adsabs/AstroCLIMB huggingface dataset:
Paper: The Sensitivity of Eclipse Mapping to Planetary Rotation
Authors: Arthur D. Adams, Emily Rauscher
Figure caption: The first 10 modes of eigenmaps identified by PCA for the Warm Jupiter case with ψ sky = 30°. We show the maps in a Mollweide projection that shows all longitudes and latitudes. The reference hemisphere, which is the hemisphere that faces the observer at the midpoint phase of ingress, is centered in each projection and outlined with a dotted white circle. Green dashed contours represent the equator and ±45° latitude lines, with arrows indicating the direction of rotation. Rotation rates span the scale from “slow” where the planet rotates a small fraction of a full rotation across eclipse (N tot < 1), to “fast” where the planet rotates through a considerable fraction of a full rotation. At the fastest rate the planet’s rotation period approaches the duration of ingress or egress (N i,e → 1). For reference, with our prototypical 10 day Warm Jupiter, N tot = 1 corresponds to ω rot/ω orb ≈ 71, and N i,e = 1 corresponds to ω rot/ω orb ≈ 432.
Paper: Detection of Strongly Lensed Arcs in Galaxy Clusters with Transformers
Authors: Peng Jia, Ruiqi Sun, Nan Li, Yu Song, Runyu Ning, Hongyan Wei, Rui Luo
Figure caption: Detection results of our algorithm for images containing A2744 (﹩3\buildrel{\,\prime}\over{.} 05\times 4\buildrel{\,\prime}\over{.} 38﹩ with 3662 × 5253 pixels), MACS J1149.5+2223 (﹩1\buildrel{\,\prime}\over{.} 90\times 1\buildrel{\,\prime}\over{.} 90﹩ with 3800 × 3800 pixels), and CIG 1358+62 (﹩1\buildrel{\,\prime}\over{.} 06\times 0\buildrel{\,\prime}\over{.} 96﹩ with 640 × 583 pixels). These results show that our algorithm could directly detect gravitational arcs from real observation data, when our algorithm is only trained with ideal simulated data without noise. Generally speaking, a model trained only with simulated data usually needs some methods to adapt to real observation data. However, our algorithm can detect strong gravitational lensing on real data without further training, which shows that it is effective to train an effective neural network with simulated data, if the simulation reflects real physical processes. Original image of A2744 by NASA, ESA, and D. Coe (STScI)/J. Merten (Heidelberg/Bologna). Original image of MACS J1149.5+2223 by NASA, ESA, S. Rodney (John Hopkins University, USA), and the FrontierSN team; T. Treu (University of California Los Angeles, USA), P. Kelly (University of California Berkeley, USA), and the GLASS team; J. Lotz (STScI) and the Frontier Fields team; M. Postman (STScI) and the CLASH team; and Z. Levay (STScI). Original image of CIG 1358+62 by Marijn Franx (University of Groningen, The Netherlands), Garth Illingworth (University of California, Santa Cruz), and NASA/ESA.
Paper: Detection of Strongly Lensed Arcs in Galaxy Clusters with Transformers
Authors: Peng Jia, Ruiqi Sun, Nan Li, Yu Song, Runyu Ning, Hongyan Wei, Rui Luo
Figure caption: Detection results for images containing Abell S1063 (﹩2\buildrel{\,\prime}\over{.} 07\times 2\buildrel{\,\prime}\over{.} 32﹩) in images of different size, 2243 × 2511 pixels in the left panel and 1280 × 1433 pixels in the right panel. A star with a bright arc nearby is wrongly classified as a CGSL because it is relatively large and contains a central bright source and arcs nearby. However, our algorithm could detect the CGSL from an image with a smaller size, when the star and the arc have smaller size. Original image of Abell S1063 by NASA, ESA, and J. Lotz (STScI).
Paper: Detection of Strongly Lensed Arcs in Galaxy Clusters with Transformers
Authors: Peng Jia, Ruiqi Sun, Nan Li, Yu Song, Runyu Ning, Hongyan Wei, Rui Luo
Figure caption: These figures show self-attention and cross-attention of our algorithm in detection of CGSLs from observation images. These two images contain the same target SMACS0723 observed by the Hubble Space Telescope and the James Webb Space Telescope. As shown in this figure, we find that our algorithm could detect locations of the CGSLs in both of these figures. Besides, attention maps are similar to each other, which indicates that our method could reveal similarities between these two images.
