adsabs/AstroCLIMB huggingface dataset:
Paper: Quantifying the Contamination from nearby Stellar Companions in Gaia DR3 Photometry
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Daniel Huber
Figure caption: Gaia contrast versus separation, with the colorbar showing the Gaia G magnitude error. The Gaia magnitude error may be correlated with binary separation and contrast, indicating that elevated G mag error may be a weak indicator of stellar multiplicity.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Dark-subtracted, flipped, stacked and unsharp-masked z-band images of HD 165054 through the MagAO-X camsci1 and camsci2 channels before rotation to place north-up. Overlaid circles indicate the background stars measured in M. M. Nguyen et al. (2020) that were visible above the background in these data, using the indexing in that work. The overlaid squares correspond to additional sources whose measured positions are being reported in this work for future use in calibration.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Unsharp-masked image of HD 165054 from our 2022 observations in which the background stars can be seen, rotated to place north-up and east-left. The predicted angular positions of the background stars from 2014 January to 2023 June are plotted using the updated astrometric solutions (Table 3). The prediction for the date of observation is indicated with the white circle. Note that most of the apparent motion is due to the motion of the foreground star.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Apparent motion of the seven background stars relative to HD 165054 when using the 50th percentile astrometric solution values from Table 3. Left: the paths predicted by the astrometric solution for each star’s motion relative to HD 165054 from 2014 January 1 to 2022 April 14. (HD 165054 is responsible for most of the apparent motion.) Measured historical points measured with GPI and NIRC2 from M. M. Nguyen et al. (2020) are overlaid as scatter plot points. Right: differences between predicted and measured angular coordinates from the historical data. The standard deviation of the magnitudes of the residual vectors is 1.55 mas, roughly one-quarter of a MagAO-X pixel. Detail plots of the individual stars’ tracks are included in Section 7.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Example of the 2D Gaussian plus background fit of a single star in a single frame from the 20-frame ﹩z^{\prime} /z^{\prime} ﹩ sequence. The left panel shows star #4 in the original numbering scheme, imaged with camsci1. The middle panel is the model in Equation (2), evaluated for the parameters chosen from the medians of the posterior distributions. The final panel shows the first panel minus the second panel, with no obvious pattern in the residuals.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Visualization of the uncertainties in point-source pixel coordinates from camsci1 frames used for the pixel-scale computation in 2022A. The error bars represent the range from the 16th to 84th percentiles of the marginal distributions of x and y for the fit. The coordinates shown are raw detector pixel coordinates, which means there is both jitter in the images and the effect of a small amount of sky rotation spreading out the distribution. These are both accounted for as described in Section 5. The box with a dotted border indicates the size of one pixel.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Distribution of angular position predictions for one star (#0) at the time of the 2022 MagAO-X observations, with marginal distributions of R.A. in the top panel and decl. in the right panel. The 16th, 50th, and 84th percentile values are overlaid as dashed lines. The solid black outline represents the 6 × 6 mas solid angle subtended by a single pixel in camsci1 and camsci2, as predicted from the MagAO-X optical design. (The actual pixel scale is calibrated and reported in Table 3).
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Corner plot of the posterior distributions for the background-star location fit shown in Figure 7. The 16th, 50th, and 84th percentile values for each parameter are overlaid on the 1D histograms on the diagonal as dashed lines.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Corner plot of the posterior distributions for the parameters reported in Table 4 for 2022. The 16th, 50th, and 84th percentile values for each parameter are overlaid on the 1D histograms on the diagonal as dashed lines. As expected, the corresponding parameter values are tightly correlated between the camsci1 and camsci2 channels.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Distribution of measured angles of the vectors connecting DM spikes using data from the 50/50 and Hα beamsplitter modes in 2022. The data set taken in the 50/50 beamsplitter served as the reference.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Visualization of the space of accepted solutions for the background-star astrometry from the MCMC analysis. Fifty random parameter vectors are drawn from the chain and used to predict the angular locations for each star as a function of time. The predictions from each solution are shown evaluated from 2014 January 1 to 2023 June 15. Error bars as reported in M. M. Nguyen et al. (2020) are overlaid in black. The distribution can be seen to get wider and less certain as we extrapolate forwards in time. The inset region provides a zoomed-in view around two historical measurements of star #1 to illustrate the scale of the error bars and width of the distribution of solutions.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Corner plot of the posterior distributions for the parameters reported in Table 4 for 2023. The 16th, 50th, and 84th percentile values for each parameter are overlaid on the 1D histograms on the diagonal as dashed lines.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Corner plot of the posterior distributions for the parameters reported in Table 4 for 2024. The 16th, 50th, and 84th percentile values for each parameter are overlaid on the 1D histograms on the diagonal as dashed lines.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Distribution of measured angles of the vectors connecting DM spikes using data from the 50/50 and Hα beamsplitter modes in 2024. The data set taken in the 50/50 beamsplitter served as the reference.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Distribution of measured angles of the vectors connecting DM spikes using data from the 50/50 and Hα beamsplitter modes in 2023. The data set taken in the Hα beamsplitter served as the reference.
