HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen

Abstract We present confirmation of HD 143811 AB b, a substellar companion to spectroscopic binary HD 143811 AB through direct imaging with the Gemini Planet Imager (GPI) and Keck NIRC2. HD 143811 AB was observed as a part of the GPI Exoplanet Survey in 2016 and 2019 and is a member of the Sco-Cen star formation region. The exoplanet is detected ∼430 mas from the host star by GPI. With two GPI epochs and one from Keck/NIRC2 in 2022, we confirm through common proper motion analysis that the object is bound to its host star. We derive an orbit with a semimajor axis of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>6</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>14</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>32</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> au and eccentricity <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>0.23</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.16</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.24</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> . Spectral analysis of the GPI H -band spectrum and NIRC2 L′ photometry provides additional proof that this object is a substellar companion. We compare the spectrum of HD 143811 AB b to PHOENIX stellar models and Exo-Radioactive-Convective Equilibrium Model (REM) exoplanet atmosphere models and find that Exo-REM models provide the best fits to the data. From the Exo-REM models, we derive an effective temperature of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>104</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>132</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>178</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> K for the planet and translate the derived luminosity of the planet to a mass of 5.6 ± 1.1 M Jup assuming hot-start evolutionary models. HD 143811 AB b is the first directly imaged planet around a binary that is not on an ultrawide orbit. Future characterization of this object will shed light on the formation of planets around binary star systems.

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Journal
The Astrophysical Journal Letters
Published
2025-12-11
DOI
https://doi.org/10.3847/2041-8213/ae2007
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2
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Stellar, planetary, and galactic studies
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article
Field-Weighted Citation Impact
2.31
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article

HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen

Brenda C. Matthews, Adam C. Schneider, Christian Marois, William Roberson et al.
2 citations
The Astrophysical Journal Letters
Stellar, planetary, and galactic studies
2.31
article

HD 143811 AB b: A Directly Imaged Planet Orbiting a Spectroscopic Binary in Sco-Cen

Brenda C. Matthews, Adam C. Schneider, Christian Marois, William Roberson, Stephen J. Goodsell, Maxwell A. Millar‐Blanchaer, Gaspard Duchêne, Aniket Sanghi, Dmitry Savransky, Robert J. De Rosa, Vanessa P. Bailey, S. Mark Ammons, E. Nielsen, Adam J. R. W. Smith, Katherine B. Follette, Eugene Chiang, Patrick Ingraham, Thomas M. Esposito, Stanimir Metchev, Anand Sivaramakrishnan, Marshall D. Perrin, Paul Kalas, Pascale Hibon, Bruce Macintosh, Kimberly Ward-Duong, Schuyler Wolff, Jean-Baptiste Ruffio, J. Patience, Inseok Song, Abhijith Rajan, Bin Ren, Dimitri Mawet, Jeffrey Chilcote, Rebecca Oppenheimer, Julien Rameau, Anne E. Peck, Fredrik T. Rantakyrö, Quinn Konopacky, Travis Barman, Franck Marchis, Rémi Soummer, Jérôme Maîre, Lisa Poyneer, Alexandra Z. Greenbaum, J. Bulger, Sandrine Thomas, Michael P. Fitzgerald, Jerry W. Xuan, Michael C. Liu, Jason Wang, David W. Palmer, Laurent Pueyo, N. Jones, James R. Graham
article en
2 citations

Abstract

Abstract We present confirmation of HD 143811 AB b, a substellar companion to spectroscopic binary HD 143811 AB through direct imaging with the Gemini Planet Imager (GPI) and Keck NIRC2. HD 143811 AB was observed as a part of the GPI Exoplanet Survey in 2016 and 2019 and is a member of the Sco-Cen star formation region. The exoplanet is detected ∼430 mas from the host star by GPI. With two GPI epochs and one from Keck/NIRC2 in 2022, we confirm through common proper motion analysis that the object is bound to its host star. We derive an orbit with a semimajor axis of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>6</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>14</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>32</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> au and eccentricity <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>0.23</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.16</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.24</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> . Spectral analysis of the GPI H -band spectrum and NIRC2 L′ photometry provides additional proof that this object is a substellar companion. We compare the spectrum of HD 143811 AB b to PHOENIX stellar models and Exo-Radioactive-Convective Equilibrium Model (REM) exoplanet atmosphere models and find that Exo-REM models provide the best fits to the data. From the Exo-REM models, we derive an effective temperature of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>104</mml:mn> <mml:msubsup> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>132</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>178</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> K for the planet and translate the derived luminosity of the planet to a mass of 5.6 ± 1.1 M Jup assuming hot-start evolutionary models. HD 143811 AB b is the first directly imaged planet around a binary that is not on an ultrawide orbit. Future characterization of this object will shed light on the formation of planets around binary star systems.

The Astrophysical Journal LettersVol. 995(2)
New Mexico State University (US), University of Notre Dame (US), Northwestern University (US), California Institute of Technology (US), Herzberg Institute of Astrophysics (CA), Western University (CA), Lawrence Livermore National Laboratory (US), Centre National de la Recherche Scientifique (FR), Space Telescope Science Institute (US), Planetary Science Institute (US), University of Hawaii System (US), Jet Propulsion Laboratory (US), American Museum of Natural History (US), University of Arizona (US), University of California, Santa Barbara (US), University of California, Los Angeles (US), George Mason University (US), University of Georgia (US), Amherst College (US), University of California, Santa Cruz (US), Durham University (GB), Smith College (US), Cornell University (US), University of Victoria (CA), University of California San Diego (US), Gemini South Observatory (CL), Observatoire de la Côte d’Azur (FR), European Southern Observatory (CL), United States Naval Observatory (US), NSF-DOE Vera C. Rubin Observatory (CL), Infrared Processing and Analysis Center (US), Arizona State University (US), Université de Montréal (CA), Search for Extraterrestrial Intelligence (US), Foundation for Research and Technology Hellas (GR), Université Grenoble Alpes (FR), University of California, Berkeley (US)
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Stellar, planetary, and galactic studies
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