The EREBOS project -- Investigating the effect of substellar and low-mass stellar companions on late stellar evolution

• Published in: arXiv.org 2019-07
• Main Authors: Schaffenroth, V, Barlow, B N, Geier, S, M Vu{č}ković, Kilkenny, D, Wolz, M, Kupfer, T, Heber, U, Drechsel, H, Kimeswenger, S, Marsh, T, Wolf, M, Pelisoli, I, Freudenthal, J, Dreizler, S, Kreuzer, S, Ziegerer, E
• Format: Article
• Language: English
• Subjects: Algorithms; Binary stars; Eclipsing binary stars; Envelope theory; Gaia Mission; Galactic bulge; Light curve; Machine learning; Photometry; Planetary nebulae; Red giant stars; Reflection; Stellar evolution; Subdwarf stars; Visual effects; White dwarf stars
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1907.09892

Eclipsing post-common envelope binaries are highly important for resolving the poorly understood, very short-lived common envelope phase. Most hot subdwarfs (sdO/Bs) are the bare He-burning cores of red giants which have lost almost all of their hydrogen envelopes. This mass loss is often triggered by common envelope interactions with close stellar or even sub-stellar companions. In the recently published catalog of eclipsing binaries in the Galactic Bulge and in the ATLAS survey, we discovered 161 new eclipsing systems showing a reflection effect by visual inspection of the light curves and using a machine-learning algorithm. The EREBOS (Eclipsing Reflection Effect Binaries from Optical Surveys) project aims at analyzing all newly discovered eclipsing binaries with reflection effect based on a spectroscopic and photometric follow up. To constrain the nature of the primary we derived the absolute magnitude and the reduced proper motion of all our targets with the help of the parallaxes and proper motions measured by the Gaia mission and compared those to the Gaia white dwarf catalogue. For a sub-set of our targets with observed spectra the nature could be derived by measuring the atmospheric parameter of the primary confirming that less than 10\% of our systems are not sdO/Bs with cool companions but white dwarfs or central stars of planetary nebula. This large sample of eclipsing hot subdwarfs with cool companions allowed us to derive a significant period distribution for hot subdwarfs with cool companions for the first time showing that the period distribution is much broader than previously thought and ideally suited to find the lowest mass companions to hot subdwarf stars. In the future several new photometric surveys will be carried out, which will increase the sample of this project even more giving the potential to test many aspects of common envelope theory and binary evolution.