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24 April 2024 |
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TOI-1468: A system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley | | P. Chaturvedi
; P. Bluhm
; E. Nagel
; A. P. Hatzes
; G. Morello
; M. Brady
; J. Korth
; K. Molaverdikhani
; D. Kossakowski
; J. A. Caballero
; E. W. Guenther
; E. Pallé
; N. Espinoza
; A. Seifahrt
; N. Lodieu
; C. Cifuentes
; E. Furlan
; P. J. Amado
; T. Barclay
; J. Bean
; V. J. S. Béjar
; G. Bergond
; A. W. Boyle
; D. Ciardi
; K. A. Collins
; K. I. Collins
; E. Esparza-Borges
; A. Fukui
; C. L. Gnilka
; R. Goeke
; P. Guerra
; Th. Henning
; E. Herrero
; S. B. Howell
; S. V. Jeffers
; J. M. Jenkins
; E. L. N. Jensen
; D. Kasper
; T. Kodama
; D. W. Latham
; M. J. López-González
; R. Luque
; D. Montes
; J. C. Morales
; M. Mori
; F. Murgas
; N. Narita
; G. Nowak
; H. Parviainen
; V. M. Passegger
; A. Quirrenbach
; S. Reffert
; A. Reiners
; I. Ribas
; G. R. Ricker
; E. Rodríguez
; C. Rodríguez-López
; M. Schlecker
; R. P. Schwarz
; A. Schweitzer
; S. Seager
; G. Stefánsson
; C. Stockdale
; L. Tal-Or
; J. D. Twicken
; S. Vanaverbeke
; G. Wang
; D. Watanabe
; J. N. Winn
; M. Zechmeister
; | | Date: |
Mon, 22 Aug 2022 14:26:22 GMT (18088kb,D) | | Abstract: | We report the discovery and characterization of two small transiting planets
orbiting the bright M3.0V star TOI-1468 (LSPM J0106+1913), whose transit
signals were detected in the photometric time series in three sectors of the
TESS mission. We confirm the e planetary nature of both of them using precise
radial velocity measurements from the CARMENES and MAROON-X spectrographs, and
supplement them with ground-based transit photometry. A joint analysis of all
these data reveals that the shorter-period planet, TOI-1468 b ($P_{
m b}$ =
1.88 d), has a planetary mass of $M_{
m b} = 3.21pm0.24$ $M_{oplus}$ and a
radius of $R_{
m b} =1.280^{+0.038}_{-0.039} R_{oplus}$, resulting in a
density of $
ho_{
m b} = 8.39^{+ 1.05}_{- 0.92}$ g cm$^{-3}$, which is
consistent with a mostly rocky composition. For the outer planet, TOI-1468 c
($P_{
m c} = 15.53$ d), we derive a mass of $M_{
m c} = 6.64^{+ 0.67}_{-
0.68}$ $M_{oplus}$, a radius of $R_{
m c} = 2.06pm0.04,R_{oplus}$, and a
bulk density of $
ho_{c} = 2.00^{+ 0.21}_{- 0.19}$ g cm$^{-3}$, which
corresponds to a rocky core composition with a H/He gas envelope. These planets
are located on opposite sides of the radius valley, making our system an
interesting discovery as there are only a handful of other systems with the
same properties. This discovery can further help determine a more precise
location of the radius valley for small planets around M dwarfs and, therefore,
shed more light on planet formation and evolution scenarios. | | Source: | arXiv, 2208.10351 | | Services: | Forum | Review | PDF | Favorites | |
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