adsabs/AstroCLIMB huggingface dataset:
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 difference between the spherical and fiducial cases. Left: the difference in polarization fraction. Middle: the difference in polarization orientation. Note that Δη = ±90° denote the same polarization state. Right: histogram of angle difference Δη. The angle difference between the dipole  P  1 and ﹩{\hat{e}}_{1}﹩, i.e., Δη  y  = 4.7°, is also plotted as a vertical dashed line.
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: Timescale comparisons for grain alignment.
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: the two metrics of the angle difference as a function of the different dust aspect ratio s. Right: the two metrics for the angle difference as a function of the incoming light inclination angle i for a fixed grain aspect ratio of s = 1.5. See the text for the definitions of the two metrics.
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: Results for an extremely flattened oblate grain with s = 100. The left two panels are the same as Figure A2. The right panel is the same as the right panel of Figure A3.
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 mass, number density, and extinction opacity as a function of different grain sizes at the τ = 1 surface of R = 30 au.
Paper: Inhomogeneity within Local Interstellar Clouds 
Authors: Jeffrey L. Linsky, Seth Redfield, Diana Ryder, Adina Chasan-Taber
Figure caption: Plot of the filling fraction of neutral hydrogen clouds along sight lines to stars vs. stellar distance. On the right side is the scale of neutral hydrogen density if the sight lines are completely filled with clouds. The left colored box identifies sight lines that would be filled by clouds with a mean density n(H I) ≈ 0.10 cm−3. The right colored box identifies sight lines with distant clouds that are widely separated. The four stars within 4 pc of the Sun with only LIC and astrospheric absorption are identified in the figure and are discussed in the text.
Paper: Inhomogeneity within Local Interstellar Clouds 
Authors: Jeffrey L. Linsky, Seth Redfield, Diana Ryder, Adina Chasan-Taber
Figure caption: Plots of the mean density assuming filling factor of unity vs. temperature (left) and the sum of thermal and turbulent pressure (right). The solid lines are least-squares linear fits to the data.
Paper: Inhomogeneity within Local Interstellar Clouds 
Authors: Jeffrey L. Linsky, Seth Redfield, Diana Ryder, Adina Chasan-Taber
Figure caption: Plots of turbulent velocities for the full data set (left) and the LIC-only data set (right) vs. the log of the neutral hydrogen column density. The solid lines are least-squares linear fits to the data.
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: Image configurations for SIS+XS lens systems with the source at various positions in one quadrant of the diamond caustic. The cyan Wynne circles and Wynne ellipses are centered at the source position. The lower left shows the limiting case of shear γ → 0, while the upper right shows γ = 1/3 and has been rotated 180°. The γ → 0 diamond caustic is scronched parallel to the elongation of the potential to produce the γ = 1/3 diamond caustic. The γ = 1/3 Wynne ellipses are scronched perpendicular to the elongation of the potential and the diamond caustic. Apart from the 180° rotation, the causticities ζ and astroidal angles α are the same for both sets of configurations.
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: The two plots compare the FSQ (orange) and the surface corresponding to the configuration invariant (blue). Panel (a) shows the FSQ and the surface of configuration invariant superimposed on each other, restricted to θ 23 > 0. Panel (b) shows the difference between the FSQ and the configuration invariant. Blue denotes the zero plane, and orange denotes the difference function. Note the different scales on the vertical axes. The planar axes are the same for both panels, while the vertical axes are θ 23 and Δθ 23, respectively.
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: The red filled circles are quadruple configurations of lensed quasars arising from different source positions within a diamond caustic—the blue astroid for which ζ = 1. Two of the pale blue circles are centered at ζ = 0.95, with ﹩{\phi }_{s}=\tfrac{\pi }{2}﹩ and ﹩-\tfrac{\pi }{4}﹩, respectively. The leftmost configuration has (ζ, ϕ  s ) = (0.75, π). The dashed curves are astroids of constant causticity, with ζ = 0.75 (red), ζ = 0.5 (orange), and ζ = 0.25 (green).
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: For consistency with the notation of Woldesenbet & Williams (2012), we label the images as shown in this figure. Images 2 and 3 are the closest pair of images. The quadrant in which they lie depends on the angular position of the source relative to the lens, ϕ  s . For the configuration shown, ϕ  s  lies in the fourth quadrant.
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: The “scronched” Wynne ellipse for an SIS+XS lens in blue and its auxiliary circle in green. The blue filled circle is an image formed by the SIS+XS at angle θ; the green filled circle shows its projection onto the auxiliary circle at η, the “eccentric angle.”
