adsabs/AstroCLIMB huggingface dataset:
Paper: Search for Extraterrestrial Intelligence with the ngVLA
Authors: C. Ng, L. Rizk, C. Mannion, E. F. Keane
Figure caption: Transmitter rate vs. EIRP for several SETI projects. The vertical lines indicate characteristic EIRP powers, while the dashed line represents the EIRP of the Arecibo planetary radar and the dotted–dashed line represents the total solar power incident on the Earth's surface, also known as the energy usage of a Kardashev Type I civilization (Kardashev 1964).
Paper: Search for Extraterrestrial Intelligence with the ngVLA
Authors: C. Ng, L. Rizk, C. Mannion, E. F. Keane
Figure caption: Observation time per individual target for all receivers on the VLA.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: The phase-folded light curves for these 26 eclipsing binaries.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: Color–magnitude diagram for the observation filed with variables. The red, blue, green, and orange symbols mark the eclipsing binaries, pulsators, rotating variables, and unclear variable stars, respectively.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: Left panels: comparisons of the photometry presented in this study with that of Clem & Landolt (2016) for field J234139 + 453900 in V magnitudes and (U − B)—(B − V) colors. Right panels: photometric errors against its corresponding U, B, V, R, and I magnitudes on the standard system from top to bottom.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: Light curves of pulsating stars Y31-Y42 and other type variables W1-W4.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: Same as Figure 3, but for pulsating stars of Y1-Y30.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: Comparison of PERIOD04 and Lomb–Scargle extracted pulsating variable star frequencies.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: The different phase-folded light curves for J9. left panel: the light curve of J9 with the period given by us. Right panel: the light curve with the period given by Chen et al. (2018) based on our observation data.
Paper: Searching for Variable Stars in the Open Cluster NGC 2355 and Its Surrounding Region
Authors: Hong Wang, Yu Zhang, Xiangyun Zeng, Qingshun Hu, Jinzhong Liu, Mingfeng Qin, Guoliang Lü
Figure caption: The light curves of this six long-period unclear variable stars, which are listed in Table 6.
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Boosting up the predicting accuracy for the disequilibrium state of the atmospheric chemical reaction networks with multivariate information. Each panel of the plot shows the predicting accuracy of variables for atmospheric networks associated with K zz = 0, 106, 108, and 1010 at a given mean temperature between 500 and 1900 K with uncertainty ±50 K. The three variables with the highest predictive power at each mean temperature compared to other individual variables (in gray) are colored red (for detailed information about topological variables used in this plot, see Table 1 and Section 2.2). T*, A*, and N* represent multidimensional variable sets composed of the three top predictors, the abundance of the four chemical species shown in this plot, and the six network topological measures represented in Figure 9, respectively. The three different multivariable sets demonstrated higher predicting accuracy than individual variables even in the cases where the highest predictors are not included.
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Predictive power of variables for the disequilibrium state of the atmospheric chemical reaction networks. Each panel of the plot shows the predicting accuracy of an individual variable for atmospheric networks associated with K zz = 0, 106, 108, and 1010 as a function of the mean temperature with uncertainty ±250 K (where gray lines show the data on all plots for ease of comparison). The variables include G (Gibbs free energy); the abundances of chemical species NH3, CH4, CO, and H2O; and the average topological properties (see Table 1 and Section 2.2).
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Predictive power of variables for the disequilibrium state of the atmospheric chemical reaction networks. Each panel of the plot shows the predicting accuracy of an individual variable for atmospheric networks associated with K zz = 0, 106, 108, and 1010 as a function of the mean temperature with uncertainty ±500 K (where gray lines show the data on all plots for ease of comparison). The variables include G (Gibbs free energy); the abundances of chemical species NH3, CH4, CO, and H2O; and the average topological properties (see Table 1 and Section 2.2).
