adsabs/AstroCLIMB huggingface dataset:
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The results of the resampling experiment for TOI-669 b. Each cell represents a resampled realization of the full data set according to specified MOC (left y-axis) and N RV (x-axis) values. The right y-axis is the same as the left, but it is now shown in units of the orbital period of the planet. The color of each cell represents the difference between the planet’s measured semiamplitude using that cell’s resampled data set, K fit, and the measured semiamplitude of the planet from the baseline model (K baseline), in units of the error on K baseline. Gray regions represent combinations of MOC and N RV that are not supported by the data.
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The same as the top panel of Figure 3, but instead of using the baseline model, we intentionally apply a model that does not account for the orbit of HIP 8152 c.
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The same as Figure 2 but for HIP 8152 b (top) and c (bottom). In the top (bottom) panel, black horizontal dashed lines represent harmonics of the orbital period of planet c (b).
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The same as Figure 8 but now σ RV,inst = 0.4 m s−1 (i.e., the “KPF” case for internal RV precision).
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The same as Figure 3 but for TOI-1272 b (top) and c (bottom). In the top (bottom) panel, black horizontal dashed lines represent harmonics of the orbital period of planet c (b).
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The same as Figure 2 but for TOI-1444 b (top) and c (bottom). In the top (bottom) panel, black horizontal dashed lines represent harmonics (aliases) of the orbital period of planet c (b).
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The same as Figure 6, but now a GP has been included to account for correlated noise due to stellar activity.
Paper: The Impact of Observing Cadence and Undetected Companions on the Accuracy of Planet Mass Measurements from Radial Velocity Monitoring
Authors: Joseph M. Akana Murphy, Rafael Luque, Natalie M. Batalha
Figure caption: The same as Figure 8 but now σ RV,astro = 1.2 m s−1 (i.e., the “active” case for stellar jitter).
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: In each panel, stars studied here are represented by squares and lines connect components in a pair. Open squares indicate components A and BC in the non-twin triple KX Com. (Top left)—P rot vs. Hα EW, with fully convective stars (M < 0.35) from E. R. Newton et al. (2017) underplotted. All points for bona fide twins are color coded by mass except our stars that have less reliable mass estimates, shown in black. Bars on the squares for the stars studied here show the range of observed Hα values for each star, excluding flares or epochs without A and B observed back-to-back. System letter labels are placed next to the A components in each pair. (Bottom left)—The same as above, now with L X and underplotting fully convective stars from N. J. Wright et al. (2011) and N. J. Wright et al. (2018). An arrow indicates the upper limit in L X for NLTT 44989 A (Section 3.4.1). The multiple Chandra epochs for GJ 1183 and KX Com are shown with multiple connected points. (Right)—Hα EW vs. L X, again showing the observed Hα ranges as shaded bars and multiple connected points for the multiple Chandra visit cases. Underplotted gray points show field M dwarfs from J. G. Doyle (1989) for comparison. The vertical dashed blue line at EW = 0 divides active emission and inactive absorption stars. An arrow again indicates the upper limit in L X for NLTT 44989 A. Overall, among twin pairs, strong Hα emission is correlated with high L X, and each of those observables is correlated with fast rotation.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: The 0.9 m V-band rotation amplitudes (peak-to-peak Δ) vs. (a) the rotation period, (b) Hα EW, and (c) L X. Lines connect the A (red) and B (black) components in a pair, with open squares indicating the non-twin triple KX Com A-BC. Overall, no clear correlations are seen. Blue horizontal dashed lines in panel (a) at 10 and 70 days bound the approximate region of intermediate rotation periods where few FC M dwarfs are found (E. R. Newton et al. 2018). The blue horizontal dashed line in panel (b) at EW = 0 marks the approximate transition between active Hα emission and inactive Hα absorption. Shaded red and gray bars in panel (b) are the ranges of observed Hα EW values for each star, excluding flares or epochs without A and B observed back-to-back. Stars in panel (c) with three vertically stacked connected points show the three epochs of Chandra L X measurements in those cases. An arrow in panel (c) indicates the upper limit in L X for NLTT 44989 A.
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: The same as Figure 2, now for all of the remaining X-ray data sets. NLTT 44989 A is not shown, given its lack of a confident detection (see Section 3.4.1).
Paper: The Solar Neighborhood. LII. M Dwarf Twin Binaries—Presumed Identical Twins Appear Fraternal in Variability, Rotation, Hα, and X-Rays
Authors: Andrew A. Couperus, Todd J. Henry, Rachel A. Osten, Wei-Chun Jao, Eliot Halley Vrijmoet, Aman Kar, Elliott Horch
Figure caption: The same as Figure 3, now for all of the remaining quiescent X-ray data sets. NLTT 44989 A is not shown, given its lack of a confident detection (see Section 3.4.1).
