Consistent radial velocities of classical Cepheids from the cross-correlation technique

Abstract

Accurate radial velocities ($v_{\mathrm{rad}}$) of Cepheids are mandatory within the context of distance measurements via the Baade-Wesselink technique. The most common $v_{\mathrm{rad}}$ derivation method consists in cross-correlating the observed spectrum with a binary template and measuring a velocity on the resulting profile. Yet for Cepheids, the spectral lines selected within the template as well as the way of fitting the cross-correlation function (CCF) have a significant impact on the measured $v_{\mathrm{rad}}$. We detail the steps to compute consistent Cepheid CCFs and $v_{\mathrm{rad}}$, and we characterise the impact of Cepheid spectral properties and $v_{\mathrm{rad}}$ computation method on the resulting line profiles. We collected more than 3900 high-resolution spectra from seven different spectrographs of 64 classical Cepheids. These spectra were standardised through a single process on pre-defined wavelength ranges. We built six correlation templates selecting un-blended lines of different depths from a synthetic Cepheid spectrum, on three different wavelength ranges from 390 to 800 nm. Each spectrum was cross-correlated with these templates to build the corresponding CCFs. We derived a set of line profile observables as well as three different $v_{\mathrm{rad}}$ measurements from each CCF. This study confirms that both the template wavelength range, its mean line depth and width, and the $v_{\mathrm{rad}}$ computation method significantly impact the $v_{\mathrm{rad}}$. Deriving more robust Cepheid $v_{\mathrm{rad}}$ time series require to minimise the asymmetry of the line profile and its impact on the $v_{\mathrm{rad}}$. Centroid $v_{\mathrm{rad}}$, that exhibit slightly smaller amplitudes but significantly smaller scatter than Gaussian or biGaussian $v_{\mathrm{rad}}$, should thus be favoured. Stronger lines are also less asymmetric and lead to more robust $v_{\mathrm{rad}}$ than weaker lines.

24 pages, 18 figures, 4 tables. Formally accepted for publication in Astronomy & Astrophysics on August 5th, 2019

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