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Robo-AO Kepler Asteroseismic Survey. II. Do Stellar Companions Inhibit Stellar Oscillations?

Schonhut-Stasik, Jessica and Huber, Daniel and Baranec, Christoph and Lamman, Claire and Salama, Maïssa and Jensen-Clem, Rebecca and Duev, Dmitry A. and Riddle, Reed and Kulkarni, S. R. and Law, Nicholas M. (2020) Robo-AO Kepler Asteroseismic Survey. II. Do Stellar Companions Inhibit Stellar Oscillations? Astrophysical Journal, 888 (1). Art. No. 34. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20191121-145928839

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Abstract

The Kepler Space Telescope observed over 15,000 stars for asteroseismic studies. Of these, 75% of dwarfs (and 8% of giants) were found to show anomalous behavior, such as suppressed oscillations (low amplitude) or no oscillations at all. The lack of solar-like oscillations may be a consequence of multiplicity, due to physical interactions with spectroscopic companions or due to the dilution of oscillation amplitudes from "wide" (AO detected; visual) or spectroscopic companions introducing contaminating flux. We present a search for stellar companions to 327 of the Kepler asteroseismic sample, which were expected to display solar-like oscillations. We used direct imaging with Robo-AO, which can resolve secondary sources at ~0.”15, and followed up detected companions with Keck AO. Directly imaged companion systems with both separations of ≤0.”5 and amplitude dilutions >10% all have anomalous primaries, suggesting these oscillation signals are diluted by a sufficient amount of excess flux. We also used the high-resolution spectrometer ESPaDOnS at the Canada–France–Hawai'i Telescope to search for spectroscopic binaries. We find tentative evidence for a higher fraction of spectroscopic binaries with high radial velocity scatter in anomalous systems, which would be consistent with previous results suggesting that oscillations are suppressed by tidal interactions in close eclipsing binaries.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/ab50c3DOIArticle
https://arxiv.org/abs/1910.03803arXivDiscussion Paper
ORCID:
AuthorORCID
Schonhut-Stasik, Jessica0000-0002-1043-8853
Huber, Daniel0000-0001-8832-4488
Baranec, Christoph0000-0002-1917-9157
Lamman, Claire0000-0002-6731-9329
Salama, Maïssa0000-0002-5082-6332
Jensen-Clem, Rebecca0000-0003-0054-2953
Duev, Dmitry A.0000-0001-5060-8733
Riddle, Reed0000-0002-0387-370X
Kulkarni, S. R.0000-0001-5390-8563
Law, Nicholas M.0000-0001-9380-6457
Additional Information:© 2020 The American Astronomical Society. Received 2018 December 18; revised 2019 September 6; accepted 2019 October 8; published 2020 January 3. D.H. acknowledges support by the National Science Foundation (AST-1717000) and the National Aeronautics and Space Administration (80NSSC19K0597). C.B. acknowledges support from the Alfred P. Sloan Foundation. The Robo-AO instrument was developed with support from the National Science Foundation under grants AST-0906060, AST-0960343, and AST-1207891, IUCAA, the Mt. Cuba Astronomical Foundation, and by a gift from Samuel Oschin. The Robo-AO team thanks NSF and NOAO for making the Kitt Peak 2.1 m telescope available. We thank the observatory staff at Kitt Peak for their efforts to assist Robo-AO KP operations. The authors are honored to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham Nation. Robo-AO KP is a partnership between the California Institute of Technology, the University of Hawai'i, the University of North Carolina at Chapel Hill, the Inter-University Centre for Astronomy and Astrophysics (IUCAA) at Pune, India, and the National Central University, Taiwan. The Murty family feels very happy to have added a small value to this important project. Robo-AO KP is also supported by grants from the John Templeton Foundation and the Mt. Cuba Astronomical Foundation. Some data are based on observations at Kitt Peak National Observatory, National Optical Astronomy Observatory (NOAO Prop. ID: 15B-3001), which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Based on observations obtained at the Canada–France–Hawai'i Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawai'i. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawai'ian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of NASA's Astrophysics Data System Bibliographic Services. We thank Dani Atkinson, Claire Moutou, Pascal Fouqué, and Nadine Manset for vital communications and important advice. We acknowledge the Exoplanet Follow-up Observing Program (ExoFOP) and Kepler Asteroseismic Science Operations Center (KASOC) databases, Python modules cv2 and pillow. Facilities: KPNO:2.1 m (Robo-AO) - , Keck:II (NIRC2-NGS) - , CFHT (ESPaDOnS). - Software: Astropy (Astropy Collaboration et al. 2013), Pyasl (https://pyastronomy.readthedocs.io/en/latest/), Libre-Esprit (Donati et al. 1997), Aperture Photometry Tool (APT) (Laher et al. 2012), DS9 (Smithsonian Astrophysical Observatory 2000; Joye & Mandel 2003).
Group:Astronomy Department
Funders:
Funding AgencyGrant Number
NSFAST-1717000
NASA80NSSC19K0597
Alfred P. Sloan FoundationUNSPECIFIED
NSFAST-0906060
NSFAST-0960343
NSFAST-1207891
Inter-University Centre for Astronomy and AstrophysicsUNSPECIFIED
Mt. Cuba Astronomical FoundationUNSPECIFIED
Samuel OschinUNSPECIFIED
John Templeton FoundationUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Canadian Space Agency (CSA)UNSPECIFIED
Subject Keywords:asteroseismology – binaries: close – instrumentation: adaptive optics – methods: data analysis – methods: observational – stars: fundamental parameters – techniques: high angular resolution
Issue or Number:1
Record Number:CaltechAUTHORS:20191121-145928839
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20191121-145928839
Official Citation:Jessica Schonhut-Stasik et al 2020 ApJ 888 34
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:100000
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:21 Nov 2019 23:17
Last Modified:08 Jan 2020 23:53

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