adsabs/AstroCLIMB huggingface dataset:
Paper: A Differentiable Binary Microlensing Model Using Adaptive Contour Integration Method
Authors: Haibin Ren, 海滨 任, Wei Zhu, 伟 祝
Figure caption: This figure shows the source star (green) and the caustic curve (blue) that correspond to the grid point in Figure 3 with the largest deviation in microlensing magnification between microlux and VBBinaryLensing. The key binary-lens parameters are ρ = 9.43 × 10−2, s = 2.04, and q = 1.81 × 10−4. The orange dots are the sampled points according to the strategy of microlux. The inset plot shows a zoom-in view around the intersection between the giant source and the tiny caustic. The cusp to the left is undersampled (i.e., a hidden cusp), which results in a relatively large deviation of 2.22 × 10−3 in the microlensing magnification. Such extreme cases are rarely encountered in realistic microlensing events.
Paper: A Differentiable Binary Microlensing Model Using Adaptive Contour Integration Method
Authors: Haibin Ren, 海滨 任, Wei Zhu, 伟 祝
Figure caption: The left panel shows the fractional difference in microlensing magnification between VBBinaryLensing and microlux, color coded by the number counts. The red and blue dashed horizontal lines indicate the precision tolerance used in this test and twice that tolerance, respectively. Of the ∼8 × 107 grid points shown here, 50 are above the red dashed line, the majority of which remain very close to the precision requirement. The maximum difference reaches 2.22 × 10−3, due to the hidden cusp (see Figure 4). All cases (19 in total) that failed to reach the precision requirement due to the same reason are marked in orange.
Paper: A Differentiable Binary Microlensing Model Using Adaptive Contour Integration Method
Authors: Haibin Ren, 海滨 任, Wei Zhu, 伟 祝
Figure caption: The left panel shows the total number of sample points used in the contour integration as the function of the microlensing magnification, color coded by the number counts. The right panel shows the histogram distribution of the sampling points.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Joint posterior distributions for 22 parameters used in the MCMC fitting for the 3D orbits of the outer planet HD 73344 d. The values and histogram distributions of all parameters are shown, along with 1σ uncertainties.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Same as Figure 9, but with an initial mutual inclination of 20° between HD 73344 b and c.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Same as Figure 9, but with an initial mutual inclination of 70° between HD 73344 b and c.
Paper: Discovery of a Jupiter Analog Misaligned to the Inner Planetary System in HD 73344
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Jerry W. Xuan, Michael Bottom, Benjamin J. Fulton, Howard Isaacson, Mason G. MacDougall, Nicholas Saunders
Figure caption: Joint posterior distributions for 16 parameters used in the RV-only fitting of a three-planet Keplerian orbital model for the HD 7334 system.
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: On the left, the blue light curve represents data synthesized by PHOEBE, while the orange curve illustrates the output generated by the model (more massive filling) when using the same input parameters. On the right, we present the distribution of the standard deviation for the residuals between the light curves predicted by our model and those synthetic curves created by PHOEBE.
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: The fitting results for five targets are depicted, with the blue dots indicating the original light curves. The red lines represent the light curves generated by the trained model (contact binary model), and the green “x” dots denote the light curves produced by PHOEBE.
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: The posterior parameter distributions for TIC 144522855 are presented.
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: Fitting results for TIC 144522855 are presented.
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: The fitting results for four targets are depicted, with the blue dots indicating the original light curves. The red lines represent the light curves generated by the trained model (less massive filling), and the green “x” dots denote the light curves produced by PHOEBE.
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: The fitting results for three targets are depicted, with the light blue dots indicating the original light curves. The red lines represent the light curves generated by the trained model (more massive filling), and the green lines denote the light curves produced by the trained model (less massive filling).
