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Transits of Known Planets Orbiting a Naked-Eye Star | | Stephen R. Kane
; Selçuk Yalçınkaya
; Hugh P. Osborn
; Paul A. Dalba
; Louise D. Nielsen
; Andrew Vanderburg
; Teo Močnik
; Natalie R. Hinkel
; Colby Ostberg
; Ekrem Murat Esmer
; Stéphane Udry
; Tara Fetherolf
; Özgür Baştürk
; George R. Ricker
; Roland Vanderspek
; David W. Latham
; Sara Seager
; Joshua N. Winn
; Jon M. Jenkins
; Romain Allart
; Jeremy Bailey
; Jacob L. Bean
; Francois Bouchy
; R. Paul Butler
; Tiago L. Campante
; Brad D. Carter
; Tansu Daylan
; Magali Deleuil
; Rodrigo F. Diaz
; Xavier Dumusque
; David Ehrenreich
; Jonathan Horner
; Andrew W. Howard
; Howard Isaacson
; Hugh R.A. Jones
; Martti H. Kristiansen
; Christophe Lovis
; Geoffrey W. Marcy
; Maxime Marmier
; Simon J. O'Toole
; Francesco Pepe
; Darin Ragozzine
; Damien Ségransan
; C.G. Tinney
; Margaret C. Turnbull
; Robert A. Wittenmyer
; Duncan J. Wright
; Jason T. Wright
; | | Date: |
21 Jul 2020 | | Abstract: | Some of the most scientifically valuable transiting planets are those that
were already known from radial velocity (RV) surveys. This is primarily because
their orbits are well characterized and they preferentially orbit bright stars
that are the targets of RV surveys. The Transiting Exoplanet Survey Satellite
({it TESS}) provides an opportunity to survey most of the known exoplanet
systems in a systematic fashion to detect possible transits of their planets.
HD~136352 (Nu$^2$~Lupi) is a naked-eye ($V = 5.78$) G-type main-sequence star
that was discovered to host three planets with orbital periods of 11.6, 27.6,
and 108.1 days via RV monitoring with the HARPS spectrograph. We present the
detection and characterization of transits for the two inner planets of the
HD~136352 system, revealing radii of $1.482^{+0.058}_{-0.056}$~$R_oplus$ and
$2.608^{+0.078}_{-0.077}$~$R_oplus$ for planets b and c, respectively. We
combine new HARPS observations with RV data from Keck/HIRES and the AAT, along
with {it TESS} photometry from Sector 12, to perform a complete analysis of
the system parameters. The combined data analysis results in extracted bulk
density values of $
ho_b = 7.8^{+1.2}_{-1.1}$~gcm$^{-3}$ and $
ho_c =
3.50^{+0.41}_{-0.36}$~gcm$^{-3}$ for planets b and c, respectively, thus
placing them on either side of the radius valley. The combination of the
multi-transiting planet system, the bright host star, and the diversity of
planetary interiors and atmospheres means this will likely become a cornerstone
system for atmospheric and orbital characterization of small worlds. | | Source: | arXiv, 2007.10995 | | Services: | Forum | Review | PDF | Favorites | |
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