adsabs/AstroCLIMB huggingface dataset:
Paper: Characterizing the Time Variability of 2M1207 A + b with JWST NIRSpec/PRISM
Authors: Arthur D. Adams, Yifan Zhou, Gabriel-Dominique Marleau, Daniel Apai, Beth A. Biller, Aarynn L. Carter, Johanna M. Vos, Niall Whiteford, Stephan Birkmann, Theodora Karalidi, Xianyu Tan, Jason Wang, Yuhiko Aoyama, Brendan P. Bowler, Mickaël Bonnefoy, Jun Hashimoto
Figure caption: The IFU image of the 2M1207 data after PSF subtraction, integrated across all wavelength elements. The dashed white circles show the positions and radii of the four areas used to sample the background flux. The orientation and color scale of the image are identical to those of Figure 1.
Paper: A Sample of Eccentric Eclipsing Binaries in TESS
Authors: Yanke Tang, Xiaodian Chen, Ning Gai, Shu Wang, Zichuan Li, Zhikai Li, Kai Li, Yifan Wang
Figure caption: LC analysis and eclipses determination for EEB TIC 425549135 as an example.(a) LC. (b), (c) The original LC is folded and smoothed to obtain the folded LC and the differential folded LC, which are used to determine the eclipses. Pink solid lines represent the rough minimum moments, and light-blue solid lines represent the rough starts and ends. (d), (e) Two eclipses (black dots) are fitted by the Gaussian function (red solid curve) to determine mideclipse phases (red dashed lines). Blue dashed lines represent the start or end phases of the eclipses.
Paper: Asteroid Mass Estimation by Mutual Perturbations During Close Encounters After Gaia Focused Product Release
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Jon D. Giorgini, Ryan S. Park
Figure caption: Differences in mass estimates of largest main-belt objects except 1 Ceres and 4 Vesta from this work (FM+2025, at the origin with error bars) and A. Fienga et al. (2020a, 2020b), E. Goffin (2014), and P. Kuchynka & W. M. Folkner (2013). The right panel shows histograms of the differences normalized by σGM of the selected references. Mean, standard deviation and outliers are reported in Table 3.
Paper: Asteroid Mass Estimation by Mutual Perturbations During Close Encounters After Gaia Focused Product Release
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Jon D. Giorgini, Ryan S. Park
Figure caption: Density estimates of masses converted to Gaussian pdf for the various taxonomic types.
Paper: Asteroid Mass Estimation by Mutual Perturbations During Close Encounters After Gaia Focused Product Release
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Jon D. Giorgini, Ryan S. Park
Figure caption: Relative difference (GMtax − GMfin)/GMfin between GM estimates via taxonomy and final estimates. We only include estimates with SNR > 10, color coded by taxonomic types. The right panel is a detailed view of the region of GM < 5 km3 s−2 and ﹩\left|{\rm{\Delta }}{\rm{GM/GM}}\right|﹩ < 0.5. The error bars show uncertainties and relative uncertainties (1σ) of the final estimates.
Paper: Asteroid Mass Estimation by Mutual Perturbations During Close Encounters After Gaia Focused Product Release
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Jon D. Giorgini, Ryan S. Park
Figure caption: Comparison of initial and final mass estimates to the literature. The references are B. Carry (2012; Carry+2012), J. Baer & S. R. Chesley (2017; Baer+2017), A. Fienga et al. (2020a; Fienga+2020b), L. Siltala & M. Granvik (2021) or L. Siltala & M. Granvik (2022; Siltala+2022), and F. Li et al. (2023; Li+2023).
Paper: Asteroid Mass Estimation by Mutual Perturbations During Close Encounters After Gaia Focused Product Release
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Jon D. Giorgini, Ryan S. Park
Figure caption: Comparison of final mass estimates and masses derived from binary systems, either from P. Vernazza et al. (2021) or the references listed in Table 5, complete as supplementary information.
Paper: Asteroid Mass Estimation by Mutual Perturbations During Close Encounters After Gaia Focused Product Release
Authors: Oscar Fuentes-Muñoz, Davide Farnocchia, Jon D. Giorgini, Ryan S. Park
Figure caption: Total main-belt mass as a function of the absolute magnitude threshold H with 3σ error bars. The right axis shows the number of asteroids included to obtain each value of total mass.