Paper: Detection of Semidetached Eclipsing Binaries from TESS
Authors: Xu Ding, KaiFan Ji, QiYuan Cheng, ZhiMing Song, JinLiang Wang, XueFen Tian, ChuanJun Wang
Figure caption: The fitting results for three targets are depicted, with the blue dots indicating the original light curves. The red lines represent the light curves generated by the trained model (more massive filling), and the green “x” dots denote the light curves produced by PHOEBE.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: The vertical distances as a function of radial distances for the clusters. The left panel displays their current positions, while the right panel shows their original positions calculated through orbital integration. Blue and red circles represent the clusters younger and older than 1 Gyr, respectively. For each age bin, the scatters in the radial and vertical directions are respectively displayed in the lower right corner of each panel.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: The migration distances (RGC − Rb,GC) as a function of age for the OCs.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: [El/H] as a function of the magnitude of the vertical distance (﹩\left|Z\right|﹩) from the Galactic plane for the clusters at their original and current positions. The symbols are the same as in Figure 10.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: The radial and vertical gradients of average [α/Fe] for the OCs at their original and current positions. The symbols are the same as in Figure 10.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: The vertical [El/H] gradients for the OCs at their original and current positions. The symbols are the same as in Figure 4.
Paper: Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Authors: Guochao Yang, Jingkun Zhao, Yong Yang, Nian Liu, Yangping Luo, Gang Zhao
Figure caption: The radial [El/H] gradients for the OCs at their original and current positions. The symbols are the same as in Figure 10.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: The optical properties of the soot haze. From left to right, the panels show the optical depth per bar, the single-scattering albedo (ϖ0), and asymmetry parameter (g0). The wavelengths that correspond to the starlight and thermal double-gray channels are also marked in white. Importantly, the optical depth per bar shows how the soot haze can be a major contribution to layer optical depths in the upper atmosphere, especially at the shorter starlight wavelengths. For thermal wavelengths, the asymmetry parameter varies from close to zero at low pressures near the top of the atmosphere (below approximately 0.1 mbar), increasing to approximately 0.5 by a pressure of 100 mbar.
Paper: Clouds and Hazes in GJ 1214 b’s Metal-rich Atmosphere
Authors: Isaac Malsky, Emily Rauscher, Kevin Stevenson, Arjun B. Savel, Maria E. Steinrueck, Peter Gao, Eliza M.-R. Kempton, Michael T. Roman, Jacob L. Bean, Michael Zhang, Vivien Parmentier, Anjali A. A. Piette, Tiffany Kataria
Figure caption: Pressure–temperature profiles of a clear model of GJ 1214 b with no clouds or hazes and solar metallicity. Equatorial profiles are represented by colored lines, where the longitude is denoted by the color (zero corresponds to the substellar point). Pressure–temperature profiles for all nonequatorial profiles are represented by gray lines. Without aerosols, GJ 1214 b has equatorial day–night temperature differences of less than 50 K.
Paper: The Infrared-bright SW Knots in the Complex Ejecta of VY CMa
Authors: Roberta M. Humphreys, Terry J. Jones, Kris Davidson, A. M. S. Richards, R. Ravi, A. P. Singh, L. M. Ziurys
Figure caption: Left: the 2.2 μm K-band image of VY CMa from P. Cruzalebes et al. (1998) obtained in 1994. Right: the HST F656N image observed in 1999 with the separate knots and arcs identified (R. M. Humphreys et al. 2021). The + marks the position of the star.
Paper: The Infrared-bright SW Knots in the Complex Ejecta of VY CMa
Authors: Roberta M. Humphreys, Terry J. Jones, Kris Davidson, A. M. S. Richards, R. Ravi, A. P. Singh, L. M. Ziurys
Figure caption: Top: the HST F1042 image (left) from 1999 with the visual knots identified, see Figure 1, and the Ks image (right) from D. P. Shenoy et al. (2013) with the knots marked. Bottom: the 9–12 μm LBTI/NOMIC images from M. S. Gordon et al. (2019).