Paper: An In-depth Investigation of the Primordial Cluster Pair ASCC 19 and ASCC 21
Authors: Qingshun Hu, Yuting Li, Mingfeng Qin, Chenglong Lv, Yang Pan, Yangping Luo, Shuo Ma
Figure caption: Distributions of the members of ASCC 19 and ASCC 21 with an RV-to-error ratio greater than or equal to 3 in multidimensional parameter spaces. Members with normal RVs, corresponding to those within the red boxes in Figure 3, are marked by red (ASCC 19) and blue (ASCC 21), respectively, with members with abnormal RVs that are those outside of the red boxes in Figure 3 being colored by green (ASCC 19) and yellow (ASCC 21). Top left panel: distribution of the member stars of both clusters in the 2D celestial coordinate system. Gray bars represent the errors of α and δ. Top right panel: parallax histograms for the member stars for both clusters. Bottom left panel: distribution of the member stars of both clusters in proper-motion space. Gray bars represent the errors of proper motion in both directions. Bottom right panel: CMD of the two clusters. Filled pentagrams represent the member stars with RVs exceeding 100 km s−1 in both clusters. All member data are sourced from M. G. J. van Groeningen et al. (2023).
Paper: An In-depth Investigation of the Primordial Cluster Pair ASCC 19 and ASCC 21
Authors: Qingshun Hu, Yuting Li, Mingfeng Qin, Chenglong Lv, Yang Pan, Yangping Luo, Shuo Ma
Figure caption: Radial density profiles of ASCC 19 (left) and ASCC 21 (right) in 3D spatial space. The stellar radial densities in each subplot are represented by black plus signs. The purple and blue curves correspond to the EFF and King models, respectively. The green and cyan solid lines denote the core radius estimated by the EFF model and the tidal radius obtained from the intersection of the two density profile fitting lines, respectively. The red dotted lines represent the tidal radii calculated using the von Hoerner formula in Section 5. The parameters presented in this figure are calculated via the member data sourced from M. G. J. van Groeningen et al. (2023).
Paper: An In-depth Investigation of the Primordial Cluster Pair ASCC 19 and ASCC 21
Authors: Qingshun Hu, Yuting Li, Mingfeng Qin, Chenglong Lv, Yang Pan, Yangping Luo, Shuo Ma
Figure caption: The 3D projection distribution of the cluster pair on X–Y (left), Y–Z (middle), and X–Z (right) planes. The red and blue crosses indicate the members of ASCC 19 and ASCC 21, respectively. The red and blue circles indicate the tidal radii, derived from the intersection points, as detailed in Figure 11. The parameters presented in this figure are calculated via the member data sourced from M. G. J. van Groeningen et al. (2023).
Paper: An In-depth Investigation of the Primordial Cluster Pair ASCC 19 and ASCC 21
Authors: Qingshun Hu, Yuting Li, Mingfeng Qin, Chenglong Lv, Yang Pan, Yangping Luo, Shuo Ma
Figure caption: Left panel: the distribution of the metallicity [Fe/H] of the members of ASCC 19, derived from Gaia DR3 (green), APOGEE-DR17 (blue), and GALAH-DR4 (yellow), and the distances (Δd) to clusters’ centers (3D centers). Right panel: the distribution of the [Fe/H] of the members of ASCC 21, again from Gaia DR3, APOGEE-DR17, and GALAH-DR4, and the distances (Δd) to clusters’ centers. The black dashed lines represent the 3D centers of the two clusters, with the red dashed lines indicating their tidal radii. The calculation of the tidal radii and the process of deriving distances are detailed in Section 4.4.
