adsabs/AstroCLIMB huggingface dataset:
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Left: comparison of ACIS broad energy-band photon flux in the ECF 90% PSF aperture, photflux_aper90_b, with crpoisim determined using detection likelihoods, for a sample of isolated point sources; the best linear fit computed from Equation (23) using the broad band's scale factors from Table 15 is shown in red. Right: same, except the energy flux, flux_aper90_b, is plotted.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: Example candidate detections overlaid on a single observation of the Tycho supernova remnant. Compact detections from wavdetect and mkvtbkg are shown in blue and cyan, respectively, and the mkvtbkg extended detection is shown in green. This plot was created for human quality assurance review of the field. As described in the text, wavdetect identifies numerous spurious compact detections on the extended emission of the supernova remnant.
Paper: The Chandra Source Catalog Release 2 Series
Authors: Ian N. Evans, Janet D. Evans, J. Rafael Martínez-Galarza, Joseph B. Miller, Francis A. Primini, Mojegan Azadi, Douglas J. Burke, Francesca M. Civano, Raffaele D'Abrusco, Giuseppina Fabbiano, Dale E. Graessle, John D. Grier, John C. Houck, Jennifer Lauer, Michael L. McCollough, Michael A. Nowak, David A. Plummer, Arnold H. Rots, Aneta Siemiginowska, Michael S. Tibbetts
Figure caption: High-level flow of the background determination and source detection steps. Functional steps are shown in boxes with rounded corners. Archival data products are identified between thick horizontal bars, while temporary data products are shown between thin horizontal bars. For more information on the individual steps and data products, consult the text. The references identify the relevant sections of the text that describe the methods and algorithms used.
Paper: Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Authors: Valeri V. Makarov
Figure caption: Histograms of robust variability parameters in G for the general Gaia CRF sample. Left panel: dispersion of measured magnitudes smad ﹩(\hat{G})﹩. The red curve shows the closest analytical fit, which is the Maxwell [0.078] distribution. Right panel: normalized dispersion of measured magnitudes ﹩\hat{Z}﹩.
Paper: Catalog of Proper Orbits for 1.25 Million Main-belt Asteroids and Discovery of 136 New Collisional Families
Authors: David Nesvorný, Fernando Roig, David Vokrouhlický, Miroslav Brož
Figure caption: Fourier spectrum of ﹩e\cos (\varpi ),e\sin (\varpi )﹩ obtained for (5) Astraea from two different intervals: 0.6 Myr in green and 5 Myr in purple. The Fourier spectrum obtained from the 5 Myr long interval illustrates the splitting of the proper frequency into several terms.
Paper: Catalog of Proper Orbits for 1.25 Million Main-belt Asteroids and Discovery of 136 New Collisional Families
Authors: David Nesvorný, Fernando Roig, David Vokrouhlický, Miroslav Brož
Figure caption: The orbital eccentricity of (5) Astraea shows large oscillations due to the interaction with the secular resonance g + g 5 − 2g 6.
Paper: Optical Variability of Gaia CRF3 Sources with Robust Statistics and the 5000 Most Variable Quasars
Authors: Valeri V. Makarov
Figure caption: Histogram of median G BP − G RP colors for 0.8 million Gaia CRF3 sources, in logarithmic scale.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Distribution of the V magnitudes for the current sample of stars are shown in the red histogram. The V magnitudes of the stars in this study lie between 13.0 and 15.8, making it the faintest RPA sample of stars by more than 1 mag. The cumulative RPA samples (T. T. Hansen et al. 2018; C. M. Sakari et al. 2018; R. Ezzeddine et al. 2020; E. M. Holmbeck et al. 2020) are shown in the background (light-blue histogram).
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Top panel: Heliocentric radial velocities for our sample stars compared to the Gaia RVs. The black line is the one-to-one line. The diamond symbols indicate potential binaries. Lower panel: differences between the two quantities.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Metallicity distribution of our sample of stars, shown as the red histogram. Stars from all other previous RPA data releases are shown in the background (light-blue) histogram. The current sample spans a metallicity range of −3.3 ≤ [Fe/H] ≤ −0.2, with a peak at [Fe/H] = −2.8.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: The HR diagram showing the sample stars color coded by metallicity, as indicated by the color bar. The stellar evolutionary tracks correspond to ages of 12 (blue-dotted lines) and 13 Gyr (green-dotted lines) for a metallicity of [Fe/H] = −2.3.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Left panel: Distribution of the LTE abundances for Al and Na for stars in the halo and GCs. The black dots mark the halo stars obtained from T. Suda et al. (2008), including E. Carretta et al. (2009) and A. Bandyopadhyay et al. (2020b), and the blue triangles denote the GC stars from E. Carretta et al. (2009). The stars from this study are shown in red; the likely GC escapee 2MASS J11052721+3305150 is marked with a green-filled star while other potential GC escapees from I. U. Roederer & O. Y. Gnedin (2019) are marked in green-filled diamonds. Right panel: the position of 2MASS J11052721+3305150 is compared to bona fide GC stars from several clusters in the anticorrelated Na–O plane; based on the O upper limit, it is seen to fall along the GC population.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Left panel: Distribution of [Mg/Eu] as a function of [Fe/H] for r-I, r-II and non-RPE stars. The red stars are the non-RPE stars from this study, the r-I and r-II stars are taken from C. M. Sakari et al. (2018), T. T. Hansen et al. (2018), R. Ezzeddine et al. (2020), and E. M. Holmbeck et al. (2020), and the gray-filled circles are the stars from A. Abohalima & A. Frebel (2018). The r-I and r-II stars from this study are marked in the corresponding color. The histogram at the right compares the distributions of [Mg/Eu] from these sources over all metallicities. Right panel: The positive correlation of [(Sr+Ba)/H], as a function of [Eu/H]. The black-solid line indicates the yields for the main r-process from NSMs.
Paper: The R-process Alliance: Fifth Data Release from the Search for R-process-enhanced Metal-poor Stars in the Galactic Halo with the GTC 
Authors: Avrajit Bandyopadhyay, Rana Ezzeddine, Carlos Allende Prieto, Nima Aria, Shivani P. Shah, Timothy C. Beers, Anna Frebel, Terese T. Hansen, Erika M. Holmbeck, Vinicius M. Placco, Ian U. Roederer, Charli M. Sakari
Figure caption: Left panel: Classification of CEMP stars. The CEMP-no stars fall among the Group II and Group III stars in the low-C band while the CEMP-s stars fall among the Group I stars in the high-C band. The new CEMP stars from this study are shown in red. Right panel: Distribution of the light element Na and the α-element Mg for the Group II (black symbols) and Group III (blue symbols) CEMP-no stars, as a function of [Fe/H] (upper right panel) and A(C) (lower right panel). The literature data are taken from J. Yoon et al. (2016).
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Left: Histogram of normalized position offset magnitudes D (Equation (1)) for VLBI sources with more than 10 measurements. The expected Rayleigh distribution with scale 1 is shown as a black curve. Right: Histogram of 68th percentiles of normalized offsets D for 5370 VLBI sources. The black vertical line indicates the expected 68th percentile for a Rayleigh [1] distribution.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Median p-values of the standard binormal distribution test vs. decimal logarithm of n obs for 5138 VLBI sources with more than two position measurements.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Histogram of normalized position offset magnitudes D (Equation (1)) for the VLBI source 0016+731 with 1249 single-epoch measurements. The expected Rayleigh distribution with scale 1 is shown as a blue curve. The best-fitting Fréchet distribution with location −0.40, shape 1.20, and scale 1.84 is shown with a red curve.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Single-epoch position measurements (black dots) and their associated error ellipses (dotted gray curves) obtained with the VLBI for the source IVS 0010+336. The plot is centered at the ML position computed in this analysis with the red ellipse representing its formal error ellipse. The blue circled dot marks the ICRF3 position for this source. The orange circled dot shows the position of the Gaia DR3 optical counterpart. Note the reversed x-axis, in accordance with the astronomical convention.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Left: Source STR values as a function of the number of sessions in their time series, separated by coordinate component. From top to bottom are R.A., decl., and total magnitude. Sources with fewer sessions have seemingly low average STR values with large scatter, dramatically converging on a stable flat trend at a threshold of ∼15 sessions. Right: Histograms of the STR distributions for all ICRF3 sources, again separated by component. The defining sources are plotted with lighter shading, and the full set of ICRF3 sources with at least 15 observing sessions appear in darker shading. The ICRF3 sources with fewer than 15 sessions are also shown for reference with the light gray line, and demonstrate that time series with few observations (≤15 sessions) are distributed differently.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Comparison of R.A. and decl. component values of excess error. The left column shows the excess errors alone, while the right column shows combined formal and excess error values. The top row includes all ICRF3 X/S sources and the bottom row shows only the ICRF3 X/S defining sources. The data points are colored by source decl., and show that excess and combined errors are somewhat larger for sources observed at lower declinations, though with a large spread. Marginal distributions of the R.A. and decl. components are displayed in gray on the side axes.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Example measurement “jitter” offsets from the ICRF3 catalog position for a single source, 0322+222. The color of the scatter points corresponds to the number of delays observed for this source in each individual diurnal session measurement. Marginal distributions of the R.A. and decl. component offsets are shown on the top and right subaxes, respectively. The covariance-weighted mean value and its components are indicated in the top corner.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Smoothed time-series and component STR metrics for ICRF3-defining source 0016+731. Time is on the x-axis. Gray background points are the unsmoothed time series, while colored points show the smoothed series. Vertical axis ranges have been optimized for the smoothed series. Panels from top to bottom show the R.A.·cos(decl.) and decl. offset components, the total offset magnitude, and the offset position angle (CCW from north).
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Jitter—covariance-weighted mean offsets from ICRF3 positions, for the time series of all ICRF3 sources (top) and the defining sources (bottom). The data points are colored by source decl. Marginal distributions of the R.A. and decl. components are displayed in the side axes, and show a slightly larger dispersion in the N–S than the E–W direction owing to typical baseline geometry.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Histograms of excess error in R.A. and decl. components computed from the time series of each source. The full ICRF3 source list is denoted by the darker shading while the defining sources are denoted by the lighter shading. The ICRF3 X/S noise floor values of 30 μas are shown by the vertical dashed lines, for reference.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Distributions of the total magnitude (combined R.A. and decl.) of jitter (covariance-weighted mean) offsets for the full ICRF3 source list and the ICRF3-defining source list.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Distributions of variability metrics in milliarcseconds for the full ICRF3 source list, by tangential coordinate component: R.A. in the left panels, and decl. in the right panels. The top row shows the distributions for sources detected in at least four diurnal sessions (and at least 10 delays in each), reflecting nearly all sources. The bottom row shows the same distributions but only for sources with 15 or more sessions, which excludes a large fraction of sources but represents those with more robust values. The dashed vertical line denotes the 30 μas ICRF3 noise floor in each component, for reference. The red steps denote STR values, the yellow steps show the distribution of covariance-weighted mean jitter values, the gray hatched steps show the WRMS, and the blue shaded histogram shows the combined (formal plus excess) error.
Paper: Metrics of Astrometric Variability in the International Celestial Reference Frame. I. Statistical Analysis and Selection of the Most Variable Sources
Authors: Phil Cigan, Valeri V. Makarov, Nathan J. Secrest, David Gordon, Megan C. Johnson, Sebastien Lambert
Figure caption: Comparison of combined (formal plus excess) error with source decl. for all ICRF3 sources with at least four sessions. From top to bottom, the panels show the combined error for the R.A. and decl. components independently, followed by the total error (R.A. and decl. components added in quadrature). Each panel shows the source data along with a rolling median in 5° bins, and histograms of values on the side axes. Data are color coded by the number of observations, showing that the sources with more observations tend to have somewhat lower errors. There is a clear increase in typical source error as decl. decreases to ∼−40°, owing primarily to the network of stations mostly being located at northern latitudes. The effect is most pronounced for the decl. component in particular, because of baselines typically being longer in E–W than N–S directions.
Paper: The Simons Observatory: Design, Integration, and Testing of the Small Aperture Telescopes
Authors: Nicholas Galitzki, Tran Tsan, Jake Spisak, Michael Randall, Max Silva-Feaver, Joseph Seibert, Jacob Lashner, Shunsuke Adachi, Sean M. Adkins, Thomas Alford, Kam Arnold, Peter C. Ashton, Jason E. Austermann, Carlo Baccigalupi, Andrew Bazarko, James A. Beall, Sanah Bhimani, Bryce Bixler, Gabriele Coppi, Lance Corbett, Kevin D. Crowley, Kevin T. Crowley, Samuel Day-Weiss, Mark J. Devlin, Simon Dicker, Brooke DiGia, Peter N. Dow, Cody J. Duell, Shannon M. Duff, Remington G. Gerras, John C. Groh, Jon E. Gudmundsson, Kathleen Harrington, Masaya Hasegawa, Erin Healy, Shawn W. Henderson, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keating, Ben Keller, Kenji Kiuchi, Anna M. Kofman, Brian J. Koopman, Akito Kusaka, Adrian T. Lee, Richard A. Lew, Lawrence T. Lin, Michael J. Link, Tammy J. Lucas, Marius Lungu, Aashrita Mangu, Jeffrey J McMahon, Amber D. Miller, Jenna E. Moore, Magdy Morshed, Hironobu Nakata, Federico Nati, Laura B. Newburgh, David V. Nguyen, Michael D. Niemack, Lyman A. Page, Kana Sakaguri, Yuki Sakurai, Mayuri Sathyanarayana Rao, Lauren J. Saunders, Jordan E. Shroyer, Junna Sugiyama, Osamu Tajima, Atsuto Takeuchi, Refilwe Tanah Bua, Grant Teply, Tomoki Terasaki, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R Vissers, Liam Walters, Yuhan Wang, Zhilei Xu, Kyohei Yamada, Kaiwen Zheng
Figure caption: A cross-sectional view of an SAT showing the principal components. Inset: a detailed view of the three primary G10 fiberglass and carbon fiber reinforced polymer (CFRP) mechanical trusses as they are situated in the overall assembly with all surrounding components hidden.
Paper: The Simons Observatory: Design, Integration, and Testing of the Small Aperture Telescopes
Authors: Nicholas Galitzki, Tran Tsan, Jake Spisak, Michael Randall, Max Silva-Feaver, Joseph Seibert, Jacob Lashner, Shunsuke Adachi, Sean M. Adkins, Thomas Alford, Kam Arnold, Peter C. Ashton, Jason E. Austermann, Carlo Baccigalupi, Andrew Bazarko, James A. Beall, Sanah Bhimani, Bryce Bixler, Gabriele Coppi, Lance Corbett, Kevin D. Crowley, Kevin T. Crowley, Samuel Day-Weiss, Mark J. Devlin, Simon Dicker, Brooke DiGia, Peter N. Dow, Cody J. Duell, Shannon M. Duff, Remington G. Gerras, John C. Groh, Jon E. Gudmundsson, Kathleen Harrington, Masaya Hasegawa, Erin Healy, Shawn W. Henderson, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keating, Ben Keller, Kenji Kiuchi, Anna M. Kofman, Brian J. Koopman, Akito Kusaka, Adrian T. Lee, Richard A. Lew, Lawrence T. Lin, Michael J. Link, Tammy J. Lucas, Marius Lungu, Aashrita Mangu, Jeffrey J McMahon, Amber D. Miller, Jenna E. Moore, Magdy Morshed, Hironobu Nakata, Federico Nati, Laura B. Newburgh, David V. Nguyen, Michael D. Niemack, Lyman A. Page, Kana Sakaguri, Yuki Sakurai, Mayuri Sathyanarayana Rao, Lauren J. Saunders, Jordan E. Shroyer, Junna Sugiyama, Osamu Tajima, Atsuto Takeuchi, Refilwe Tanah Bua, Grant Teply, Tomoki Terasaki, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R Vissers, Liam Walters, Yuhan Wang, Zhilei Xu, Kyohei Yamada, Kaiwen Zheng
Figure caption: Left: a schematic of an array of three SATPs inside their ground shields. Each SAT receiver is mounted to an SATP and surrounded by a ground shield. Center: detailed view of the small aperture telescope platform (SATP) with the receiver mounted as reference. Right: detailed view of the SAT receiver with the forebaffle and sparse wire grid loading mechanism with labeled components including the dilution refrigerator (DR) and pulse tube cooler (PTC).