Abstract
We report the independent discovery and characterization of two K2 planets: K2-180b, a mini-Neptune-sized planet in an 8.9-d orbit transiting a V=12.6mag, metal-poor ([Fe/H] = -0.65 ± 0.10) K2V star in K2 campaign 5; K2-140b, a transiting hot Jupiter in a 6.6-d orbit around a V=12.6mag G6V ([Fe/H] = +0.10 ± 0.10) star in K2 campaign 10. Our results are based on K2 time-series photometry combined with high-spatial resolution imaging and high-precision radial velocity measurements. We present the first mass measurement of K2-180b. K2-180b has a mass of Mp = 11.3 ± 1.9M⊕ and a radius of Rp = 2.2 ± 0.1R⊕, yielding a mean density of ρp = 5.6 ± 1.9 g cm-3, suggesting a rocky composition. Given its radius, K2-180b is above the region of the so-called 'planetary radius gap'. K2-180b is in addition not only one of the densest mini-Neptune-sized planets, but also one of the few mini-Neptune-sized planets known to transit a metal-poor star. We also constrain the planetary and orbital parameters of K2-140b and show that, given the currently available Doppler measurements, the eccentricity is consistent with zero, contrary to the results of a previous study.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 1807-1823 |
| Number of pages | 17 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 482 |
| Issue number | 2 |
| DOIs | |
| State | Published - Jan 11 2019 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Keywords
- Planets and satellites: fundamental parameters
- Stars: fundamental parameters
- Stars: individual: K2-140
- Stars: individual: K2-180
- Techniques: photometric
- Techniques: radial velocities
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In: Monthly Notices of the Royal Astronomical Society, Vol. 482, No. 2, 11.01.2019, p. 1807-1823.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - K2-140b and K2-180b - Characterization of a hot Jupiter and a mini-Neptune from the K2 mission
AU - Korth, J.
AU - Csizmadia, Sz
AU - Gandolfi, D.
AU - Fridlund, M.
AU - Pätzold, M.
AU - Hirano, T.
AU - Livingston, J.
AU - Persson, C. M.
AU - Deeg, H. J.
AU - Justesen, A. B.
AU - Barragán, O.
AU - Grziwa, S.
AU - Endl, M.
AU - Tronsgaard, R.
AU - Dai, F.
AU - Cochran, W. D.
AU - Albrecht, S.
AU - Alonso, R.
AU - Cabrera, J.
AU - Cauley, P. W.
AU - Cusano, F.
AU - Eigmüller, Ph
AU - Erikson, A.
AU - Esposito, M.
AU - Guenther, E. W.
AU - Hatzes, A. P.
AU - Hidalgo, D.
AU - Kuzuhara, M.
AU - Montañes, P.
AU - Napolitano, N. R.
AU - Narita, N.
AU - Niraula, P.
AU - Nespral, D.
AU - Nowak, G.
AU - Palle, E.
AU - Petrillo, C. E.
AU - Redfield, S.
AU - Prieto-Arranz, J.
AU - Rauer, H.
AU - Smith, A. M.S.
AU - Tortora, C.
AU - Van Eylen, V.
AU - Winn, J. N.
N1 - Funding Information: We are very grateful to the Nordic Optical Telescope (NOT) and Telescopio Nazionale Galileo (TNG) staffmembers for their unique and superb support during the observations. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2013-2016) under grant agreement No. 312430 (Optical Infrared Coordination Network for Astronomy (OPTICON)). Based on observations obtained with the NOT, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos (ORM) of the Instituto de Astrof ísica de Canarias (IAC). The WIYN/NASA Exoplanet Star and Speckle Imager (NESSI) observations were conducted as part of National Optical Astronomy Observatory (NOAO) observing program ID 2017A-0377 (P.I. Livingston). Data presented herein were obtained at the WIYN Observatory from telescope time allocated to NN-EXPLORE through the scientific partnership of the National Aeronautics and Space Administration, the National Science Foundation, and the NOAO. This work was supported by a National Aeronautics and Space Administration (NASA) WIYN PI Data Award, administered by the NASA Exoplanet Science Institute. NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). Space Telescope Science Institute (STScI) is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. 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 data products from the Two Micron All Sky Survey (2Mass), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/ California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no. DNRF106). JK, SG, MP, SC, APH, and HR acknowledge support by Deutsche Forschungsgemeinschaft (DFG) grants PA525/18-1, PA525/19-1, PA525/20-1, HA 3279/12-1, and RA 714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. SC acknowledges the Hungarian Hungarian Scientific Research Fund (OTKA) Grant K113117. DG acknowledges the financial support of the Programma Giovani Ricercatori-Rita Levi Montalcini-Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education, Universities and Research (MIUR).MF and CMP gratefully acknowledge the support of the Swedish National Space Board. CEP and CT are supported through an NWO-VICI grant (project number 639.043.308). This work is partly supported by Japan Society for the Promotion of Science(JSPS) KAKENHI Grant Number JP18H01265 Funding Information: We are very grateful to the Nordic Optical Telescope (NOT) and Telescopio Nazionale Galileo (TNG) staff members for their unique and superb support during the observations. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2013-2016) under grant agreement No. 312430 (Optical Infrared Coordination Network for Astronomy (OPTICON)). Based on observations obtained with the NOT, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observa-torio del Roque de los Muchachos (ORM) of the Instituto de As-trofísica de Canarias (IAC). The WIYN/NASA Exoplanet Star and Speckle Imager (NESSI) observations were conducted as part of National Optical Astronomy Observatory (NOAO) observing program ID 2017A-0377 (P.I. Livingston). Data presented herein were obtained at the WIYN Observatory from telescope time allocated to NN-EXPLORE through the scientific partnership of the National Aeronautics and Space Administration, the National Science Foundation, and the NOAO. This work was supported by a National Aeronautics and Space Administration (NASA) WIYN PI Data Award, administered by the NASA Exoplanet Science Institute. NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). Space Telescope Science Institute (STScI) is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. 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 data products from the Two Micron All Sky Survey (2Mass), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no. DNRF106). JK, SG, MP, SC, APH, and HR acknowledge support by Deutsche Forschungsgemeinschaft (DFG) grants PA525/18-1, PA525/19-1, PA525/20-1, HA 3279/12-1, and RA 714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. SC acknowledges the Hungarian Hungarian Scientific Research Fund (OTKA) Grant K113117. DG acknowledges the financial support of the Programma Giovani Ricercatori – Rita Levi Montalcini – Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education, Universities and Research (MIUR). MF and CMP gratefully acknowledge the support of the Swedish National Space Board. CEP and CT are supported through an NWO-VICI grant (project number 639.043.308). This work is partly supported by Japan Society for the Promotion of Science(JSPS) KAKENHI Grant Number JP18H01265. Publisher Copyright: © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2019/1/11
Y1 - 2019/1/11
N2 - We report the independent discovery and characterization of two K2 planets: K2-180b, a mini-Neptune-sized planet in an 8.9-d orbit transiting a V=12.6mag, metal-poor ([Fe/H] = -0.65 ± 0.10) K2V star in K2 campaign 5; K2-140b, a transiting hot Jupiter in a 6.6-d orbit around a V=12.6mag G6V ([Fe/H] = +0.10 ± 0.10) star in K2 campaign 10. Our results are based on K2 time-series photometry combined with high-spatial resolution imaging and high-precision radial velocity measurements. We present the first mass measurement of K2-180b. K2-180b has a mass of Mp = 11.3 ± 1.9M⊕ and a radius of Rp = 2.2 ± 0.1R⊕, yielding a mean density of ρp = 5.6 ± 1.9 g cm-3, suggesting a rocky composition. Given its radius, K2-180b is above the region of the so-called 'planetary radius gap'. K2-180b is in addition not only one of the densest mini-Neptune-sized planets, but also one of the few mini-Neptune-sized planets known to transit a metal-poor star. We also constrain the planetary and orbital parameters of K2-140b and show that, given the currently available Doppler measurements, the eccentricity is consistent with zero, contrary to the results of a previous study.
AB - We report the independent discovery and characterization of two K2 planets: K2-180b, a mini-Neptune-sized planet in an 8.9-d orbit transiting a V=12.6mag, metal-poor ([Fe/H] = -0.65 ± 0.10) K2V star in K2 campaign 5; K2-140b, a transiting hot Jupiter in a 6.6-d orbit around a V=12.6mag G6V ([Fe/H] = +0.10 ± 0.10) star in K2 campaign 10. Our results are based on K2 time-series photometry combined with high-spatial resolution imaging and high-precision radial velocity measurements. We present the first mass measurement of K2-180b. K2-180b has a mass of Mp = 11.3 ± 1.9M⊕ and a radius of Rp = 2.2 ± 0.1R⊕, yielding a mean density of ρp = 5.6 ± 1.9 g cm-3, suggesting a rocky composition. Given its radius, K2-180b is above the region of the so-called 'planetary radius gap'. K2-180b is in addition not only one of the densest mini-Neptune-sized planets, but also one of the few mini-Neptune-sized planets known to transit a metal-poor star. We also constrain the planetary and orbital parameters of K2-140b and show that, given the currently available Doppler measurements, the eccentricity is consistent with zero, contrary to the results of a previous study.
KW - Planets and satellites: fundamental parameters
KW - Stars: fundamental parameters
KW - Stars: individual: K2-140
KW - Stars: individual: K2-180
KW - Techniques: photometric
KW - Techniques: radial velocities
UR - http://www.scopus.com/inward/record.url?scp=85057187414&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85057187414&partnerID=8YFLogxK
U2 - 10.1093/mnras/sty2760
DO - 10.1093/mnras/sty2760
M3 - Article
AN - SCOPUS:85057187414
SN - 0035-8711
VL - 482
SP - 1807
EP - 1823
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -