adsabs/AstroCLIMB huggingface dataset:
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Secular evolution of the g−r color of K2 pre-perihelion. Colors were measured with two different aperture radii ρ, each equivalent to the coma regions covered by photometry (pink diamonds) and photometry (purple diamonds). Three numbered vertical lines denote the epochs of VLT polarimetric observations. Blue central solid and its two dashed horizontal lines indicate the average g−r dust color of 31 active solar system comets and its standard deviations observed by the Sloan Digital Sky Survey (Solontoi 2012).
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Maps of null parameters N  Q  and N  U  of the first-epoch imaging polarimetric data taken in FILT_691_55 (left) and FILT_834_48 (right) filters. Comet is located in the center of the maps. Any values outside the range of ±1% appear white.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Heliocentric evolution of the semimajor axis’ position angle (the PC1 eigenvector) of K2 coma. The solid lines indicate the anti-sunward ﹩{{\boldsymbol{r}}}_{\odot }﹩ (brown) and negative velocity ﹩-{\boldsymbol{v}}﹩ vectors (green), while the dashed lines in the same colors show 180° apart directions. We plotted inner coma components (filled circles) only when they were aligned differently from the outer coma components (open diamonds), omitting circles well inside the diamonds for simplicity. Three epochs of our VLT polarimetric observations are marked with dotted vertical lines.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Maps of polarimetric uncertainties of K2. Each row corresponds to the ones in Figure 3, where the photocenter of the coma is located at the center (0, 0). Smaller and larger dotted circles in each panel indicate the inner and outer coma boundaries of interest.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Same as Figure A1 but for the third-epoch data.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Median-combined W1- and W2-band coma images of K2 (upper panels) and the spectral distribution of their measured fluxes (lower panel). North is to the up and east is to the left.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Same as Figure A1 but for the second-epoch data.
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: The black dotted line represent the simulated periodic motion of the target star caused by the presence of a planet around it. The gray forks in (a) and dots with error bars in (b) depict the residual motion that remains after eliminating the relative proper motion and parallax of the target and reference stars in the fit based on the relative measurement method. The red dots illustrate the outcome of the fit to this periodic motion. Left panel: component at R.A. and decl. Right panel: periodic motion of the target star on the celestial sphere.
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: The black dotted line represents the simulated periodic motion of the target star caused by the presence of both planets around it. The gray forks in (a) and dots with error bars in (b) depict the residual motion that remains after eliminating the relative proper motion and parallax of the target and reference stars in the fit with the relative measurement method. Left panel: component at R.A. and decl. Right panel: periodic motion of the target star on the celestial sphere.
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: The black dotted lines in the upper and lower panels represent the simulated periodic motion of the target star caused by the presence of two planets around it. (a) and (b) correspond to the inner Earth-like planets. (c) and (d) correspond to the outer planet. The red dots illustrate the outcome of the fit to these periodic motions. Left panel: component at R.A. and decl. Right panel: periodic motion of the target star on the celestial sphere.
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: Observable part of the parallax ellipse (target: HD 88230; Gaia Collaboration 2020).
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: Coverage of planetary orbit period. The blue line indicates the mean value, while the gray ranges indicate the distribution of period coverage under each planetary period for all target stars.
Paper: Closeby Habitable Exoplanet Survey (CHES). II. An Observation Strategy for the Target Stars
Authors: Dongjie Tan, Jianghui Ji, Chunhui Bao, Xiumin Huang, Guo Chen, Su Wang, Yao Dong, Haitao Li, Junbo Zhang, Liang Fang, Dong Li, Lei Deng, Jiacheng Liu, Zi Zhu
Figure caption: Distribution of observation moments for each target (five for illustration) overlapped in 1 yr.
Paper: The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-floating Planets
Authors: Adam B. Langeveld, Aleks Scholz, Koraljka Mužić, Ray Jayawardhana, Daniel Capela, Loïc Albert, René Doyon, Laura Flagg, Matthew de Furio, Doug Johnstone, David Lafrèniere, Michael Meyer
Figure caption: Histogram of the K-band magnitudes (Vega) for the catalog of objects derived from our F200W images. The by-design photometric depth of K ∼ 21 is marked with the orange dashed line. The blue histogram is the distribution of magnitudes for our long list candidates, examined further by spectral fitting (see Section 4.1). In orange we show the distribution for objects on the long list with very low signal-to-noise insufficient for a meaningful analysis. Some approximate mass limits are indicated; see the text for details.
