adsabs/AstroCLIMB huggingface dataset:
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: Residual light fractions of our Fornax dwarf ETG sample as a function of their total g − r color. Left panel: g-band residual light fraction vs. total g − r color. Right panel: r-band residual light fraction vs. total g − r color. Galaxies classified as disky are shown as red points, while galaxies classified as clumpy are shown as blue points. The measurements are performed within one and two effective radii of the galaxies, shown as filled and empty circles, respectively. The error bars are given by the 16th and 84th percentiles of the distributions.
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Location of the spectroscopic fields targeting the NE Shelf (red open boxes; Table 1, Section 2.1) in M31-centric coordinates overlaid on a star count map from the PAndAS survey (McConnachie et al. 2018). The black ellipse represents M31's disk assuming a projected radius of 17 kpc, a major-axis position angle of 38°, and an inclination angle of 77°. The dashed purple lines correspond to 50 projected kpc. The approximate size and orientation of each DEIMOS field are represented by a 16′ × 4′ rectangle. We also show spectroscopic fields from the Elemental Abundances in M31 survey (filled boxes; Gilbert et al. 2019; Escala et al. 2020a, 2020b) and fields previously observed as part of the SPLASH survey (open boxes; Kalirai et al. 2006; Gilbert et al. 2007, 2009; Fardal et al. 2012) spanning the SE shelf (blue), W shelf (pink), and GSS (green). The black points are the edges of the NE and W shelves defined by Fardal et al. (2007) via applying an edge filter to the Irwin et al. (2005) star count map.
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Heliocentric radial velocity distributions for stars with successful velocity measurements (gray filled histograms; Section 2.1) in spectroscopic fields targeting the NE shelf (Table 1), including both M31 RGB stars and MW foreground dwarf stars. From top to bottom and left to right, the fields probe larger M31-centric projected radii, approaching the “tip” of the tidal shell pattern (Section 3.4). The black dashed lines show the velocity distribution of stars classified as likely M31 members by the probabilistic model of Escala et al. (2020b), which includes radial velocity as a membership diagnostic. This model mistakenly classifies NE shelf stars in field NE3 with MW-like velocities (v helio ≳ −150 km s−1; Section 3.1) as likely MW contaminants. Thus, we assigned stars with v helio > −100 (−150) km s−1 for the inner (outer) fields or spectral signatures of strong Na I λ8190 absorption as MW contaminants (red open histograms; Section 3.1).
Paper: Kinematics and Metallicity of Red Giant Branch Stars in the Northeast Shelf of M31 
Authors: Ivanna Escala, Karoline M. Gilbert, Mark Fardal, Puragra Guhathakurta, Robyn E. Sanderson, Jason S. Kalirai, Bahram Mobasher
Figure caption: Extinction-corrected (V 0, I 0) CMD (Section 2.2) for all stars in the NE shelf fields (Table 1), including stars without successful radial velocity measurements (gray points), MW foreground stars (black crosses; Section 3.1), and M31 RGB stars (red circles). The median photometric uncertainties as a function of magnitude are shown as black error bars on the left. For reference, we show PARSEC isochrones (black lines; Marigo et al. 2017), assuming 12 Gyr ages and [α/Fe] = 0, with [Fe/H] = −2.0, −1.0, −0.5, and 0 (from left to right).
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Molecular clouds identified in three CO surveys: (top) the MWISP survey, (middle) the OGS, and (bottom) the CfA-Chile survey. In order to reveal details, the demonstrated images zoom in on a part of the PPV data cubes (130° ≤ l ≤ 135°, −2° ≤ b ≤ −1°, and −20 ≤ V LSR ≤ −10 km s−1). The background and color lines are the integrated CO maps and the integrated regions of molecular clouds (defined by DBSCAN) from −20 to −10 km s−1, respectively. Numbers of molecular clouds only take account of those in the above-mentioned PPV range.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Variation of molecular cloud number, the total angular area, and the total flux with respect to velocity resolution. In order to see the distance effects, molecular cloud samples are split into four parts, approximately corresponding to four arm segments (Sun et al. 2021), the Local (−25 to 15 km s−1), the Perseus (−65 to −25 km s−1), the Outer (−95 to −65 km s−1), and the Outer Scutum Centaurus (OSC, −125 to −95 km s−1) arms.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Molecular cloud edges defined with three algorithms: DBSCAN (top), HDBSCAN (middle), and SCIMES (bottom). In order to display edges clearly, this demonstration zooms in on a small PPV range (130° ≤ l ≤ 135°, −2° ≤ b ≤ −1°, and −20 ≤ V LSR ≤ −10 km s−1). The background images and color lines are the integrated CO maps and projection edges, respectively. Numbers of molecular clouds only take account of those in the above-mentioned PPV range.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Angular area distributions of molecular clouds in three GMCs, W3, W5, and NGC 7538. See Figure 11 for a view of those samples. As a comparison, distributions of the molecular cloud samples in the entire PPV region (see Table 1) are shown in the upper left panel.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Flux distributions of molecular clouds in three GMCs, W3, W5, and NGC 7538. See Figure 11 for a view of those samples. As a comparison, distributions of the molecular cloud samples in the entire PPV region (see Table 1) are shown in the upper left panel.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Molecular cloud samples of three GMCs, W3, W5, and NGC 7538, in three CO surveys. The left, middle, and right columns show results of the CfA-Chile survey, the OGS, and the MWISP survey, respectively. See Table 2 for the PPV range of the GMCs.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Distribution of the angular area and the flux of molecular clouds in three CO surveys: the MWISP survey, the OGS, and the CfA-Chile survey.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Molecular clouds with three DBSCAN parameter combinations based on the MWISP survey. Each combination corresponds to one connectivity and an appropriate MinPts value. Connectivity 1 identifies slightly more molecular clouds than the other two cases.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Variation of molecular cloud properties with respect to algorithms and sensitivity (cutoffs). From left to right, this demonstration shows the number, the total angular area, and the total flux of molecular clouds identified with three algorithms, DBSCAN (blue), HDBSCAN (green), and SCIMES (red).
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption: WISE IR excess (observed − expected [3.4]−[12]) for gold member stars unlikely to be pulsators, in bins of ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩, as shown in each panel. The black dots are stars without disks; the red circles are stars with high-confidence disks. An additional green symbol means that there are multiple periods associated with the object, e.g., it could be a multiple or subject to source confusion. UCL/LCC stars with disks tend to rotate more slowly than the ensemble, or, rather, fast-rotating stars tend not to have disks. The blue vertical dotted lines in the bottom four panels are located at the mean period for disked stars with ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩>4.5 and ([3.4] − [12])observed − ([3.4] − [12])expected > 0.3 in each panel (2.5, 1.8, 1.8, and 1.5 days, respectively). Among the disked mid-M stars with large IR excesses, M5 stars rotate faster than M3 stars.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption:  P (in days) vs. ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩ for M stars, with disks (high-confidence and possible) removed, and just UCL/LCC gold members. Top row: observations (the dotted lines are breakups); bottom row: medians of the observations in ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩ bins. Column 1: USco; Column 2: UCL/LCC; Column 3: Pleiades; and Column 4: Praesepe. In the top row, USco fit: red line; UCL/LCC fit: blue line; Pleiades fit: green line; and Praesepe fit: yellow line. In the bottom row, USco binned data: red symbols; UCL/LCC binned data: blue symbols; Pleiades binned data: green symbols; and Praesepe binned data: yellow symbols. The USco binned data are shifted in the second panel to match UCL/LCC, and shifted in the third panel to match Pleiades. Pleiades is shifted in the fourth panel to attempt to match Praesepe. UCL/LCC fits neatly in between USco and Pleiades, with a slope that is indistinguishably the same.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption:  P (in days) vs. ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩ for all stars in nine clusters, all from K2, except UCL/LCC. Stars with IR excesses (e.g., disks) are shown with an additional red circle. The first row has the youngest, most populous cluster, USco, underplotted in gray. The second row has the Pleiades underplotted in gray. The third row has Praesepe underplotted in gray. The points are smaller for UCL/LCC because there are so many points that it is hard to see the patterns otherwise. The UCL/LCC points are all from the gold member sample. It again seems to fit well “in sequence” with the other clusters around it. References for data—Rho Oph: Paper V; Lagoon: Rebull et al. (in preparation); Taurus: Paper VI; USco: Paper V; UCL/LCC: this work; Taurus Foreground: Paper VI; Pleiades: Papers I and II; Hyades: L. M. Rebull et al. (2022, in preparation); and Praesepe: Paper IV.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption:  P (in days) vs. ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩ for M stars from the gold member sample, where the black points are disk-free M stars, the red circles are high-confidence disked M stars, and the yellow circles are lower-confidence disked M stars. The left panel is USco, and the other two panels are UCL/LCC (the black dots are the same in the middle and right panels). The disked stars have an obvious “pileup” near 2 days among the M stars, and there may be a slope to that 2 day pileup; see the text. The lack of structure in the last panel reinforces our lack of confidence in those disks in general.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption: The locations of the targets in Galactic coordinates, as in Figure 1. Stars with high-confidence disks from UCL/LCC (or USco; Paper IV) are marked with red points; stars with lower-confidence disks from UCL/LCC are marked with yellow points. The gray points are simply stars with LCs. The high-confidence disks are clustered, but not nearly as much as they were in USco. The high-confidence disk fractions in both UCL and LCC are ∼7%–8%, and there is no obvious large-scale gradient in disk fraction with position among UCL/LCC.
