adsabs/AstroCLIMB huggingface dataset:
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: Features of the 5pGP model. Left: phase-folded best-fit orbit of planet d. Center: median GP prediction; note the dominance of signal drift over periodicity. Right: residual of the 5pGP model. Note the changing vertical axis scales. This plot uses the same color scheme as Figures 1 and 4.
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: Distribution of residuals normalized by the reported observation uncertainty. The best-fit Gaussian distributions are superposed. We interpret the distributions being broader than a standard normal distribution ﹩{ \mathcal N }(0,1)﹩ as arising from jitter unaccounted for in the reported error bars. We estimate this combination of stellar and instrumental jitter via Equation (A4). Insets: CDF fits for each normalized residual.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Original images (top row), ground-truth silhouettes (second row), corresponding silhouettes (third row), and silhouette differences (bottom row) of (a, b) Itokawa and (c, d) Bennu.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Workflow of the proposed method for optimized asteroid rotation and shape modeling.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Schematic of the asteroid observation scenario.
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Moment-zero map (left) and p–v diagram (right) of K 3-35. The cross and triangle mark the positions of the bubble center and PN, respectively. The approximate extent of H I absorption associated with the K 3-35 bubble in the p–v diagram is shown as a dashed rectangle.
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Same as Figure 2 but for Sh 2-71.
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Channel maps in the velocity range from 0 to 40 km s−1 with a channel width of 2 km s−1. The plus represents the position of K 3-35. The cross marks the position of a carbon star vul 10. The galactic coordinate system is shown by the white dashed line in the upper right panel, and the arrow in the upper left panel indicates the proper-motion direction.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Visualization of Itokawa reconstruction quality at observation latitude of 30° and Sun phase angle of 60°. Reconstruction quality viewed from the (a) +x-, (b) +y-, (c) +z-, (d) -x-, (e) -y-, and (f) -z-axes. The color bar graph indicates the absolute distance from our model to the referenced shape model of Itokawa.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Visualization of Itokawa reconstruction quality at different observation distances (top to bottom: 350, 300, 250, 200, 150, 100, and 50 km). Reconstruction quality viewed from the (a) +x-, (b) +y-, and (c) +z-axes. The color bar graph indicates the absolute distance from our model to the referenced shape model of Itokawa.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Visualization of Bennu reconstruction quality at different observation distances (top to bottom: 200, 150, 100, and 50 km). Reconstruction quality viewed from the (a) +x-, (b) +y-, and (c) +z-axes. The color bar graph indicates the absolute distance from our model to the referenced shape model of Bennu.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Estimated surface displacement at observation latitude of 30° and Sun phase angle of 60°. (a) Frame 54, (b) Frame 55, (c) Reference optical flow, and (d) Estimated surface displacement.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Three-sided views of the ground-truth shape model of Bennu. Views from the positive directions of the (a) x-, (b) y-, and (c) z-axes.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: The extraction of large l3s from BFs. The left two panels ((a) and (c)) compare the BFs corresponding to two different phases of a system containing a large l3 (blue curves) to the BF of a slowly rotating single star (orange curves). The right two panels ((b) and (d)) contrast the results of subtracting a Gaussian fit to l3 (producing the blue curves) with the results of subtracting the scaled, shifted single star’s BF (producing the orange curves). The latter yields a superior subtraction of l3.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: The top panel shows the phase-folded Kepler data for KIC03443519 with the joint fit LC solution (magenta curve). The lower panel shows the residuals with a spline fit (green curve) to guide the eye to any systematics.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system KIC03443519 (blue lines) with joint PHOEBE fits (black lines) and residuals (salmon lines). The pale blue spike is the tertiary that we subtracted before the performing the joint fit. Labels “1” and “2” denote the primary and secondary components, respectively. While not visible here due to small required shifts, the gray curves show the unshifted model BFs. The average required shift is taken to be the systemic velocity, γ, given at the top of the bottom panel.