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: Plots of the transit model fits, with residuals after subtracting the median models provided in the lower panel of each phase diagram. Black points show observations with offsets subtracted and jitter terms added in quadrature with uncertainties, while colored circles represent binned data. Colored lines represent median model values. In each planet’s phase diagram, the best-fit models for the other two planets have been subtracted from the data.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: SPOC PDCSAP light curve for TOI-6276 from Sectors 63 and 64 before detrending (top panel) and after detrending (bottom panel) with wotan. The transits of TOI-6276.01, 6276.02, and 6276.03 are indicated by green, orange, and red dots, respectively, based on our TLS search.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: RV observations from PFS (green), UCLES (blue), and HARPS (orange). PUCHEROS+ RVs are not included due to the large uncertainties (∼50 m s−1). While the expected RV semiamplitudes of the three planets are too small to be resolved (<0.4 m s−1), the observations do not feature large RV variations corresponding to stellar-mass companions.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: The field within 60″ of HD 101581 in blue (far left-hand panel), infrared (center left-hand panel), and red (center right-hand panel) filters from the SERC and AAO-SES Surveys, and from LCO/CTIO observations taken shortly after the end of the TESS observations in 2023 (far right-hand panel). The location of HD 101581 at the time of each image is marked with a blue cross, while the location at the start of TESS Sector 63 in 2023 March is marked in orange. The width of a TESS pixel (21″) is marked in the top left-hand corner of each panel. HD 101581 has moved ∼32″ between 1977 and 2023.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: SED of HD 101581. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit PHOENIX atmosphere model (black). The absolute flux-calibrated Gaia spectrum is shown as a gray swathe in the inset figure.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: Linear acceleration model for HD 101581 in Hipparcos-Gaia astrometry (R.A., top left-hand panel; decl., top right-hand panel), and RV (bottom left-hand panel) across >20 yr of observations. In each dimension we find that the acceleration terms are consistent with zero at high precision. We leverage this to achieve strong limits on the existence of bound unresolved companions as a function of projected separation (bottom right-hand panel). Based on the velocities alone, stellar-mass companions to HD 101581 can be entirely excluded within <110 au.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: Differences between observed and calculated transit times (assuming linear ephemerides) for each planet in the TOI-6276 system. Each data point corresponds to the median with 16th to 84th percentile error bars. The transits of HD 101581 b are consistent with no variation, though we potentially see variations with a ∼15 minutes amplitude for HD 101581c. We also see >1σ variations among the first two transits of TOI-6276.03, but it is less clear if these are reliable given the low SNR of the transits.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: GLS periodograms of the RVs and S-indices measured by PFS. The horizontal lines mark 1% (dotted line) and 0.1% (dashed–dotted line) FAP levels. Only one peak is stronger than the 0.1% level, at P = 29.4 days in the power spectrum for S-indices, which likely corresponds to the P rot ∼ 30 days rotation period estimated through relation to the chromospheric emission parameter ﹩\mathrm{log}{R}_{{HK}}^{{\prime} }=-4.77﹩.
Paper: Two Earth-size Planets and an Earth-size Candidate Transiting the nearby Star HD 101581 
Authors: Michelle Kunimoto, Zifan Lin, Sarah Millholland, Alexander Venner, Natalie R. Hinkel, Avi Shporer, Andrew Vanderburg, Jeremy Bailey, Rafael Brahm, Jennifer A. Burt, R. Paul Butler, Brad Carter, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Knicole D. Colón, Jeffrey D. Crane, Tansu Daylan, Matías R. Díaz, John P. Doty, Fabo Feng, Eike W. Guenther, Jonathan Horner, Steve B. Howell, Jan Janik, Hugh R. A. Jones, Petr Kabáth, Shubham Kanodia, Colin Littlefield, Hugh P. Osborn, Simon O'Toole, Martin Paegert, Pavel Pintr, Richard P. Schwarz, Steve Shectman, Gregor Srdoc, Keivan G. Stassun, Johanna K. Teske, Joseph D. Twicken, Leonardo Vanzi, Sharon X. Wang, Robert A. Wittenmyer, Jon M. Jenkins, George R. Ricker, Sara Seager, Joshua Winn
Figure caption: Contrast curves and high-resolution images from archival VLT/NACO AO observations (top panel) and Gemini-S/Zorro speckle observations (bottom panel). No stellar companions were detected in any observations.