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Boosting up the predicting accuracy for the disequilibrium state of the atmospheric chemical reaction networks with multivariate information. Each panel of the plot shows the predicting accuracy of variables for atmospheric networks associated with K zz = 0, 106, 108, and 1010 at a given mean temperature between 500 and 1900 K with uncertainty ±250 K. The three variables with the highest predictive power at each mean temperature compared to other individual variables (in gray) are colored red (for detailed information about topological variables used in this plot, see Table 1 and Section 2.2). T*, A*, and N* represent multidimensional variable sets composed of the three top predictors, the abundance of the four chemical species shown in this plot, and the six network topological measures represented in Figure 9, respectively. The three different multivariable sets demonstrated higher predicting accuracy than individual variables even in the cases where the highest predictors are not included.
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Distributions of molecular abundances, interpolated from a 10,000-point normal distribution of initial conditions centered on a temperature of 1200 K, at K zz values of 0, 106, 108, and 1010, and uncertainties in temperature of 50, 250, and 1000 K. The bimodal distributions seen in the +/−1000 K distributions are an artifact of inserting noise into the system.
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption:  T = 1200 K w/ perturbations w/ all C-bearing compounds removed. Distributions of network parameters when species containing carbon are removed from the network (dashed line) vs. complete networks (solid line), at 1200 K and 1 solar metallicity. Interestingly, while the absolute values of the parameters change, the overall shape of them remains the same, despite the significant reduction in the network.
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Distributions of network parameters when species containing carbon are removed from the network, at 1200 K and 1 solar metallicity. While the absolute values of the parameters changed compared to the complete networks, the distributions are still distinguishable from each other as a function of K  zz .
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Distributions of network and thermodynamic measurements, interpolated from a 10,000-point normal distribution of initial conditions centered on a temperature of 1200 K, at K zz  values of 0, 106, 108, and 1010, and uncertainties in temperature of 50, 250, and 1000 K. The bimodal distributions seen in the +/−1000 K distributions are an artifact of discarding members of the distribution that fell outside the bounds of the original model grid and thus could not be interpolated.
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Phi distributions over a range of uncertainties and K zz values, drawn from a 10,000-point normal distribution of initial conditions centered at 2000 K.
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: [P/Fe] vs. [Fe/H] ratios from this work (blue stars) as well as other studies (gray markers) are plotted. We include phosphorus abundance ratios from Caffau et al. (2011) as circles, from Jacobson et al. (2014) as squares, from Maas et al. (2017) as triangles, from Maas et al. (2019) as rotated triangles, from Caffau et al. (2019) as “x” symbols, and from Sneden et al. (2021) as “+” symbols. The solar abundance ratios are shown as black dashed lines, and the [Fe/H] representative error bar for this work is shown in the upper right of the plot. The chemical evolution model from Cescutti et al. (2012) is a red dashed line, and the model from Prantzos et al. (2018) is a purple solid line. Three Ritter et al. (2018) models with different numbers of stars undergoing C-O shell mergers are included as orange lines, with the 0% model as a dotted line, the 10% model as a dotted–dashed line, and the 50% model as a solid line.
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: [P/Fe] vs. [Fe/H] from multiple studies. Stars that are highly likely thin disk members (red points) and thick disk members (black points) are plotted (as defined in Section 4.1). Red and black lines are linear fits (lin. fits) to the thin disk population and thick disk population, respectively, dashed lines represent the 2σ confidence intervals, and the fainter lines represent 1,000 samples from the MCMC fit. Data from this work are represented as stars, data from Maas et al. (2017) are squares, and data from Maas et al. (2019) are circles.
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: Top panel: the galactocentric velocity V and the sum of the squares of the U and W velocity components are plotted for the observed stars. Dashed lines represent radii at 50 km s−1, 100 km s−1, and 150 km s−1. Bottom panel: [P/Fe] ratio compared to the [Fe/H] ratio. In both panels, the color bar represents the thin disk to thick disk probability ratio, with black stars being likely thick disk members and gold stars probable thin disk stars. The gray “x” in the bottom left corner is a representative [Fe/H] error bar. Stars in red boxes have halo-to-thick-disk probabilities above 50%.