Paper: The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-floating Planets
Authors: Adam B. Langeveld, Aleks Scholz, Koraljka Mužić, Ray Jayawardhana, Daniel Capela, Loïc Albert, René Doyon, Laura Flagg, Matthew de Furio, Doug Johnstone, David Lafrèniere, Michael Meyer
Figure caption: Color composite of the two NIRISS WFSS images of NGC1333 observed in this spectroscopic survey. To create the composite, we used the F150W image for the blue channel and the F200W image for the green and red channels. For the red/green channels, the highest/lowest values were cropped. The narrow gaps between the images in the mosaic were interpolated.
Paper: The DECam Ecliptic Exploration Project (DEEP). VII. The Strengths of Three Superfast Rotating Main-belt Asteroids from a Preliminary Search of DEEP Data
Authors: Ryder Strauss, Andrew McNeill, David E. Trilling, Francisco Valdes, Pedro H. Bernardinelli, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Mario Jurić, Hsing Wen Lin, 省文 林, Larissa Markwardt, Michael Mommert, Kevin J. Napier, William J. Oldroyd, Matthew J. Payne, Andrew S. Rivkin, Hilke E. Schlichting, Scott S. Sheppard, Hayden Smotherman, Chadwick A. Trujillo, Fred C. Adams, Colin Orion Chandler
Figure caption: Diameter vs. Period for ∼22,000 main-belt asteroids as compiled by the asteroid lightcurve database. The red dashed line at 2.2 hr indicates the spin barrier. Very few asteroids with diameters >0.2 km have rotation periods less than 2.2 hr, making this our “region of interest” for SFRs. Overplotted in magenta is the approximate region to which the DEEP survey is sensitive (The bright limit is the diameter that begins to saturate the Dark Energy Camera (DECam) at 120 s). This region has considerable overlap with the SFR region of interest. The three colored dots indicate the position of three DEEP SFRs presented in this paper. We estimate the diameter of the DEEP objects from their absolute magnitude, assuming a geometric albedo of 0.15. Our estimated diameter uncertainties are based on imposing lower and upper albedo limits of 0.05 and 0.5.
Paper: The DECam Ecliptic Exploration Project (DEEP). VII. The Strengths of Three Superfast Rotating Main-belt Asteroids from a Preliminary Search of DEEP Data
Authors: Ryder Strauss, Andrew McNeill, David E. Trilling, Francisco Valdes, Pedro H. Bernardinelli, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Mario Jurić, Hsing Wen Lin, 省文 林, Larissa Markwardt, Michael Mommert, Kevin J. Napier, William J. Oldroyd, Matthew J. Payne, Andrew S. Rivkin, Hilke E. Schlichting, Scott S. Sheppard, Hayden Smotherman, Chadwick A. Trujillo, Fred C. Adams, Colin Orion Chandler
Figure caption: Minimum cohesive strength ranges for three DEEP SFRs as a function of bulk density. The solid lines indicate the best-fit solutions, while the dashed lines show the one-sigma uncertainty regions. The red vertical lines denote the limits of “typical” asteroid density ranges. The black horizontal lines indicate the range of likely subsurface strengths for Ryugu (M. Arakawa et al. 2020). For comparison purposes, the strength curves of all three SFRs are plotted on the same axes. Each set of three lines in matching colors corresponds to an individual asteroid.
Paper: The DECam Ecliptic Exploration Project (DEEP). VII. The Strengths of Three Superfast Rotating Main-belt Asteroids from a Preliminary Search of DEEP Data
Authors: Ryder Strauss, Andrew McNeill, David E. Trilling, Francisco Valdes, Pedro H. Bernardinelli, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Mario Jurić, Hsing Wen Lin, 省文 林, Larissa Markwardt, Michael Mommert, Kevin J. Napier, William J. Oldroyd, Matthew J. Payne, Andrew S. Rivkin, Hilke E. Schlichting, Scott S. Sheppard, Hayden Smotherman, Chadwick A. Trujillo, Fred C. Adams, Colin Orion Chandler
Figure caption: Top: unphased lightcurves for the 3 SFRs presented in this work. The scale of the photometric variation is far greater than that of the photometric uncertainties, implying rapid intrinsic variation. Middle: relative power spectra from the periodogram analysis. The periodogram power is presented here as a function of time rather than frequency, and the x-axis has been doubled to account for the double-peaked lightcurve from a full rotation. The strong peaks correspond to the strongest periodic signal within the lightcurve, which we interpret as the most likely rotation period of the object. Bottom: lightcurves phased to the best-fit rotation period for the object.