Paper: A Sample of Eccentric Eclipsing Binaries in TESS
Authors: Yanke Tang, Xiaodian Chen, Ning Gai, Shu Wang, Zichuan Li, Zhikai Li, Kai Li, Yifan Wang
Figure caption: Histogram of the periastron argument ω for EEBs.
Paper: A Sample of Eccentric Eclipsing Binaries in TESS
Authors: Yanke Tang, Xiaodian Chen, Ning Gai, Shu Wang, Zichuan Li, Zhikai Li, Kai Li, Yifan Wang
Figure caption: Spatial distribution of 514 EEBs (black star symbols). The sky coverage of TESS’s 26 sector observations is shown as the colorful background.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: UBV and Gaia based CMDs for Czernik 41 (panels (a), (b), (c)) and NGC 1342 (panels (d), (e), (f)). The blue solid lines are the PARSEC isochrones that best fit the observed data, providing estimates for the clusters’ distance moduli and ages. Purple solid lines represent the uncertainties in the age estimates. The color scales and symbol meanings are consistent with those described in Figure 4.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The distances of Czernik 41 (a), (b) and NGC 1342 (c), (d) from the Galactic center, along with their orbital trajectories perpendicular to the Galactic plane, are presented. The yellow-filled circles and triangles represent the current and early orbital positions of the clusters, respectively, while the red arrows indicate the direction of motion vectors of the OCs. The red-shaded regions in the right panels illustrate the uncertainty areas associated with the ages of the OCs. The vertical solid lines correspond to the ages of both OCs, marking their respective early orbital positions.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: Corner plot illustrating the two-dimensional joint and one-dimensional marginalized posterior distributions for the properties of Czernik 41 and NGC 1342. The contours in the two-dimensional joint posterior distributions represent confidence levels of 68%, 90%, and 95%. In the one-dimensional posterior distributions, vertical lines indicate the median as well as the 16th and 84th percentile confidence intervals. The CMDs of the OCs are displayed on the right side of the corner plots. Black dots correspond to the most probable member stars. The red solid lines are the PARSEC isochrones derived from the median values of the posterior distributions, and green dashed lines indicate calculated age errors of the OCs.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: TCD for nine F-G type main-sequence stars (P ≥ 0.5) in NGC 1342 is shown in the top panel. The blue curve in this panel represents the Hyades main sequence. The bottom panel illustrates the histogram of normalized UV-excesses (δ0.6), with a Gaussian function fitted to the distribution, depicted by the blue curve.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: For Czernik 41 (a) and NGC 1342 (b), the mass distributions (red points) are shown along with the blue linear line applied to the distribution. The green lines indicate the prediction levels (±1σ) of the linear fit.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The TCDs of the most probable main-sequence stars in the regions of the OCs Czernik 41 (a) and NGC 1342 (b) are presented. The reddened ZAMS, as defined by H. Sung et al. (2013), is depicted by the red dashed curves, while the green solid curves indicate the ±1σ standard deviations.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: Color excess histograms for the (a) Czernik 41 and (b) NGC 1342 OCs, estimated using the three-dimensional dust maps and distances between the Sun and individual stars calculated from trigonometric parallax data. The red line represents the mean color excess, while the gray-shaded area indicates the ±1σ standard deviation range.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The spatial distributions of member stars in Czernik 42 (top) and NGC 1342 (bottom) are presented in Galactic coordinates (l, b). Contour lines were generated based on color excess values derived from dust maps. The color scale in the right-hand panels indicates the magnitude of the color excess corresponding to the contour levels.
Paper: A Comprehensive Study of Czernik 41 and NGC 1342 Using CCD UBV and Gaia DR3 Data
Authors: Burçin Tanık Öztürk, Selçuk Bilir, Talar Yontan, Olcay Plevne, Tansel Ak, Serap Ak, Remziye Canbay, Timothy Banks
Figure caption: The histograms of LFs for Czernik 41 (a) and NGC 1342 (b).
