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, HR8799e, at Hband for the first time. The H and KS magnitudes of HR8799e are similar to those of planets c and d, with planet e being slightly brighter. Therefore, HR8799e 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 5M J for b and 7MJ for the other planets are adopted. Significant regions of dynamical stability for timescales of tens ofMyr are found when adopting planetary masses of about 3.5, 5, 5, and 5 MJ for HR8799b, c, d, and e respectively. These masses are below the current estimates based on the stellar age (30Myr) and theoretical models of substellar objects.
AB - We have performed H and KS band observations of the planetary system around HR8799 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, HR8799e, at Hband for the first time. The H and KS magnitudes of HR8799e are similar to those of planets c and d, with planet e being slightly brighter. Therefore, HR8799e 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 5M J for b and 7MJ for the other planets are adopted. Significant regions of dynamical stability for timescales of tens ofMyr are found when adopting planetary masses of about 3.5, 5, 5, and 5 MJ for HR8799b, c, d, and e respectively. These masses are below the current estimates based on the stellar age (30Myr) and theoretical models of substellar objects.
KW - Instrumentation: adaptive optics
KW - Planetary systems
KW - Planets and satellites: dynamical evolution and stability
KW - Planets and satellites: physical evolution
KW - Stars: individual: HR 8799
KW - Techniques: high angular resolution
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U2 - 10.1051/0004-6361/201219212
DO - 10.1051/0004-6361/201219212
M3 - Article
AN - SCOPUS:84871330392
SN - 0004-6361
VL - 549
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A52
ER -