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gaia data release 3 documentation

10.14 Upper main-sequence oscillators

10.14.1 Introduction

Many stars in the upper part of the main-sequence (early-F and hotter) show photometric variability, intrinsic and/or extrinsic. This population not only includes pulsators such as γ Doradus, δ Scuti, SX Phoenicis, Slowly Pulsating B, and β Cephei stars, but also (often chemically peculiar) spotted stars that show rotational modulation of their brightness, such as α2 Canum Venaticorum and SX Arietis stars. Other examples of variability classes present in this part of the Hertzsprung–Russell diagram include Be and Ae stars, as well as the eruptive γ Cassiopeiae variables.

The catalogue described here (see table vari_ms_oscillator) contains 54 thousand candidates of the five classes of main-sequence κ-oscillators mentioned above, where the main selection criterion is the presence of a significant peak in the Fourier spectrum of the Gaia light curve in the relevant frequency range. We purposely did not attempt to aggressively remove possible contamination of extrinsic variables using Gaia data alone, as this is best done using a multi-survey approach including other data products in addition to G-band photometry. The catalogue does explicitly exclude binary stars, as these are listed in a separate catalogue.