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Cited by 38Stellar, planetary, and galactic studiesAstronomy and Astrophysical ResearchGalaxies: Formation, Evolution, Phenomena

Pan-Planets: Searching for hot Jupiters around cool dwarfs

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Obermeier, C., Koppenhoefer, J., Saglia, R. P., Henning, Th., Bender, R., Kodric, M., Deacon, N., Riffeser, A. +13 more·2016·Astronomy & Astrophysics
DOI 10.1051/0004-6361/201527633
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Abstract

The Pan-Planets survey observed an area of 42 sq deg. in the galactic disk for about 165 h. The main scientific goal of the project is the detection of transiting planets around M dwarfs. We establish an efficient procedure for determining the stellar parameters Teff and log g of all sources using a method based on SED fitting, utilizing a three-dimensional dust map and proper motion information. In this way we identify more than 60 000 M dwarfs, which is by far the largest sample of low-mass stars observed in a transit survey to date. We present several planet candidates around M dwarfs and hotter stars that are currently being followed up. Using Monte Carlo simulations we calculate the detection efficiency of the Pan-Planets survey for different stellar and planetary populations. We expect to find 3.0+3.3-1.6 hot Jupiters around F, G, and K dwarfs with periods lower than 10 days based on the planet occurrence rates derived in previous surveys. For M dwarfs, the percentage of stars with a hot Jupiter is under debate. Theoretical models expect a lower occurrence rate than for larger main sequence stars. However, radial velocity surveys find upper limits of about 1% due to their small sample, while the Kepler survey finds a occurrence rate that we estimate to be at least 0.17b(+0.67-0.04) %, making it even higher than the determined fraction from OGLE-III for F, G and K stellar types, 0.14 (+0.15-0.076) %. With the large sample size of Pan-Planets, we are able to determine an occurrence rate of 0.11 (+0.37-0.02) % in case one of our candidates turns out to be a real detection. If, however, none of our candidates turn out to be true planets, we are able to put an upper limit of 0.34% with a 95% confidence on the hot Jupiter occurrence rate of M dwarfs. This limit is a significant improvement over previous estimates where the lowest limit published so far is 1.1% found in the WFCAM Transit Survey. Therefore we cannot yet confirm the theoretical prediction of a lower occurrence rate for cool stars.

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  • Obermeier et al. (2016) found the occurrence rate of hot Jupiters orbiting M-stars vs. FGK stars could be the same, but for the former, they only have an upper limit.

    “Obermeier et al. (2016) found the occurrence rate of hot Jupiters orbiting M-stars vs. FGK stars c ould be the same, but for the former, they only have an upper limit.”

    From Origins of Hot Jupiters (2018) · cites this paper as Obermeier et al. (2016)

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Authors
Obermeier, C., Koppenhoefer, J., Saglia, R. P., Henning, T., Bender, R., Kodric, M., Deacon, N., Riffeser, A., Burgett, W., Chambers, K. C., Draper, P. W., Flewelling, H., Hodapp, K. W., Kaiser, N., Kudritzki, R.-P., Magnier, E. A., Metcalfe, N., Price, P. A., Sweeney, W., Wainscoat, R. J., & Waters, C.
Affiliations
  • Max Planck Institute for Extraterrestrial Physics (DE)
  • University of Hertfordshire (GB)
  • University of Hawaiʻi at Mānoa (US)
  • Durham University (GB)
  • Princeton University (US)
ORCID
Venue
Astronomy & Astrophysics
Publisher
EDP Sciences
Published
2016-02-16
Volume
587
Pages
A49
ISSN
  • 0004-6361 (ISSN-L)
  • 1432-0746
DOI
10.1051/0004-6361/201527633
OpenAlex
W2239125316
Cited by
38
References
3
Citations by year
2026: 1 · 2025: 4 · 2024: 1 · 2023: 3 · 2022: 8 · 2021: 3 · 2020: 8 · 2019: 2 · 2018: 4 · 2017: 2 · 2016: 2
FWCI
1.52
Type
journal article
Language
en
Open access
Locations
  • Astronomy and Astrophysics (publishedVersion)
  • University of Hertfordshire Research Archive (University of Hertfordshire) (acceptedVersion)
  • Durham Research Online (Durham University) (acceptedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • Springer Link (Chiba Institute of Technology) (submittedVersion)
  • Durham Research Online (Durham University) (submittedVersion, cc-by)
  • University of Hertfordshire Research Archive (University of Hertfordshire) (submittedVersion)
  • Max Planck Institute for Plasma Physics (submittedVersion)
  • Max Planck Digital Library (submittedVersion)
  • MPG.PuRe (Max Planck Society) (submittedVersion)
  • arXiv (Cornell University)
Funders
  • National Science Foundation (1238877)
  • Smithsonian Institution
  • National Aeronautics and Space Administration (NNX08AR22G, AST-1238877)
  • California Institute of Technology
  • Johns Hopkins University
  • Pennsylvania State University
  • University of Texas at Austin
  • Space Telescope Science Institute (NNX08AR22G)
  • Strong
  • University of Edinburgh
  • Queen's University Belfast
  • Durham University
  • Queen's University
  • Georg-August-Universität Göttingen
  • National Central University
  • Ludwig-Maximilians-Universität München
  • Universidad Nacional Autónoma de México
  • Eötvös Loránd Tudományegyetem
  • Max-Planck-Institut für Astronomie
  • Smithsonian Astrophysical Observatory
  • Science Mission Directorate (NNX08AR22G)
  • Planetary Science Division (NNX08AR22G)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Keywords
hot Jupiters, M dwarfs, transiting exoplanets, planet occurrence rate, stellar parameters, spectral energy distribution fitting, proper motions, planet candidates, low-mass stars

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