Paper: TOI-880 is an Aligned, Coplanar, Multiplanet System
Authors: Elina Y. Zhang, Huan-Yu Teng, Fei Dai, Andrew W. Howard, Samuel P. Halverson, Howard Isaacson, Ryan A. Rubenzahl, Xian-Yu Wang, Songhu Wang, Benjamin J. Fulton, Louise D. Nielsen, Jack Lubin, Steven Giacalone, Luke B. Handley, Erik A. Petigura, Emma V. Turtelboom, Alex S. Polanski, Steve R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Christopher L. Smith, Josh Walawender, Joshua N. Winn
Figure caption: Top: KPF Hα line during the transit of planet c. There are 32 spectra in total, color-coded by their observation number (epoch). The vertical solid green line marks the line center at 6564.7463 Å, and the two dashed green lines are 1 Å away from the center. Left: excess absorption of Hα variation as a function of time, calculated in a bandpass of 2 Å around the line center. The color scale is the same as the top panel. The red line shows the best-fit trapezoid model with a quadratic baseline (best-fit top width =0.13 ± 0.90 hr, base width =1.23 ± 0.66 hr, and height/depth =0.004 ± 0.003 Å), while the blue line represents the white-light-curve transit model of planet c. Bottom right: The measured Hα line profile residuals as a function of time and wavelength. The vertical solid and dashed green lines are the same as the top panel. The predicted planetary velocity is marked by the black solid line. The horizontal dashed yellow lines denote the duration of the transit.
Paper: TOI-880 is an Aligned, Coplanar, Multiplanet System
Authors: Elina Y. Zhang, Huan-Yu Teng, Fei Dai, Andrew W. Howard, Samuel P. Halverson, Howard Isaacson, Ryan A. Rubenzahl, Xian-Yu Wang, Songhu Wang, Benjamin J. Fulton, Louise D. Nielsen, Jack Lubin, Steven Giacalone, Luke B. Handley, Erik A. Petigura, Emma V. Turtelboom, Alex S. Polanski, Steve R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Christopher L. Smith, Josh Walawender, Joshua N. Winn
Figure caption: Precession geometry of the TOI-880 system. In this framework, the z-axis is fixed to the system’s total angular momentum (Ltotal)—the sum of the stellar rotational component (L⋆) and the total planetary orbital component (Lp). Specifically for TOI-880, the system has L⋆ ∼ Lp with both components being non-negligible and simultaneously precessing around the system’s total angular momentum. Per Laplace–Lagrange theory, the planetary inclinations in the TOI-880 system undergo tiny oscillations around a common orbital plane (I = Ib = Ic = Id), and thus the total orbital angular momentum is Lp = Lp,b + Lp,c + Lp,d. Hence, the true stellar obliquity is simply derived from ψ = I + ψ⋆.
Paper: TOI-880 is an Aligned, Coplanar, Multiplanet System
Authors: Elina Y. Zhang, Huan-Yu Teng, Fei Dai, Andrew W. Howard, Samuel P. Halverson, Howard Isaacson, Ryan A. Rubenzahl, Xian-Yu Wang, Songhu Wang, Benjamin J. Fulton, Louise D. Nielsen, Jack Lubin, Steven Giacalone, Luke B. Handley, Erik A. Petigura, Emma V. Turtelboom, Alex S. Polanski, Steve R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Christopher L. Smith, Josh Walawender, Joshua N. Winn
Figure caption: Normalized flux vs. time from mid-transit time (in hours) for TOI-880 b (left), TOI-880 c (middle), and TOI-880 d (right). The planets are ordered in terms of increasing orbital periods. The star was observed at 2 minutes cadence in sector 33. The pink points with blue edges are the phase-folded binned data. The faint red lines are 20 curves from random posterior samples, and the darker purple line is the median fitted model from allesfitter. The bottom panels show the residuals, subtracting the best-fit model.
