The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system

A. L. Maire, A. J. Skemer, Philip M Hinz, S. Desidera, S. Esposito, R. Gratton, F. Marzari, M. F. Skrutskie, B. A. Biller, D. Defrère, V. P. Bailey, J. M. Leisenring, Daniel Apai, M. Bonnefoy, W. Brandner, E. Buenzli, R. U. Claudi, Laird M Close, J. R. Crepp, R. J. De RosaJoshua A Eisner, J. J. Fortney, T. Henning, K. H. Hofmann, T. G. Kopytova, J. R. Males, D. Mesa, K. M. Morzinski, A. Oza, J. Patience, E. Pinna, A. Rajan, D. Schertl, J. E. Schlieder, K. Y L Su, A. Vaz, K. Ward-Duong, G. Weigelt, C. E. Woodward

Research output: Contribution to journalArticle

12 Citations (Scopus)

Abstract

Context. Astrometric monitoring of directly imaged exoplanets allows the study of their orbital parameters and system architectures. Because most directly imaged planets have long orbital periods (>20 AU), accurate astrometry is challenging when based on data acquired on timescales of a few years and usually with different instruments. The LMIRCam camera on the Large Binocular Telescope is being used for the LBT Exozodi Exoplanet Common Hunt (LEECH) survey to search for and characterize young and adolescent exoplanets in L′ band (3.8 μm), including their system architectures. Aims. We first aim to provide a good astrometric calibration of LMIRCam. Then, we derive new astrometry, test the predictions of the orbital model of 8:4:2:1 mean motion resonance proposed for the system, and perform new orbital fitting of the HR 8799 bcde planets. We also present deep limits on a putative fifth planet inside the known planets. Methods. We use observations of HR 8799 and the Θ<sup>1</sup> Ori C field obtained during the same run in October 2013. Results. We first characterize the distortion of LMIRCam. We determine a platescale and a true north orientation for the images of 10.707±0.012 mas/pix and -0.430±0.076°, respectively. The errors on the platescale and true north orientation translate into astrometric accuracies at a separation of 1′′ of 1.1 mas and 1.3 mas, respectively. The measurements for all planets agree within 3σ with a predicted ephemeris. The orbital fitting based on the new astrometric measurements favors an architecture for the planetary system based on 8:4:2:1 mean motion resonance. The detection limits allow us to exclude a fifth planet slightly brighter or more massive than HR 8799 b at the location of the 2:1 resonance with HR 8799 e (∼9.5 AU) and about twice as bright as HR 8799 cde at the location of the 3:1 resonance with HR 8799 e (∼7.5 AU).

Original languageEnglish (US)
JournalAstronomy and Astrophysics
Volume576
DOIs
StatePublished - Apr 1 2015

Fingerprint

extrasolar planets
planets
planet
orbitals
astrometry
planetary systems
ultrahigh frequencies
cameras
telescopes
calibration
timescale
monitoring
prediction
predictions

Keywords

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

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system. / Maire, A. L.; Skemer, A. J.; Hinz, Philip M; Desidera, S.; Esposito, S.; Gratton, R.; Marzari, F.; Skrutskie, M. F.; Biller, B. A.; Defrère, D.; Bailey, V. P.; Leisenring, J. M.; Apai, Daniel; Bonnefoy, M.; Brandner, W.; Buenzli, E.; Claudi, R. U.; Close, Laird M; Crepp, J. R.; De Rosa, R. J.; Eisner, Joshua A; Fortney, J. J.; Henning, T.; Hofmann, K. H.; Kopytova, T. G.; Males, J. R.; Mesa, D.; Morzinski, K. M.; Oza, A.; Patience, J.; Pinna, E.; Rajan, A.; Schertl, D.; Schlieder, J. E.; Su, K. Y L; Vaz, A.; Ward-Duong, K.; Weigelt, G.; Woodward, C. E.

In: Astronomy and Astrophysics, Vol. 576, 01.04.2015.

