Extended Data for Publication "Testing the Spectroscopic Extraction of Suppression of Convective Blueshift"

<p>Efforts to detect low-mass exoplanets using stellar radial velocities (RVs) are currently limited by magnetic photospheric activity. Suppression of convective blueshift is the dominant magnetic contribution to RV variability in low-activity Sun-like stars. Due to convective plasma motions, the magnitude of RV contributions from the suppression of convective blueshift is roughly correlated with the depth of formation of photospheric spectral lines used to compute the RV time series. Meunier et al. (2017), used this relation to demonstrate a method for spectroscopic extraction of the suppression of convective blueshift in order to isolate RV contributions, including planetary RVs, that contribute equally to the timeseries for each spectral line. In this publication, we extract disk-integrated solar RVs from observations over a 2.5 year time span made with the solar telescope integrated with the HARPS-N spectrograph at the Telescopio Nazionale Galileo (La Palma, Canary Islands, Spain). We apply the methods outlined by Meunier et al. (2017) - as part of this analysis, we fit Gaussian line profiles to 765 iron lines measured over 457 exposures.</p> <p>Here, we provide the complete line list (Table 1; Table1_LineList.csv) used in our analysis, and the resulting RVs time series in their entirety (Table 3; Table3_TimeSeries.csv). Wavelengths are given in Angstroms, and RVs in m/s.</p> <p>We also include 4 CSV files with the line fit parameters of each line profile: Each row corresponds to a single exposure time (corresponding to the JDs in Table 3) and each column corresponds to a specific spectral line (with wavelength specified in Table 1).</p> <p>We fit each spectral line to a Gaussian of the form:</p> <p><span class="math-tex">\(f(\lambda) = p_1 - p_2 \exp \left[- {1 \over 2} \left({{\lambda - p_3} \over p_4}\right)^2 \right]\)</span></p> <p>p₁ is the continuum level in arbitrary units (LineProfiles_Continuum.csv)<br> p₂ is the line strength in arbitrary units (LineProfiles_Amplitude.csv)<br> p₃ is the line shift in Angstroms (LineProfiles_Shift.csv)<br> p₄ is the line width in Angstroms (LineProfiles_Width.csv)</p>