Paper: Line-by-line Velocity Measurements: an Outlier-resistant Method for Precision Velocimetry
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Thomas Vandal, Jean-François Donati, Claire Moutou, Xavier Delfosse, Pascal Fouqué, Eder Martioli, François Bouchy, Jasmine Parsons, Andres Carmona, Xavier Dumusque, Nicola Astudillo-Defru, Xavier Bonfils, Lucille Mignon
Figure caption: Proxima Centauri activity modeling with the dLW and the CCF FWHM. Left panels: changes in the dLW line shape parameter compared to the CCF FWHM. The green and red curves represent the mean prediction of the best-fit quasiperiodic Gaussian process (GP; described in Appendix C), each surrounded by a 68% confidence envelope. Middle panel: direct comparison between the dLW (expressed in FWHM) and the CCF FWHM. One does not expect a perfect correspondence between the two variables, as the equivalence between the dLW and the FWHM is only strictly true for Gaussian lines. Right panel: posterior distributions on P rot from the quasiperiodic GP model of the dLW and CCF FWHM time series. The 68% confidence intervals on P rot are represented with green (LBL) and red (CCF) regions. The black dashed lines show the 10% relative uncertainty interval for Proxima’s rotation period (P rot = 89 days) from Newton et al. (2018). There is no specific uncertainty for the Newton et al. (2018) rotation period, but the typical uncertainties in their sample are at the 10% level.
Paper: Line-by-line Velocity Measurements: an Outlier-resistant Method for Precision Velocimetry
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Thomas Vandal, Jean-François Donati, Claire Moutou, Xavier Delfosse, Pascal Fouqué, Eder Martioli, François Bouchy, Jasmine Parsons, Andres Carmona, Xavier Dumusque, Nicola Astudillo-Defru, Xavier Bonfils, Lucille Mignon
Figure caption: Phase-folded radial velocity (RV) curves (top panels) and orbital fit residuals (bottom panels) for Proxima b and d (model M bd+dLW), with systemic velocity and activity Gaussian process removed. Binned RVs (0.1 phase bin) are represented with black data points. The best-fit Keplerian models for Proxima b and d are shown with solid blue curves, with 68% confidence interval envelopes in light blue.
Paper: Line-by-line Velocity Measurements: an Outlier-resistant Method for Precision Velocimetry
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Thomas Vandal, Jean-François Donati, Claire Moutou, Xavier Delfosse, Pascal Fouqué, Eder Martioli, François Bouchy, Jasmine Parsons, Andres Carmona, Xavier Dumusque, Nicola Astudillo-Defru, Xavier Bonfils, Lucille Mignon
Figure caption: Left: for a sample Barnard’s star observation, the histogram of the per-line velocity difference from the mean velocity divided by the corresponding line uncertainty closely follows a normal distribution (dashed line) with only a handful of >5σ outliers. Right: spectral distribution of >5σ outliers in a random Barnard’s star observation.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Radial velocities from APOGEE (Jönsson et al. 2020) for KOI-3876 as a function of the planet’s orbital phase and colored by the rotational phase. The velocities rule out any companion more massive than ≃2 M  J , thus also ruling out any possibility of an eclipsing binary at the transit period. The scatter is larger than expected for the uncertainties by ≃100m s−1, most likely due to stellar jitter common in young stars (Brems et al. 2019; Tran et al. 2021). The residual jitter is still far below the expected variation for a tight eclipsing binary.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: The current census of young (Hyades-age or younger) transiting planets within clusters or young associations. Points are color-coded by age. The two stars are KOI-3876b and Kepler-970 b. The contours represent the density of (mostly older) transiting planets from Kepler. Planet parameters taken from the NASA exoplanet archive (NASA Exoplanet Science Institute 2020).
