Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars
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2024
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| author | Stefansson, Gudmundur Mahadevan, Suvrath Winn, Joshua Marcussen, Marcus Kanodia, Shubham Albrecht, Simon Fitzmaurice, Evan Mikulskitye, One Cañas, Caleb Espinoza-Retamal, Juan Ignacio Zwart, Yiri Krolikowski, Daniel Hotnisky, Andrew Robertson, Paul Alvarado-Montes, Jaime A. Bender, Chad Blake, Cullen Callingham, Joe Cochran, William Delamer, Megan Diddams, Scott Dong, Jiayin Fernandes, Rachel Giovanazzi, Mark Halverson, Samuel Libby-Roberts, Jessica Logsdon, Sarah E McElwain, Michael Ninan, Joe Rajagopal, Jayadev Reji, Varghese Roy, Arpita Schwab, Christian Wright, Jason |
| author_facet | Stefansson, Gudmundur Mahadevan, Suvrath Winn, Joshua Marcussen, Marcus Kanodia, Shubham Albrecht, Simon Fitzmaurice, Evan Mikulskitye, One Cañas, Caleb Espinoza-Retamal, Juan Ignacio Zwart, Yiri Krolikowski, Daniel Hotnisky, Andrew Robertson, Paul Alvarado-Montes, Jaime A. Bender, Chad Blake, Cullen Callingham, Joe Cochran, William Delamer, Megan Diddams, Scott Dong, Jiayin Fernandes, Rachel Giovanazzi, Mark Halverson, Samuel Libby-Roberts, Jessica Logsdon, Sarah E McElwain, Michael Ninan, Joe Rajagopal, Jayadev Reji, Varghese Roy, Arpita Schwab, Christian Wright, Jason |
| contents | Gaia astrometry of nearby stars is precise enough to detect the tiny displacements induced by substellar companions, but radial velocity data are needed for definitive confirmation. Here we present radial velocity follow-up observations of 28 M and K stars with candidate astrometric substellar companions, which led to the confirmation of two systems, Gaia-4b and Gaia-5b, and the refutation of 21 systems as stellar binaries. Gaia-4b is a massive planet ($M = 11.8 \pm 0.7 \:\mathrm{M_J}$) in a $P = 571.3 \pm 1.4\:\mathrm{day}$ orbit with a projected semi-major axis $a_0=0.312 \pm 0.040\:\mathrm{mas}$ orbiting a $0.644 \pm 0.02 \:\mathrm{M_\odot}$ star. Gaia-5b is a brown dwarf ($M = 20.9 \pm 0.5\:\mathrm{M_J}$) in a $P = 358.58 \pm 0.19\:\mathrm{days}$ eccentric $e=0.6412 \pm 0.0027$ orbit with a projected angular semi-major axis of $a_0 = 0.947 \pm 0.038\:\mathrm{mas}$ around a $0.34 \pm 0.03 \mathrm{M_\odot}$ star. Gaia-4b is one of the first exoplanets discovered via the astrometric technique, and is one of the most massive planets known to orbit a low-mass star. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_05654 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars Stefansson, Gudmundur Mahadevan, Suvrath Winn, Joshua Marcussen, Marcus Kanodia, Shubham Albrecht, Simon Fitzmaurice, Evan Mikulskitye, One Cañas, Caleb Espinoza-Retamal, Juan Ignacio Zwart, Yiri Krolikowski, Daniel Hotnisky, Andrew Robertson, Paul Alvarado-Montes, Jaime A. Bender, Chad Blake, Cullen Callingham, Joe Cochran, William Delamer, Megan Diddams, Scott Dong, Jiayin Fernandes, Rachel Giovanazzi, Mark Halverson, Samuel Libby-Roberts, Jessica Logsdon, Sarah E McElwain, Michael Ninan, Joe Rajagopal, Jayadev Reji, Varghese Roy, Arpita Schwab, Christian Wright, Jason Earth and Planetary Astrophysics Instrumentation and Methods for Astrophysics Solar and Stellar Astrophysics Gaia astrometry of nearby stars is precise enough to detect the tiny displacements induced by substellar companions, but radial velocity data are needed for definitive confirmation. Here we present radial velocity follow-up observations of 28 M and K stars with candidate astrometric substellar companions, which led to the confirmation of two systems, Gaia-4b and Gaia-5b, and the refutation of 21 systems as stellar binaries. Gaia-4b is a massive planet ($M = 11.8 \pm 0.7 \:\mathrm{M_J}$) in a $P = 571.3 \pm 1.4\:\mathrm{day}$ orbit with a projected semi-major axis $a_0=0.312 \pm 0.040\:\mathrm{mas}$ orbiting a $0.644 \pm 0.02 \:\mathrm{M_\odot}$ star. Gaia-5b is a brown dwarf ($M = 20.9 \pm 0.5\:\mathrm{M_J}$) in a $P = 358.58 \pm 0.19\:\mathrm{days}$ eccentric $e=0.6412 \pm 0.0027$ orbit with a projected angular semi-major axis of $a_0 = 0.947 \pm 0.038\:\mathrm{mas}$ around a $0.34 \pm 0.03 \mathrm{M_\odot}$ star. Gaia-4b is one of the first exoplanets discovered via the astrometric technique, and is one of the most massive planets known to orbit a low-mass star. |
| title | Gaia-4b and 5b: Radial Velocity Confirmation of Gaia Astrometric Orbital Solutions Reveal a Massive Planet and a Brown Dwarf Orbiting Low-mass Stars |
| topic | Earth and Planetary Astrophysics Instrumentation and Methods for Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2410.05654 |