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: The orbit of (1911) Schubart numerically propagated and projected onto the Cartesian-like eccentricity–perihelion plane of ﹩e\,\exp (\imath \,\varpi )﹩ (left panel) and inclination-node plane of ﹩\sin I\,\exp \left(\imath \,{\rm{\Omega }}\right)﹩ (right panel). The simulation spanned 5 kyr in the first case and 30 kyr in the second case and the output is shown by the black line (the initial epoch J2000.0 of the propagation is shown by red dot). These results confirm decomposition onto the forced part (shown by the start symbol) and the proper term (highlighted by the gray circle) from Equations (B12) and (B13). The proper eccentricity parameter ep and inclination parameter ﹩\sin {I}_{{\rm{p}}}﹩ are the respective radii of the gray circle and shown by blue vector. The arrow with the Pp label indicates the sense of time evolution driven mainly by proper precession frequency, g and s, respectively. For (1911) Schubart, they read Pp = 3059.8 yr for eccentricity and Pp = 20879.5 yr for inclination.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Cumulative absolute magnitude distribution of the background and the collisional families in the Hilda population. Black symbols denote the background population, and the principal families are color-coded as follows: Hilda (blue), Schubart (red), Potomac (pink), Francette (green), and Guinevere (cyan). The dispersed nature of the Hilda family may be the reason for paucity of its members beyond H ≃ 15. The slanted lines are power-law approximations N(<H) ∝ 10γH, with the following exponents: background γ = 0.34, Hilda γ = 0.47, Schubart γ = 0.6, Potomac γ = 0.6, Francette γ = 0.95, and Guinevere γ = 0.9. At small sizes, population in families becomes comparable (or even larger) to the background.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Members of the Schubart family projected onto the plane defined by the proper eccentricity (abscissa) and absolute magnitude (ordinate); the star is (1911) Schubart itself. The dashed line highlights higher detection efficiency at larger eccentricities (also discussed in Figures 4 and 5). The gray arrows indicate suspected past flow of small Schubart members toward smaller/larger ep values by synergy of the Yarkovsky and YORP effects (see the Appendix of M. Brož & D. Vokrouhlický 2008).
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Synthetic proper elements for all Hildas shown in 2D projections: (ap, Ip) (left panel), and (ep, Ip) (right panel; width and grayscale of the symbol are roughly proportional to the absolute magnitude; see the bar). The largest members of the collisional families are indicated by circles, color-coded, and identified by the label. The horizontal dashed line at 10∘ proper inclination is the auxiliary boundary used to separate the dispersed Hilda and Potomac families.
Paper: Orbital and Absolute Magnitude Distribution of Hilda Population
Authors: David Vokrouhlický, David Nesvorný, Miroslav Brož, William F. Bottke, Rogerio Deienno, Carson D. Fuls, Frank C. Shelly
Figure caption: Synthetic proper elements of members in Hilda-population collisional families identified by the label at the top of the respective panel.
Paper: I-band Asymptotic Giant Branch (IAGB) Stars. II. A First Estimate of Their Precision and a Differential Zero Point 
Authors: Wendy L. Freedman, Barry F. Madore, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: DDO galaxies: I-band AGB color–magnitude diagrams (left half of each panel) and I-band (F814W) luminosity functions (right half of each panel). Horizontal black lines in the left panel mark the mode of the luminosity function (center line), flanked by lines at  ±1σ in the Gaussian fit to the smoothed luminosity function. A shorter, yellow-on-black line marks the measured level of the TRGB. Thick (smooth) black lines in the right panels are symmetric Gaussian fits to the peak and wings of the smoothed/main luminosity function, also shown in black. Blue and red luminosity functions correspond to color cuts that are shown in the CMD (left panel) on either side of the adopted color cut (blue vertical line). Blue luminosity functions use the bluer color cut (larger numbers) and the red luminosity functions use the redder color cut (smaller numbers). See the main text for additional details.
Paper: I-band Asymptotic Giant Branch (IAGB) Stars. II. A First Estimate of Their Precision and a Differential Zero Point 
Authors: Wendy L. Freedman, Barry F. Madore, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: A differential comparison of the TRGB and IAGB distance scales. The apparent magnitude of the TRGB discontinuity is plotted on the horizontal axis. The apparent magnitude of the mode of the IAGB luminosity function is plotted on the vertical axis. The red dashed line has a slope of unity and has been fit to minimize the scatter of the data points around it. This minimization occurs at a value of −0.589 ± 0.003 mag (sigma on the mean) in the sense that the IAGB stars are brighter than the level of the TRGB. The measured inter-method scatter is  ±0.119 mag. The solid red lines are  ±  two sigma bounds. The residuals are plotted as a function of the IAGB apparent I-band magnitude in the lower panel. The marginalized histogram of residuals is shown in the small inset found in the upper left corner of the main plot.