Research output: Contribution to journalArticle

Maire, AL, Skemer, AJ, Hinz, PM, Desidera, S, Esposito, S, Gratton, R, Marzari, F, Skrutskie, MF, Biller, BA, Defrère, D, Bailey, VP, Leisenring, JM, Apai, D, Bonnefoy, M, Brandner, W, Buenzli, E, Claudi, RU, Close, LM, Crepp, JR, De Rosa, RJ, Eisner, JA, Fortney, JJ, Henning, T, Hofmann, KH, Kopytova, TG, Males, JR, Mesa, D, Morzinski, KM, Oza, A, Patience, J, Pinna, E, Rajan, A, Schertl, D, Schlieder, JE, Su, KYL, Vaz, A, Ward-Duong, K, Weigelt, G & Woodward, CE 2015, 'The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system', Astronomy and Astrophysics, vol. 576. https://doi.org/10.1051/0004-6361/201425185
Maire, A. L. ; Skemer, A. J. ; Hinz, Philip M ; Desidera, S. ; Esposito, S. ; Gratton, R. ; Marzari, F. ; Skrutskie, M. F. ; Biller, B. A. ; Defrère, D. ; Bailey, V. P. ; Leisenring, J. M. ; Apai, Daniel ; Bonnefoy, M. ; Brandner, W. ; Buenzli, E. ; Claudi, R. U. ; Close, Laird M ; Crepp, J. R. ; De Rosa, R. J. ; Eisner, Joshua A ; Fortney, J. J. ; Henning, T. ; Hofmann, K. H. ; Kopytova, T. G. ; Males, J. R. ; Mesa, D. ; Morzinski, K. M. ; Oza, A. ; Patience, J. ; Pinna, E. ; Rajan, A. ; Schertl, D. ; Schlieder, J. E. ; Su, K. Y L ; Vaz, A. ; Ward-Duong, K. ; Weigelt, G. ; Woodward, C. E. / The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system. In: Astronomy and Astrophysics. 2015 ; Vol. 576.
@article{fecf3efb389e459cb39291c85d3b181d,
title = "The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system",
abstract = "Context. Astrometric monitoring of directly imaged exoplanets allows the study of their orbital parameters and system architectures. Because most directly imaged planets have long orbital periods (>20 AU), accurate astrometry is challenging when based on data acquired on timescales of a few years and usually with different instruments. The LMIRCam camera on the Large Binocular Telescope is being used for the LBT Exozodi Exoplanet Common Hunt (LEECH) survey to search for and characterize young and adolescent exoplanets in L′ band (3.8 μm), including their system architectures. Aims. We first aim to provide a good astrometric calibration of LMIRCam. Then, we derive new astrometry, test the predictions of the orbital model of 8:4:2:1 mean motion resonance proposed for the system, and perform new orbital fitting of the HR 8799 bcde planets. We also present deep limits on a putative fifth planet inside the known planets. Methods. We use observations of HR 8799 and the Θ1 Ori C field obtained during the same run in October 2013. Results. We first characterize the distortion of LMIRCam. We determine a platescale and a true north orientation for the images of 10.707±0.012 mas/pix and -0.430±0.076°, respectively. The errors on the platescale and true north orientation translate into astrometric accuracies at a separation of 1′′ of 1.1 mas and 1.3 mas, respectively. The measurements for all planets agree within 3σ with a predicted ephemeris. The orbital fitting based on the new astrometric measurements favors an architecture for the planetary system based on 8:4:2:1 mean motion resonance. The detection limits allow us to exclude a fifth planet slightly brighter or more massive than HR 8799 b at the location of the 2:1 resonance with HR 8799 e (∼9.5 AU) and about twice as bright as HR 8799 cde at the location of the 3:1 resonance with HR 8799 e (∼7.5 AU).",
keywords = "Instrumentation: adaptive optics, Methods: data analysis, Planetary systems, Planets and satellites: dynamical evolution and stability, Stars: individual: HR 8799, Techniques: high angular resolution",
author = "Maire, {A. L.} and Skemer, {A. J.} and Hinz, {Philip M} and S. Desidera and S. Esposito and R. Gratton and F. Marzari and Skrutskie, {M. F.} and Biller, {B. A.} and D. Defr{\`e}re and Bailey, {V. P.} and Leisenring, {J. M.} and Daniel Apai and M. Bonnefoy and W. Brandner and E. Buenzli and Claudi, {R. U.} and Close, {Laird M} and Crepp, {J. R.} and {De Rosa}, {R. J.} and Eisner, {Joshua A} and Fortney, {J. J.} and T. Henning and Hofmann, {K. H.} and Kopytova, {T. G.} and Males, {J. R.} and D. Mesa and Morzinski, {K. M.} and A. Oza and J. Patience and E. Pinna and A. Rajan and D. Schertl and Schlieder, {J. E.} and Su, {K. Y L} and A. Vaz and K. Ward-Duong and G. Weigelt and Woodward, {C. E.}",
year = "2015",
month = "4",
day = "1",
doi = "10.1051/0004-6361/201425185",
language = "English (US)",
volume = "576",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",

}

TY - JOUR

T1 - The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system

AU - Maire, A. L.

AU - Skemer, A. J.

AU - Hinz, Philip M

AU - Desidera, S.

AU - Esposito, S.

AU - Gratton, R.

AU - Marzari, F.

AU - Skrutskie, M. F.

AU - Biller, B. A.

AU - Defrère, D.

AU - Bailey, V. P.

AU - Leisenring, J. M.

