adsabs/AstroCLIMB huggingface dataset:
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Performance of the kinegeometric distance estimate (median of the posterior) as a function of distance for the constant fraction sample in the mock catalog. The left panel shows the fractional bias in the estimates. The right panel shows the fractional scatter. The color scale shows the density of stars on a log scale. The solid orange line shows the median bias or scatter at each distance; the dotted lines are the 5th and 95th percentiles. The blue lines show the same metrics for the geometric distances, for comparison.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Fractional distance residuals—(estimated-true)/true—per HEALpixel for the constant number sample in the mock catalog. The top row shows the median fractional residual (the bias); the bottom row shows the median absolute fractional residual (the scatter). The left column is for geometric estimates, and the right column is for kinegeometric estimates. The color bars span the full common range in each of the top and bottom rows. The top row uses a bilinear color bar (separate scales for negative and positive values): The dominance of red HEALpixels over blue ones at high latitudes is because the positive red scale extends to smaller values than the negative blue scale; the absolute biases are more or less the same overall.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Performance of the kinegeometric velocity estimate (median of the posterior) as a function of distance for the constant fraction sample in the mock catalog. The left panel shows the bias in the estimates. The right panel shows the scatter. The color scale shows the density of stars on a log scale. The solid orange line shows the median bias or scatter at each distance; the dotted lines the 5th and 95th percentiles. The blue lines show the same metrics for the geometric method (geometric distance times proper motion).
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Estimated distances and velocities vs. their true values for the constant fraction sample in the mock catalog. The color scale denotes the density of points on a logarithmic scale relative to the maximum in that panel, with densities less than a thousandth of the peak in white.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Median fractional differences between the kinegeometric and geometric distances per HEALpixel (computed on the individual stars), for the constant number sample in the mock catalog. The color bar has white at zero and diverges on different linear scales to the maximum negative and positive differences.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: As Figure 7, but now as a function of parallax S/N.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: As Figure 4, but now showing ﹩\sqrt{{\sigma }_{\alpha * }^{2}+{\sigma }_{\delta }^{2}}﹩, where σ  α* and σ  δ  are the standard deviations of the two components of the velocity prior.
Paper: Estimating Distances from Parallaxes. VI. A Method for Inferring Distances and Transverse Velocities from Parallaxes and Proper Motions Demonstrated on Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: As Figure 2, but now for HEALpixel 7593 at HEALpixel 7593 at (l, b) = (29.°0, 7.°7).
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: Left panel: color curve for one of the Mira in our sample constructed using Equation (1). The “MJD” (modified Julian date) for the (g − r) data points are at the midpoint of the gr-band MJDs. The magenta circles and green triangles are for the pairs of gr-band data points taken in the same night (ΔMJD < 0.5 day) and taken on different nights up to 0.02P  n  days, respectively. Crosses are rejected data points either with errors larger than 0.35 or with anomaly C  m  values. Right panel: the gr-band light curves for the same Miras as in the left panel. Open and filled circles in the gr-band light curves are those without and with the color-term corrections, respectively. Note that the color-term corrections did not apply to all gr-band data points, only for those with the (g − r) counterparts. For clarity, error bars are omitted in the right panels.
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: Left panel: the multiband LS periodograms based on the ZTF light curves, at which the highest peaks corresponding to P  n  (upper panel) and P  c  (lower panel). The vertical dashed line indicates the literature period of P  l  = 156 days. Middle panel: folded r-band light curves with our determined period P  n  (upper panel) and literature period P  l  (lower panel). The filled and open circles are data points with and without color-terms correction, respectively. Right panel: ZTF light curves and color curve for NGC 6638 V15, where the symbols are same as the right panels of Figure 2.
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: ZTF light curves for two Miras after corrected for the color-terms (open circles). The filled black squares are the determined magnitudes at maximum light, using the method described further in the text. Left panels show a Mira that only two m  i   X  can be determined, while the right panels are for a Mira with a total of 10 determined m  i   X .
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: Comparison of the multiband Lomb–Scargle (LS) periodograms for NGC 6642 V1 based on the light curves with (upper panel) and without (lower panel) the corrections of color terms.
