EPJ Web Conf.
Volume 160, 2017Seismology of the Sun and the Distant Stars 2016 – Using Today’s Successes to Prepare the Future – TASC2 & KASC9 Workshop – SPACEINN & HELAS8 Conference
|Number of page(s)||5|
|Section||Synergies: Stellar Evolution, Galactic Populations, Binaries and Planets|
|Published online||27 October 2017|
Probing the Deep End of the Milky Way with New Oscillating Kepler Giants
Center for Extrasolar Planetary Systems, Space Science Institute
4750 Walnut street Suite#205, Boulder, CO 80301, USA
2 Laboratoire AIM, CEA/DRF-CNRS-Université Paris Diderot; IRFU/SAp, Centre de Saclay, 91191, Gif-sur-Yvette Cedex, France
3 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia
4 SETI Institute, 189 Bernardo Avenue, Mountain View, CA 94043, USA
5 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Aarhus C, DK-8000, Denmark
6 Universidad de La Laguna, Dpto de Astrofísica, 38206, Tenerife, Spain
7 Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain
⋆ e-mail: email@example.com
Published online: 27 October 2017
The Kepler mission has been a success in both exoplanet search and stellar physics studies. Red giants have actually been quite a highlight in the Kepler scene. The Kepler long and almost continuous four-year observations allowed us to detect oscillations in more than 15,000 red giants targeted by the mission. However by looking at the power spectra of 45,000 stars classified as dwarfs according to the Q1–16 Kepler star properties catalog, we detected red-giant like oscillations in 850 stars. Even though this is a small addition to the known red–giant sample, these misclassified stars represent a goldmine for galactic archeology studies. Indeed they happen to be fainter (down to Kp~16) and more distant (d>10kPc) than the known red giants, opening the possibility to probe unknown regions of our Galaxy. The faintness of these red giants with detected oscillations is very promising for detecting acoustic modes in red giants observed with K2 and TESS. In this talk, I will present this new sample of red giants with their revised stellar parameters derived from asteroseismology. Then I will discuss about the distribution of their masses, distances, and evolutionary states compared to the previously known sample of red giants.
© Owned by the authors, published by EDP Sciences, 2017
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