Paper: TOI-880 is an Aligned, Coplanar, Multiplanet System
Authors: Elina Y. Zhang, Huan-Yu Teng, Fei Dai, Andrew W. Howard, Samuel P. Halverson, Howard Isaacson, Ryan A. Rubenzahl, Xian-Yu Wang, Songhu Wang, Benjamin J. Fulton, Louise D. Nielsen, Jack Lubin, Steven Giacalone, Luke B. Handley, Erik A. Petigura, Emma V. Turtelboom, Alex S. Polanski, Steve R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Christopher L. Smith, Josh Walawender, Joshua N. Winn
Figure caption: Time-varying probability that a fixed observer sees all three TOI-880 planets transit. The color of the solid lines indicate the initial true obliquity of the common orbital plane. As the planets undergo nodal precession, a fixed observer will no longer see all three planets transit. However, because of the low J2, the timescale if of order Myr hence unlikely to be observable for TOI-880.
Paper: TOI-880 is an Aligned, Coplanar, Multiplanet System
Authors: Elina Y. Zhang, Huan-Yu Teng, Fei Dai, Andrew W. Howard, Samuel P. Halverson, Howard Isaacson, Ryan A. Rubenzahl, Xian-Yu Wang, Songhu Wang, Benjamin J. Fulton, Louise D. Nielsen, Jack Lubin, Steven Giacalone, Luke B. Handley, Erik A. Petigura, Emma V. Turtelboom, Alex S. Polanski, Steve R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Christopher L. Smith, Josh Walawender, Joshua N. Winn
Figure caption: The radial velocity variations during the transit of TOI-880 c on UTC 2024 January 20, as observed by KPF. In the top panel, the fainter pink curves are from random posterior samples. The darker purple line is the best-fit model with a sky-projected obliquity of ﹩{\lambda }_{c}=-7.{4}_{-7.2}^{+6.8}﹩°. The bottom panel shows the residuals, subtracting the best-fit model.
Paper: TOI-880 is an Aligned, Coplanar, Multiplanet System
Authors: Elina Y. Zhang, Huan-Yu Teng, Fei Dai, Andrew W. Howard, Samuel P. Halverson, Howard Isaacson, Ryan A. Rubenzahl, Xian-Yu Wang, Songhu Wang, Benjamin J. Fulton, Louise D. Nielsen, Jack Lubin, Steven Giacalone, Luke B. Handley, Erik A. Petigura, Emma V. Turtelboom, Alex S. Polanski, Steve R. Gibson, Kodi Rider, Arpita Roy, Ashley Baker, Jerry Edelstein, Christopher L. Smith, Josh Walawender, Joshua N. Winn
Figure caption: The sky-projected obliquity λ vs. planet radius (top), mass (middle), and semimajor axis over star radius (bottom). Systems that have obliquity measurement using more than one planet are shown as points of the same symbol with dark-blue edges. The three well-known misaligned systems—HD 3167,K2-290, and Kepler-56 (which exhibits planet–stellar core misalignment; D. Huber et al. 2013a; J. M. J. Ong 2025)—are represented by the connected gray diamonds, blue crosses, and green triangles, respectively. Our target, TOI-880 c, is the red dot with darker edges. It has a fitted sky-projected obliquity of ﹩| {\lambda }_{c}| =7.{4}_{-7.2}^{+6.8}﹩°, radius of 4.95 ± 0.20R⊕, a/R⋆ of ﹩16.4{8}_{-0.76}^{+0.67}﹩, and a predicted mass of ﹩21.{5}_{-9.2}^{+17.0}\,{M}_{\oplus }﹩ from J. Chen & D. Kipping (2017). For the middle panel, only planets with mass measurements are shown.
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: (a) The same data as in Figure 6 but with projected obliquity as a function of orbital period. Dashed lines connect planets within the same system. For planets with σλ > 30° the points are colored gray. The red shaded region indicates retrograde orbits. (b) Planet radius vs. orbital period for the same sample. Points are color-coded according to their obliquity ∣λ∣. The star denotes TOI-1759A b and black points are the sample of Kepler planets from the California–Kepler Survey (E. A. Petigura et al. 2017). (c) Similar to (a) but planets are color-coded according to their classification as compact or isolated. The definition of compact is taken from B. T. Radzom et al. (2024) and defined as having an adjacent planet within a period ratio of 4. (d) Distribution of isolated, misaligned planets after 100,000 iterations of sampling with replacement and a Gaussian fit given in black. The orange line indicates the one compact, misaligned planet in our sample showing that misaligned systems are more likely to be isolated to 3.1σ.