Paper: Detection of Strongly Lensed Arcs in Galaxy Clusters with Transformers
Authors: Peng Jia, Ruiqi Sun, Nan Li, Yu Song, Runyu Ning, Hongyan Wei, Rui Luo
Figure caption: Detection results with top two scores for an image that contains A370 (﹩3\buildrel{\,\prime}\over{.} 91\times 4\buildrel{\,\prime}\over{.} 45﹩ with 4164 × 4634 pixels). As shown in this figure, these two detection results locate the same CGSL with a little horizontal shift, which indicates that the detection results of our algorithm are reliable. Original image of A370 by NASA, ESA, A. Koekemoer, M. Jauzac, C. Steinhardt, and the BUFFALO team.
Paper: Detection of Strongly Lensed Arcs in Galaxy Clusters with Transformers
Authors: Peng Jia, Ruiqi Sun, Nan Li, Yu Song, Runyu Ning, Hongyan Wei, Rui Luo
Figure caption: The ROC curve of our algorithm, which has an area of 0.99.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Precise CMDs used for selecting likely single-star members of the NGC 752 cluster, with Gaia EDR3, Strömgren (Twarog et al. 2015), and Vilnius (Zdanavičius et al. 2010) photometry shown from left to right. Gaia-selected likely binary members are shown in black, with photometrically selected single-star members in red. Open circles show known chemically peculiar stars (Garrison 1972). Photometry of BD +37 410 is shown with the cyan point, the DS And system at quadrature is the larger red point, and the positions of the DS And primary and secondary stars (as inferred from light curves) are shown with green points.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Precise CMDs of likely single-star members of the NGC 752 cluster. Photometry of BD +37 410 is shown with cyan points, the DS And system at quadrature is shown with red points, and the positions of the primary and secondary stars (as inferred from light curves) are shown with green points.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Spectral energy distribution for DS And A as derived from light curves with observations of the secondary star eclipse (red points for photometry). A fitted ATLAS9 model for T eff = 7070 K, ﹩\mathrm{log}g=4.0﹩, and [Fe/H] = 0 (solid line, and green points for integrations over filter response curves) is shown. Horizontal error bars represent the effective width of the filter. Bottom: fractional difference between the stellar fluxes and the best-fit model fluxes for the ATLAS9 (green) model.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Top: SED for PLA 255, the proxy for DS And B (red points) and a fitted ATLAS9 model for T eff = 6290 K (solid line, and green points for integrations over filter response curves). Horizontal error bars represent the effective width of the filter. Bottom: fractional difference between the stellar fluxes and the best-fit fluxes for the ATLAS9 (green) model.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Top: SED for turnoff star BD +37 417 (red points for photometry) and a fitted ATLAS9 model for T eff = 6955 K, ﹩\mathrm{log}g=4.0﹩, and [Fe/H] = 0 (solid line, and green points for integrations over filter response curves). Bottom: fractional difference between the stellar fluxes and the best-fit model fluxes for the ATLAS9 (green) model.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: DS And light curve from SuperWASP camera 141, computed differentially relative to nearby star NGC 752 165.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: DS And W1 and W2 light curves from WISE (magenta points) and NEOWISE-R (red) photometry (Chen et al. 2018).
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Mass–radius plot for measured members of DS And and BD +37 410 A, with 2σ uncertainties indicated by the red error ellipses. Models use Z = 0.0152, 0.0149, 0.0142, and 0.0162, respectively for PARSEC (Bressan et al. 2012), BaSTI-IAC (Hidalgo et al. 2018), MIST (Choi et al. 2016; Dotter 2016), and YaPSI (Spada et al. 2017) isochrones. In the BaSTI-IAC panel, dotted lines show models without convective core overshooting. Solid black lines connect the lower turnoff points on the different isochrones (with the dashed lines in the BaSTI-IAC panel for models without convective core overshooting).
