adsabs/AstroCLIMB huggingface dataset:
Paper: KW-Sun: The Konus-Wind Solar Flare Database in Hard X-Ray and Soft Gamma-Ray Ranges
Authors: A. L. Lysenko, M. V. Ulanov, A. A. Kuznetsov, G. D. Fleishman, D. D. Frederiks, L. K. Kashapova, Z. Ya. Sokolova, D. S. Svinkin, A. E. Tsvetkova
Figure caption: Annual rate of solar flares registered by Konus-Wind in the triggered mode categorized by the GOES classes.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: The confirmed companions and detected companions found in this work, successively compared with previous companions whose relative mass uncertainty is less than 100%. The left panel shows the distribution over mass and semimajor axis, while the right panel shows the distribution over companion–host mass ratio and semimajor axis. The companions are selected from this work and from the exoplanet.eu catalog (denoted by the black squares and labeled “Literature”), if their relative mass uncertainties are less than 100%, their inclinations and eccentricities are estimated, their host-star masses are higher than 0.2  M ⋆, and their orbital periods are longer than 1000 days. The mass ratios for some previous companions are missing in the right panel plots because their host-star masses are not given.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: Combined fits to RV, Gaia–Hipparcos astrometry, and direct imaging data for all BD targets. The left panels show the RV fits, the second and third columns show the fits to the proper-motion and positional differences between Gaia and Hipparcos, respectively, and the right panels show the fit to the direct imaging data collected from the literature. For each target, the linear motion is subtracted from the proper motion and position to show planet-induced nonlinear motion. The RV data sets as well as the Gaia and Hipparcos astrometric data are encoded by the same colors as shown in the left-hand legends. The covariances of the Gaia and Hipparcos proper motions and positions are denoted by error ellipses. The straight line connects the data point to the best-fitting model, which represents where the companion is expected to be. The parameters at the maximum a posteriori (MAP) are shown on the right-hand side of the figure. For stars with multiple companions, only the astrometry fits for companions with periods longer than 1000 days are shown, because the contribution of the short-period companions to the astrometry is minor. The right panels show the orbits of all companions in a system, as well as the relative astrometry derived from imaging data.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: Combined fits to the RV and Gaia–Hipparcos data for all BD targets. The left panels show the RV fits, while the middle and right panels show the fits to the proper-motion and positional differences between Gaia and Hipparcos, respectively. For each target, the linear motion is subtracted from the proper motion and position to show planet-induced nonlinear motion. The RV data sets as well as the Gaia and Hipparcos astrometric data are encoded by the same colors as shown in the left-hand legends. The covariances of the Gaia and Hipparcos proper motions and positions are denoted by error ellipses. The straight line connects the data point to the best-fitting model, which represents where the companion is expected to be. The parameters at the MAP are shown on the right-hand side of the figure. For stars with multiple companions, only the astrometry fits for companions with periods longer than 1000 days are shown, because the contribution of short-period companions to the astrometry is minor.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: Corner plot for the distribution of the 161 companion hosts over various parameters. The diagonal panels show the histograms of the corresponding parameters. Each of the lower panels shows the distribution of the sample over a parameter pair. The red and light green points, respectively, represent the hosts of the known companions and the new companions identified in this work. From left to right on the top, the parameters are stellar mass (M), G magnitude, number of RV points (N rv), effective temperature (T eff), log(η  r ), log(η  μ ), and heliocentric distance (d). The nonlinear positional difference Δr is derived by subtracting the positional difference caused by proper motion from the total positional difference. The logarithmic scales are defined using base 10.