Paper: Zwicky Transient Facility and Globular Clusters: The gr-band Period–Luminosity Relations for Mira Variables at Maximum Light and their Applications to Local Galaxies
Authors: C.-C. Ngeow, Jia-Yu Ou, Anupam Bhardwaj, Josiah Purdum, Ben Rusholme, Avery Wold
Figure caption: Distributions of color coefficients, C  m , retrieved from the PSF catalogs for our sample of Miras. Upper and lower panels are for the g and r band, respectively.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: We present the BPT diagram for the Hα-detected pilot-study sample. Objects measured by WRALF or re-examined and labeled as a Category 1 measurement are displayed as blue circles. Objects with the [N II] or Hβ line re-examined and labeled as a Category 2 measurement are shown as left-pointing, orange triangles or upward-pointing, red triangles. Objects that are a Category 2 measurement for both the [N II] and Hβ re-examination have been excluded. Characteristic error bars for the two groups of objects (WRALF+Category 1 or Category 2) are shown. The dashed–dotted line is from Dopita & Evans (1986) and is derived from stellar photoionization models. The dashed line is from Kauffmann et al. (2003) and is an empirical delimiter between the star-forming galaxies and AGN.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: Spectra of four QSOs detected in the pilot study. The red dashed vertical lines denote the wavelength range covered by the narrowband filter in which the source was detected. Key emission lines are labeled. The flux scales on the y-axes are in units of erg s−1 cm−2 Å−1. (a): A QSO detected via Mg II λ2798 in NB3. C III] λ1908 is also visible. (b): A C III] λ1908, NB2-detected QSO, with C IV λ1549 also visible. (c): A QSO detected by C IV λ1549 in the NB1 filter. Lyα is also visible. (d): A color-selected quasar detected in NB2 without any emission line present in the filter. See text for explanation on how this object was detected.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: Spectra of three objects detected by their Hα lines. The red dashed vertical lines denote the wavelength range covered by the narrowband filter in which the source was detected. Key emission lines are labeled in the middle panel. The flux scales on the y-axes are in units of erg s−1 cm−2 Å−1. (a): Detection in NB2 of an outlying HII region in a dwarf irregular galaxy. This is the lowest-redshift source in the SFACT pilot-study fields. (b): An HII region detected in a spiral galaxy with the NB1 filter. (c): A star-forming galaxy detected in the NB3 filter. Its [O III]λ5007/Hβ ratio indicates that this is a low-metallicity system.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: Histogram of SFACT ELGs binned by redshift. SFACT samples the Universe in discrete redshift windows with each line-filter combination probing a different redshift range. The bin width changes between the left and right sections of the plot. Bins in the left panel have a widths of 0.05, and bins on the right have widths of 0.25.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: Spectra of four galaxies detected by a nonprimary emission line (i.e., not their Hα, [O III], or [O II] lines). The red dashed vertical lines denote the wavelength range covered by the narrowband filter in which the source was detected. Key emission lines are labeled. The flux scales on the y-axes are in units of erg s−1 cm−2 Å−1. (a): An object detected by the [S II] doublet in the NB1 filter. This object is not from the pilot study. (b): A star-forming galaxy detected via [O III]λ4959 in the NB2 filter. (c): An Hβ detection discovered in NB1. (d): An object detected by its [Ne III]λ3869 line in the NB1 filter.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: Spectra of three objects detected by their [O II]λ3727 doublet. The red dashed vertical lines denote the wavelength range covered by the narrowband filter in which the source was detected. Key emission lines are labeled in the middle panel. The flux scales on the y-axes are in units of erg s−1 cm−2 Å−1. (a): An NB2-detected galaxy, included to show the faint nature of some of our sources. (b): A galaxy detected by the NB1 filter. [Ne III]λ3869 is visible in both this spectrum and in panel (a). (c): An NB3-detected source, showing the limited information present in the spectra of the NB3 [O II] detections.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: Spectra of three objects detected by their [O III]λ5007 lines. The red dashed vertical lines denote the wavelength range covered by the narrowband filter in which the source was detected. Key emission lines are labeled in the top panel. The flux scales on the y-axes are in units of erg s−1 cm−2 Å−1. (a): Seyfert 2 galaxy detected in the NB2 filter. (b): Star-forming galaxy detected in the NB1 filter. (c): Star-forming system detected in the NB3 filter.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: Spectrum of an SFACT-detected QSO. The red dashed vertical lines denote the wavelength range covered by the narrowband filter in which the source was detected. Key emission lines are labeled. The flux scale on the y-axis is in units of erg s−1 cm−2 Å−1. This QSO was detected by its C III]λ1908 line.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. III. Spectroscopy of the Initial Catalog of Emission-line Objects
Authors: David J. Carr, Jennifer Sieben, John J. Salzer, Samantha W. Brunker, Bryce Cousins
Figure caption: We present the [O III]-detected sample plotted on a log([O III]/Hβ) vs. log([O II]/[O III]) emission-line diagnostic diagram. The symbols are as in Figure 9, except this time orange left-pointing triangles are [O II] Category 2 re-examination measurements. Characteristic error bars for the two groups of objects (WRALF+Category 1 or Category 2) are shown. The dashed–dotted line is from Baldwin et al. (1981), Figure 1, and fits emission-line ratios of approximately solar-metallicity HII regions.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Example of four DIA sets from the first season of the DES. From left to right, the images correspond to the tmpl, srch, and diff image; the diff is generated as the subtraction of tmpl and srch. Each pair of tmpl and srch images is mapped to the same color range. We refer to these three-image sets as “image triplets” or DIA sets. Panels (a) and (b) show artifacts human-labeled as bogus (label=1). Panels (c) and (d) show transients labeled as real (label=0). Above each triplet is the unique ID of the transient (see Goldstein et al. 2015).