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Color–magnitude diagram for NGC 752 (magenta points) and NGC 6811 (green) cluster members selected based on Gaia proper motions and parallaxes from Early Data Release 3. PARSEC isochrones for Z = 0.0152 and ages 1.00 and 1.60 Gyr are shown. The black marks shows where stars with the mass of KIC 9777062 A, DS And A, and BD +37 410 A would be in the respective isochrones. The large red points show the mean photometry for all three binaries, the large green point shows the approximate characteristics of KIC 9777062 A, and the blue point shows the characteristics of a proxy for BD +37 410 A.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Precise CMDs of likely single-star members of the NGC 752 cluster (small red points) and binary members (black points). Photometry of the DS And system at quadrature is shown with large red points, and the positions of the primary and secondary stars (as inferred from light curves) are shown with green points. Photometry of the BD +37 410 system is shown with cyan points, and a proxy for BD +37 410 A (PLA 641) is shown with blue points. PARSEC isochrones (Bressan et al. 2012) for Z = 0.0152 are shown with ages from 1.3 (blue) to 1.8 (black) Gyr with 0.1 Gyr spacing. Horizontal lines mark the position of a star of BD +37 410 A’s mass on the isochrone.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: HR diagrams showing NGC 752 single-star candidates (red points), DS And A (green point), and eclipsing binary components of similar mass (cyan points). Left panel: 1.4 Gyr isochrone (cyan dotted line) and a 1.692 ± 0.01M ⊙ evolution tracks (black dotted lines) from the MIST database (Choi et al. 2016; Dotter 2016) for Z = 0.0152. Right panel: PARSEC isochrones for Z = 0.0152 and ages 1.4 (cyan), 1.5 (green), 1.6 (red), and 1.7 (black) Gyr.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Mass–luminosity plot for measured eclipsing binary stars from the DEBCat database (retrieved 2019; Southworth 2015), with 2σ error bars (showing primary stars in blue and secondary stars in red). The 2σ uncertainties for DS And A are indicated by the red error ellipse. PARSEC (Bressan et al. 2012) isochrones are shown for Z = 0.0152.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Evolution of model characteristics for DS And A, according to MIST (Choi et al. 2016; Dotter 2016) models for two different metal contents Z. Black lines show evolution tracks for the measured mass, with red and blue lines showing tracks offset in mass by ±1σ. Black dots in the T eff plot show the turnoff value for the corresponding Z. Gray bars show the ±1σ uncertainty around the measured characteristics of DS And A.
Paper: Evolved Eclipsing Binaries and the Age of the Open Cluster NGC 752 
Authors: Eric L. Sandquist, Andrew J. Buckner, Matthew D. Shetrone, Samuel C. Barden, Catherine A. Pilachowski, Constantine P. Deliyannis, Dianne Harmer, Robert Mathieu, Søren Meibom, Søren Frandsen, Jerome A. Orosz
Figure caption: Photometric radii vs. effective temperature for single-star candidates in NGC 752, compared to PARSEC isochrones for 1.5, 1.6, and 1.7 Gyr.
Paper: Mass Production of 2021 KMTNet Microlensing Planets. III. Analysis of Three Giant Planets
Authors: In-Gu Shin, Jennifer C. Yee, Andrew Gould, Kyu-Ha Hwang, Hongjing Yang, Ian A. Bond, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Arisa Okamura, Greg Olmschenk, Clément Ranc, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama
Figure caption: Light curve of KMT-2021-BLG-0119 with APRX model curves, geometries, and residuals.(The data used to create this figure are available.)
Paper: FUMES. III. Ultraviolet and Optical Variability of M-dwarf Chromospheres
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Zachory K. Berta-Thompson, Kevin France, Allison Youngblood
Figure caption: HIP 23309 is one of the more active, UV-bright stars in our sample, and as a result its spectra have signal-to-noise making them ideal for variability analysis on the shortest timescales. Each line’s time series is represented by a unique marker shape and color with error bars, although the errors are minuscule and rarely extend beyond the marker itself. The time series for Hα's equivalent width, shown in the darkest red line here, is nearly perfectly flat with no observable long-term trend or short-term variability exceeding the error bars of individual measurements. The lines with the greatest variability are the Ca II H and K lines which have been plotted in a separate panel for visual clarity, although some of this variability is an offset between grating settings that we attribute to flux calibrating with a standard star spectrum taken with just one of the two settings.
Paper: FUMES. III. Ultraviolet and Optical Variability of M-dwarf Chromospheres
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Zachory K. Berta-Thompson, Kevin France, Allison Youngblood
Figure caption: Using LP 247-13 as an example, we demonstrate the variability of three optical emission lines in individual panels: Hα on the left, Ca II K in the middle, and Hδ on the right. We first normalized the spectra from each individual exposure, then resampled them onto a common wavelength grid, and then identified the median spectrum with associated error bars and boundaries for the 16th and 84th percentile values of the spectrum in each wavelength bin. The median spectra and their errors are drawn in solid black while the gaps between the median and 16/84th percentile boundaries are filled in with blue/red, respectively. The variability exceeds the error bars in each panel but the magnitude of variation relative to the continuum is higher for Ca II K and Hδ than for Hα, following a trend shared by the remainder of the sample where we measured lines other than Hα.