Paper: The DECam Ecliptic Exploration Project (DEEP). VII. The Strengths of Three Superfast Rotating Main-belt Asteroids from a Preliminary Search of DEEP Data
Authors: Ryder Strauss, Andrew McNeill, David E. Trilling, Francisco Valdes, Pedro H. Bernardinelli, Cesar Fuentes, David W. Gerdes, Matthew J. Holman, Mario Jurić, Hsing Wen Lin, 省文 林, Larissa Markwardt, Michael Mommert, Kevin J. Napier, William J. Oldroyd, Matthew J. Payne, Andrew S. Rivkin, Hilke E. Schlichting, Scott S. Sheppard, Hayden Smotherman, Chadwick A. Trujillo, Fred C. Adams, Colin Orion Chandler
Figure caption: Lightcurves for the three SFRs discussed here. The lightcurves have been phased to the best-fit periodogram solutions for each rotation period. Photometry from the original DECam detection is shown in blue. Subsequent Lowell Discovery Telescope measurements, shown in red, are in excellent agreement with the DECam photometry.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: The exact match fraction to LCDB as a function of the number of TESSC1 observations added to SS1. The top horizontal line refers to the exact match fraction when all TESSC1 observations are added to SS1, and the bottom horizontal line refers to when there are no TESSC1 observations added to SS1. These exact match fractions are 0.784 and 0.599, respectively (Table 2).
Paper: Quiet Please: Detrending Radial Velocity Variations from Stellar Activity with a Physically Motivated Spot Model
Authors: Jared C. Siegel, Samuel Halverson, Jacob K. Luhn, Lily L. Zhao, Khaled Al Moulla, Paul Robertson, Chad F. Bender, Ryan C. Terrien, Arpita Roy, Suvrath Mahadevan, Fred Hearty, Joe P. Ninan, Jason T. Wright, Eric B. Ford, Christian Schwab, Guðmundur Stefánsson, Cullen H. Blake, Michael W. McElwain
Figure caption: Throughout this study, we measured RVs from different “slices” of a one-dimensional spectrum (or CCF). For one-dimensional spectra, we either considered two large slices or six narrow slices (leftmost and central panels). We only considered the simpler case of two large slices (rightmost panel) for CCFs. Regions not included in a slice are shaded gray.
Paper: Quiet Please: Detrending Radial Velocity Variations from Stellar Activity with a Physically Motivated Spot Model
Authors: Jared C. Siegel, Samuel Halverson, Jacob K. Luhn, Lily L. Zhao, Khaled Al Moulla, Paul Robertson, Chad F. Bender, Ryan C. Terrien, Arpita Roy, Suvrath Mahadevan, Fred Hearty, Joe P. Ninan, Jason T. Wright, Eric B. Ford, Christian Schwab, Guðmundur Stefánsson, Cullen H. Blake, Michael W. McElwain
Figure caption: The RC model successfully detrends the rotation-modulation activity signal in NEID solar RVs. The columns correspond to different methods of applying the model: either using the one-dimensional spectra (left) or using only the CCFs (right). Top row: spectrum-averaged NEID solar RVs (gray) alongside the best-fit RC detrending model (purple); the spectrum-averaged RVs were measured either from the one-dimensional spectra by the line-by-line method (left) or from the CCFs (right). The rms of the observed RVs are reported for each method. For comparison, FF′ fits are shown in black; the 1σ confidence interval is indistinguishable. Second row: residuals between the spectrum-averaged RVs and the best-fit RC detrending model (gray); the residuals between the observed RVs and the median FF′ model are shown in black. Third row: ΔRV12, the relative RV between two slices of the one-dimensional spectrum (left column) or CCF (right column); the slices are shown in the left- and rightmost panels of Figure 1. Bottom row: the flux proxy, either the depth metric (left) or CCF contrast (right).
