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Title: Constraints on the architecture of the HD 95086 planetary system with the Gemini Planet Imager

Here, we present astrometric monitoring of the young exoplanet HD 95086 b obtained with the Gemini Planet Imager between 2013 and 2016. A small but significant position angle change is detected at constant separation; the orbital motion is confirmed with literature measurements. Efficient Monte Carlo techniques place preliminary constraints on the orbital parameters of HD 95086 b. With 68% confidence, a semimajor axis of $${61.7}_{-8.4}^{+20.7}$$ au and an inclination of $$153° {0}_{-13.5}^{+9.7}$$ are favored, with eccentricity less than 0.21. Under the assumption of a coplanar planet–disk system, the periastron of HD 95086 b is beyond 51 au with 68% confidence. Therefore, HD 95086 b cannot carve the entire gap inferred from the measured infrared excess in the SED of HD 95086. We use our sensitivity to additional planets to discuss specific scenarios presented in the literature to explain the geometry of the debris belts. We suggest that either two planets on moderately eccentric orbits or three to four planets with inhomogeneous masses and orbital properties are possible. As a result, the sensitivity to additional planetary companions within the observations presented in this study can be used to help further constrain future dynamical simulations of the planet–disk system.
Authors:
 [1] ;  [2] ;  [3] ;  [4] ;  [5] ;  [1] ;  [3] ; ORCiD logo [1] ; ORCiD logo [6] ; ORCiD logo [7] ;  [6] ;  [8] ; ORCiD logo [9] ; ORCiD logo [3] ;  [10] ; ORCiD logo [10] ;  [8] ; ORCiD logo [11] ; ORCiD logo [12] ; ORCiD logo [13] more »;  [13] ;  [5] ; ORCiD logo [14] ; ORCiD logo [3] ;  [5] ; ORCiD logo [15] ; ORCiD logo [16] ;  [17] ; ORCiD logo [18] ;  [19] ;  [20] ; ORCiD logo [20] ;  [21] ;  [17] « less
  1. Univ. de Montreal, Montreal, QC (Canada)
  2. SETI Institute, Mountain View, CA (United States); Stanford Univ., Stanford, CA (United States)
  3. Univ. of California, Berkeley, CA (United States)
  4. SETI Institute, Mountain View, CA (United States); Brown Univ., Providence, RI (United States)
  5. Arizona State Univ., Tempe, AZ (United States)
  6. Stanford Univ., Stanford, CA (United States)
  7. SETI Institute, Mountain View, CA (United States)
  8. Univ. of Toronto, Toronto, ON (Canada)
  9. Univ. of California, Berkeley, CA (United States); Univ. Grenoble Alpes/CNRS, Grenoble (France)
  10. Univ. of California, Los Angeles, CA (United States)
  11. Univ. of Victoria, Victoria, BC (Canada); National Research Council of Canada Herzberg, Victoria, BC (Canada)
  12. The Univ. of Western Ontario, London, ON (Canada); Stony Brook Univ., Stony Brook, NY (United States)
  13. Space Telescope Science Institute, Baltimore, MD (United States)
  14. Cornell Univ., Ithaca, NY (United States)
  15. Space Telescope Science Institute, Baltimore, MD (United States); Johns Hopkins Univ., Baltimore, MD (United States)
  16. Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
  17. European Southern Observatory, Santiago (Chile)
  18. Large Synoptic Survey Telescope, Tucson, AZ (United States)
  19. SETI Institute, Mountain View, CA (United States); Univ. of California, Berkeley, CA (United States)
  20. Univ. of Arizona, Tucson, AZ (United States)
  21. Gemini Observatory, La Serena (Chile)
Publication Date:
Report Number(s):
LLNL-JRNL-717744
Journal ID: ISSN 2041-8213
Grant/Contract Number:
AC52-07NA27344; AST-1518332; AST-1411868; AST-141378; NNX15AD95G/NEXSS; NNX15AC89G; NNX14AJ80G
Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal. Letters
Additional Journal Information:
Journal Volume: 822; Journal Issue: 2; Journal ID: ISSN 2041-8213
Publisher:
Institute of Physics (IOP)
Research Org:
Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Sponsoring Org:
USDOE; National Aeronautic and Space Administration (NASA); National Science Foundation (NSF)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; astrometry; planet; disk interactions; planetary systems; stars: individual (HD 95086)
OSTI Identifier:
1352122

Rameau, Julien, Nielsen, Eric L., De Rosa, Robert J., Blunt, Sarah C., Patience, Jenny, Doyon, René, Graham, James R., Lafrenière, David, Macintosh, Bruce, Marchis, Franck, Bailey, Vanessa, Chilcote, Jeffrey K., Duchene, Gaspard, Esposito, Thomas M., Hung, Li -Wei, Konopacky, Quinn M., Maire, Jérôme, Marois, Christian, Metchev, Stanimir, Perrin, Marshall D., Pueyo, Laurent, Rajan, Abhijith, Savransky, Dmitry, Wang, Jason J., Ward-Duong, Kimberly, Wolff, Schuyler G., Ammons, S. Mark, Hibon, Pascale, Ingraham, Patrick, Kalas, Paul, Morzinski, Katie M., Oppenheimer, Rebecca, Rantakyearö, Fredrik T., and Thomas, Sandrine. Constraints on the architecture of the HD 95086 planetary system with the Gemini Planet Imager. United States: N. p., Web. doi:10.3847/2041-8205/822/2/L29.