Paper: Aligned Stellar Obliquities for Two Hot Jupiter-hosting M Dwarfs Revealed by MAROON-X: Implications for Hot Jupiter Formation
Authors: Drew Weisserman, Erik Gillis, Ryan Cloutier, Nina Brown, Jacob L. Bean, Andreas Seifahrt, Tanya Das, Madison Brady, Bertram Bitsch, Emily Deibert, Thomas M. Evans-Soma, Noah Fenlon, Laura Kreidberg, Michael Line, Ralph Pudritz, Evgenya L. Shkolnik, Luis Welbanks
Figure caption: The distribution of projected stellar obliquities ∣λ∣ for giant exoplanets (Rp ≥ 5 R⊕) as a function of host star effective temperature. All stellar obliquity measurements come from measurements of the McLaughlin effect and are retrieved from the NASA Exoplanet Archive. Hot Jupiters around M dwarfs (HJMDs) occupy the shaded red region of parameter space with Teff < 3900 K, while host stars above the Kraft break (Teff ≥ 6100 K) occupy the shaded blue region. The HJMDs TOI-3714 b and TOI-5293 A b from this work, and TOI-4201 (T. Gan et al. 2024) are highlighted by red arrows.
Paper: Aligned Stellar Obliquities for Two Hot Jupiter-hosting M Dwarfs Revealed by MAROON-X: Implications for Hot Jupiter Formation
Authors: Drew Weisserman, Erik Gillis, Ryan Cloutier, Nina Brown, Jacob L. Bean, Andreas Seifahrt, Tanya Das, Madison Brady, Bertram Bitsch, Emily Deibert, Thomas M. Evans-Soma, Noah Fenlon, Laura Kreidberg, Michael Line, Ralph Pudritz, Evgenya L. Shkolnik, Luis Welbanks
Figure caption: Left: a comparison of the various frequency terms featured in Equation (5) obtained from the literature for early M dwarfs, FGK stars, and A stars. The terms fHJ, fCJ, fmult, and fmisaligned denote, respectively, the observed occurrence rates of hot Jupiters, cold Jupiters, the stellar multiplicity fractions, and the fraction of stellar binaries that are misaligned by ≥39° drawn from an isotropic distribution (i.e., 36.8%). The predicted frequency of HJs formed via KL migration is the distribution fHJ,pred = fCJSbin fmult fmisaligned (see Equation (5)). Right: cumulative distribution functions of the HJ formation efficiency by KL migration (fHJ/fHJ,pred) for each class of star considered herein.
Paper: Aligned Stellar Obliquities for Two Hot Jupiter-hosting M Dwarfs Revealed by MAROON-X: Implications for Hot Jupiter Formation
Authors: Drew Weisserman, Erik Gillis, Ryan Cloutier, Nina Brown, Jacob L. Bean, Andreas Seifahrt, Tanya Das, Madison Brady, Bertram Bitsch, Emily Deibert, Thomas M. Evans-Soma, Noah Fenlon, Laura Kreidberg, Michael Line, Ralph Pudritz, Evgenya L. Shkolnik, Luis Welbanks
Figure caption: Results of orbital fits to Gaia DR3 astrometric data for the binary systems TOI-3714 (upper row) and TOI-5293 (lower row). Left column: a random selection of sky-projected binary orbit solutions from our astrometric fit posteriors. Right column: the distribution of minimum mutual inclinations between each system’s planet and binary companion. The vertical dashed line at ﹩\arccos \sqrt{3/5}\approx 39\mathop{.}\limits^{^\circ }2﹩ corresponds to the minimum mutual inclination needed to drive KL migration. The percentiles of the mutual inclination distribution above and below ﹩39\mathop{.}\limits^{^\circ }2﹩ are depicted by different colors and are annotated for each system.