Paper: Quiet Please: Detrending Radial Velocity Variations from Stellar Activity with a Physically Motivated Spot Model
Authors: Jared C. Siegel, Samuel Halverson, Jacob K. Luhn, Lily L. Zhao, Khaled Al Moulla, Paul Robertson, Chad F. Bender, Ryan C. Terrien, Arpita Roy, Suvrath Mahadevan, Fred Hearty, Joe P. Ninan, Jason T. Wright, Eric B. Ford, Christian Schwab, Guðmundur Stefánsson, Cullen H. Blake, Michael W. McElwain
Figure caption: Across the three HD 26965 data sets (each of which has a significantly different cadence), the RC model successfully traces the rotation-modulation signal. The NEID and EXPRES measurements offer high-cadence coverage of multiple stellar rotation periods, while the HARPS data captures the multiyear activity cycle. Top row: spectrum-averaged line-by-line RVs (gray) alongside the best-fit RC detrending model (purple); the rms of the observed RVs are reported for each data set. For context, a FF′ fit to the NEID data is shown in black; the shaded region demarcates the 1σ confidence interval. Second row: residuals between the observed RVs and the best-fit RC detrending model (gray); the residuals between the observed RVs and the median FF′ model are shown in black. Third row: ΔRV12, the relative RV between two slices of the one-dimensional spectrum (i.e., different ranges of continuum normalized depth); the slices are diagrammed in the leftmost panel of Figure 1. Bottom row: depth metric activity indicator.
Paper: Quiet Please: Detrending Radial Velocity Variations from Stellar Activity with a Physically Motivated Spot Model
Authors: Jared C. Siegel, Samuel Halverson, Jacob K. Luhn, Lily L. Zhao, Khaled Al Moulla, Paul Robertson, Chad F. Bender, Ryan C. Terrien, Arpita Roy, Suvrath Mahadevan, Fred Hearty, Joe P. Ninan, Jason T. Wright, Eric B. Ford, Christian Schwab, Guðmundur Stefánsson, Cullen H. Blake, Michael W. McElwain
Figure caption: The RC model recovers the rotation ΔRVrot(t) and convection ΔRVC(t) rotation-modulation perturbations from the NEID solar data, using only the one-dimensional spectra. To reign in parameter–parameter degeneracies, the RC model was jointly fit for five different choices of ΔRV i,ref(t) = RV i (t) − RVref(t). Left: diagram of how RV i  and RVref were defined, in terms of continuum normalized depth (identical to the center panel of Figure 1). Center: the recovered time series of ΔRVrot(t) from the RC model, compared to the independent SDO measurements (gray). Each choice of ΔRV i,ref(t) yields a prediction for ΔRVrot(t); all five predictions are presented, following the color scheme of the spectrum diagram. Right: the recovered time series of ΔRVC(t) compared to SDO; the convection perturbation depends on the flux proxy alone, so there is only one prediction. From marginalizing over the posteriors, the 1σ uncertainties on the model’s rotation and convection components are 13 and 9 cm s−1, respectively.
Paper: Quiet Please: Detrending Radial Velocity Variations from Stellar Activity with a Physically Motivated Spot Model
Authors: Jared C. Siegel, Samuel Halverson, Jacob K. Luhn, Lily L. Zhao, Khaled Al Moulla, Paul Robertson, Chad F. Bender, Ryan C. Terrien, Arpita Roy, Suvrath Mahadevan, Fred Hearty, Joe P. Ninan, Jason T. Wright, Eric B. Ford, Christian Schwab, Guðmundur Stefánsson, Cullen H. Blake, Michael W. McElwain
Figure caption: The RC model maps the relative strengths of the rotation ΔRVrot(t) and convection ΔRVC(t) perturbations induced by active regions as a function of continuum normalized depth. The results for the Sun and HD 26965 are presented in the top and bottom rows, respectively. Left: the strength of the rotation perturbation as a function of depth in the one-dimensional spectrum (relative to the “bottom” spectral slice; see Figure 6 for a diagram); the rotation perturbation is strongest at heavily absorbed wavelengths, resulting in A  i  − A ref < 0. The central point, dark-shaded region, and light-shaded region represent the median, 1σ, and 2σ confidence intervals of the MCMC samples, respectively. Right: the strength of the convection perturbation ΔRVC(t) as a function of depth in the spectrum; the convection perturbation is strongest at weakly absorbed wavelengths, resulting in B  i  − B ref > 0. The depth of the reference spectral slice is shown as a dashed vertical line.
