adsabs/AstroCLIMB huggingface dataset:
Paper: Parallax Effect in Microlensing Events Due to Free-floating Planets
Authors: Parisa Sangtarash, Sedighe Sajadian
Figure caption: The fraction of simulated events due to FFPs that are affected by parallax as a percentage. Here, we have three definitions to extract the parallax-affected events: (i) Δχ 2 > 100 (gray solid lines), (ii) Δχ 2 > 100 and δ t E > 0.02 (red dashed lines), and (iii) Δχ 2 > 100 and δ ρ ⋆ > 0.02 (green dotted–dashed lines).
Paper: Parallax Effect in Microlensing Events Due to Free-floating Planets
Authors: Parisa Sangtarash, Sedighe Sajadian
Figure caption: Scatter plot of the relative deviation in the Einstein crossing time δ t E vs. the two parameters D l and ﹩{\mathrm{log}}_{10}[{M}_{{\rm{l}}}({M}_{\oplus })]﹩.
Paper: Parallax Effect in Microlensing Events Due to Free-floating Planets
Authors: Parisa Sangtarash, Sedighe Sajadian
Figure caption: The correlation matrix between the relative deviations in the lensing parameters (the first five rows) due to the indiscernible parallax effects and the relevant and physical parameters of simulated events (the other rows).
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: An example of the transition measurement process. The displayed line profile is the coadded spectrum in velocity space, using all transitions that were previously shown in Figure 2. The top panel shows a spectral region ±350 km s−1 (±5.0 Å at 4300 Å) surrounding the coadded transition. The dotted line indicates the adopted continuum. The bottom panel has a blowup of just the region ± 50 km s−1 around the transition. The dashed line is placed at line center. The observed velocity widths to the blue and red at flux levels 0.50 and 0.85 of the continuum are indicated by arrows of different colors and by labels (e.g., B0.50 means the width of the blue part of line profile at flux level 0.50 of the continuum).
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: An example of the transition coaddition process. The 71 individual lines used for WY Ant at pulsational phase ϕ = 0.658 are shown as faint gray profiles. The mean profile generated by coaddition of all of them is shown in black. The mean of just the weakest 37 lines is in blue, and that of the strongest 22 strongest lines is in red.
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: Statistical measures for WY Ant lines at all coadded phase points. In the top panel the line widths V  B +V  R  are shown. Open circles are used for the widths at 0.50 relative line flux level and ×  symbols for the 0.85 level, as given in the panel legend. The middle panel displays differences between blue and red widths V  R  −V  B , and the bottom panel contains the line skew values. Data for this figure are listed in Table 2.
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: An example of raw and coadded spectra in one spectral region at a single phase for program star WY Ant. This relatively bright star already with good S/N has been chosen for display. The identified atomic lines are those that were measured in this particular coadded spectrum.
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: Coadded metallic line profiles (black dots) and modeled line profiles (colored lines) for WY Ant at two pulsational phases. The velocities ΔRV are with respect to the stellar center-of-mass velocity. See the text for description of the empirical model line profiles; their relative velocities are noted in the figure legend.
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: Top panel: radial velocity variations with phase for metal lines (purple color) and Hα (orange) in WY Ant. The ordinate ΔRV values are measured relative to the WY Ant center-of-mass velocity, 203.7 km s−1. Bottom panel: photometric V-band magnitudes for WY Ant from the ASAS database (Pojmanski et al. 2005, and references therein). In both panels vertical dashed lines denote phases ϕ = 0.009 (repeated at ϕ = 1.009) and 0.849 that have been chosen for line profile display in Figure 8.
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: Hα profile for WY Ant at phase ϕ = 0.86. The lines and symbols are as in Figure 8.
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: Skew values for our sample of RRab stars, plotted as functions of phase. The three panels contain stars grouped for visual clarity according to their metallicities, with the most metal-poor in the top panel and the most metal-rich in the bottom panel. Skew values for individual stars are indicated with different colors, and their metallicities from Table 1 are in the panel legends.
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: Variations of metal line skew values for WY Ant for weaker lines (top panel), strongest lines (middle panel), and the total line set (bottom panel). The bottom panel is a repeat of the bottom panel in Figure 4.
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: Heights (ΔR in km) above Rosseland τ = 0.67 in a model from the Kurucz (2011, 2018) grid with parameters indicated in the legend.