Paper: Aligned Stellar Obliquities for Two Hot Jupiter-hosting M Dwarfs Revealed by MAROON-X: Implications for Hot Jupiter Formation
Authors: Drew Weisserman, Erik Gillis, Ryan Cloutier, Nina Brown, Jacob L. Bean, Andreas Seifahrt, Tanya Das, Madison Brady, Bertram Bitsch, Emily Deibert, Thomas M. Evans-Soma, Noah Fenlon, Laura Kreidberg, Michael Line, Ralph Pudritz, Evgenya L. Shkolnik, Luis Welbanks
Figure caption: Our raw MAROON-X data of TOI-3714 b (top panel) and TOI-5293 A b (two lower panels). The blue arm, red arm, and combined RVs are depicted by the translucent blue, red, and solid markers, respectively. The solid lines depict random draws from each planet’s known Keplerian orbit posterior (TOI-3714 b; C22, TOI-5293 A b; C23). The vertical shaded regions highlight each planet’s in-transit window.
Paper: Aligned Stellar Obliquities for Two Hot Jupiter-hosting M Dwarfs Revealed by MAROON-X: Implications for Hot Jupiter Formation
Authors: Drew Weisserman, Erik Gillis, Ryan Cloutier, Nina Brown, Jacob L. Bean, Andreas Seifahrt, Tanya Das, Madison Brady, Bertram Bitsch, Emily Deibert, Thomas M. Evans-Soma, Noah Fenlon, Laura Kreidberg, Michael Line, Ralph Pudritz, Evgenya L. Shkolnik, Luis Welbanks
Figure caption: The RM effect signatures for TOI-3714 b (left panel) and TOI-5293 A b (right panel). Each set of markers depicts the combined MAROON-X RV observations (i.e., blue plus red channels) for each transit sequence observed. The black curves represent random draws from our RM model posteriors after removing the median detrending model for each transit and the planet-induced Keplerian orbital signals.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Spot diagrams of the LAMOST NIR spectrograph prototype under three operational modes at room temperature (20°C). The rectangle in each panel represents a 2 × 2 pixel area (40 × 40 μm). All spots are calculated for key object points (|x| = 33, 52, and 64.15 mm) within the scientific field of view. Top left: mode 1 (grating angle 10﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2, covering 0.9 ∼ 1.015 μm and 1.192 ∼ 1.305 μm); top right: mode 2 (grating angle 11﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5, covering 1.015 ∼ 1.125 μm and 1.301 ∼ 1.41 μm); bottom: mode 3 (grating angle 12﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5, covering 1.1 ∼ 1.21 μm and 1.385 ∼ 1.495 μm). The root mean square (rms) spot diameter is below 40 μm for all field points and modes, which is well within the geometric image extent of the fiber and thus demonstrates uniform image quality sufficient for spectroscopic requirements.
Paper: A Systematic Search for Gaseous Debris Disks in DESI Early Data Release White Dwarfs
Authors: Ziying Ma, 紫莹 马, Xiaoxia Zhang, 小霞 张, Taotao Fang, 陶陶 方, Junfeng Wang, 俊峰 王, Jincheng Guo, 金承 郭, Xiaochuan Jiang, 小川 姜, Zhi-Xiang Zhang, 志翔 张, Hu Zou, 虎 邹
Figure caption: Pan-STARRS z-band images (top row) and SED fits (bottom row) for the three candidate gaseous-debris-disks white dwarfs showing infrared excess. From left to right: WD J0849+0923 (ID = 8), WD J1434+1508 (ID = 12), and WD J1100+7138 (ID = 14). Each z-band image is centered on the DESI source position, with a red circle of 6″ radius indicating the absence of visible contaminants within the typical WISE beam. The SED panels show photometric data from SDSS (magenta diamonds), Pan-STARRS (green triangles), 2MASS (blue squares), UKIDSS (cyan circles), and WISE (red stars), along with the DESI spectrum in gray. The best-fit model (black solid line) includes contributions from the white dwarf photosphere (blue dashed line) and a dusty disk (red dotted line). The derived disk parameters (inner radius Rin and inclination i) are listed.