adsabs/AstroCLIMB huggingface dataset:
Paper: Multiwavelength Mitigation of Stellar Activity in Astrometric Planet Detection
Authors: Avi Kaplan-Lipkin, Bruce Macintosh, Alexander Madurowicz, Krishnamurthy Sowmya, Alexander Shapiro, Natalie Krivova, Sami K. Solanki
Figure caption: The spectral transmission profiles of the DR2 revised passbands for Gaia G, B, and R, and the expected passband for the upcoming Small-JASMINE mission. The range between their half maxima are shown as thick colored lines (bottom panel). Also plotted are the spectra used by the SATIRE-S model for the bright faculae, quiet Sun, and dark spot penumbrae and umbrae (upper panel). It can be seen by the overlap of these profiles with the different spectral bands that the amplitude of the astrometric jitter due to each feature will vary across bands, since relative contrast between features varies by band. Due to the close spectral proximity of the visible-light Gaia bands, we expect their astrometry to be more highly correlated with each other than with the near-infrared Small-JASMINE band. Additionally, since the relative contrast between magnetic features is lower at redder wavelengths, we expect motion due to stellar activity to be greater at bluer wavelengths.
Paper: Multiwavelength Mitigation of Stellar Activity in Astrometric Planet Detection
Authors: Avi Kaplan-Lipkin, Bruce Macintosh, Alexander Madurowicz, Krishnamurthy Sowmya, Alexander Shapiro, Natalie Krivova, Sami K. Solanki
Figure caption: The correlation between passband pairs in X displacement due to stellar magnetic activity. Each data point corresponds to a given epoch in the solar simulation. The dashed lines have a slope of 1, corresponding to equal displacement in both passbands. The solid line shows the line of best fit for the data points of that pair of passbands, where the slope, ﹩{ \mathcal M }﹩, is the scaling factor between the amplitudes of one passband and the other, annotated at the top of each plot. Beneath that is the correlation r of the data points as defined in Equation (10).
Paper: Multiwavelength Mitigation of Stellar Activity in Astrometric Planet Detection
Authors: Avi Kaplan-Lipkin, Bruce Macintosh, Alexander Madurowicz, Krishnamurthy Sowmya, Alexander Shapiro, Natalie Krivova, Sami K. Solanki
Figure caption: Multiwavelength noise mitigation using the Gaia R and Gaia B passbands for a case where a planet cannot be detected in any single passband. A planet of mass 0.1 M E is injected into the simulations at semimajor axis 0.1 au. The amplitude spectrum and corresponding signal-to-noise plot is shown for the Gaia R simulation (left panels), with a solid vertical line at the planet’s orbital period. The same respective data is plotted for Gaia B (middle panels), but also with the amplitude spectrum multiplied by the scale factor, to scale the X displacements down to the same amplitude as in the Gaia R passband. (This factor can be found in the second row, first column of Figure 6.) In both single-passband plots, the planet is not actually detected—the S/N does not cross the 6σ threshold at the planet’s orbital period. However, subtracting the scaled down X B amplitudes from the X R amplitudes significantly reduces the noise due to stellar activity and amplifies the planet signal relative to it (right panels). Only after this subtraction is the planet signal flagged as a detection, with the spike indicated by the arrows in the upper right panel.
Paper: Multiwavelength Mitigation of Stellar Activity in Astrometric Planet Detection
Authors: Avi Kaplan-Lipkin, Bruce Macintosh, Alexander Madurowicz, Krishnamurthy Sowmya, Alexander Shapiro, Natalie Krivova, Sami K. Solanki
Figure caption: The shift in the photocenter on different days due to solar magnetic features. Distributions of bright faculae (red) and dark spot penumbrae (blue) and umbrae (black) are shown on the solar disk corresponding to the quiet Sun (gray), as used in the SATIRE-S model. The three crosses give the photocenter position according to shifts due to just faculae (red), just spots (blue), and both faculae and spots (black). Photocenter displacements from the center of the quiet Sun are scaled up by a factor of 1000 to be noticeable. The upper left panel shows a distribution dominated by dark spots repelling the photocenter, and the upper right panel shows a distribution dominated by bright faculae attracting the photocenter. The bottom panels show distributions with significant contributions from both faculae and spots, but in the bottom right panel these contributions happen to be nearly equal and opposite, canceling each other out and leaving almost no overall photocenter shift.