Radial velocity variability in post-AGB stars: V448 Lac
To investigate the binary hypothesis in the formation of planetary nebulae, we have been doing long-term photometry and radial velocity (RV) monitoring of bright post-AGB stars which possess bipolar or ellipsoidal nebulae but no indication of a disk in their spectral energy distribution, indicative of a binary companion. RV's are determined by cross correlating high-resolution spectra with a line mask. Stellar variability and companions both deform the cross correlation function (CCF) and induce periodic variations in the RV. To uniformly quantify the asymmetry of the CCF from a Gaussian, we propose to fit the CCF profile with a Gauss-Hermite series and determine all CCF parameters (RV, skewness, FWHM, and depth) in one single fit. We analyze the correlation and time series of these CCF parameters for V448 Lac and conclude that its RV variability is most likely due to stellar pulsation and not to an orbiting body.
Publication : Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time. Proceedings of the International Astronomical Union, Volume 343, pp. 533-534
DOI : 10.1017/S1743921318007214
Bibcode : 2019IAUS..343..533V
Keywords : line:profiles; methods:data analysis; techniques: radial velocities; stars: AGB and post-AGB; individual (V448 Lac)