A Caltech Library Service

An Accurate Mass Determination for Kepler-1655b, a Moderately Irradiated World with a Significant Volatile Envelope

Haywood, Raphaëlle D. and Dressing, Courtney D. and Ciardi, David R. (2018) An Accurate Mass Determination for Kepler-1655b, a Moderately Irradiated World with a Significant Volatile Envelope. Astronomical Journal, 155 (5). Art. No. 203. ISSN 1538-3881. doi:10.3847/1538-3881/aab8f3.

[img] PDF - Published Version
See Usage Policy.

[img] PDF - Accepted Version
See Usage Policy.


Use this Persistent URL to link to this item:


We present the confirmation of a small, moderately irradiated (F = 155 ± 7 F⊕) Neptune with a substantial gas envelope in a P = 11.8728787 ± 0.0000085 day orbit about a quiet, Sun-like G0V star Kepler-1655. Based on our analysis of the Kepler light curve, we determined Kepler-1655b's radius to be 2.213 ± 0.082 R⊕. We acquired 95 high-resolution spectra with Telescopio Nazionale Galileo/HARPS-N, enabling us to characterize the host star and determine an accurate mass for Kepler-1655b of 5.0±^(3.1)_(2.8) M⊕ via Gaussian-process regression. Our mass determination excludes an Earth-like composition with 98% confidence. Kepler-1655b falls on the upper edge of the evaporation valley, in the relatively sparsely occupied transition region between rocky and gas-rich planets. It is therefore part of a population of planets that we should actively seek to characterize further.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Haywood, Raphaëlle D.0000-0001-9140-3574
Dressing, Courtney D.0000-0001-8189-0233
Ciardi, David R.0000-0002-5741-3047
Additional Information:© 2018 The American Astronomical Society. Received 2017 July 10; revised 2018 March 16; accepted 2018 March 18; published 2018 April 20. We are grateful to Natalie M. Batalha and Samuel N. Quinn for insightful discussions that have helped shape our discussion on planet population properties. We would also like to thank the anonymous referee for providing constructive feedback on the manuscript. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute (R.D.H., C.D.D.). Some of this work has been carried out within the framework of the NCCR PlanetS, supported by the Swiss National Science Foundation. A.V. is supported by the NSF Graduate Research Fellowship, grant No. DGE 1144152. A.C.C. acknowledges support from STFC consolidated grant number ST/M001296/1. D.W.L. acknowledges partial support from the Kepler mission under NASA Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical Observatory. X.D. is grateful to the Society in Science-Branco Weiss Fellowship for its financial support. C.A.W. acknowledges support by STFC grant ST/P000312/1. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This material is based upon work supported by the National Aeronautics and Space Administration under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007–2013) under grant Agreement No. 313014 (ETAEARTH). The HARPS-N project has been funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origins of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), the University of St Andrews, Queen's University Belfast, and the University of Edinburgh. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This research has made use of NASA's Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research has made use of the code by Dan Foreman-Mackey at Facility: Kepler/K2 TNG:HARPS-N - .
Funding AgencyGrant Number
Swiss National Science Foundation (SNSF)UNSPECIFIED
NSF Graduate Research FellowshipDGE-1144152
Science and Technology Facilities Council (STFC)ST/M001296/1
Society in Science-Branco Weiss FellowshipUNSPECIFIED
Science and Technology Facilities Council (STFC)ST/P000312/1
John Templeton FoundationUNSPECIFIED
European Research Council (ERC)313014
Subject Keywords:stars: individual (Kepler-1655, KOI-280, KIC 4141376, 2MASS J19064546+3912428) – planets and satellites: detection – planets and satellites: gaseous planets
Issue or Number:5
Record Number:CaltechAUTHORS:20180427-155501743
Persistent URL:
Official Citation:Raphaëlle D. Haywood et al 2018 AJ 155 203
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:86091
Deposited By: Tony Diaz
Deposited On:27 Apr 2018 23:08
Last Modified:15 Nov 2021 20:35

Repository Staff Only: item control page