K2-264 : A transiting multiplanet system in the Praesepe open cluster
(2019) In Monthly Notices of the Royal Astronomical Society 484(1). p.8-18- Abstract
Planet host stars with well-constrained ages provide a rare window to the time domain of planet formation and evolution. The NASA K2 mission has enabled the discovery of the vast majority of known planets transiting stars in clusters, providing a valuable sample of planets with known ages and radii. We present the discovery of two planets transiting K2-264, an M2 dwarf in the intermediate age (600-800 Myr) Praesepe open cluster (also known as the Beehive Cluster, M44, or NGC 2632), which was observed by K2 during Campaign 16. The planets have orbital periods of 5.8 and 19.7 d, and radii of 2.2 ± 0.2 and 2.7 ± 0.2R, respectively, and their equilibrium temperatures are 496 ± 10 and 331 ± 7 K, making this a system of two warm subNeptunes.... (More)
Planet host stars with well-constrained ages provide a rare window to the time domain of planet formation and evolution. The NASA K2 mission has enabled the discovery of the vast majority of known planets transiting stars in clusters, providing a valuable sample of planets with known ages and radii. We present the discovery of two planets transiting K2-264, an M2 dwarf in the intermediate age (600-800 Myr) Praesepe open cluster (also known as the Beehive Cluster, M44, or NGC 2632), which was observed by K2 during Campaign 16. The planets have orbital periods of 5.8 and 19.7 d, and radii of 2.2 ± 0.2 and 2.7 ± 0.2R, respectively, and their equilibrium temperatures are 496 ± 10 and 331 ± 7 K, making this a system of two warm subNeptunes. When placed in the context of known planets orbiting field stars of similar mass to K2-264, these planets do not appear to have significantly inflated radii, as has previously been noted for some cluster planets. As the second known system of multiple planets transiting a star in a cluster, K2-264 should be valuable for testing theories of photoevaporation in systems of multiple planets. Follow-up observations with current near-infrared (NIR) spectrographs could yield planet mass measurements, which would provide information about the mean densities and compositions of small planets soon after photoevaporation is expected to have finished. Follow-up NIR transit observations using Spitzer or large ground-based telescopes could yield improved radius estimates, further enhancing the characterization of these interesting planets.
(Less)
- author
- publishing date
- 2019-03-21
- type
- Contribution to journal
- publication status
- published
- keywords
- Planets and satellites: detection, Techniques: high angular resolution, Techniques: photometric
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 484
- issue
- 1
- pages
- 11 pages
- publisher
- Oxford University Press
- external identifiers
-
- scopus:85063522866
- ISSN
- 0035-8711
- DOI
- 10.1093/mnras/sty3464
- language
- English
- LU publication?
- no
- additional info
- Publisher Copyright: © 2018 The Author(s).
- id
- b8cf360f-2bf7-41a7-a48b-73a29db3a2dc
- date added to LUP
- 2023-02-02 10:34:45
- date last changed
- 2023-02-20 13:40:40
@article{b8cf360f-2bf7-41a7-a48b-73a29db3a2dc,
abstract = {{<p>Planet host stars with well-constrained ages provide a rare window to the time domain of planet formation and evolution. The NASA K2 mission has enabled the discovery of the vast majority of known planets transiting stars in clusters, providing a valuable sample of planets with known ages and radii. We present the discovery of two planets transiting K2-264, an M2 dwarf in the intermediate age (600-800 Myr) Praesepe open cluster (also known as the Beehive Cluster, M44, or NGC 2632), which was observed by K2 during Campaign 16. The planets have orbital periods of 5.8 and 19.7 d, and radii of 2.2 ± 0.2 and 2.7 ± 0.2R, respectively, and their equilibrium temperatures are 496 ± 10 and 331 ± 7 K, making this a system of two warm subNeptunes. When placed in the context of known planets orbiting field stars of similar mass to K2-264, these planets do not appear to have significantly inflated radii, as has previously been noted for some cluster planets. As the second known system of multiple planets transiting a star in a cluster, K2-264 should be valuable for testing theories of photoevaporation in systems of multiple planets. Follow-up observations with current near-infrared (NIR) spectrographs could yield planet mass measurements, which would provide information about the mean densities and compositions of small planets soon after photoevaporation is expected to have finished. Follow-up NIR transit observations using Spitzer or large ground-based telescopes could yield improved radius estimates, further enhancing the characterization of these interesting planets.</p>}},
author = {{Livingston, John H. and Dai, Fei and Hirano, Teruyuki and Gandolfi, Davide and Trani, Alessandro A. and Nowak, Grzegorz and Cochran, William D. and Endl, Michael and Albrecht, Simon and Barragan, Oscar and Cabrera, Juan and Csizmadia, Szilard and De Leon, Jerome P. and Deeg, Hans and Eigmuller, Philipp and Erikson, Anders and Fridlund, Malcolm and Fukui, Akihiko and Grziwa, Sascha and Guenther, Eike W. and Hatzes, Artie P. and Korth, Judith and Kuzuhara, Masayuki and Montanes, Pilar and Narita, Norio and Nespral, David and Palle, Enric and Patzold, Martin and Persson, Carina M. and Prieto-Arranz, Jorge and Rauer, Heike and Tamura, Motohide and Eylen, Vincent Van and Winn, Joshua N.}},
issn = {{0035-8711}},
keywords = {{Planets and satellites: detection; Techniques: high angular resolution; Techniques: photometric}},
language = {{eng}},
month = {{03}},
number = {{1}},
pages = {{8--18}},
publisher = {{Oxford University Press}},
series = {{Monthly Notices of the Royal Astronomical Society}},
title = {{K2-264 : A transiting multiplanet system in the Praesepe open cluster}},
url = {{http://dx.doi.org/10.1093/mnras/sty3464}},
doi = {{10.1093/mnras/sty3464}},
volume = {{484}},
year = {{2019}},
}