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: Injection and recovery results for 9 out of 12 single planets with a measured obliquity. The remaining three (K2-105, Kepler-63, and K2-33) have too few RV measurements to be included (<10). Colored lines show the 50th percentile of recoveries for each archival radial velocity data set. The black line shows the same contour but for TOI-1759. Gray points indicate RV-discovered giant planets (﹩{m}_{\,\rm{p}\,}\sin i\gt 0.5﹩ MJ) from the NASA Exoplanet Archive while the top panel shows the occurrence rate for giant planets (0.1–20 MJup) from R. B. Fernandes et al. (2019). Sources for archival data are as follows: GJ 436 (L. J. Rosenthal et al. 2021), GJ 3470 (X. Bonfils et al. 2012; M. R. Kosiarek et al. 2019), HAT-38 (A. Jordán et al. 2020), HD 89345 (V. Van Eylen et al. 2018; L. Yu et al. 2018), K2-25 (G. Stefansson et al. 2020), TOI-3884 (J. E. Libby-Roberts et al. 2023), WASP-166 (C. Hellier et al. 2019), WASP-156 (O. D. S. Demangeon et al. 2018; A. S. Polanski et al. 2024), and TOI-1759A (N. Espinoza et al. 2022; E. Martioli et al. 2022; A. S. Polanski et al. 2024).
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: Abacus plot for all systems containing an RP < 8 R⊕ planet with a measured obliquity. Stars are colored and sized according to the temperature and radius. Blue arrows indicate the obliquity of the inner-most planet with λ measured. Red arrows are for the second inner-most planet with λ measured. In the case of TRAPPIST-1, the additional green arrow indicates the obliquity for the outer-most planet with λ measured. We also note V1298 Tau b (RP = 10 R⊕) has an obliquity measurement consistent with that of V1298 Tau c (M. C. Johnson et al. 2022).
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: Left: projected obliquity ∣λ∣ as a function of host star effective temperature for planets with R ≤ 8 R⊕ from a query of the TEPCAT catalog (J. Southworth 2011). Triangles indicate planets with 4 < R ≤ 8 R⊕, while circles indicate planets with R ≤ 4 R⊕. Open points indicate members of multiplanet systems while closed points are systems of a single detected planet. For planets with σλ > 30° the points are colored gray. The red shaded region indicates retrograde orbits. Right: the same as left but for projected obliquity as a function of scaled orbital separation.
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: Left: posterior distribution corner plot for a fitting basis of ﹩\sqrt{v\sin i}\cos \lambda ﹩ and ﹩\sqrt{v\sin i}\sin \lambda ﹩. No prior has been imposed on ﹩v\sin (i)﹩ resulting in a long velocity tail, which widens the λ distribution. Right: same as left but for a basis that fits λ directly and ﹩v\sin (i)﹩ indirectly via ﹩{v}_{\mathrm{eq}}\sqrt{1-{\cos }^{2}{i}_{* }}﹩.
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: Radial velocity vs. the various measured activity indicators from MAROON-X. Pearson R values are given with the p-value in parentheses. We observe tentative correlations in the Na D lines; however, the correlation is dependent on a single observation indicated by the open markers across all panels. The Pearson R and p-value for these indicators omitting this point are given in brackets. This observation also corresponds to the highest discrepancy in RVs derived between the blue and red arms.
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption:  ﹩v\sin (i)﹩-λ space for the maximum likelihood values of an RM model fit to 100,000 simulated data sets absent of an RM effect. A Gaussian kernel density estimate is overlaid in blue to emphasize density of points. The posterior distribution for the real MAROON-X data set is shown as the blue contours representing the 1σ, 2σ, and 3σ confidence levels.
Paper: An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Toward Alignment for Small Planets
Authors: Alex S. Polanski, Ian J. M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper
Figure caption: Radial velocity time series from MAROON-X with the median Rossiter–McLaughlin and 1σ confidence shown as the black line and blue shaded region. Black points are the binned radial velocities. The inset shows the geometry of the system with the black arrow indicating the orbital angular momentum vector and the gray shaded area representing the uncertainty. The bottom panel shows the residuals with an rms of ∼1 m s−1.