adsabs/AstroCLIMB huggingface dataset:
Paper: Modeling the Optical Colors of Galactic Cirrus Clouds in the Stripe 82 Region
Authors: Kwang-Il Seon, Jongwan Ko, Woowon Byun, Jaehyun Lee, Young-Soo Jo
Figure caption: Maps of scattered light in the SDSS wavelength bands (u, g, r, i, and z) for two realizations with different Mach numbers: Ms = 1 (top panels) and Ms = 6 (bottom panels). The homogeneous optical depth in the g band is assumed to be ﹩{\tau }_{g}^{{\rm{h}}}=1.0﹩ in both cases. The maps are based on two typical random realizations of a lognormal density structure. The numbers (#3 and #7) in parentheses indicate the sample indices among the 10 random realizations of the density distribution. Scattered-light intensities are normalized by the incident ISRF intensity, i.e., Iscatt/IISRF. The effective optical depth ﹩{\tau }_{\lambda }^{{\rm{eff}}}﹩, defined in Equation (4), and the standard deviation σλ of scattered light (for λ = u, g, r, i, and z) are indicated in each map.
Paper: Modeling the Optical Colors of Galactic Cirrus Clouds in the Stripe 82 Region
Authors: Kwang-Il Seon, Jongwan Ko, Woowon Byun, Jaehyun Lee, Young-Soo Jo
Figure caption: SEDs of the two ISRF models. The left and right panels show the SEDs in surface brightness units of erg cm−2 s−1 sr−1 Å−1 and mag arcsec−2, respectively. The models of J. S. Mathis et al. (1983; as updated by B. T. Draine 2011) and S. Bianchi (2024) are plotted as blue and red curves, respectively. The blue and red filled circles indicate the intensities at the central wavelengths of the SDSS bands, calculated by weighting with the SDSS filter functions.
Paper: High-pass Filtering and Gaussian Process Regularization: Stellar Activity Characterization Techniques Applied to the 55 Cancri Planetary System
Authors: Justin Harrell, Sarah E Dodson-Robinson
Figure caption: Best-fit Keplerian orbits for planets b, c, f, and e. In the bottom-right panel, we display the final RV residual after fitting these four planets in addition to the magnetic cycle. Note that the rightmost panels have time rather than orbital phase on the horizontal axis and matching y-axis ranges. Other panels do not necessarily use the same y-axis range. Error bars depicted here are the quadrature sum of errors reported by V. Bourrier et al. (2018) and the instrument-dependent jitter we find in the Appendix. This plot uses the same color scheme as Figure 1.
Paper: High-pass Filtering and Gaussian Process Regularization: Stellar Activity Characterization Techniques Applied to the 55 Cancri Planetary System
Authors: Justin Harrell, Sarah E Dodson-Robinson
Figure caption: Periodograms for each residual RV during the Keplerian fitting process. At this stage, our fitting is done on the GF-detrended RVs. In order of removal, we fit Keplerians to planets b, c, f, and e. The horizontal dotted line represents the 1% FAP, as estimated by a 106 iteration bootstrap simulation of the periodogram.
Paper: High-pass Filtering and Gaussian Process Regularization: Stellar Activity Characterization Techniques Applied to the 55 Cancri Planetary System
Authors: Justin Harrell, Sarah E Dodson-Robinson
Figure caption: Left: periodograms of the undetrended (red) and detrended (blue) RVs, before removing planet b (left) and after removing planet b (right). The shaded gray rectangle has width ﹩2{ \mathcal R }﹩ and shows the interval in which signals are not distinguishable from zero frequency. The black bracket has width ﹩3{ \mathcal R }/4﹩, which is the frequency separation of planet d’s orbit and the activity period given by V. Bourrier et al. (2018).