Bibcode
Hirano, T.; Fukui, Akihiko; Mann, Andrew W.; Sanchis-Ojeda, Roberto; Gaidos, Eric; Narita, Norio; Dai, Fei; Van Eylen, Vincent; Lee, Chien-Hsiu; Onozato, Hiroki; Ryu, Tsuguru; Kusakabe, Nobuhiko; Ito, Ayaka; Kuzuhara, Masayuki; Onitsuka, Masahiro; Tatsuuma, Misako; Nowak, G.; Pallè, E.; Ribas, Ignasi; Tamura, Motohide; Yu, Liang
Referencia bibliográfica
The Astrophysical Journal, Volume 820, Issue 1, article id. 41, 11 pp. (2016).
Fecha de publicación:
3
2016
Revista
Número de citas
52
Número de citas referidas
49
Descripción
We validate a {R}p=2.32+/- 0.24{R}\oplus planet
on a close-in orbit (P = 2.260455 ± 0.000041 days) around K2-28
(EPIC 206318379), a metal-rich M4-type dwarf in the Campaign 3 field of
the K2 mission. Our follow-up observations included multi-band transit
observations from the optical to the near-infrared, low-resolution
spectroscopy, and high-resolution adaptive optics (AO) imaging. We
perform a global fit to all of the observed transits using a Gaussian
process-based method and show that the transit depths in all of the
passbands adopted for the ground-based transit follow-ups
({r}2\prime
,{z}s,2,J,H,{K}s) are within ∼2σ
of the K2 value. Based on a model of the background stellar population
and the absence of nearby sources in our AO imaging, we estimate the
probability that a background eclipsing binary could cause a false
positive to be <2 × 10‑5. We also show that
K2-28 cannot have a physically associated companion of stellar type
later than M4, based on the measurement of almost identical transit
depths in multiple passbands. There is a low probability for an M4 dwarf
companion (≈ {0.072}-0.04+0.02), but even if
this were the case, the size of K2-28b falls within the planetary
regime. K2-28b has the same radius (within 1σ) and experiences
irradiation from its host star similar to the well-studied GJ 1214b.
Given the relative brightness of K2-28 in the near-infrared
({m}{Kep}=14.85 mag and mH = 11.03 mag) and
relatively deep transit (0.6%–0.7%), a comparison between the
atmospheric properties of these two planets with future observations
would be especially interesting.