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Transit timing of Kepler-970 b from Holczer et al. (2016). The orange is our best-fit to the data, assuming the variation is from a companion on a circular orbit.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Representative sections of the two planet host light curves. The top two are for KOI-3876, while the bottom two are for Kepler-970. The gray points are the Kepler data, the red line shows the best-fit GP model, and the arrows indicate transits.
Paper: Recalculated Orbits Of Binaries and New Linear Solutions
Authors: Z. Cvetković, R. Pavlović
Figure caption: Apparent orbits for the binaries: EGG 2Aa, Ab, COU 1085, COU 1897, COU 1006, A 578Aa, Ab and A 1400; the previously published orbits are shown as dashed lines. In each plot, the primary component is located at the coordinate origin; new orbits are represented by solid lines; filled circles and cross signs denote spackle interferometric and visual micrometric measurements, respectively; a Hipparcos measurement is denoted by open circle; CCD measurements are marked by triangle sign; and the direction of motion is indicated in the northeast orientation in the lower right corner. The shaded part is the confidence region.
Paper: Recalculated Orbits Of Binaries and New Linear Solutions
Authors: Z. Cvetković, R. Pavlović
Figure caption: Apparent orbits for the binaries: A 606, BU 984, and BU 992; symbols as in Figure 1.
Paper: Recalculated Orbits Of Binaries and New Linear Solutions
Authors: Z. Cvetković, R. Pavlović
Figure caption: The previously published orbits (left) and our linear fits (right) for the pairs: COU 966, J838, and A 1247; symbols as in Figures 1 and 2. In each plot of linear fit, the arrow in the lower right corner indicates the direction of the relative motion of the secondary; the dashed perpendicular line from the linear fit to the origin indicates the closest relative separation.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Top: normalized transit light curves of KOI-340 from the Kepler DR25 (Thompson et al. 2018) data release are shown as a function of phase. The out-of-transit data are displayed in green, the ingress and egress are in red, and the measurements made when the companion is in transit (between the second and third contact points) are in blue. The black line model is generated by using the DR25 parameters for KOI-340 with the batman software (Kreidberg 2015). Bottom: residual Kepler transit light curves of KOI-340 compared to the model generated from the parameters from the DR25 (Thompson et al. 2018) data release vs. phase. The out-of-transit data are in green, and the measurements made between the second and third contact points are in blue. The significant increase in in-transit scatter compared to the immediately adjacent out-of-transit data is the signature of the secondary star occulting starspots on the surface of the primary star. We have chosen not to plot the ingress and egress points to highlight the difference between the in-transit and out-of-transit points.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Top: four normalized transit light curves of KOI-340 that show little or no starspot crossing features. The data are phase-folded with the period in Table 1 and plotted vs. phase. The red line Mandel & Agol (2002) model is generated from the MCMC analysis of these primary transits, along with the RV measurements and secondary transits from Kepler. The depth of the transit derived from only unspotted transits is δ = 0.020164 ± 0.000096. Bottom: all normalized secondary transits observed in the long-cadence Kepler data of KOI-340 phase-folded with the ephemeris presented in Table 1 and plotted vs. phase. The red line model is generated from the MCMC analysis described in Section 2. The phase of the secondary transit occurs at 0.319 owing to the eccentricity of the system.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: RV points from Lillo-Box et al. (2015) of KOI-340 phase-folded with the ephemeris presented in Table 1 and plotted vs. phase. The red line model is generated from the MCMC analysis described in Section 2.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: The LS periodogram over all Kepler data with primary transits removed. The period at maximum power suggests a rotational period for KOI-340 of 13.02 ± 0.97 days.