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: The plots show the construction of several asymptotically circular image configurations. Panel (b) shows a “kite” configuration, symmetric around one of the two diagonals connecting the images. The system in panel (c) can be thought of as a “super-kite,” symmetric around both diagonals. The system in panel (a) is symmetric about neither diagonal and hence an “un-kite.”
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: The blue filled circles are the centers of the Witt’s hyperbolae (red), which are drawn tangent to the Wynne’s circle (black). A configuration (green stars) is constructed for an arbitrary position of center of Witt’s hyperbola (yellow) to illustrate how configurations are generated from points inside the Witt–Wynne diamond.
Paper: The Quadruple Image Configurations of Asymptotically Circular Gravitational Lenses
Authors: Chirag Falor, Paul L. Schechter
Figure caption: Contours of angle difference between the closest two images over a quadrant of astroid caustic.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: Recovered distribution of periods of the stars in the sample as a function of Gaia color, extinction-corrected, color-coded by their age, annotated with the features of the parameter space. Sources redder than the labeled “Kraft break” have the dominant mode of variability being caused by rotation. They can be separated into slow rotators (sources that show a clear evolution of their periods with age), and fast rotators, having typical periods <1 day. Sources bluer than the Kraft break are commonly pulsators. γ Dor sources have pulsation frequency comparable to the stellar rotation period, consisting only of the main-sequence stars. δ Scuti stars in the age-limited sample form a bimodal distribution, with the main-sequence δ Scuti variables having periods shorter than 1.2 hr, and the subgiants having periods longer than 2 hr. Slowly pulsating B-type variables (SPB) are found among the early-type stars.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: Same as Figure 6, but as a function of temperature instead of color, zooming on the stars with convective envelopes and splitting sources in different age bins into different panels. T eff is obtained from TESS Input Catalog. The 2D histogram shows the distribution of periods in this work, color-coded by the number of sources in each bin. Blue dots are from the literature: Upper Sco (Rebull et al. 2018), Pleiades (Rebull et al. 2016a), NGC 3532 (Fritzewski et al. 2021), Praesepe (Douglas et al. 2019), and NGC 6811 (Curtis et al. 2019a). The black line is drawn at the period of 7 days, corresponding to half an orbital period from TESS. Note that the overdensity at that period that is apparent at older ages is artificial, most likely dominated by real rotators with a longer period aliased to the harmonic period close to the half an orbit of TESS. Additionally, the sample in TESS may be more incomplete than the samples from the literature due to the magnitude limits.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: Top left: an HR diagram for the stars with ages between 8 and 8.3 dex; sources are color-coded by the recovered rotation period. Top right: a kernel density estimate showing the period distribution in the same age and color range for the sources located on the main sequence vs. those found on the binary sequence. Fast rotators with periods shorter than 2 days are preferentially found on the binary sequence. Bottom left: fraction of fast rotators (sources with extinction-corrected colors 0.8 < (G BP,0 − G RP,0) < 2.2, with period <1 day), relative to all of the stars (periodic or not) in the same color range. Bottom right: contour plot showing periods and temperatures of fast rotators as a function of age. As the population ages, fast rotator sequence tends to shift toward longer periods and cooler temperatures.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: Fraction of sources as a function of Gaia color and age in which a confident periodic signal (up to 12 days) is observed in TESS data. The dashed line shows the sample solely among the strings of stars, defined in Kounkel & Covey (2019). Note that in almost all of the cases, the stellar strings have members with a similar fraction of the periodic variables as the full sample, and it is usually somewhat higher.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: A fit of the angular momentum L. Yellow dots show the data within each age bin; small dots are for sources with period measured in this work, larger dots are from the literature: Upper Sco (Rebull et al. 2018), Pleiades (Rebull et al. 2016a), NGC 3532 (Fritzewski et al. 2021), Praesepe (Douglas et al. 2019), and NGC 6811 (Curtis et al. 2019a). The red line shows the median L estimated within each age/T eff bin. The thick blue line shows the fit of L for that age. Thinner blue lines are offset by ±0.3 dex in age, and dotted lines are offset by ±0.6 dex in age. σ  L  shows the typical scatter in L relative to the fit in a given age bin. The range in L corresponds to the valid domain for the fit.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: Angular momentum of the full sample for “slow-sequence” stars with rotation periods longer than 2 days. Larger points are from the literature for clusters observed by Kepler. Note the significant change in L as a function of age for the M dwarfs, despite the lack of a significant change in the rotation period (Figure 6).
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: Distributions of the light-curve standard deviations (σ var), standard deviation normalized by the point-to-point rms (σ var/σ p2p), and standard deviation normalized by the reported mean flux uncertainty (σ var/σ inst). Sources for which periodicity was recovered in all sectors are shown in black, and sources that appear to be aperiodic in all sectors are in yellow. Sources that were detected as periodic in some but not all sectors are shown in blue and red, with blue corresponding to the specific sectors in which the source is recovered as periodic, and red corresponding to the sectors where the same sources are not recovered as periodic.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: Top left: comparison of periods presented in this work for the same sources observed in multiple sectors. Top right: comparison of periods in this work relative to periods in the ASAS-SN survey (Jayasinghe et al. 2019). Note the difference in beat frequency of 0.02 day in TESS and 1 day in ASAS-SN. Bottom left: comparison of periods to McQuillan et al. (2014) sample for the Kepler field. Dashed lines correspond to 2× and 0.5× harmonics. Bottom right: comparison of periods to Gaia DR3 periods (Eyer et al. 2022) from the Short Timescale Variability and Rotational Modulation catalogs.
Paper: Untangling the Galaxy. IV. Empirical Constraints on Angular Momentum Evolution and Gyrochronology for Young Stars in the Field
Authors: Marina Kounkel, Keivan G. Stassun, Luke G. Bouma, Kevin Covey, Lynne A. Hillenbrand, Jason Lee Curtis
Figure caption: Top: a comparison of residuals between the age derived from angular momentum vs. original ages derived from isochrone fitting. Bottom: same as above, but with the uncertainty in the isochrone age subtracted in quadrature from the difference. Different lines show the typical scatter at different ages: it is most pronounced at the younger age bins. Sources older than 8.5 dex are from Kepler, younger sources are from TESS.
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: The total velocity dispersion and the velocity dispersion of the individual components (σ  U , σ  V , and σ  W ) as a function of [Fe/H]. We have used a running average with a bin size of 1000 and a step size of 200. The error bar on the velocity dispersion are computed following Binney et al. (2000). On the right hand y-axis are the corresponding ages computed using Equation (4). The same axis and error bar as well as binning scheme is followed for all subsequent figures.
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: The total velocity dispersion and the velocity dispersion of the individual components (σ  U , σ  V , and σ  W ) as a function of [C/Fe].
Paper: Carbon Abundance of Stars in the LAMOST-Kepler Field
Authors: Athira Unni, Mayank Narang, Thirupathi Sivarani, Manoj Puravankara, Ravinder K Banyal, Arun Surya, S. P. Rajaguru, C. Swastik
Figure caption: The total velocity dispersion and the velocity dispersion of the individual components (σ  U , σ  V , and σ  W ) as a function of [C/H].
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: The UVIT-PHAT results (x-axes) for log(age) (top panel) and log(M) (bottom panel) compared to the results from Johnson et al. (2016) (y-axes) for the 99 clusters in both samples. Errors are ±1σ for both cases.
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: Distributions of age for the 134 clusters in the UVIT-PHAT sample (this work), with a cluster model lower log(age) limit of 6.6, and the Johnson et al. (2016) sample, with cluster model log(age) limits of 7.0 and 8.5.
Paper: AstroSat/UVIT Cluster Photometry in the Northern Disk of M31
Authors: Denis Leahy, Megan Buick, Cameron Leahy
Figure caption: Panels (a), (b), (c), and (d): values of log(Z/Z ⊙), log(Age/yr), log(M/M ⊙), and E(B–V), respectively, for each cluster (blue dots with error bars) and average values per bin (red dots with the dashed line).
Paper: Evidence of Long-term Period Variations in the Exoplanet Transit Database (ETD)
Authors: Simone R. Hagey, Billy Edwards, Aaron C. Boley
Figure caption: Timing residuals of WASP-12 b (top) and WASP-4 b (bottom) with future projections of the three transit-timing models shown with 150 random draws from the MCMC posterior chains. Note that for esthetic reasons, the scaling of the y-axis varies for each plot. Each datum is the difference between an observed time and the time predicted by the best-fit constant-period model. The size of the data points correspond to the data quality index from 1 to 3, with the higher-quality transits being larger. The red crosses represent observations removed during the sigma-clipping process.
Paper: Evidence of Long-term Period Variations in the Exoplanet Transit Database (ETD)
Authors: Simone R. Hagey, Billy Edwards, Aaron C. Boley
Figure caption: Similar to Figure 1, but for WASP-10 b (top) and HAT-P-19 b (bottom).
Paper: A CHEOPS Search for Massive, Long-period Companions to the Warm Jupiter K2-139 b
Authors: Alexis M. S. Smith, Szilárd Csizmadia
Figure caption: Maximum allowed mass of a perturbing outer body as a function of its orbital period, for different orbital eccentricities of the perturber (solid colored lines). The approximate masses delimiting massive planets from brown dwarfs and brown dwarfs from low-mass stars are indicated with dashed black lines, and the region of parameter space excluded by our TTV observations is shaded.
Paper: A CHEOPS Search for Massive, Long-period Companions to the Warm Jupiter K2-139 b
Authors: Alexis M. S. Smith, Szilárd Csizmadia
Figure caption: Transit times of K2-139 b. The differences between the observed transit times and our newly-derived ephemeris (O − C) are plotted against the midtransit time (see Table 5).
Paper: Supporting Evidence for a Galactic Lyα Background from Cassini UVIS Data
Authors: Wayne R. Pryor, G. Randall Gladstone, Kurt D. Retherford, W. Kent Tobiska
Figure caption: The Cassini spacecraft’s trajectory to Saturn placed it downwind of the Sun with respect to the interstellar hydrogen flow in late 2000 during the Jupiter flyby. The view is looking from ecliptic north down onto the ecliptic plane. The interstellar wind flow direction is indicated by the black arrow. The Cassini spacecraft was downwind of the Sun and moving sidewind in 2003−2004. Source: adapted from Wikimedia Commons to include the flow axis and the approximate Cassini locations at the start of the years 2003, 2004, and 2005.
Paper: Supporting Evidence for a Galactic Lyα Background from Cassini UVIS Data
Authors: Wayne R. Pryor, G. Randall Gladstone, Kurt D. Retherford, W. Kent Tobiska
Figure caption: Top panel: Cassini UVIS occultation slit Lyα upwind brightness data from 2003.7 to 2004.9. The data are represented by black dots. Each dot is an average of seventy 25 s measurements. Cassini–Earth opposition, when both view the same solar longitude, is indicated. A heliospheric Lyα model scaled upward by a factor of 1.18 is shown in red dots. The same model scaled by a factor of 1.01 and added to an isotropic 43 R galactic signal is shown in yellow. A ±5σ statistical error bar is shown on one data point near the right. Bottom panel: Cassini UVIS occultation slit Lyα downwind brightness data from 2003.7 to 2004.9. The data are represented by black dots. Each dot is an average of seventy 25 s measurements. Cassini–Earth opposition is indicated. A heliospheric Lyα model scaled upward by a factor of 1.28 is shown in red dots. The same model scaled by a factor of 1.00 and added to an isotropic 43 R galactic signal is shown in yellow. A ±5σ statistical error bar is shown on one data point near the right.
Paper: Supporting Evidence for a Galactic Lyα Background from Cassini UVIS Data
Authors: Wayne R. Pryor, G. Randall Gladstone, Kurt D. Retherford, W. Kent Tobiska
Figure caption: Top panel: Cassini UVIS low-resolution slit Lyα roll brightness (black dots) from 2004 day 78 is plotted as a function of ecliptic latitude. Each dot is an average of five 25 s measurements. A model for the brightness using a hydrogen-lifetime asymmetry parameter of A = 0.4 is also shown, scaled by a factor of 1.03 and with an added background of 43 R (yellow dots). Data–model is also shown (+ symbols). A 5σ statistical error bar is shown on one data point. Bottom panel: Cassini UVIS low-resolution slit Lyα roll brightness (black dots) from 2004 day 78 is plotted as a function of ecliptic latitude. A model for the brightness using an isotropic hydrogen-lifetime asymmetry parameter of A = 0.0 is also shown, scaled by a factor of 1.07 and with an added background of 43 R (yellow dots). The differences between the data and the model values are also shown (+ symbols). A 5σ statistical error bar is shown on one data point.
Paper: Determining Which Binary Component Hosts the TESS Transiting Planet
Authors: Kathryn V. Lester, Steve B. Howell, David R. Ciardi, Rachel A. Matson
Figure caption: The probability of a primary star host (P 1) vs. the binary magnitude difference (Δm) for each binary in our sample. The “likely primary host” systems are plotted in blue, the “likely secondary host” systems are plotted in green, and the “uncertain host” systems are plotted in gray. The preference for primary star hosts in systems with faint companions is easily visible.
Paper: Determining Which Binary Component Hosts the TESS Transiting Planet
Authors: Kathryn V. Lester, Steve B. Howell, David R. Ciardi, Rachel A. Matson
Figure caption: Stellar density vs. effective temperature plots for TOI 141—492. The dervied value for the primary component is shown as the blue circle, the secondary component is shown as the green diamond, and any tertiary components are shown as red triangles. The solid purple line shows the model density- T eff relation built from the single TOI’s (purple points). The host probabilities of each component are also listed.