Paper: FUMES. III. Ultraviolet and Optical Variability of M-dwarf Chromospheres
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Zachory K. Berta-Thompson, Kevin France, Allison Youngblood
Figure caption: This figure shows the time series measurements for the equivalent widths of Ca II K (top panel), Hη (middle panel), and Hα (bottom panel) for every star in the sample with measurements of those respective lines. No variability is seen in Hα except for one star, HIP 112312. Ca II and Hη both exhibit significant variability in all targets. Note that all light curves are plotted with error bars, but that the scale of the error is minuscule, even in Figure 2 which focuses on the optical time series data for just one star.
Paper: FUMES. III. Ultraviolet and Optical Variability of M-dwarf Chromospheres
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Zachory K. Berta-Thompson, Kevin France, Allison Youngblood
Figure caption: This figure demonstrates the line-fitting process for the first time bin spectrum of CD-35 2722, including photon events that occurred during the first 150 s of observation. The panels show the data in black and best-fit model in blue for the C II multiplet on top and the N V doublet on the bottom. The blue swath represents the 1σ boundaries of the model fit. Both fits include a sloped continuum, although the slope is very shallow, and the C II multiplet is fit with a single Gaussian while the N V doublet is fit using two Gaussians. The models are convolved with the line-spread function before evaluating the fit statistic.
Paper: FUMES. III. Ultraviolet and Optical Variability of M-dwarf Chromospheres
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Zachory K. Berta-Thompson, Kevin France, Allison Youngblood
Figure caption: This figure shows the Balmer decrements for all stars in the FUMES sample for which we were able to measure the higher-order Balmer lines. The error bars on the points represent the maximum range of values for the decrement across the time series for that emission line. The values of the Balmer decrements are also recorded in Table 5.
Paper: FUMES. III. Ultraviolet and Optical Variability of M-dwarf Chromospheres
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Zachory K. Berta-Thompson, Kevin France, Allison Youngblood
Figure caption: On a logarithmic scale, the time series of CD-35 2722's Balmer decrements show variations exceeding the error bars of individual measurements. A stellar atmosphere model allowed to vary over time with different magnetic heating processes could compare the scale of its decrement variability to this data set.
Paper: FUMES. III. Ultraviolet and Optical Variability of M-dwarf Chromospheres
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Zachory K. Berta-Thompson, Kevin France, Allison Youngblood
Figure caption: This figure shows the time series measurements of the line fluxes for three UV emission features: N V in the bottom panel, C IV in the middle panel, and Si IV in the top panel. No clear stochastic or long-term trends are apparent in these time series.
Paper: FUMES. III. Ultraviolet and Optical Variability of M-dwarf Chromospheres
Authors: Girish M. Duvvuri, J. Sebastian Pineda, Zachory K. Berta-Thompson, Kevin France, Allison Youngblood
Figure caption: This figure shows the time series of UV line flux measurements for HIP 23309. Unlike Figure 2, the point-to-point variability is not visibly distinguishable from the photometric uncertainty.
Paper: The Sensitivity of Eclipse Mapping to Planetary Rotation
Authors: Arthur D. Adams, Emily Rauscher
Figure caption: Eclipse maps and curves from fits to simulated data from model planets rotating at a range of rates ω rot/ω orb = 1–30, and each with a spin axis that is inclined at 45°, both toward the line of sight and with respect to the plane of the sky (ψ LOS = ψ sky = 45°). The input map is shown at the top in green, as it would be oriented to the observer at the time of mid-ingress. The equivalent full-globe Mollweide projection is shown just below to compare with the equivalent projections of the retrieved maps. ω rot/ω orb is equivalent to how many times the planet rotates per orbit. We generate 10,000 realizations of Gaussian noise for each simulated eclipse curve and fit each with some number n of eigencurves (i.e., parameters), where n is determined by a Bayesian Information Criterion (BIC). The mode and ±1σ of n are shown for each case. Recovered curves and maps are shown based on the rotation rate of the model used to generate the data (x-axis), vs. the rotation rate of the eigenbasis used to fit the data (y-axis). Each subplot of the eclipse curve grid shows the range of uncertainty used to artificially noise the simulated data, with one example realization of the 10,000 in colored points. The fit is shown in greyscale; the solid line is the median of all fits and a shaded region shows the ±1σ (≈16th and 84th percentiles) range of fits. We show maps generated using the median values of the coefficients from each eigenmap.