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: Molar N/C ratios compared to P/C ratios. The orange star is the solar abundance from Lodders et al. (2009). All stars in the plot have C and N abundances adopted from the Hypatia Catalog (Hinkel et al. 2014). Stars with P abundances measured in this work are shown as circles, and a color bar denotes the [Fe/H]. Literature P abundances from Hypatia are plotted as open-faced purple squares. A representative error bar is also shown in the bottom left corner.
Paper: The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars 
Authors: Zachary G. Maas, Keith Hawkins, Natalie R. Hinkel, Phillip Cargile, Steven Janowiecki, Tyler Nelson
Figure caption: [P/X] vs. [Fe/H] ratios are plotted using P abundances from this work, and other abundances from Bensby et al. (2014; as black circles) and APOGEE DR16 (red squares).
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Illustration of the positioning of the CSU bars (black horizontal lines) on MOSFIRE to obtain simultaneous multiobject spectroscopy of the field of 2M0050–3322 as produced by MAGMA, the MOSFIRE Automatic GUI-based Mask Application. Our target (named as 2M0050–33) is placed in the center of the field. The positions of the comparison stars as shown in Table 1 are also marked. The round colored points show the expected positions of the target and calibration stars. The different colors indicate the weight given to each object for MAGMA to prioritize the desired objects in the field of view. As shown in the color bar, red is weight 100 and blue weight 0. The yellow squares show the position of the stars used for the alignment of the mask. The blue circle indicates the field of MOSFIRE. The vertical red lines delimit the area in which the slits are positioned for spectroscopy in any filter.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Corrected J-imaging, J-band, H-band, and CH4–H2O light curves of 2M0050–3322, and the peak-to-peak amplitudes of their fluctuations.(The data used to create this figure are available.)
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Median-combined, flux-calibrated J- and H-band MOSFIRE spectrum of 2M0050–3322, and its uncertainties in lighter colors. We mark in violet the wavelength range used to obtain the J-band spectroscopic light curve, in blue the H-band spectroscopic light curve, and in orange the CH4–H2O light curve.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Normalized noncorrected (left) and corrected (right) CH4–H2O-band light curves of 2M0050–3322. We indicate the peak-to-peak amplitudes of their fluctuations.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Normalized noncorrected (left) and corrected (right) J-band imaging light curves of 2M0050–3322. We indicate the peak-to-peak amplitudes of their fluctuations.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: 2M0050–3322 light curve is shown by the orange points, with the best-fit nonvariable (flat) model shown in orange and variable (sinusoidal) model shown in blue. The BIC test shows that the flat model is strongly favored by the light curve.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Normalized noncorrected (left) and corrected (right) H-band light curves of 2M0050–3322. We indicate the peak-to-peak amplitudes of their fluctuations.
Paper: Top-of-the-atmosphere and Vertical Cloud Structure of a Fast-rotating Late T Dwarf
Authors: Elena Manjavacas, Theodora Karalidi, Xianyu Tan, Johanna M. Vos, Ben W. P. Lew, Beth A. Biller, Natalia Oliveros-Gómez
Figure caption: Normalized noncorrected (left) and corrected (right) J-band light curves of 2M0050–3322. We indicate the peak-to-peak amplitudes of their fluctuations.
Paper: Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars
Authors: Henry A. Kobulnicky, William T. Chick
Figure caption: Histogram of ΔPA, the difference between the morphological position angle of the arcuate nebulae and the position angle of the central star’s projected peculiar velocities. The distribution is well approximated by the sum (solid curve) of a Gaussian component representing a highly aligned population (dashed curve) and a random (flat, nonaligned) component.
Paper: Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars
Authors: Henry A. Kobulnicky, William T. Chick
Figure caption: ΔPA vs. v 2D peculiar velocity. Colors distinguish the I, FB/H, and FH environment classes. The gray shaded region marks the regime of runaway stars (v 2D > 25 km s−1) that have nebular morphological position angles aligned with the central stars’ velocity vectors (∣ΔPA∣ < 45°).
