adsabs/AstroCLIMB huggingface dataset:
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Temporal medians of “extreme,” “moderate,” and “quiescent” simulations for Temperature (T in K). Medians are taken from 8 yr and for (a) 1.223 × 10−5 mbar and (b) 0.008 mbar atmospheric levels. Extreme and moderate medians are only taken for days when flares occur. Stippling uses a two-tailed Wilcoxon rank-sum test to represent “extreme” and “moderate” areas that are not statistically different from the “Qquiescent” one at p < 0.01.
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Same as Figure 1, but for Wind Speed (WS, m s−1) and water vapor (H2O, mol mol−1) as natural logarithms.
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Vertical profile of wind speed (m s−1) temporal and field median difference between two sets of simulations over −15∘–15∘N, 0∘–50∘E. Circles represent differences that are not statistically significant at the 1% level following a two-tailed Wilcoxon rank-sum test.
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Same as Figure 1, but for nitrogen oxide (NO in mol mol−1) and hydroxide (OH in mol mol−1). Given the large spread between the simulations, values are shown as natural logarithms.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The logarithm of median CO (2–1) flux in each F2100W flux bin for each galaxy is shown as black circles with error bars (for real data, the error bar represents 1σ uncertainty of the median) and blue circles (for mock data generated by the best-fitting results of the KS-test-based method). The best-fitting relations of the KS-test-based method, mODR, and LINMIX on real data are shown as blue, red, and green lines, respectively. The two vertical dotted lines in each panel indicate the 5th and 95th percentiles of the F2100W flux distribution, which is shown in each upper subpanel. Note that the data points with negative F2100W flux measurements are discarded when plotting the marginalized distribution in logarithm space, while they are included when calculating 5th and 95th percentiles.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The difference in the estimated k (top row), b (middle row), and σ (bottom row) by mODR (red circles) and LINMIX (green squares) relative to the estimates obtained from the KS-test-based method is shown as a function of the typical S/N of the independent variable. The error bars indicate 1σ uncertainties. This analysis is applied on real data (left column), generated data based on the results of the KS-test-based method with noise (middle column), and generated data without noise (right column). The LINMIX is not applied on generated data without the noise, due to the numerical issue caused by the zero uncertainty.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The best-fitting parameters k, b, and σ (alongside their 1σ uncertainties represented as error bars) of the loglinear correlation between the CO (2–1) flux and the MIR fluxes at four JWST bands (F770W, F1000W, F1130W, and F2100W, ordered from left to right for a given galaxy), as obtained for the four galaxies (as indicated) and using three regression methods: the KS-test-based method (black circles), mODR (red circles), and LINMIX (green circles).
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: In the top row, the distributions of all data points are shown as the black contours. The blue, red, and green contours represent the distribution of mock data points generated based on the best-fitting loglinear relationship obtained by the KS-test-based method, mODR, and LINMIX, respectively. The blue, red, and green lines represent the underlying relationship. In the bottom row, the differences in the number of data points in each bin between the generated data and the real data (Nreal − Ngenerated) are color-coded.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: Same as Figure 3, but for sample size.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: Left and middle: 10 different predefined distributions of ﹩P(\mathrm{log}x)﹩ used for all samples except Sample 3. Right: three different predefined distributions of ﹩P(\mathrm{log}x)﹩ used for Sample 3.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: Comparisons between loglinear correlations (orange lines) and their saturated versions (red lines). The light-blue circles represent the data points with saturated loglinear relationship and intrinsic scatter.
Paper: Regression for Astronomical Data with Realistic Distributions, Errors, and Nonlinearity
Authors: Tao Jing, Cheng Li
Figure caption: The examples of different correlations between x and xerr.
Paper: The Disks In Scorpius–Centaurus Survey (DISCS). I. Four Newly Resolved Debris Disks in Polarized Intensity Light
Authors: Justin Hom, Thomas M. Esposito, Katie A. Crotts, Gaspard Duchêne, Jennifer Patience, Johan Mazoyer, Robert J. De Rosa, Christine H. Chen, Paul Kalas, Bruce Macintosh, Brenda C. Matthews
Figure caption:  ﹩{{ \mathcal Q }}_{\phi }﹩ images of all sample targets, oriented with north pointing up and east pointing left, in flux units of mJy arcsec−2. The white circle represents the extent of the FPM of GPI, 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩12 in radius. To maintain a consistent color bar for all images, the ﹩{{ \mathcal Q }}_{\phi }﹩ images of HD 112810 and HD 113556 are scaled up by a factor of two. HD 98363, HD 109832, and HD 146181 show the clearest detections. The HD 112810 image shows a lower-SNR detection, and a hint of an arc is seen east of the star in the image of HD 113556. The detections in HD 112810 and HD 113556 become more obvious after smoothing with a Gaussian kernel, shown in Figure 2.
