The Göttingen Solar Radial Velocity Project: Sub-m s−1 Doppler Precision from FTS Observations of the Sun as a Star. (23rd June 2016)

• Record Type: Journal Article
• Authors: Lemke, U.; Reiners, A.
• Is Part Of: Publications of the Astronomical Society of the Pacific. Volume 128:Number 967(2016)
• Publication Date: 2016-06-23
• Subjects: line: profiles -- instrumentation: spectrographs -- methods: data analysis -- methods: observational -- techniques: radial velocities -- techniques: spectroscopic -- Sun: general -- planets and satellites: detection; Astronomy -- Periodicals; Astronomy; Periodicals; Periodicals; 520.5
• DOI: 10.1088/1538-3873/128/967/095002
• Languages: English
• ISSNs: 0004-6280

Abstract

Abstract: Radial velocity observations of stars are entering the sub-m s −1 domain revealing fundamental barriers for Doppler precision experiments. Observations of the Sun as a star can easily overcome the m s −1 photon limit but face other obstacles. We introduce the Göttingen Solar Radial Velocity Project with the goal of obtaining high-precision (cm s −1 ) radial velocity measurements of the Sun as a star with a Fourier Transform Spectrograph. In this first paper, we present the project and first results. The photon limit of our 2 minute observations is at the 2 cm s −1 level but is currently limited by strong instrumental systematics. A drift of a few m s −1 hr −1 is visible in all observing days, probably caused by vignetting of the solar disk in our fiber-coupled setup, and imperfections of our guiding system add further offsets in our data. Binning the data into 30 minute groups shows m s −1 stability after correcting for a daily and linear instrumental trend. Our results show the potential of Sun-as-a-star radial velocity measurements that can possibly be achieved after a substantial upgrade of our spectrograph coupling strategy. Sun-as-a-star observations can provide crucial empirical information about the radial velocity signal of convective motion and stellar activity and on the wavelength dependence of radial velocity signals caused by stellar line profile variations.