Rameau, Julien, Nielsen, Eric L., De Rosa, Robert J., Blunt, Sarah C., Patience, Jenny, Doyon, René, Graham, James R., Lafrenière, David, Macintosh, Bruce, Marchis, Franck, Bailey, Vanessa, Chilcote, Jeffrey K., Duchene, Gaspard, Esposito, Thomas M., Hung, Li -Wei, Konopacky, Quinn M., Maire, Jérôme, Marois, Christian, Metchev, Stanimir, Perrin, Marshall D., Pueyo, Laurent, Rajan, Abhijith, Savransky, Dmitry, Wang, Jason J., Ward-Duong, Kimberly, Wolff, Schuyler G., Ammons, S. Mark, Hibon, Pascale, Ingraham, Patrick, Kalas, Paul, Morzinski, Katie M., Oppenheimer, Rebecca, Rantakyearö, Fredrik T., & Thomas, Sandrine. Constraints on the architecture of the HD 95086 planetary system with the Gemini Planet Imager. United States. doi:10.3847/2041-8205/822/2/L29.
Rameau, Julien, Nielsen, Eric L., De Rosa, Robert J., Blunt, Sarah C., Patience, Jenny, Doyon, René, Graham, James R., Lafrenière, David, Macintosh, Bruce, Marchis, Franck, Bailey, Vanessa, Chilcote, Jeffrey K., Duchene, Gaspard, Esposito, Thomas M., Hung, Li -Wei, Konopacky, Quinn M., Maire, Jérôme, Marois, Christian, Metchev, Stanimir, Perrin, Marshall D., Pueyo, Laurent, Rajan, Abhijith, Savransky, Dmitry, Wang, Jason J., Ward-Duong, Kimberly, Wolff, Schuyler G., Ammons, S. Mark, Hibon, Pascale, Ingraham, Patrick, Kalas, Paul, Morzinski, Katie M., Oppenheimer, Rebecca, Rantakyearö, Fredrik T., and Thomas, Sandrine. 2016. "Constraints on the architecture of the HD 95086 planetary system with the Gemini Planet Imager". United States. doi:10.3847/2041-8205/822/2/L29. https://www.osti.gov/servlets/purl/1352122.
@article{osti_1352122,
title = {Constraints on the architecture of the HD 95086 planetary system with the Gemini Planet Imager},
author = {Rameau, Julien and Nielsen, Eric L. and De Rosa, Robert J. and Blunt, Sarah C. and Patience, Jenny and Doyon, René and Graham, James R. and Lafrenière, David and Macintosh, Bruce and Marchis, Franck and Bailey, Vanessa and Chilcote, Jeffrey K. and Duchene, Gaspard and Esposito, Thomas M. and Hung, Li -Wei and Konopacky, Quinn M. and Maire, Jérôme and Marois, Christian and Metchev, Stanimir and Perrin, Marshall D. and Pueyo, Laurent and Rajan, Abhijith and Savransky, Dmitry and Wang, Jason J. and Ward-Duong, Kimberly and Wolff, Schuyler G. and Ammons, S. Mark and Hibon, Pascale and Ingraham, Patrick and Kalas, Paul and Morzinski, Katie M. and Oppenheimer, Rebecca and Rantakyearö, Fredrik T. and Thomas, Sandrine},
abstractNote = {Here, we present astrometric monitoring of the young exoplanet HD 95086 b obtained with the Gemini Planet Imager between 2013 and 2016. A small but significant position angle change is detected at constant separation; the orbital motion is confirmed with literature measurements. Efficient Monte Carlo techniques place preliminary constraints on the orbital parameters of HD 95086 b. With 68% confidence, a semimajor axis of ${61.7}_{-8.4}^{+20.7}$ au and an inclination of $153° {0}_{-13.5}^{+9.7}$ are favored, with eccentricity less than 0.21. Under the assumption of a coplanar planet–disk system, the periastron of HD 95086 b is beyond 51 au with 68% confidence. Therefore, HD 95086 b cannot carve the entire gap inferred from the measured infrared excess in the SED of HD 95086. We use our sensitivity to additional planets to discuss specific scenarios presented in the literature to explain the geometry of the debris belts. We suggest that either two planets on moderately eccentric orbits or three to four planets with inhomogeneous masses and orbital properties are possible. As a result, the sensitivity to additional planetary companions within the observations presented in this study can be used to help further constrain future dynamical simulations of the planet–disk system.},
doi = {10.3847/2041-8205/822/2/L29},
journal = {The Astrophysical Journal. Letters},
number = 2,
volume = 822,
place = {United States},
year = {2016},
month = {5}
}