Paper: The Disks In Scorpius–Centaurus Survey (DISCS). I. Four Newly Resolved Debris Disks in Polarized Intensity Light
Authors: Justin Hom, Thomas M. Esposito, Katie A. Crotts, Gaspard Duchêne, Jennifer Patience, Johan Mazoyer, Robert J. De Rosa, Christine H. Chen, Paul Kalas, Bruce Macintosh, Brenda C. Matthews
Figure caption:  ﹩{{ \mathcal Q }}_{\phi }﹩ images of HD 112810 and HD 113556, smoothed with Gaussian kernels of FWHM ∼ 2 and 4, respectively. The eastern arc (indicated by white arrows) seen in HD 113556 is more noticeable but still faint.
Paper: Improving Source Positions in the OCARS Catalog: A First Approach
Authors: Zinovy Malkin
Figure caption: Differences between the RFC catalog transformed to the ICRF3 GA model and the original RFC catalog.
Paper: Improving Source Positions in the OCARS Catalog: A First Approach
Authors: Zinovy Malkin
Figure caption: Differences between the USN and ICRF3-SX catalogs (USN minus ICRF3-SX) after removing outliers. The bottom panel shows results of VSH decomposition for degrees l = 1…4.
Paper: Improving Source Positions in the OCARS Catalog: A First Approach
Authors: Zinovy Malkin
Figure caption: Differences between the RFC and ICRF3-SX catalogs (RFC minus ICRF3-SX) after removing outliers The bottom panel shows results of VSH decomposition for degrees l = 1…4.
Paper: Improving Source Positions in the OCARS Catalog: A First Approach
Authors: Zinovy Malkin
Figure caption: VSH decomposition of the differences between the OCARS and ICRF3-SX catalogs (OCARS minus ICRF3-SX).
Paper: The Disks In Scorpius–Centaurus Survey (DISCS). I. Four Newly Resolved Debris Disks in Polarized Intensity Light
Authors: Justin Hom, Thomas M. Esposito, Katie A. Crotts, Gaspard Duchêne, Jennifer Patience, Johan Mazoyer, Robert J. De Rosa, Christine H. Chen, Paul Kalas, Bruce Macintosh, Brenda C. Matthews
Figure caption: Comparison of surface brightness profiles between two identical convolved disk models at distances of 50 and 100 pc. The measurement of surface brightness around the fitted ansae of both models is comparable, with the 100 pc disk ansae fainter by a factor of ∼1.12. As a result, Fans/F* for the 100 pc model is higher by a factor of ∼3.58 compared to the 50 pc model.
Paper: The Disks In Scorpius–Centaurus Survey (DISCS). I. Four Newly Resolved Debris Disks in Polarized Intensity Light
Authors: Justin Hom, Thomas M. Esposito, Katie A. Crotts, Gaspard Duchêne, Jennifer Patience, Johan Mazoyer, Robert J. De Rosa, Christine H. Chen, Paul Kalas, Bruce Macintosh, Brenda C. Matthews
Figure caption: Background tracks calculated for both HD 108904 (left) and HD 113556 (right). The ΔR.A. and Δdecl. offsets for both candidate companions are consistent with being background objects.
Paper: The Disks In Scorpius–Centaurus Survey (DISCS). I. Four Newly Resolved Debris Disks in Polarized Intensity Light
Authors: Justin Hom, Thomas M. Esposito, Katie A. Crotts, Gaspard Duchêne, Jennifer Patience, Johan Mazoyer, Robert J. De Rosa, Christine H. Chen, Paul Kalas, Bruce Macintosh, Brenda C. Matthews
Figure caption: Fans/F* as a function of ﹩\cos i﹩ for identical systems at different inclinations. The slope of the trend is negative but spans less than an order of magnitude in difference. By comparison, the GPIES and DISCS samples combined span several orders of magnitude across the same space in inclination.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: A randomly selected 200 kyr stability test of the HD 3167 system having a configuration that planets d, c, and e are initially coplanar, while planet b is significantly inclined relative to the other three planets. Upper left: the position of all planets during the 200 kyr simulation in Cartesian coordinates. Upper right: the evolution of true stellar obliquity (ψ). The shaded region illustrates the true stellar obliquity of planet b is lower than 30°. Lower right: the evolution of ascending node (Ω). Lower left: the 6 kyr evolution of the impact factor for all planets for an observer positioned at a random and fixed location where transits of HD 3167 b and c are detectable at time equal to zero. The shaded regions indicate the time during which the selected observer can detect the planets transiting the host star.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: Nodal precession by varying the J2 value for the HD 93963 system, as a supplement to Figure 4. The dominant precession rate of the planet b (USP) changes as the J2 value changes. Planets b and c precess separately at different eigenvalues when J2 ≳ 0.8 × 10−5 while they precess together at the same eigenvalue when J2 ≲ 0.6 × 10−5. J2 = 1.0 × 10−5, shown in the bottom right, represents the value we derived for the host star HD 93963 A.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: Same as Figure 8: the time-varying probability that an observer at a fixed position could detect both HD 93963 Ab and Ac transiting their host star, but obtained from N-body simulations as comparison. The left and right panels are coplanar and noncoplanar initialization, respectively. The colors of the solid lines indicate the initial true obliquity.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: Time-varying probability that an observer at a fixed position could detect both HD 3167 b and c transiting their host star. The system is initialized from the configuration that planets d, c, and e are initially coplanar, while planet b is significantly inclined relative to the other three planets. The first 6 kyr is shown and the different colors represent results from various initial conditions.
