Bright Southern Variable Stars in the bRing Survey
Type de record:
The corresponding data and plots for the 353 variables in the comprehensive survey of bright stars from the bRing telescopes. The paper has been accepted to the Astrophysical Journal Supplemental Series (July 27, 2019). An arXiv pre-print article is now available.
If these data are to be used in future works, we ask that a short list of the bRing team be included as co-authors. Please contact Samuel Mellon (smellon@ur.rochester.edu) or Matthew Kenworthy (kenworthy@strw.leidenuniv.nl) for details.
Paper Abstract:
Besides monitoring the bright star β Pic during the near transit event for its giant exoplanet, the β Pictoris b Ring (bRing) observatories at Siding Springs Observatory, Australia and Sutherland, South Africa have monitored the brightnesses of bright stars (V ≃ 4--8 mag) centered on the south celestial pole (δ ≤ -30∘) for approximately two years. Here we present a comprehensive study of the bRing time series photometry for bright southern stars monitored between 2017 June and 2019 January. Of the 16762 stars monitored by bRing, 353 of them were found to be variable. Of the variable stars, 80% had previously known variability and 20% were new variables. Each of the new variables was classified, including 3 new eclipsing binaries (HD 77669, HD 142049, HD 155781), 26 δ Scutis, 4 slowly pulsating B stars, and others. This survey also reclassified four stars based on their period of pulsation, light curve, spectral classification, and color-magnitude information. The survey data were searched for new examples of transiting circumsecondary disk systems, but no candidates were found.
Data are organized by HD number and camera ID (SAW, SAE, AUE, AUW). If no HD number exists, a HIP number or proper name was used. These data are the FITS files the bRing team has access to. These fits files are described in Stuik, R., Bailey, J. I., Dorval, P., et al. 2017, A&A, 607, A45. Additional detrending steps are described in the article referenced by this repository. The plots are simply organized into variability type (corresponding to the tables in the paper). They are named by their HD number. If there was no HD number, a HIP number or proper name was used instead. The top left panel contains the light curve. The top right panel contains a phase-folded light curve on the primary bRing period. The bottom panel contains the periodogram.