Paper: An In-depth Investigation of the Primordial Cluster Pair ASCC 19 and ASCC 21
Authors: Qingshun Hu, Yuting Li, Mingfeng Qin, Chenglong Lv, Yang Pan, Yangping Luo, Shuo Ma
Figure caption: 3D spatial structure of the cluster pair (ASCC 19 and ASCC 21), shown with ellipsoidal curves. The green ellipsoid, with its fitted center marked by a red filled pentagram, represents ASCC 19, while the purple ellipsoid, with its fitted center marked by a blue filled pentagram, represents ASCC 21. The small red and blue circles represent the member stars of ASCC 19 and ASCC 21, respectively. The black dashed line indicates the distance between the fitted centers of the two clusters, which is 24.49 pc. The differently colored bars represent the various axes of the ellipsoids, as shown in the legend. The parameters presented in this figure are calculated via the member data sourced from M. G. J. van Groeningen et al. (2023).
Paper: An In-depth Investigation of the Primordial Cluster Pair ASCC 19 and ASCC 21
Authors: Qingshun Hu, Yuting Li, Mingfeng Qin, Chenglong Lv, Yang Pan, Yangping Luo, Shuo Ma
Figure caption: Top panel: light curve of TIC 264682835. Bottom panel: phase diagram of TIC 264682835. The red curve represents the fitting curve to the phase. Its RV, period, and amplitude are labeled in the diagram. All data are sourced from TESS.
Paper: An In-depth Investigation of the Primordial Cluster Pair ASCC 19 and ASCC 21
Authors: Qingshun Hu, Yuting Li, Mingfeng Qin, Chenglong Lv, Yang Pan, Yangping Luo, Shuo Ma
Figure caption: The “mass segregation ratio” (ΛMSR) for ASCC 19 and ASCC 21. NMST denotes the ordinal number of the member stars sorted by G-band magnitude, from bright to faint. The parameters are calculated according to the member data sourced from M. G. J. van Groeningen et al. (2023).
Paper: An In-depth Investigation of the Primordial Cluster Pair ASCC 19 and ASCC 21
Authors: Qingshun Hu, Yuting Li, Mingfeng Qin, Chenglong Lv, Yang Pan, Yangping Luo, Shuo Ma
Figure caption: Top panel: light curve of TIC 50788524. Middle panel: light curve of TIC 427451326. Bottom panel: light curve of TIC 50587538. All data are sourced from TESS.
Paper: An In-depth Investigation of the Primordial Cluster Pair ASCC 19 and ASCC 21
Authors: Qingshun Hu, Yuting Li, Mingfeng Qin, Chenglong Lv, Yang Pan, Yangping Luo, Shuo Ma
Figure caption: Top panel: light curve of TIC 264739961. Bottom panel: phase diagram of TIC 264739961. All symbols are the same as those in Figure 8. All data are sourced from TESS.
Paper: Orbits of Six Triple Systems
Authors: Andrei Tokovinin
Figure caption: Orbits of HIP 64836 (YSC 149) in the plane of the sky (top) and the RV curve of the inner pair (bottom, the outer orbit is subtracted). In the orbit plot, asterisks, crosses, and triangles show the resolved outer, unresolved outer, and inner positions, respectively. The inner orbit is plotted by the small dashed ellipse. The outer orbit is plotted by the solid line (with wobble) and by the dashed line (with wobble removed). The insert shows the speckle ACF recorded in 2021.
Paper: Orbits of Six Triple Systems
Authors: Andrei Tokovinin
Figure caption: Inner and outer periods of known hierarchical systems within 100 pc (small crosses) and the six triple systems studied here (large asterisks). The line indicates the dynamical stability limit Pout/Pin > 4.7 (R. A. Mardling & S. J. Aarseth 2001). Some systems with crudely estimated periods are located below this line.
Paper: Orbits of Six Triple Systems
Authors: Andrei Tokovinin
Figure caption: Top: fragment of the outer orbit with wobble. Accurate measurements (Hipparcos, Gaia, and SOAR) are plotted as asterisks, less accurate data by crosses. The dashed line depicts the center-of-mass trajectory. Bottom: the RV curve of star A. Plus signs denote RVs potentially biased by blending; the center-of-mass RV is subtracted.
Paper: Orbits of Six Triple Systems
Authors: Andrei Tokovinin
Figure caption: Orbit of HIP 11783 Aa,Ab in the plane of the sky (top) and its RV curve (bottom). Squares plot the measurements, the curves depict the orbits. Crosses in the RV curve mark the less accurate RVs.
Paper: Orbits of Six Triple Systems
Authors: Andrei Tokovinin
Figure caption: Four CCFs of HIP 64836 derived from the CHIRON spectra. The dates are indicated. The color ticks mark the measured heliocentric RVs of Aa (red, on the right) and Ab (green).