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Theoretical throughput of the LAMOST NIR spectrograph prototype. Solid lines show the efficiency of the refractive camera design presented in this work across three operational modes. The dashed line shows, for comparison, the efficiency of a Schmidt camera design within the same optical layout. The refractive design achieves a peak efficiency of 65%, significantly exceeding the 35% requirement, and outperforms the Schmidt design (peak efficiency ∼50%) by approximately 10% on average across the band, primarily due to its unobstructed optical layout.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Comparison of international camera designs for similar spectrographs. Left: the PFS (Subaru) NIR camera employs a Mangin–Schmidt design, comprising a double-Schmidt corrector, two spherical camera mirrors, and an aspheric field lens. Right: the DESI NIR camera uses an all-refractive design with five lenses, including a triplet group; two aspheric surfaces are located on the front of the first and the last lens, respectively. The design in this work is also refractive, akin to DESI, but was independently optimized for the LAMOST interface parameters.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Spectral resolution under the three operational modes. Solid lines represent the resolution with the nominal slit width (R ≈ 900–1530); dashed lines show the resolution with the slit reduced to two-thirds of its width (R ≈ 1400–2300). The segmented nature of the curves results from physical gaps in the 2 × 2 detector mosaic. Despite this, the resolution at all wavelengths and for all modes meets the design requirement of R > 1500 at the central wavelength.
Paper: Optical Design of a Near-infrared Spectrograph Prototype for LAMOST
Authors: Xiaojie Zhang, Yonghui Hou, Jun Li, Haoran Yu, Hangxin Ji
Figure caption: Comparison of spot diagrams for the LAMOST NIR spectrograph prototype at different temperatures. Top left: 15°C before focus adjustment; top right: 15°C after adjustment; bottom left: 25​​​​​°C before adjustment; bottom right: 25°C after adjustment. All refocusing displacements were within ±0.04 mm. The results demonstrate that active focus compensation effectively mitigates thermal defocus, maintaining image quality consistent with the 20°C reference state across the 15°C–25°C operational range.
Paper: A Systematic Search for Gaseous Debris Disks in DESI Early Data Release White Dwarfs
Authors: Ziying Ma, 紫莹 马, Xiaoxia Zhang, 小霞 张, Taotao Fang, 陶陶 方, Junfeng Wang, 俊峰 王, Jincheng Guo, 金承 郭, Xiaochuan Jiang, 小川 姜, Zhi-Xiang Zhang, 志翔 张, Hu Zou, 虎 邹
Figure caption: Normalized spectra of the 22 white dwarfs with candidate gaseous debris disks in the vicinity of the Ca II infrared triplet, displayed in order of their IDs (labeled at top left). For each source, the black curve shows the continuum-subtracted spectrum, the red curve shows the best-fit model comprising three Gaussians, and the vertical ticks mark the rest-frame wavelengths of the triplet.
Paper: A Systematic Search for Gaseous Debris Disks in DESI Early Data Release White Dwarfs
Authors: Ziying Ma, 紫莹 马, Xiaoxia Zhang, 小霞 张, Taotao Fang, 陶陶 方, Junfeng Wang, 俊峰 王, Jincheng Guo, 金承 郭, Xiaochuan Jiang, 小川 姜, Zhi-Xiang Zhang, 志翔 张, Hu Zou, 虎 邹
Figure caption: Gaia color–magnitude diagram for the 22 candidate debris disks (blue diamonds), compared to the parent DESI EDR white dwarf sample (gray circles).
Paper: Was there a (Super)nova in 1408?
Authors: Boshun Yang, Nikolaus Vogt, Susanne M Hoffmann
Figure caption: Model lightcurves for typical novae (left) and the specific Nova Vulpeculae 1968 after J. E. Isles (1972; right) with our highlighting of the first 10 days: the slight variability (﹩4.{9}_{-0.3}^{+0.2}﹩ mag) would not be recognized by naked eye observers. The t3 time would still be ∼100 days for a fast nova (Na-type).
Paper: Was there a (Super)nova in 1408?