Paper: Variations in Line Profiles of Atomic Transitions in RR Lyrae Stars
Authors: Christopher Sneden, George W. Preston
Figure caption: Skew measurements for the RRc stars.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Distribution of the six Gaia EDR3 parameters relative to G or BP − RP for a random sample of 60,671 LAMOST sources with BRExcess ≤ 2.37. In each panel, the red line and accompanying text represent the selection criteria employed in this study. Additionally, the percentages displayed indicate the proportion of randomly sampled LAMOST sources that fall below the selection criteria.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Parameter distribution of the 585 sources with BRExcess > 5, compared to a random sample of 60,671 LAMOST sources. The comparison sample is represented by gray dots, while sources with BRExcess > 5, excluding those near the center of M31, are depicted by blue dots. The wrong candidate is indicated by the red dot. In the first subplot of the second row, the blue line is a second-order regression for G − r vs. g − r of the comparison sample. The two orange lines indicate the position ±3σ away from the regression line.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Distribution of BRExcess as a function of BP − RP for all 6,138,049 sources. The color bar indicates the number density. The sample is divided into three subsamples by the two red lines.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Distribution of parameters for the candidate with 2.37 < BRExcess ≤ 5. The light gray dots represent the 60,671 random LAMOST sources, while the dark gray dots correspond to the sources with 2.37 < BRExcess ≤ 5. The HCSC candidate is denoted as the red dot. The subplot of the first column of the second row is made similarly to that in Figure 3.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Wrong candidate with BRExcess > 5, whose image (1′ × 1′) is from the PS1 i band and the spectrum is from LAMOST. The green cross in the center of the left panel denotes the candidate.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Example of the identifications of a wide binary. Blue and red dots represent sources located within 1′ of the target source in Gaia DR3. One of the two red dots is the target source, while the other is considered to be another component of a wide binary system, together with the target source.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Left: example of a contamination I case, whose image is from SDSS. Right: example of a contamination II case, whose image is from SDSS.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Example of a wrong match, whose image (1′ × 1′) is from the PS1 i band. The green cross denotes the location of the LAMOST source, while the white represents the Gaia source after a wrong match process.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Examples of a wide binary, whose image is from SDSS and spectrum is from LAMOST.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Spatial distribution of the 585 sources with BRExcess > 5, with different categories identified by different colors.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Example of an outer GC of M31, whose image is from SDSS and spectrum is from LAMOST.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Example of a galaxy, whose image and spectrum are from SDSS.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Distribution of Δmag g  with g PSF, where gray dots represent the comparison sample with BRExcess ≤ 2.37, while blue dots denote sources with 2.37 < BRExcess ≤ 5. The central solid orange line is the best linear fitting for the comparison sample, and the two dashed orange lines are ±3σ away from the best-fitting line.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Spatial distribution of the 4085 sources with 2.37 < BRExcess ≤ 5. The light gray dots represent the 60,671 random LAMOST sources, while the dark gray dots correspond to the sources with 2.37 < BRExcess ≤ 5. The HCSC candidate is represented by the red dot, while the post-AGB star is indicated by the blue dot.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Single-source resolved HCSC candidate, whose image is from SDSS and the spectrum is from LAMOST.
Paper: Searching for Hypercompact Star Clusters in the Milky Way Using LAMOST and Gaia
Authors: Hao Wu, Haibo Yuan, Yilun Wang, Zexi Niu, Huawei Zhang
Figure caption: Post-AGB Star: IRAS 04296+3429, whose image is from PS1 (1′ × 1′) i band and the spectrum is from LAMOST.
Paper: The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824 
Authors: Sarah Lange, Joseph M. Akana Murphy, Natalie M. Batalha, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, David R. Ciardi, Andrew W. Boyle
Figure caption: An example of our Savitzky–Golay filtering procedure for TOI-1824’s Sector 21 SAP photometry. The black points are the SAP data, the green line is the data after being smoothed by the Savitzky–Golay filter, and the blue points are the in-transit data, which are not subjected to the outlier rejection. Outliers are marked in red.
Paper: The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824 
Authors: Sarah Lange, Joseph M. Akana Murphy, Natalie M. Batalha, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, David R. Ciardi, Andrew W. Boyle
Figure caption: The Palomar-PHARO contrast curve for TOI-1824 in the Brγ filter. Note that in the postage stamp image (inset), the field of view shown is too small to include the stellar companion, TIC 142387022 (which has a separation of about 7″). North is up, and east is left.
Paper: The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824 
Authors: Sarah Lange, Joseph M. Akana Murphy, Natalie M. Batalha, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, David R. Ciardi, Andrew W. Boyle
Figure caption: Top row: the results of our CV analysis for a Keplerian-only model of the RVs. The left column shows the distribution of the residuals in units of the total model uncertainty (measurement error and telescope jitter added in quadrature) for all 100 CV iterations for the the Keck-HIRES training (solid black) and evaluation data (open hatched gray) and the APF-Levy training (semitransparent green) and evaluation data (open bright green). The right column shows the distribution of the rms of the residuals in units of m s−1 for all 100 CV iterations. A vertical black dashed (solid green) line shows the raw rms of the Keck-HIRES (APF-Levy) RVs before applying any models. Bottom row: the same as the top row but now for the model that includes the GP. For this row, the left panel’s x-axis units also include the uncertainty in the GP prediction. The spread of the distribution of the residuals for the Keplerian-only model is consistent for both telescopes between the training and evaluation data, suggesting that the model is not overfitting. For the GP-enabled model, the distribution of the residuals for the training data is slightly narrower compared to the distribution for the evaluation data. The rms of the evaluation data residuals is systematically larger than the rms of the training data residuals for the GP-enabled model—though, as seen in the distribution of the residuals, this scatter is typically within 2σ of zero. Takeaway: our CV tests suggest that a GP-enabled model of the RVs might be slightly overfitting the data compared to a Keplerian-only model, but the GP is not leading to model inaccuracy as the residuals of the evaluation data are still centered around zero and typically fall within 1σ–2σ.
