LBT observations of the HR8799 planetary system â†: First detection of HR8799e in H band

S. Esposito, D. Mesa, A. Skemer, C. Arcidiacono, R. U. Claudi, S. Desidera, R. Gratton, F. Mannucci, F. Marzari, E. Masciadri, Laird M Close, Philip M Hinz, C. Kulesa, Donald W Mccarthy, J. Males, G. Agapito, J. Argomedo, K. Boutsia, R. Briguglio, G. BrusaL. Busoni, G. Cresci, L. Fini, A. Fontana, J. C. Guerra, J. M. Hill, D. Miller, D. Paris, E. Pinna, A. Puglisi, F. Quiros-Pacheco, A. Riccardi, P. Stefanini, V. Testa, M. Xompero, C. Woodward

Research output: Contribution to journalArticle

19 Citations (Scopus)

Abstract

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.

Original languageEnglish (US)
Article numberA52
JournalAstronomy and Astrophysics
Volume549
DOIs
StatePublished - 2012

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planetary systems
planets
planet
planetary mass
circular orbits
orbits
orbitals
detection
eccentricity
cameras
telescopes
timescale
estimates
configurations

Keywords

  • Instrumentation: adaptive optics
  • Planetary systems
  • Planets and satellites: dynamical evolution and stability
  • Planets and satellites: physical evolution
  • Stars: individual: HR 8799
  • Techniques: high angular resolution

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Esposito, S., Mesa, D., Skemer, A., Arcidiacono, C., Claudi, R. U., Desidera, S., ... Woodward, C. (2012). LBT observations of the HR8799 planetary system â†: First detection of HR8799e in H band. Astronomy and Astrophysics, 549, [A52]. https://doi.org/10.1051/0004-6361/201219212

LBT observations of the HR8799 planetary system ↠: First detection of HR8799e in H band. / Esposito, S.; Mesa, D.; Skemer, A.; Arcidiacono, C.; Claudi, R. U.; Desidera, S.; Gratton, R.; Mannucci, F.; Marzari, F.; Masciadri, E.; Close, Laird M; Hinz, Philip M; Kulesa, C.; Mccarthy, Donald W; Males, J.; Agapito, G.; Argomedo, J.; Boutsia, K.; Briguglio, R.; Brusa, G.; Busoni, L.; Cresci, G.; Fini, L.; Fontana, A.; Guerra, J. C.; Hill, J. M.; Miller, D.; Paris, D.; Pinna, E.; Puglisi, A.; Quiros-Pacheco, F.; Riccardi, A.; Stefanini, P.; Testa, V.; Xompero, M.; Woodward, C.

In: Astronomy and Astrophysics, Vol. 549, A52, 2012.

Research output: Contribution to journalArticle

Esposito, S, Mesa, D, Skemer, A, Arcidiacono, C, Claudi, RU, Desidera, S, Gratton, R, Mannucci, F, Marzari, F, Masciadri, E, Close, LM, Hinz, PM, Kulesa, C, Mccarthy, DW, Males, J, Agapito, G, Argomedo, J, Boutsia, K, Briguglio, R, Brusa, G, Busoni, L, Cresci, G, Fini, L, Fontana, A, Guerra, JC, Hill, JM, Miller, D, Paris, D, Pinna, E, Puglisi, A, Quiros-Pacheco, F, Riccardi, A, Stefanini, P, Testa, V, Xompero, M & Woodward, C 2012, 'LBT observations of the HR8799 planetary system â†: First detection of HR8799e in H band', Astronomy and Astrophysics, vol. 549, A52. https://doi.org/10.1051/0004-6361/201219212
Esposito, S. ; Mesa, D. ; Skemer, A. ; Arcidiacono, C. ; Claudi, R. U. ; Desidera, S. ; Gratton, R. ; Mannucci, F. ; Marzari, F. ; Masciadri, E. ; Close, Laird M ; Hinz, Philip M ; Kulesa, C. ; Mccarthy, Donald W ; Males, J. ; Agapito, G. ; Argomedo, J. ; Boutsia, K. ; Briguglio, R. ; Brusa, G. ; Busoni, L. ; Cresci, G. ; Fini, L. ; Fontana, A. ; Guerra, J. C. ; Hill, J. M. ; Miller, D. ; Paris, D. ; Pinna, E. ; Puglisi, A. ; Quiros-Pacheco, F. ; Riccardi, A. ; Stefanini, P. ; Testa, V. ; Xompero, M. ; Woodward, C. / LBT observations of the HR8799 planetary system ↠: First detection of HR8799e in H band. In: Astronomy and Astrophysics. 2012 ; Vol. 549.
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title = "LBT observations of the HR8799 planetary system {\^a}†: First detection of HR8799e in H band",
abstract = "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.",
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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, Laird M

AU - Hinz, Philip M

AU - Kulesa, C.

AU - Mccarthy, Donald W

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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