Paper: Orbits of Six Triple Systems
Authors: Andrei Tokovinin
Figure caption: Orbits of the outer (top) and inner (bottom) pairs in 41 Ara.
Paper: Orbits of Six Triple Systems
Authors: Andrei Tokovinin
Figure caption: Orbits of HIP 89234. The insert shows the latest speckle ACF recorded in 2024.7 in negative rendering.
Paper: Interior Convection Regime, Host Star Luminosity, and Predicted Atmospheric CO2 Abundance in Terrestrial Exoplanets
Authors: Antonin Affholder, Stéphane Mazevet, Boris Sauterey, Dániel Apai, Régis Ferrière
Figure caption: Effect of relative luminosity, S/S⊕, on simulated steady-state atmospheres (pCO2, temperature). (A) Terrestrial exoplanets in the ML interior convection regime. (B) Terrestrial exoplanets in the SL regime. Vertical arrows represent simulations that reach the maximal value of atmospheric CO2 of our grid with a positive derivative of pCO2. Arrow size scales with the fraction of simulations in the binned interval that reach this CO2 limit. (C) and (D) Distributions of simulations across a discretized range of S/S⊕. In (A) and (B), simulation points are colored according to the planetary age used as a model parameter (planets with an age similar to Earth appear in yellow). Red circles indicate modern Earth and Mars. Nominal Earth trajectory (change in luminosity and pCO2 over time; J. Krissansen-Totton et al. 2018) is represented with the red line ending with modern values (red circle), and intersecting vertical lines are placed at 1, 2, and 3 Byr from formation. The dark blue, light blue, gold, and orange contour lines indicate temperatures of 248 K, 273 K, 298 K, and 340 K, respectively, predicted from the climate model run with fixed average values for pCH4 and pH2. Linear regression of ﹩{\mathrm{log}}_{10}p{{\rm{CO}}}_{2}﹩ vs. S/S⊕ infers a slope (in units of ﹩{\mathrm{log}}_{10}({\rm{b}}{\rm{a}}{\rm{r}})\,{S}_{\oplus }^{-1}﹩) of −5.37 ± 0.02 (standard deviation) with a correlation coefficient value r2 = 0.63 in (A) and −2.26 ± 0.04 with a correlation coefficient value r2 = 0.08 in (B). In (C) and (D), blue (left part of each distribution graph) and orange (right) distributions are compiled from simulations in the ML and SL regimes, respectively. Dotted–dashed lines indicate median values, and horizontal dark bars indicate simulations that have reached the CO2 modeling limit. In (D), the horizontal blue dashed line (lower straight line) corresponds to the temperature of 248 K, at which B. Charnay et al. (2013) report global glaciation including at the equatorial band. The vertical blue dashed line (to the left) corresponds to the OHZ of 1 bar atmosphere planets reported by R. K. Kopparapu et al. (2013). The horizontal orange dashed line (upper) corresponds to the 340 K temperature, at which R. K. Kopparapu et al. (2013) calculate that depletion of the water reservoir through hydrogen escape can occur on the timescale of Earth's age. The vertical orange dashed line (to the right) corresponds to the moist runaway inner HZ limit, and the solid orange line corresponds to the greenhouse runaway limit (R. K. Kopparapu et al. 2013).
Paper: Interior Convection Regime, Host Star Luminosity, and Predicted Atmospheric CO2 Abundance in Terrestrial Exoplanets
Authors: Antonin Affholder, Stéphane Mazevet, Boris Sauterey, Dániel Apai, Régis Ferrière
Figure caption: Key geophysical and geochemical processes of SL and ML convection regimes in the interior-ocean-atmosphere-coupled model. (A) Key geophysical processes. The dashed curves in the mantle represent isotherms highlighting convective plumes. (B) Key geochemical processes and their influence on global temperature. Brown and blue arrows indicate the contribution of continental and seafloor weathering, respectively, to the climate-stabilizing negative feedback. Triangle-headed arrows indicate positive effects (increase in quantity), whereas flat-headed arrows indicate negative effects (removal or decrease). Two-way arrows represent dissolution or chemical equilibrium. Brown arrows correspond to processes exclusive to the silicate–carbonate feedback. Dotted blue arrows correspond to processes exclusive to the basalt dissolution (seafloor weathering) feedback. (C) CO2 volcanic outgassing rate as a function of planetary age as proposed for the Earth that we use as the ML regime nominal model (dashed curve; KrissansenT18 indicates the model from J. Krissansen-Totton et al. 2018) and for 1 M⊕ SL planets (solid curve; Dorn18 indicates the model from C. Dorn et al. 2018)