Paper: Quiet Please: Detrending Radial Velocity Variations from Stellar Activity with a Physically Motivated Spot Model
Authors: Jared C. Siegel, Samuel Halverson, Jacob K. Luhn, Lily L. Zhao, Khaled Al Moulla, Paul Robertson, Chad F. Bender, Ryan C. Terrien, Arpita Roy, Suvrath Mahadevan, Fred Hearty, Joe P. Ninan, Jason T. Wright, Eric B. Ford, Christian Schwab, Guðmundur Stefánsson, Cullen H. Blake, Michael W. McElwain
Figure caption: Injected Keplerian signals were successfully recovered using the RC model. Using the NEID HD 26965 data set, we considered a single planet on a circular orbit with a semiamplitude of K = 1 m s−1. Left: recovered semiamplitudes for different combinations of the injected planet’s orbital period and phase. The approximately 42 day rotation period of HD 26965, along with the lowest–order harmonics, are demarcated by shaded regions. The colors correspond to the orbital phase of the injected planet (diagrammed in the upper right panel). Right: breakdown of the injection recovery process for P = 27 days. Upper row: spectrum-averaged RVs (gray) alongside the injected Keplerian signal for three different orbital phases (described in Section 5.2). Middle row: periodograms of the RV time series before (gray) and after (blue), the activity component of the model was subtracted; the vertical line demarcates the injected planet’s orbital period and the horizontal line shows the 1% false alarm probability. Bottom row: activity-detrended phase-folded RVs against the injected Keplerian signal (dashed line); phase-binned RVs are shown in blue.
Paper: Quiet Please: Detrending Radial Velocity Variations from Stellar Activity with a Physically Motivated Spot Model
Authors: Jared C. Siegel, Samuel Halverson, Jacob K. Luhn, Lily L. Zhao, Khaled Al Moulla, Paul Robertson, Chad F. Bender, Ryan C. Terrien, Arpita Roy, Suvrath Mahadevan, Fred Hearty, Joe P. Ninan, Jason T. Wright, Eric B. Ford, Christian Schwab, Guðmundur Stefánsson, Cullen H. Blake, Michael W. McElwain
Figure caption: The contributions of the rotation ΔRVrot(t) and convection ΔRVC(t) perturbations as a function of the average temperature of formation in the stellar atmosphere. Using only spectral features well reproduced by the stellar atmosphere model, the NEID solar RVs were jointly fit with the RC model for five choices of RV i (t) − RVref(t). Left: the relative strength of ΔRVrot(t) between RV i (t) and RVref(t) as a function of the average formation temperature; the average formation temperature of RVref(t) is shown as a dashed vertical line. Right: the relative strength of ΔRVC(t) between RV i (t) and RVref(t).
Paper: Quiet Please: Detrending Radial Velocity Variations from Stellar Activity with a Physically Motivated Spot Model
Authors: Jared C. Siegel, Samuel Halverson, Jacob K. Luhn, Lily L. Zhao, Khaled Al Moulla, Paul Robertson, Chad F. Bender, Ryan C. Terrien, Arpita Roy, Suvrath Mahadevan, Fred Hearty, Joe P. Ninan, Jason T. Wright, Eric B. Ford, Christian Schwab, Guðmundur Stefánsson, Cullen H. Blake, Michael W. McElwain
Figure caption: Inferred rotation ΔRVrot(t) and convection ΔRVC(t) perturbations for the NEID HD 26965 data set, using only the one-dimensional spectra. To reign in parameter–parameter degeneracies, the RC model was jointly fit for five different choices of RV i,ref(t) = RV i (t) − RVref(t), diagrammed in Figure 6. The recovered ΔRVrot(t) signals (one for each choice of ΔRV i,ref) are presented following the color scheme of Figure 6. The recovered time series of ΔRVC(t) is presented in solid purple. From marginalizing over the posteriors, the 1σ uncertainties on the model’s rotation and convection components are 15 and 9 cm s−1, respectively.