Paper: Stellar Obliquity of the Ultra-short-period Planet System HD 93963
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Samuel Halverson, Howard Isaacson, Eiichiro Kokubo, 英一郎 小久保, Ryan A. Rubenzahl, Benjamin Fulton, Aaron Householder, Jack Lubin, Steven Giacalone, Luke Handley, Judah Van Zandt, Erik A. Petigura, J. M. Joel Ong, 加冕 王, Pranav Premnath, Haochuan Yu, 皓川 于, Steven R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Chris Smith, Josh Walawender, Byeong-Cheol Lee, Yu-Juan Liu, 玉娟 刘, Joshua N. Winn
Figure caption: The posterior distribution of the fitted parameters in Table 3, derived from MCMC sampling.
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: Panel of periodograms of RV residuals for all accelerating stars from this analysis. Dashed, vertical red lines are denoted for every system’s highest-signal periodicity, and false-alarm probabilities at a level of 0.1% are given for each case. The period range searched spans from 1 day to 27.4 yr.
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: Comparison of our dynamical stellar mass estimates with recent photometric mass relationships. The HD 68017 AB pair is unresolved in both 2MASS and Gaia and therefore has no reported Ks or GRP magnitudes. However, J. R. Crepp et al. (2012) used NIRC2 to resolve the two stars in its ﹩{K}^{{\prime} }﹩ filter, which is nearly identical to that of 2MASS Ks (e.g., A. Stolte et al. 2010; M. R. Giovinazzi et al. 2024), allowing us to deconvolve the system’s composite Ks magnitude to estimate photometric masses for HD 68017 A and HD 68017 B using the MK method. Similarly, Gaia (but not 2MASS) resolves the HD 24496 AB pair, and so the GORP method is shown for HD 24496 B. HD 24496 A is not provided because a mass prior is used, while HD 4614 A is not shown because it is too massive for either of these two relations.
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: Top panel: resulting arguments of periastra of HD 217107 b from MCMC fits using subsets of the RVs from our analysis. The rightmost bin of observations consist solely of those taken from NEID. Both high-cadence observations at lesser precision and fewer RVs at higher precision are shown to be capable of achieving the same level of constraint. The best-fit slope representing precession is shown as the solid red line. The blue stripe corresponds to the 1σ region for HD 217107 c’s argument of periastron from Table 7. Bottom panel: RVs of the HD 217017 system with the best-fit model for HD 217107 c subtracted off. The vertical dashed lines show the corresponding bins of RVs used to search for ﹩\dot{\omega }﹩.
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 relative separation models for the three giant outer planets presented in this analysis.
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: Projected relative orbits for the four binary star systems considered here (top left: HD 68017 B around HD 68017 A; top right: 61 Cygni A around 61 Cygni B; bottom left: HD 24496 B around HD 24496 A; bottom right: HD 4614 B around HD 4614 A). The filled blue points represent the relative astrometric measurements included in our analysis, while the open circles are the predicted positions of the maximum-likelihood orbital models at past and future specified epochs.
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: Observed proper-motion values for the accelerating stars in our three planetary systems: HD 217107, HD 190360, and HD 154345. Each panel shows the proper-motion values as measured by Hipparcos and Gaia, as well as colored trial orbits that correspond to companion mass, in the same way as Figure 7.
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: Same as Figure 5 but for 61 Cygni A. Here, we only show the best-fit model, given as a black line. The colored points correspond to RV instruments Hamilton, HIRES-post, APF, MINERVA T1-T4, and NEID, as shown in Figure 2.
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: Phase-folded RV curve for 61 Cygni B. The best-fit period from our periodogram is fit for and shown in blue. NEID RVs, which are our analysis’ most precise, are highlighted in red, while the remaining data are shown in light black. We bin all data by phase in increments of 0.1, and show those as white triangles.
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: Same as Figure 13 but for 61 Cygni A.