adsabs/AstroCLIMB huggingface dataset:
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Time-series analysis of astronomical solutions. Top and bottom: g and s spectra determined from our solar system integrations using fast Fourier transform (FFT ﹩={ \mathcal F }(k,q)﹩) over 20 Myr intervals and Earth’s k and q variables (see Section 2). Frequencies in arcsec yr −1 = ″ yr −1. Left: Standard spectra in the recent past centered at t = −10 Myr (nearly identical in all solutions). Right: spectra of solution R28 centered at t = −1450 Myr (see Figure 6(b)). The dashed lines indicate frequencies in the recent past (left) in all panels. During σ 12-resonance intervals (right), g 2 shows reduced power and generally splits into two peaks (red circles and inset). In the recent past (left), ∣g 2 − g 1∣ > ∣s 2 − s 1∣, whereas during σ 12 resonances (right) ∣g 2 − g 1∣ ≃ ∣s 2 − s 1∣ (see double arrows).
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Relative errors in total energy (E) and angular momentum (L  z ) of 3.5 Gyr test integrations (solar mass = const.). ∣ΔE/E∣ = ∣E(t) − E(0)/E(0)∣, ∣ΔL  z /L∣ = ∣L  z (t) − L  z (0)/L(0)∣. Due to J 2, only L  z  is conserved, not the horizontal components.
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Past Earth–Moon distance (R) in units of Earth radii (R E). Green dashed line: integration of precession equations starting at the present rate dR 0/dt (see text), yielding (well-known) unrealistic past R/R E. Red diamonds: observational estimates based on robust data sets from cyclostratigraphic studies. Blue and cyan lines: used in the present study. Blue: linear extrapolation into the past starting with dR 0/dt close to the present rate. Cyan: third-order polynomial fit to observations. Using R/R E based on the blue and cyan lines made essentially no difference in our computations; both approaches yielded solutions including σ 12-resonance intervals at a similar frequency (see Section 3).
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Same as Figure 5 but using the ﹩{\chi }_{\nu }^{2}﹩ derived from fitting the empirical spectra to the 2022 February CHARIS spectrum rather than the 2022 December data.
Paper: Direct-imaging Discovery of a Substellar Companion Orbiting the Accelerating Variable Star HIP 39017
Authors: Taylor L. Tobin, Thayne Currie, Yiting Li, Jeffrey Chilcote, Timothy D. Brandt, Brianna Lacy, Masayuki Kuzuhara, Maria Vincent, Mona El Morsy, Vincent Deo, Jonathan P. Williams, Olivier Guyon, Julien Lozi, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Tyler Groff, N. Jeremy Kasdin, Taichi Uyama, Motohide Tamura, Aidan Gibbs, Briley L. Lewis, Rachel Bowens-Rubin, Maïssa Salama, Qier An, Minghan Chen
Figure caption: Similar to Figure 7 but using the 2022 February CHARIS spectrum rather than the 2022 December data to fit the Sonora Diamondback model grid.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: Derived template spectra and photometry. The stars and offset constants from top to bottom are: (1) 16 Cyg B, C = 0.315; (2) 18 Sco, C = –0.005; (3) HD 37962, C = 0.860; (4) HD 106252, C = 0.687; (5) HD 142331, C = 1.105; (6) HD 159222, C = 0.218; (7) HD 167060, C = 1.135; and (8) HD 205905, C = 0.235. The error bars are set to 1.5% for all the photometry except those at 7.8 μm for HD 37962 and HD 106252, where they are 2%. The photometry is from Table 2 for K  S , Krick et al. (2021) for IRAC Band 1, Bohlin et al. (2022) for the other IRAC bands corrected as in Appendix A, and Engelbracht et al. (2007) for 24 μm.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: Upper panel: comparison of the solar spectrum with a BOSZ model with parameters matched to the Sun, and normalized to the solar spectrum at wavelengths > 4 μm. The model is high between ∼1.5 and 3.5 μm, by up to 1%–1.5%. [The conventional units for absolute calibrations are in the mixed units of W cm−2 μm−1, originating with Johnson 1966, as used in this figure. They can be converted to Janskies by multiplying by 3.3357 × 1015 × λ(μm)2.] Lower panel: correction factor to reconcile the BOSZ model with the spectrum of the Sun.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: Region of overlap for the STIS and BOSZ/solar spectra of 18 Sco, showing how they were joined.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: Spectral fitting for V583 Lyr. Refer to Table 2 for the stellar parameters used for calculating the model spectrum.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: The results of the least-squares minimization to estimate the initial value of the mass ratio q. The fitting residuals are plotted for 0.07 ≤ q ≤ 0.13 with steps of 0.0005.