Paper: I-band Asymptotic Giant Branch (IAGB) Stars. II. A First Estimate of Their Precision and a Differential Zero Point 
Authors: Wendy L. Freedman, Barry F. Madore, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: Differences between the TRGB and IAGB true distance moduli as a function of the width of the IAGB luminosity function (expressed as a sigma). Broken lines are the 1σ uncertainties on the statistically flat slope. The lack of a correlation with sigma suggests that star formation history over the age interval sampled by the IAGB stars is not perceptibly imprinted on the mode of the IAGB luminosity function.
Paper: I-band Asymptotic Giant Branch (IAGB) Stars. II. A First Estimate of Their Precision and a Differential Zero Point 
Authors: Wendy L. Freedman, Barry F. Madore, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: Uppsala General Catalog (UGC) galaxies. See Figure 3 for description.
Paper: I-band Asymptotic Giant Branch (IAGB) Stars. II. A First Estimate of Their Precision and a Differential Zero Point 
Authors: Wendy L. Freedman, Barry F. Madore, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: Index Catalogue (IC)galaxies (cont.) See Figure 3 for description.
Paper: I-band Asymptotic Giant Branch (IAGB) Stars. II. A First Estimate of Their Precision and a Differential Zero Point 
Authors: Wendy L. Freedman, Barry F. Madore, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: UGC galaxies (cont.) See Figure 3 for description.
Paper: I-band Asymptotic Giant Branch (IAGB) Stars. II. A First Estimate of Their Precision and a Differential Zero Point 
Authors: Wendy L. Freedman, Barry F. Madore, Taylor Hoyt, In Sung Jang, Abigail J. Lee, Kayla A. Owens
Figure caption: UGCA galaxies. See Figure 3 for description.
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: We include a variety of plots summarizing our training and analysis of Kepler-21. Top left: Kepler and TESS training data, as well as our best-fit GP model overlaid. Top right: RV time series and training posteriors. Bottom: results of our injection-recovery analysis in the two cases described in Section 4. The left plots show the preference for models including the injected planet when no GP training is applied. The middle two plots show the improvements gained when training on Kepler or TESS. The rightmost plots highlight the differences between Kepler and TESS training. A dashed black line indicates the orbital period and amplitude of the system's known planet(s).
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: We include a variety of plots summarizing our training and analysis of HD 173701. Top left: Kepler and TESS training data, as well as our best-fit GP model overlaid. Top right: RV time series and training posteriors. Bottom: results of our injection-recovery analysis in the two cases described in Section 4. The left plots show the preference for models including the injected planet when no GP training is applied. The middle two plots show the improvements gained when training on Kepler or TESS. The rightmost plots highlight the differences between Kepler and TESS training.
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: We include a variety of plots summarizing our training and analysis of HD 4256. Top left: K2 and TESS training data, as well as our best-fit GP model overlaid. Top right: RV time series and training posteriors. Bottom: results of our injection-recovery analysis in the two cases described in Section 4. The left plots show the preference for models including the injected planet when no GP training is applied. The middle two plots show the improvements gained when training on K2 or TESS. The rightmost plots highlight the differences between Kepler and TESS training.
Paper: Jitter Across 15 yr: Leveraging Precise Photometry from Kepler and TESS to Extract Exoplanets from Radial Velocity Time Series
Authors: Corey Beard, Paul Robertson, Jack Lubin, Te Han, Rae Holcomb, Pranav Premnath, R. Paul Butler, Paul A. Dalba, Brad Holden, Cullen H. Blake, Scott A. Diddams, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Dan Li, Andrea S.J. Lin, Sarah E. Logsdon, Emily Lubar, Suvrath Mahadevan, Michael W. McElwain, Joe P. Ninan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Gudmundur Stefansson, Ryan C. Terrien, Jason T. Wright
Figure caption: We show the increased or decreased performance of our activity models when trained on simultaneous data instead of nonsimultaneous data. The y-axis indicates ΔBF between models trained on simultaneous vs. nonsimultaneous photometry. Positive values indicate that the simultaneous photometry is improving sensitivity to injected planets, while negative values indicate worse performance. Red bars correspond to our “transiting” planet runs, and the blue bars correspond to “RV-detected” injected planets. There is not consistent improvement gained from simultaneous photometric training. We note that for HD 24040, the negative preference goes far below our axes limits, which we set for a clearer analysis of the other systems. As mentioned in the text, we believe these fits may not be reliable.