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption: Characteristics of best-fit models to various observations of XZ Tau AB over time, from published work and analysis of unpublished publicly available data. Rows display (top to bottom) optical brightness as represented by V magnitude, X-ray flux (absorbed and unabsorbed), plasma temperatures, plasma emission measures, and N H. Each column spans one set of observations, from 2000 (Güdel et al. 2007), 2004 (Giardino et al. 2006), 2017–2018 (Skinner & Güdel 2020), 2018, and 2020. Dotted lines connect points representing ObsIDs that were jointly fit.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption: Comparison of models of various observations of XZ Tau AB over time to model fits to COUP. Left: as with COUP model fits, XZ Tau AB over time exhibits a steady cool component and variable hot component that increase in brightness with increasing absorption-corrected X-ray luminosity. Right: as with COUP model fits, the ratio of emission measures of warm and cool components increases (i.e., the warm component increases in emission) as a function of absorption-corrected X-ray luminosity.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption: Evolution of XZ Tau AB over the course of a flare decay in ObsID 0865040401. The decrease in the emission measure of the “hot” component over time clearly tracks the decrease in count rate for photons at energies >1 keV, while the temperature of the “hot” component remains stable.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption: Evolution of XZ Tau AB over the course of a flare rise and decay in ObsID 0865040601. The change in the emission measure of the “hot” component over time clearly tracks the rise in count rate for photons at energies >1 keV. The “cool” component stays fairly stable over time, indicating that most of the change in brightness is due to the hot component.
Paper: Stable Coronal X-Ray Emission over 20 yr of XZ Tau
Authors: Steven M. Silverberg, Hans Moritz Günther, Pragati Pradhan, David A. Principe, P. C. Schneider, Scott J. Wolk
Figure caption:                       ﹩\mathrm{log}(T)﹩ of the five time-resolved spectra of observation 601, as a function of ﹩\mathrm{log}(\sqrt{\mathrm{EM}})﹩. Arrows indicate the time order of observations. The orange line reflects the slope ζ of the flare decay in this space.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Mean wind speeds in meters per second. (A) is the annual mean for Case 1 (zero obliquity) when its eccentricity is at zero. (B) is Case 3 (45° obliquity) when its eccentricity is at zero. (C) is Case 1 in the month of January when the planet is at perihelion in the Southern Hemisphere summer. In the Southern Hemisphere, there tends to be more ocean than land where wind differences are more easily seen. (D) is meant to contrast with that of (C) where Case 1 now has an eccentricity of 0.283 demonstrating that the mean wind speeds are not markedly different. The same applies in plots (D) and (E) at aphelion/July.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Maximum northern and southern latitudes of oceanic ice sheets. Note that part of the irregular patterns are related to the continents and their influence.
Paper: Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: M. J. Way, Nikolaos Georgakarakos, Thomas L. Clune
Figure caption: Total meridional transport: atmosphere + ocean. Different obliquities are plotted (Case 1–4) with snapshots (yearly means) at different eccentricities. Here we see the critical role played by obliquity for meridional transport, whereas eccentricity plays a less prominent role.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: Top: original properties of small planets included in the Dressing & Charbonneau (2015) study of Kepler's M dwarfs (T eff < 4000 K). Rectangles represent the optimistic (purple) and conservative (green) habitable zone boundaries used in Dressing & Charbonneau (2015). Translucent red points denote planets later labeled as false positives in Kepler DR25 (Thompson et al. 2018), while opaque colored points represent “Earth-sized” candidates considered relevant to the habitable zone. Bottom: current planet properties with updates from Gaia DR2 (Gaia Collaboration et al. 2018; Berger et al. 2020b), split between stars that are still below 4000 K (left) and stars that are now warmer than 4000 K (right). Translucent points represent the original properties from Dressing & Charbonneau (2015), while opaque points denote the updated properties of those planets, with lines connecting the two for each individual planet. Black arrows denote the average (log10) change in planet properties, measured independently along either axis. The host star of one of the six original habitable zone planets (K01681.04; blue) was not included in the Gaia–Kepler Stellar Properties Catalog (Berger et al. 2020b) and thus does not appear in either of the updated parameter panels.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: The current sample of Kepler small confirmed and candidate planets with Gaia-updated properties, plotted in orbital period (left) and instellation (right). Error bars represent 1σ uncertainties, and opacity is determined by reliability (fully opaque corresponds to a reliability score of 1; Bryson et al. 2020a). The average Kepler completeness maps for these M dwarfs are plotted in the background, with contours denoting relevant orders of magnitude (0.01%–10%). Gray rectangles denote the parameter range(s) of interest for this study.
Paper: No Evidence for More Earth-sized Planets in the Habitable Zone of Kepler's M versus FGK Stars
Authors: Galen J. Bergsten, Ilaria Pascucci, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Jessie L. Christiansen, Gijs D. Mulders
Figure caption: Distribution of stellar effective temperatures (from Berger et al. 2020b) for our sample of Kepler M-dwarf stars (T eff < 4000 K). The distribution of stars hosting Earth-sized planets is highlighted in blue and is not significantly distinct from the overall distribution (a two-sample Kolmogorov–Smirnov test provides a K-S statistic of 0.16 and a p-value of 0.38).