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: The same sky area captured by the near-ultraviolet telescope (left panel) and the optical telescope (right panel), when they are pointing to R.A. = 148.88822 and decl. = 69.06529. Since these two telescopes have different spatial resolutions, these two images have different field of views (0.°11 × 0.°11 for optical images and 0.°17 × 0.°17 for near-ultraviolet images).
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: The left panel shows the throughput of the optical telescope, and the right panel shows that of the near-ultraviolet telescope.
Paper: Is the RSGC4 (Alicante 8) Cluster a Real Star Cluster? Peculiar Radial Velocities of Red Supergiant Stars
Authors: Sang-Hyun Chun, GyuChul Myeong, Jae-Joon Lee, Heeyoung Oh
Figure caption: Left: (J − H, G − K  s ) color–color diagram of stars with K  s  < 8 in the 6° × 2° Scutum complex area and RSG candidates in the six RSGCs. The arrow indicates an increasing reddening vector, and the dashed line shows the linear distribution of stars. Right: ﹩(J-H,{Q}_{{{GK}}_{s}})﹩ diagram for the stars in the left panel. The MIST isochrones with [Fe/H] = −0.25 and log (t yr) = 7.0, 7.2, 7.4, 7.8, 8.6, and 9.6 are indicated by solid lines of different colors. The core helium-burning (CHeB) phases in isochrones are represented by thick lines, while EAGB or TPAGB phases are shown by thin lines. The dashed–dotted line indicates the limit Q  GK  s   value of 1.7, which stars in the CHeB cannot attain.
Paper: Is the RSGC4 (Alicante 8) Cluster a Real Star Cluster? Peculiar Radial Velocities of Red Supergiant Stars
Authors: Sang-Hyun Chun, GyuChul Myeong, Jae-Joon Lee, Heeyoung Oh
Figure caption: Radial velocity distributions as a function of radial distance from the cluster center in the sky for six RSGCs. Symbol size represents the measured radial velocity error of an individual star, with larger symbols indicating larger errors. Four symbols corresponding to different velocity error categories (﹩{\sigma }_{{V}_{\mathrm{LSR}}}=4.0,1.0,0.6﹩, and 0.3 km s−1) are adopted. The solid line indicates the mean radial velocity (V LSR = 96 km s−1) for all RSG candidates in the clusters. The dashed lines represent the 1σ (34 km s−1) range from the mean velocity. Histograms of radial velocity for each cluster are also presented in the three panels on the right.
Paper: Is the RSGC4 (Alicante 8) Cluster a Real Star Cluster? Peculiar Radial Velocities of Red Supergiant Stars
Authors: Sang-Hyun Chun, GyuChul Myeong, Jae-Joon Lee, Heeyoung Oh
Figure caption: Left: IGRINS K-band spectra with only heliocentric correction for all observed stars in RSGC4 in the region around the CO bandhead. The ID numbers of the stars correspond with those of the stars in RSGC4 by Negueruela et al. (2010). Right: K-band spectra with only heliocentric correction for observed stars in RSGC2 in this study. The ID numbers for RSGC2 follow those of Davies et al. (2007). The dotted vertical line indicates the rest wavelength position of the blue edge of the CO bandhead.
Paper: Is the RSGC4 (Alicante 8) Cluster a Real Star Cluster? Peculiar Radial Velocities of Red Supergiant Stars
Authors: Sang-Hyun Chun, GyuChul Myeong, Jae-Joon Lee, Heeyoung Oh
Figure caption: The stellar number density maps for the Scutum complex region constructed using different selection criteria. The selection criteria are indicated in each panel. The positions of the six RSGCs are indicated by red circles with labels. The color bars in each panel show the number density smoothed by the Gaussian filter.
Paper: How Well is the International Celestial Reference System Maintained in Official IAU Implementations?
Authors: Zinovy Malkin
Figure caption: Systematic differences between ICRF (I1), ICRF2 (I2), and ICRF3-SX (I3) represented by a 16-parameter VSH expansion. Plots labeled with “50” and “58” correspond to the catalogs recomputed with A = 5.0 and A = 5.8, respectively; labels “2000” and “2015” correspond to the catalogs recomputed with t 0 = 2000 and t 0 = 2015, respectively; plots labeled with “original” correspond to originally published catalogs. The vertical error bars show 1σ  uncertainty of the VSH coefficients.
Paper: How Well is the International Celestial Reference System Maintained in Official IAU Implementations?
