TY - JOUR
T1 - K2-264
T2 - A transiting multiplanet system in the Praesepe open cluster
AU - Livingston, John H.
AU - Dai, Fei
AU - Hirano, Teruyuki
AU - Gandolfi, Davide
AU - Trani, Alessandro A.
AU - Nowak, Grzegorz
AU - Cochran, William D.
AU - Endl, Michael
AU - Albrecht, Simon
AU - Barragan, Oscar
AU - Cabrera, Juan
AU - Csizmadia, Szilard
AU - De Leon, Jerome P.
AU - Deeg, Hans
AU - Eigmuller, Philipp
AU - Erikson, Anders
AU - Fridlund, Malcolm
AU - Fukui, Akihiko
AU - Grziwa, Sascha
AU - Guenther, Eike W.
AU - Hatzes, Artie P.
AU - Korth, Judith
AU - Kuzuhara, Masayuki
AU - Montanes, Pilar
AU - Narita, Norio
AU - Nespral, David
AU - Palle, Enric
AU - Patzold, Martin
AU - Persson, Carina M.
AU - Prieto-Arranz, Jorge
AU - Rauer, Heike
AU - Tamura, Motohide
AU - Eylen, Vincent Van
AU - Winn, Joshua N.
N1 - Funding Information:
This work was carried out as part of the KESPRINT consortium. J H L gratefully acknowledges the support of the Japan Society for the Promotion of Science (JSPS) Research Fellowship for Young Scientists. This work was supported by JSPS KAKENHI Grant Number JP16K17660. ME and W D C were supported by NASA grant NNX16AJ11G to The University of Texas. A A T acknowledges support from JSPS KAKENHI grant number JP17F17764. N N acknowledges support from KAKENHI Grant Number JP18H01265. A P H, Sz Cs, S G, J K, M P, and H R acknowledge support by DFG grants HA 3279/12-1, PA525/18-1, PA525/19-1, PA525/20-1, and RA 714/14-1 within the DFG Schwerpunkt SPP 1992, ‘Exploring the Diversity of Extrasolar Planets.’ The simulations were run on the Calculation Server at the NAOJ Center for Computational Astrophysics. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https: //www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publication makes use of VOSA, developed under the Spanish Virtual Observatory project supported from the Spanish MINECO through grant AyA2017-84089. A A T would like to thank Hori Yasunori and Michiko Fujii for helpful discussions on the system’s dynamics.
Publisher Copyright:
© 2018 The Author(s).
PY - 2019/3/21
Y1 - 2019/3/21
N2 - 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.
AB - 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.
KW - Planets and satellites: detection
KW - Techniques: high angular resolution
KW - Techniques: photometric
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U2 - 10.1093/mnras/sty3464
DO - 10.1093/mnras/sty3464
M3 - Article
AN - SCOPUS:85063522866
SN - 0035-8711
VL - 484
SP - 8
EP - 18
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -