Details

Autor(en) / Beteiligte

• Audenaert, J.
• Kuszlewicz, J. S.
• Handberg, R.
• Tkachenko, A.
• Armstrong, D. J.
• Hon, M.
• Kgoadi, R.
• Lund, M. N.
• Bell, K. J.
• Bugnet, L.
• Bowman, D. M.
• Johnston, C.
• García, R. A.
• Stello, D.
• Molnár, L.
• Plachy, E.
• Buzasi, D.
• Aerts, C.

Titel

TESS Data for Asteroseismology (T’DA) Stellar Variability Classification Pipeline: Setup and Application to the Kepler Q9 Data

Ist Teil von

• The Astronomical journal, 2021-11, Vol.162 (5), p.209

Ort / Verlag

Madison: The American Astronomical Society

Erscheinungsjahr

2021

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• Abstract The NASA Transiting Exoplanet Survey Satellite (TESS) is observing tens of millions of stars with time spans ranging from ∼27 days to about 1 yr of continuous observations. This vast amount of data contains a wealth of information for variability, exoplanet, and stellar astrophysics studies but requires a number of processing steps before it can be fully utilized. In order to efficiently process all the TESS data and make it available to the wider scientific community, the TESS Data for Asteroseismology working group, as part of the TESS Asteroseismic Science Consortium, has created an automated open-source processing pipeline to produce light curves corrected for systematics from the short- and long-cadence raw photometry data and to classify these according to stellar variability type. We will process all stars down to a TESS magnitude of 15. This paper is the next in a series detailing how the pipeline works. Here, we present our methodology for the automatic variability classification of TESS photometry using an ensemble of supervised learners that are combined into a metaclassifier. We successfully validate our method using a carefully constructed labeled sample of Kepler Q9 light curves with a 27.4 days time span mimicking single-sector TESS observations, on which we obtain an overall accuracy of 94.9%. We demonstrate that our methodology can successfully classify stars outside of our labeled sample by applying it to all ∼167,000 stars observed in Q9 of the Kepler space mission.