Authors: Zinovy Malkin
Figure caption: Systematic differences of the three Gaia astrometric solutions Gaia-CRF1 (G1), Gaia-CRF2 (G2), and Gaia-CRF3 (G3) with ICRF3-SX (I3; upper panel), and of the two latter Gaia solutions with ICRF3-SX (bottom panel) represented by a 16-parameter VSH expansion. The vertical error bars show 1-sigma uncertainty of the VSH coefficients.
Paper: How Well is the International Celestial Reference System Maintained in Official IAU Implementations?
Authors: Zinovy Malkin
Figure caption: Sky distribution of the three Gaia-CRF catalogs and sources in common for Gaia-CRF catalogs and ICRF3-SX.
Paper: A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World
Authors: Stephen R. Kane, Tara Fetherolf, Zhexing Li, Alex S. Polanski, Andrew W. Howard, Howard Isaacson, Teo Močnik, Sadie G. Welter
Figure caption: The predicted blackbody flux of TOI-6713.01, assuming a calculated temperature of ∼2600 K. The passband boundaries of TESS are indicated by the vertical dashed lines. Of the integrated flux, 16.64% falls within the TESS passband.
Paper: Foreground Dust Properties toward the Cluster NGC 7380
Authors: Sadhana Singh, Jeewan C. Pandey, Thiem Hoang, Neelam Panwar, Biman J. Medhi, Vishal Joshi, Shashikiran Ganesh
Figure caption: (a) The variation of ﹩{P}_{\max }﹩ with E(B − V). The magenta, blue, and cyan curves denote the maximum efficiency line, average efficiency for diffuse ISM, and lower bound on efficiency, respectively. (b) ﹩{P}_{\max }/{A}_{V}﹩ vs. A  V  in log–log scale along with the residual plot. The marker with the red circle denotes the member stars of the cluster.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Demonstration of our LBL pipeline on NEID solar spectra, compared to the standard NEID DRP. To compute the LBL RVs, we constructed a high-S/N solar template using NEID spectra from an exemplary “good weather” day, which includes 192 spectra. Top: solar bulk RVs calculated using the LBL pipeline (purple) as compared to the NEID DRP (yellow) using the same spectral lines (offset added for clarity). Data were manually selected for days with no measurable clouds. Our LBL pipeline produces nearly identical results for the full time series. Middle: residual time series shows little structure and is broadly consistent with the photon errors. Bottom: periodograms of NEID pipeline and LBL RVs, highlighting the similar temporal structure.
Paper: Foreground Dust Properties toward the Cluster NGC 7380
Authors: Sadhana Singh, Jeewan C. Pandey, Thiem Hoang, Neelam Panwar, Biman J. Medhi, Vishal Joshi, Shashikiran Ganesh
Figure caption: (a, b) Variation of ﹩{\lambda }_{\max }﹩ with A  V  and ﹩{P}_{\max }/{A}_{V}﹩. (c, d) The variation of ﹩{P}_{\max }/{A}_{V}﹩ and ﹩{\lambda }_{\max }﹩ from the center outward for the cluster NGC 7380. The member stars are denoted by the red circles in all panels.
Paper: Foreground Dust Properties toward the Cluster NGC 7380
Authors: Sadhana Singh, Jeewan C. Pandey, Thiem Hoang, Neelam Panwar, Biman J. Medhi, Vishal Joshi, Shashikiran Ganesh
Figure caption: Variation of P  V  and A  V  with distance. The red and blue markers are for P  V  and A  V , respectively. Filled markers show the observed stars by us, and open markers are for the sources from Heiles (2000). The filled marker with an additional marker layer shows the member stars. One background Heiles star (distance > 6 kpc) is left for the plot. The vertical line at 1.2 kpc distance denotes the location of the dust layer.
Paper: Foreground Dust Properties toward the Cluster NGC 7380
Authors: Sadhana Singh, Jeewan C. Pandey, Thiem Hoang, Neelam Panwar, Biman J. Medhi, Vishal Joshi, Shashikiran Ganesh
Figure caption: The color composite image of the observed region of the cluster NGC 7380 (red: WISE-W4; green: WISE-W3; blue: DSS2-R). Cyan contours represent the distribution of the dust extinction in the region. Polarization vectors in the V band are overplotted, similar to Figure 2(b).
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Left: NEID data of HD 26965, showing velocities and activity indicator time series for spectra used in this study. Computed data products include velocities, CCF FWHM, BIS, contrast, S HK index, Hα index, Ca IRT index, and depth metric (see Section 4.3.1; Siegel et al. 2022). The red diamonds show the peak period in each periodogram. All data show clear rotational modulation at or near the 42-day period. Right: corresponding periodograms showing clear power at the stellar rotation period of ∼42 days.
Paper: Foreground Dust Properties toward the Cluster NGC 7380
Authors: Sadhana Singh, Jeewan C. Pandey, Thiem Hoang, Neelam Panwar, Biman J. Medhi, Vishal Joshi, Shashikiran Ganesh
Figure caption: Polarization vectors are overplotted over the DSS image (﹩{22}^{{\prime} }\times {22}^{{\prime} }﹩) of the observed region. The length of the polarization vectors corresponds to the polarization value, whereas their orientation reveals the POS magnetic fields along the line of sight toward the stars. Member stars are marked with red circles. The dotted line shows the orientation of the projection of the GP at the region. The plus sign shows the center of the cluster NGC 7380. The magnetic fields toward these stars are essentially parallel to the Galactic magnetic field.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Left: LBL bulk velocities with corresponding FF’-based velocities derived using the depth metric, ﹩{ \mathcal D }(t)﹩ (Siegel et al. 2022), to create corresponding theoretical activity signal (see Section 5.2.4). Typical velocity error bars are smaller than the plotting symbols (∼30–50 cm s−1). The rms of the residuals is 1.04 m s−1. Right: Lomb–Scargle periodogram of the bulk RVs (gray) and FF’ (purple) residuals, showing a significant reduction in the power at the ∼42-day candidate period (red dash). False-alarm probability thresholds are shown with the horizontal lines for 0.1% (dotted), 1% (dashed), and 10% (solid). We do note that a potential P rot/2 alias may remain (∼21 days) after subtraction of the best-fit activity signal, but it has a comparably low significance.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Top: HD 26965 bulk RVs calculated through our LBL pipeline (gray) with linear trend removed (purple) as compared to the NEID pipeline RVs (yellow, offset added for clarity). Middle: residual time series after linearly detrending the LBL RVs (purple) retains approximately 2.5 ms−1 modulation in the first half of the time series. Bottom: Lomb–Scargle periodograms of all three RV time series. All show the same peak period of around 42 days. Linearly detrending LBL RVs (purple) removes the long period power seen in the Lomb–Scargle periodogram and results in a better agreement between the NEID pipeline RVs and the integrated LBL RVs. Possible causes for the differences between the two RVs are detailed in Section 4.1.5. As we are primarily interested in signals at or near the 42-day period, we remove this trend from the LBL bulk RV for the remainder of the analysis.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Left: LBL bulk RV time series when detrended (purple circles) for each metric based on correlations shown in Figure 7. The original bulk RVs are show with gray squares. Right: original RV periodogram (gray dashed line) plotted under the detrended periodogram (purple solid line). The majority of detrended time series show a substantial decrease in the relative power at or near the 42.6-day rotation period. For the line index and depth metric cases, power reduction ranges between 57.6% when detrending for the Ca IRT and 82.99% when detrending for S HK. Note that the first few days of observations are omitted in this analysis to avoid potential issues with extrapolation. The period with the highest remaining power is noted by the red diamond.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Example GP-modeled phase lag between S HK activity indicator and LBL bulk RV time series with an additional term included to account for smaller-timescale RV jitter. Our model detects a phase lag of ∼6.7 days between the S HK index and the bulk RVs (with the RVs following behind the line indicator). Thin solid lines show a set of random draws from the model posterior distributions for clarity.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Posteriors from MCMC best-fit Keplerian periods, per, and semiamplitudes, K, for the symmetric, 2σ lines (left) and the symmetric, 2σ, R > 0.3 lines (right). Fits for each depth bin highlighted in Figure 9 are shown in yellow for deep lines, blue for mid-depth lines, and purple for shallow lines. The contour lines mark the 68%, 95%, and 99.7% confidence limits. The recovered planet semiamplitude (K) varies significantly as a function of line depth in both cases.
Paper: The Death of Vulcan: NEID Reveals That the Planet Candidate Orbiting HD 26965 Is Stellar Activity 
Authors: Abigail Burrows, Samuel Halverson, Jared C. Siegel, Christian Gilbertson, Jacob Luhn, Jennifer Burt, Chad F. Bender, Arpita Roy, Ryan C. Terrien, Selma Vangstein, Suvrath Mahadevan, Jason T. Wright, Paul Robertson, Eric B. Ford, Gumundur Stefánsson, Joe P. Ninan, Cullen H. Blake, Michael W. McElwain, Christian Schwab, Jinglin Zhao
Figure caption: Correlations between bulk RV and each activity metric (described in Section 5.1.1). The two time series are correlated and plotted before (gray) and after (purple) being phase-shifted to maximize correlation with bulk RV. Correlation coefficients for both sets show general improvement in correlation after shifting each indicator by its best-fit GP-modeled phase lag.