Obermeier, C. and Steuer, J. and Kellermann, H. and Saglia, R. P. and Henning, Th. and Riffeser, A. and Hopp, U. and Stefansson, G. and Cañas, C. and Ninan, J. and Mahadevan, S. and Isaacson, H. and Howard, A. W. and Livingston, J. and Koppenhoefer, J. and Bender, R. (2020) Following the TraCS of exoplanets with Pan-Planets: Wendelstein-1b and Wendelstein-2b. Astronomy and Astrophysics, 639 . Art. No. A130. ISSN 0004-6361. doi:10.1051/0004-6361/202037715. https://resolver.caltech.edu/CaltechAUTHORS:20200612-084218961
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Abstract
Hot Jupiters seem to get rarer with decreasing stellar mass. The goal of the Pan-Planets transit survey was the detection of such planets and a statistical characterization of their frequency. Here, we announce the discovery and validation of two planets found in that survey, Wendelstein-1b and Wendelstein-2b, which are two short-period hot Jupiters that orbit late K host stars. We validated them both by the traditional method of radial velocity measurements with the HIgh Resolution Echelle Spectrometer and the Habitable-zone Planet Finder instruments and then by their Transit Color Signature (TraCS). We observed the targets in the wavelength range of 4000−24 000 Å and performed a simultaneous multiband transit fit and additionally determined their thermal emission via secondary eclipse observations. Wendelstein-1b is a hot Jupiter with a radius of 1.0314_(−0.0061)^(+0.0061) R_J and mass of 0.592_(−0.129)^(+0.0165) M_J, orbiting a K7V dwarf star at a period of 2.66 d, and has an estimated surface temperature of about 1727₋₉₀⁺⁷⁸ K. Wendelstein-2b is a hot Jupiter with a radius of 1.1592_(−0.0210)^(+0.0204) R_J and a mass of 0.731_(−0.311)^(+0.0541) M_J, orbiting a K6V dwarf star at a period of 1.75 d, and has an estimated surface temperature of about 1852₋₁₄₀⁺¹²⁰ K. With this, we demonstrate that multiband photometry is an effective way of validating transiting exoplanets, in particular for fainter targets since radial velocity follow-up becomes more and more costly for those targets.
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| Additional Information: | © 2020 ESO. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Open Access funding provided by Max Planck Society. Received: 12 February 2020; Accepted: 25 May 2020; Published online 21 July 2020. Based on observations obtained with the Hobby-Eberly Telescope, which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians- Universität München, and Georg-August-Universität Göttingen. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). This paper contains data obtained with the 2.1 m Fraunhofer Telescope of the Wendelstein observatory of the Ludwig-Maximilians University Munich. We thank the staff of the Wendelstein observatory for technical help and strong support, including observing targets for us, during the data acquisition. This publication makes use of data products from the Two Micron All Sky Survey, 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. This paper includes data taken at The McDonald Observatory of The University of Texas at Austin. The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. These results are based on observations obtained with the Habitable-zone Planet Finder Spectrograph on the Hobby-Eberly Telescope. We thank the Resident astronomers and Telescope Operators at the HET for the skillful execution of our observations of our observations with the Habitable-zone Planet Finder (HPF). This work was partially supported by funding from the Center for Exoplanets and Habitable Worlds. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. This work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program through grants NNX16AO28H and 80NSSC18K1114. We acknowledge support from NSF grants AST-1006676, AST-1126413, AST-1310885, AST-1517592, AST-1310875, the NASA Astrobiology Institute (NAI; NNA09DA76A), and PSARC in our pursuit of precision radial velocities in the NIR. Computations for this research were performed on the Pennsylvania State University’s Institute for CyberScience Advanced CyberInfrastructure (ICS-ACI). The authors are honored to be permitted to conduct observations on Iolkam Du’ag (Kitt Peak), a mountain within the Tohono O’odham Nation with particular significance to the Tohono O’odham people. | ||||||||||||||||||||||||||||||||||||||||
| Group: | Astronomy Department | ||||||||||||||||||||||||||||||||||||||||
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| Subject Keywords: | planets and satellites: detection – planets and satellites: gaseous planets – stars: low-mass – techniques: image processing – techniques: photometric – occultations | ||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1051/0004-6361/202037715 | ||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20200612-084218961 | ||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20200612-084218961 | ||||||||||||||||||||||||||||||||||||||||
| Official Citation: | Following the TraCS of exoplanets with Pan-Planets: Wendelstein-1b and Wendelstein-2b. C. Obermeier, J. Steuer, H. Kellermann, R. P. Saglia, Th. Henning, A. Riffeser, U. Hopp, G. Stefansson, C. Cañas, J. Ninan, S. Mahadevan, H. Isaacson, A. W. Howard, J. Livingston, J. Koppenhoefer and R. Bender. A&A, 639 (2020) A130; DOI: https://doi.org/10.1051/0004-6361/202037715 | ||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||
| ID Code: | 103864 | ||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||
| Deposited By: | Tony Diaz | ||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 12 Jun 2020 16:53 | ||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 16 Nov 2021 18:26 |
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