Skip to main content

Lund University Publications

LUND UNIVERSITY LIBRARIES

K2-290 : A warm Jupiter and a mini-Neptune in a triple-star system

Hjorth, M. ; Justesen, A. B. ; Hirano, T. ; Albrecht, S. ; Gandolfi, D. ; Dai, F. ; Alonso, R. ; Barragán, O. ; Esposito, M. and Kuzuhara, M. , et al. (2019) In Monthly Notices of the Royal Astronomical Society 484(3). p.3522-3536
Abstract

We report the discovery of two transiting planets orbiting K2-290 (EPIC 249624646), a bright (V = 11.11) late F-type star residing in a triple-star system. It was observed during Campaign 15 of the K2 mission, and in order to confirm and characterize the system, follow-up spectroscopy and AO imaging were carried out using the FIES, HARPS, HARPS-N, and IRCS instruments. From AO imaging and Gaia data we identify two M-dwarf companions at a separation of 113 ± 2 and 2467+−177155 au. From radial velocities, K2 photometry, and stellar characterization of the host star, we find the inner planet to be a mini-Neptune with a radius of 3.06 ± 0.16 R and an orbital period of P = 9.2 d. The radius of the... (More)

We report the discovery of two transiting planets orbiting K2-290 (EPIC 249624646), a bright (V = 11.11) late F-type star residing in a triple-star system. It was observed during Campaign 15 of the K2 mission, and in order to confirm and characterize the system, follow-up spectroscopy and AO imaging were carried out using the FIES, HARPS, HARPS-N, and IRCS instruments. From AO imaging and Gaia data we identify two M-dwarf companions at a separation of 113 ± 2 and 2467+−177155 au. From radial velocities, K2 photometry, and stellar characterization of the host star, we find the inner planet to be a mini-Neptune with a radius of 3.06 ± 0.16 R and an orbital period of P = 9.2 d. The radius of the mini-Neptune suggests that the planet is located above the radius valley, and with an incident flux of F ∼ 400 F, it lies safely outside the super-Earth desert. The outer warm Jupiter has a mass of 0.774 ± 0.047 MJ and a radius of 1.006 ± 0.050 RJ, and orbits the host star every 48.4 d on an orbit with an eccentricity e < 0.241. Its mild eccentricity and mini-Neptune sibling suggest that the warm Jupiter originates from in situ formation or disc migration.

(Less)
Please use this url to cite or link to this publication:
author
; ; ; ; ; ; ; ; and , et al. (More)
; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; and (Less)
publishing date
type
Contribution to journal
publication status
published
keywords
Planets, Planets and satellites: detection, Planets and satellites: formation, Planets and satellites: individual: K2-290, Satellites: individual: EPIC 249624646
in
Monthly Notices of the Royal Astronomical Society
volume
484
issue
3
pages
15 pages
publisher
Oxford University Press
external identifiers
  • scopus:85067056184
ISSN
0035-8711
DOI
10.1093/mnras/stz139
language
English
LU publication?
no
additional info
Publisher Copyright: © 2019 The Author(s)
id
8747c293-88fc-426f-9810-eedb903a355f
date added to LUP
2023-02-02 10:28:13
date last changed
2023-02-27 13:02:56
@article{8747c293-88fc-426f-9810-eedb903a355f,
  abstract     = {{<p>We report the discovery of two transiting planets orbiting K2-290 (EPIC 249624646), a bright (V = 11.11) late F-type star residing in a triple-star system. It was observed during Campaign 15 of the K2 mission, and in order to confirm and characterize the system, follow-up spectroscopy and AO imaging were carried out using the FIES, HARPS, HARPS-N, and IRCS instruments. From AO imaging and Gaia data we identify two M-dwarf companions at a separation of 113 ± 2 and 2467<sup>+</sup><sub>−</sub><sup>177</sup><sub>155</sub> au. From radial velocities, K2 photometry, and stellar characterization of the host star, we find the inner planet to be a mini-Neptune with a radius of 3.06 ± 0.16 R and an orbital period of P = 9.2 d. The radius of the mini-Neptune suggests that the planet is located above the radius valley, and with an incident flux of F ∼ 400 F, it lies safely outside the super-Earth desert. The outer warm Jupiter has a mass of 0.774 ± 0.047 M<sub>J</sub> and a radius of 1.006 ± 0.050 R<sub>J</sub>, and orbits the host star every 48.4 d on an orbit with an eccentricity e &lt; 0.241. Its mild eccentricity and mini-Neptune sibling suggest that the warm Jupiter originates from in situ formation or disc migration.</p>}},
  author       = {{Hjorth, M. and Justesen, A. B. and Hirano, T. and Albrecht, S. and Gandolfi, D. and Dai, F. and Alonso, R. and Barragán, O. and Esposito, M. and Kuzuhara, M. and Lam, K. W.F. and Livingston, J. H. and Montanes-Rodriguez, P. and Narita, N. and Nowak, G. and Prieto-Arranz, J. and Redfield, S. and Rodler, F. and Van Eylen, V. and Winn, J. N. and Antoniciello, G. and Cabrera, J. and Cochran, W. D. and Csizmadia, Sz and De Leon, J. and Deeg, H. and Eigmüller, Ph and Endl, M. and Erikson, A. and Fridlund, M. and Grziwa, S. and Guenther, E. and Hatzes, A. P. and Heeren, P. and Hidalgo, D. and Korth, J. and Luque, R. and Nespral, D. and Palle, E. and Pätzold, M. and Persson, C. M. and Rauer, H. and Smith, A. M.S. and Trifonov, T.}},
  issn         = {{0035-8711}},
  keywords     = {{Planets; Planets and satellites: detection; Planets and satellites: formation; Planets and satellites: individual: K2-290; Satellites: individual: EPIC 249624646}},
  language     = {{eng}},
  month        = {{04}},
  number       = {{3}},
  pages        = {{3522--3536}},
  publisher    = {{Oxford University Press}},
  series       = {{Monthly Notices of the Royal Astronomical Society}},
  title        = {{K2-290 : A warm Jupiter and a mini-Neptune in a triple-star system}},
  url          = {{http://dx.doi.org/10.1093/mnras/stz139}},
  doi          = {{10.1093/mnras/stz139}},
  volume       = {{484}},
  year         = {{2019}},
}