Paper: Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars
Authors: Henry A. Kobulnicky, William T. Chick
Figure caption: Histogram of ΔPA, with systems color-coded by local environment class. Isolated systems peak strongly near zero, indicating alignment between morphological and kinematic vectors. FB/H and FH stars have a nearly flat distribution.
Paper: Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars
Authors: Henry A. Kobulnicky, William T. Chick
Figure caption: Three-dimensional peculiar velocity vs. two-dimensional peculiar velocity for multiple-star candidates (circles) and single-star candidates (triangles) from the SBN sample (red) and the GOSC comparison sample (blue). Only stars having multiple radial-velocity measurements and meeting the astrometric selection criteria are shown. A solid line marks the 1:1 correspondence, while a dashed line marks the ﹩\sqrt{3/2}﹩:1 relation expected for isotropic velocities in three dimensions.
Paper: Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars
Authors: Henry A. Kobulnicky, William T. Chick
Figure caption: Histogram of v 2D peculiar velocities for subsamples of SBN central stars: the multiple-star candidates (green), the single-star candidates (magenta), and the Group 3 sample (cyan). Curves denote Gaussian probability density estimates for each subsample of SBN stars and for the entire sample of 267 SBN central stars (black dashed curve) and the GOSC sample (black solid curve). The distributions of the SBN sample and the GOSC O-star sample are statistically different.
Paper: Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars
Authors: Henry A. Kobulnicky, William T. Chick
Figure caption: (upper panel) Galactic longitude vs. kinematic position angle for the SBN central star sample. (Lower panel) Distributions of SBN morphological position angles (red histogram) and central star kinematic position angles (dashed histogram). The two are consistent with having been drawn from the same parent population.
Paper: Kinematics of the Central Stars Powering Bowshock Nebulae and the Large Multiplicity Fraction of Runaway OB Stars
Authors: Henry A. Kobulnicky, William T. Chick
Figure caption: A histogram chi-squared probability distribution for velocities of 25 O stars from the Galactic O-Star Catalog and 72 central stars of bowshock nebulae.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The U  ϕ /I profiles. The red curve shows the U  ϕ /I for multiple scattering, using a simple double-scattering approximation, assuming an inclination angle of 60°. See text for discussions. The blue solid curve comes from the fiducial model, Model 1, with i = 60°. The blue dashed curve is similar to Model 1, but with ϕ  B  = − 90°. This changes the helicity of the assumed magnetic field configurations, but nothing else, resulting in U  ϕ  flipping its sign in the whole disk. This is a unique feature for polarization produced by magnetic alignments.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: Left two panels: the results for small spherical dust grains. The first left panel shows the polarization fraction for different scattered light direction (θ, ϕ). The second left panel shows the polarization orientation angle η. η = 0 means polarization along ﹩\hat{\theta }﹩. Right: the same, but for results for our fiducial case: a small oblate dust grain with an aspect ratio s = 1.5. The scattering inclination angle is i = 45°.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: Synthetic maps. The left two panels are U  ϕ /I and Q  ϕ /I for Model 1 with i = 60°. The right two panels are the same, but for Model 2 with i = 45°. Note that the color map is the same for all panels and uses symmetric logarithmic normalization while being linear between −0.1 and 0.1.
Paper: Probing Magnetic Fields in Protoplanetary Disk Atmospheres through Polarized Near-IR Light Scattered by Aligned Grains
Authors: Haifeng Yang, 海峰 杨, Zhi-Yun Li
Figure caption: The geometry of our setup in the grain frame. The dust grain is located at the origin. The incoming light is propagating along ﹩{\hat{n}}_{1}﹩, making an angle i with z-axis in xz plane, with ﹩{\hat{e}}_{1}﹩ and ﹩{\hat{e}}_{2}﹩ as the base vectors for polarization decomposition. The scattered light is propagating along ﹩{\hat{n}}_{2}﹩ with directional angles (θ, ϕ). The base vectors for polarization decomposition are ﹩\hat{\theta }﹩ and ﹩\hat{\phi }﹩. See text for more details.