Authors: Boshun Yang, Nikolaus Vogt, Susanne M Hoffmann
Figure caption: Search field of the 1408 (super)nova. The vertical dashed lines represent the boundaries between different lodges. We used coordinates (R.A./decl.)1363 as we want to show the constellations in their view of this epoch. The modern coordinates of our field (R.A./decl.)2000 are given in Table 1.
Paper: Was there a (Super)nova in 1408?
Authors: Boshun Yang, Nikolaus Vogt, Susanne M Hoffmann
Figure caption: Observation drawn by M. Hevelius (1670; left) and lightcurve (right) of the Nova Vul 1670–1672 by (M. M. Shara et al. 1985) from observations of Anthelme, Cassini, Hevelius, and various anonymous members of the Académie des Sciences, Paris.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The boxplots of the residual of estimated parameters for data sets with accuracy or inaccuracy in observed uncertainty level. In each panel, the first bin contains the first 40 data sets from Sample 1, which has accuracy in observed uncertainty level. The second and third bins include the data set from Samples 5.1 and 5.2, for which the observed uncertainty level is systematically overestimated and underestimated by a factor of 1.1 and 0.9, respectively. The last bin contains the data sets from Sample 5.3, in which the observed uncertainty level of each data point is scaled by a random number uniformly distributed in [0.9, 1.1]. Horizontal dashed red lines have the same sense as those in Figure 4.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The boxplots of the residual of estimated parameters within different k2 bins in Sample 2. A horizontal dashed red line at zero indicates no bias in the residuals. For reference, we include additional horizontal dashed red lines at +0.2 and −0.2.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The MAE of k (left), b (middle), and σ (right) as functions of typical S/N of xobs (top) and yobs (bottom), obtained using different regression methods as indicated. The error bars for the KS-test-based method and ML-based method and the shaded regions for the other methods indicate the range from 25% quantile to 75% quantile of the absolute errors within each bin of S/N.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The boxplots of the residual of estimated parameters for data sets without outliers (first 40 data sets from Sample 1), with distribution outliers (Sample 6), and with correlation outliers (Sample 7). Horizontal dashed red lines have the same sense as those in Figure 4.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The boxplots of the residual of estimated parameters for data sets without the saturation effect (first 40 data sets from Sample 1) and data sets with the saturation effect (sample 8). Horizontal dashed red lines have the same sense as those in Figure 4.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The boxplots of the residual of estimated parameters for data sets from Sample 1 and Sample 4 with different correlations between intrinsic value and uncertainty level. Horizontal dashed red lines have the same sense as those in Figure 4.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The boxplots of the residual of estimated parameters for data sets from Sample 1 and Sample 3 with different intrinsic ﹩\mathrm{log}x﹩ distributions. Horizontal dashed red lines have the same sense as those in Figure 4.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: Same as Figure 4, but for different k3 bins.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: Coverage test for the KS-test-based method, the ML-based method, and LINMIX.
Paper: The NEID Earth Twin Survey. II. Dynamical Masses in Seven High-acceleration Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake, Paul Robertson, Andrea S. J. Lin, Arvind F. Gupta, Suvrath Mahadevan, Jason T. Wright, Daniella Bardalez Gagliuffi, Jiayin Dong, Rachel B. Fernandes, Evan Fitzmaurice, Samuel Halverson, Shubham Kanodia, Sarah E. Logsdon, Jacob K. Luhn, Michael W. McElwain, Andy Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Gudmundur Stefánsson, Ryan Terrien, Jason D. Eastman, Jonathan Horner, Peter Plavchan, Sharon X. Wang, Maurice L. Wilson, Robert A. Wittenmyer
Figure caption: Best-fit RV models for the three planetary systems presented in this analysis (top left: HD 217107; top right: HD 190360; bottom middle: HD 154345). Each panel also includes phase-folded RV curves for planets. Both two-planet systems (HD 217107 and HD 190360) show planet b on top of planet c. The error bars in each panel include instrumental RV jitter terms, which have been independently fit for, and the colors of the data points corresponding to those provided in Figure 2.