Paper: Photometric Analysis of the Cataclysmic Variable Star LT Eri
Authors: Qi-Bin Sun, Sheng-Bang Qian, Li-Ying Zhu, Qin-Mei Li, Fu-Xing Li, Min-Yu Li, Ping Li
Figure caption: Comparison of different LSPs and folding curves. Left: (a) the LSP of the detrended out-of-eclipse curves of LT Eri; (b) the LSP for the eclipse-depth variation; (c) the LSPs for all (black line) and quiescent (red line) O – Cs; (d) the LSP of O – C for the reproduction of the light curves; see Section 3.7 for details. The vertical magenta dashed line is the location of the predicted precession signal. Right: the folding curves used in the left panels for the LSP analysis of the curve counterparts; the folding period and the zero-phase point agree on the use of BJD 2459176.96199 and 3.5781(6) days.
Paper: Photometric Analysis of the Cataclysmic Variable Star LT Eri
Authors: Qi-Bin Sun, Sheng-Bang Qian, Li-Ying Zhu, Qin-Mei Li, Fu-Xing Li, Min-Yu Li, Ping Li
Figure caption: Example and reproduced light curves of LT Eri. Left: (a) the black data points are the original out-of-eclipse curves, the red data points are the eclipse data, and the cyan line is the parabolic fitted curve; (b) the reproduced NSHs; (c) the reproduced eclipse curves; (d) the reproduced NSHs superimposed on the eclipse curves; and (e) the superimposed NSHs and eclipse curves with the curves of the outburst trend. Right: comparison of the original light curves with the reconstructed light curves.
Paper: A Tentative Detection of a Point Source in the Disk Gap of HD 100546 with VLT/SPHERE-IRDIS Sparse Aperture Masking Interferometry 
Authors: Dori Blakely, Doug Johnstone, Tomas Stolker, Myriam Benisty, Jens Kammerer, Brodie J. Norfolk, William Thompson, Jean-Philippe Berger
Figure caption: Corner plot from the joint fit of the PG+PS model, with the disk geometry fixed between epochs, and the companion location allowed to vary.
Paper: A Tentative Detection of a Point Source in the Disk Gap of HD 100546 with VLT/SPHERE-IRDIS Sparse Aperture Masking Interferometry 
Authors: Dori Blakely, Doug Johnstone, Tomas Stolker, Myriam Benisty, Jens Kammerer, Brodie J. Norfolk, William Thompson, Jean-Philippe Berger
Figure caption: Orbital analysis corner plot, showing only the stellar mass, semimajor axis, eccentricity, and inclination distributions.
Paper: A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey
Authors: Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu
Figure caption: Examples of LAMOST spectra of the targets cataloged in this work, smoothed by 3 pixels. From top to bottom: a PN candidate from M06, a newly discovered H II region candidate, a newly discovered yellow supergiant candidate, and a known GC from RBC V5.
Paper: A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey
Authors: Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu
Figure caption: Top panel: the original LAMOST spectrum of an A-type star. Bottom panel: the same spectrum after preprocessing. The spectrum in the wavelength region 5800–6300 Å, where the LAMOST blue and red arms are connected, is masked using a straight line.
Paper: A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey
Authors: Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu
Figure caption: Confusion matrix showing the predicted and true classifications from the trained RFC.
Paper: The Gl 229 System Revisited with the Line-by-line Framework: Planetary Signals Now Appear as Stellar Activity Ghosts
Authors: Ariane Deslières, Charles Cadieux, René Doyon, Étienne Artigau, Neil J. Cook, Clémence Fontanive, Thomas Vandal
Figure caption: Summary of the RV analysis of Gl 229. Left panels: RV contribution from stellar activity with the mean prediction of the activity model (green curve) with its 1σ confidence envelope, for the full dataset and the postfiber change data. The middle plot represent the linear component to capture the BD effects (blue curve). Following are the residuals of the best-fit joint model (activity + linear trend) for both datasets. The vertical blue dashed line in the first, third, and fourth panels separates the values obtained before and after the optical fibers change in the HARPS instrument. Right panels: the corresponding Lomb–Scargle periodogram (in black) after subtracting the different components of the model and the associated window function (in cyan). Various relevant periodicities are shown with dashed vertical lines (same as in Figure 1).
Paper: The Gl 229 System Revisited with the Line-by-line Framework: Planetary Signals Now Appear as Stellar Activity Ghosts
Authors: Ariane Deslières, Charles Cadieux, René Doyon, Étienne Artigau, Neil J. Cook, Clémence Fontanive, Thomas Vandal
Figure caption: Detection limit for a planet in the Gl 229 system. The black line represents the minimal ﹩{M}_{{\rm{p}}}\sin i﹩ at which a planet can be detected at the associated period with the LBL dataset. The tested periods are represented by the black dots. The green-shaded region delimits the system's HZ, while the vertical blue dashed line indicates the orbital period at which the received flux is the same as Earth. The previously claimed planet Gl 229 A b and c are also represented by dots, respectively in orange, green, and pink.