Paper: The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824 
Authors: Sarah Lange, Joseph M. Akana Murphy, Natalie M. Batalha, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, David R. Ciardi, Andrew W. Boyle
Figure caption: GLS periodograms for TOI-1824 are shown in black. The vertical blue line marks the orbital period of TOI-1824 b (P = 22.8 days). Dashed horizontal lines indicate the 0.1% FAP threshold (Baluev 2008). The posterior median for the periodic hyperparameter of the GP (P rot) used to model stellar activity in the RVs is marked with the dark red vertical line, and its first harmonic is marked with the light red line. The widths of the vertical lines correspond to the 68% confidence interval on the posterior of P rot and its first harmonic. Our joint model finds P rot = 24.8 ± 0.9 days. We compute the GLS periodogram of the RV window function with a minimum period slightly longer than 1 day to avoid the strong nightly alias that otherwise skews the y-axis scale.
Paper: The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824 
Authors: Sarah Lange, Joseph M. Akana Murphy, Natalie M. Batalha, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, David R. Ciardi, Andrew W. Boyle
Figure caption: Top: the TESS SAP light curve is shown in black, and the GP used to flatten the light curve is overplotted in green. TOI-1824 exhibits peak-to-peak spot modulation of close to 1% during Sectors 21 and 22, though the amplitude of this rotation signal is damped in the subsequent sectors. Blue triangles mark TOI-1824 b transits—the fifth and seventh triangles mark transits that fall in data gaps. Middle: the flattened SAP light curve is shown in black, and the TOI-1824 b transit model is overplotted in blue. Residuals are shown below. Bottom: the flattened SAP light curve folded to TOI-1824 b’s orbit is shown in black, and data in 0.5 hr bins are shown in red. The pointwise uncertainty of the (unbinned) data is annotated in the bottom left of the panel. The MAP transit model along with 25 realizations of the model generated from random posterior draws is shown in blue. Residuals are shown below in units of ppt.
Paper: The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824 
Authors: Sarah Lange, Joseph M. Akana Murphy, Natalie M. Batalha, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, David R. Ciardi, Andrew W. Boyle
Figure caption: Top: APF-Levy and Keck-HIRES RVs are shown as the green diamonds and black circles, respectively, where the markers’ 1σ error bars represent the quadrature sum of the RV measurement error and an instrument-specific RV jitter term that is fit to the data. The GP plus Keplerian MAP models for both instruments are shown in blue, with error envelopes in corresponding colors representing the 1σ GP prediction uncertainty. Residuals are shown below in units of m s−1. Bottom: data minus the GP component of the RV model are shown as the green diamonds and black circles. Data from both APF-Levy and Keck-HIRES binned in 0.125 units of phase are shown in red. The Keplerian component of the MAP model along with 25 realizations of the model generated from random posterior draws is shown in blue. Residuals are shown below in units of m s−1.
Paper: The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824 
Authors: Sarah Lange, Joseph M. Akana Murphy, Natalie M. Batalha, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, David R. Ciardi, Andrew W. Boyle
Figure caption: An example of our simultaneous transit and GP fitting for the transit of TOI-1824 b in Sector 21 (i.e., the same sector that is shown in Figure 2). The SAP data are shown in black, and data in 20 minute bins are shown in red. The GP prediction across the transit (plus a small global offset fit to the data) is shown as the green dashed line, and the best-fitting transit model is shown as the blue solid line. We visually inspected each transit to ensure that the GP prediction did not absorb any of the transit signal.
Paper: The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824 
Authors: Sarah Lange, Joseph M. Akana Murphy, Natalie M. Batalha, Ian J. M. Crossfield, Courtney D. Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Aida Behmard, Corey Beard, Sarah Blunt, Casey L. Brinkman, Ashley Chontos, Fei Dai, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Jack Lubin, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Daria Pidhorodetska, Alex S. Polanski, Malena Rice, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Judah Van Zandt, David R. Ciardi, Andrew W. Boyle
Figure caption: The S HK portion of the joint model, in which GPs, with some shared hyperparameters, are simultaneously fit to the RVs and the Keck-HIRES S HK values. The GP kernel is described in Section 9.3. The posterior median and 68% confidence interval for the GP period is P rot = 24.8 ± 0.9 days. See Figures 7 and 8 for the photometry and RV portions of the joint model. The GP posterior prediction is shown as the blue line surrounded by a 1σ error envelope. The Keck-HIRES S HK values are shown as the black points with 1σ errors, where the measurement error on each S HK value has been added in quadrature with a jitter term that has been fit to the data. Residuals are shown in the bottom panel.