AU - Apai, Daniel

AU - Bonnefoy, M.

AU - Brandner, W.

AU - Buenzli, E.

AU - Claudi, R. U.

AU - Close, Laird M

AU - Crepp, J. R.

AU - De Rosa, R. J.

AU - Eisner, Joshua A

AU - Fortney, J. J.

AU - Henning, T.

AU - Hofmann, K. H.

AU - Kopytova, T. G.

AU - Males, J. R.

AU - Mesa, D.

AU - Morzinski, K. M.

AU - Oza, A.

AU - Patience, J.

AU - Pinna, E.

AU - Rajan, A.

AU - Schertl, D.

AU - Schlieder, J. E.

AU - Su, K. Y L

AU - Vaz, A.

AU - Ward-Duong, K.

AU - Weigelt, G.

AU - Woodward, C. E.

PY - 2015/4/1

Y1 - 2015/4/1

N2 - Context. Astrometric monitoring of directly imaged exoplanets allows the study of their orbital parameters and system architectures. Because most directly imaged planets have long orbital periods (>20 AU), accurate astrometry is challenging when based on data acquired on timescales of a few years and usually with different instruments. The LMIRCam camera on the Large Binocular Telescope is being used for the LBT Exozodi Exoplanet Common Hunt (LEECH) survey to search for and characterize young and adolescent exoplanets in L′ band (3.8 μm), including their system architectures. Aims. We first aim to provide a good astrometric calibration of LMIRCam. Then, we derive new astrometry, test the predictions of the orbital model of 8:4:2:1 mean motion resonance proposed for the system, and perform new orbital fitting of the HR 8799 bcde planets. We also present deep limits on a putative fifth planet inside the known planets. Methods. We use observations of HR 8799 and the Θ1 Ori C field obtained during the same run in October 2013. Results. We first characterize the distortion of LMIRCam. We determine a platescale and a true north orientation for the images of 10.707±0.012 mas/pix and -0.430±0.076°, respectively. The errors on the platescale and true north orientation translate into astrometric accuracies at a separation of 1′′ of 1.1 mas and 1.3 mas, respectively. The measurements for all planets agree within 3σ with a predicted ephemeris. The orbital fitting based on the new astrometric measurements favors an architecture for the planetary system based on 8:4:2:1 mean motion resonance. The detection limits allow us to exclude a fifth planet slightly brighter or more massive than HR 8799 b at the location of the 2:1 resonance with HR 8799 e (∼9.5 AU) and about twice as bright as HR 8799 cde at the location of the 3:1 resonance with HR 8799 e (∼7.5 AU).

AB - Context. Astrometric monitoring of directly imaged exoplanets allows the study of their orbital parameters and system architectures. Because most directly imaged planets have long orbital periods (>20 AU), accurate astrometry is challenging when based on data acquired on timescales of a few years and usually with different instruments. The LMIRCam camera on the Large Binocular Telescope is being used for the LBT Exozodi Exoplanet Common Hunt (LEECH) survey to search for and characterize young and adolescent exoplanets in L′ band (3.8 μm), including their system architectures. Aims. We first aim to provide a good astrometric calibration of LMIRCam. Then, we derive new astrometry, test the predictions of the orbital model of 8:4:2:1 mean motion resonance proposed for the system, and perform new orbital fitting of the HR 8799 bcde planets. We also present deep limits on a putative fifth planet inside the known planets. Methods. We use observations of HR 8799 and the Θ1 Ori C field obtained during the same run in October 2013. Results. We first characterize the distortion of LMIRCam. We determine a platescale and a true north orientation for the images of 10.707±0.012 mas/pix and -0.430±0.076°, respectively. The errors on the platescale and true north orientation translate into astrometric accuracies at a separation of 1′′ of 1.1 mas and 1.3 mas, respectively. The measurements for all planets agree within 3σ with a predicted ephemeris. The orbital fitting based on the new astrometric measurements favors an architecture for the planetary system based on 8:4:2:1 mean motion resonance. The detection limits allow us to exclude a fifth planet slightly brighter or more massive than HR 8799 b at the location of the 2:1 resonance with HR 8799 e (∼9.5 AU) and about twice as bright as HR 8799 cde at the location of the 3:1 resonance with HR 8799 e (∼7.5 AU).

KW - Instrumentation: adaptive optics

KW - Methods: data analysis

KW - Planetary systems

KW - Planets and satellites: dynamical evolution and stability

KW - Stars: individual: HR 8799

KW - Techniques: high angular resolution

UR - http://www.scopus.com/inward/record.url?scp=84928347309&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84928347309&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201425185

DO - 10.1051/0004-6361/201425185

M3 - Article

AN - SCOPUS:84928347309

VL - 576

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

ER -