adsabs/AstroCLIMB huggingface dataset:
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Petersen diagram for 103 Galactic classical Cepheids pulsating simultaneously in the fundamental mode and the first overtone (black circles). The red line is the fit to the data obtained in this work, while the blue line shows the widely used relation from C. Alcock et al. (1995), modified by M. W. Feast & R. M. Catchpole (1997).
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Photometric distances derived from the W1 magnitudes for 2780 Cepheids for which both AllWISE photometry and unWISE photometry were available. Orange represents bright Cepheids with W1U < 8.25 mag, while the remaining ones are shown in blue.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Cumulative distribution of the normalized difference in the W1-based photometric and parallax-based astrometric parallaxes (Q = ∣Δϖ/σΔϖ∣).
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: The difference in Cepheid distances from this study (S24) and S19, as a function of Galactic longitude, for 2096 classical Cepheids. The mean offset is 242 ± 446 pc.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Left panel: WT at scale j = 4 of the Cepheids sample, compared to the spiral arm model from M. J. Reid et al. (2019). The black circle shows the Sun’s position, while the black plus sign at X = 8.277 kpc (assuming the distance inferred by GRAVITY Collaboration et al. 2022), Y = 0 kpc shows the Galactic center. Right panel: same as the left panel, but now compared to the spiral arm model from J. H. Taylor & J. M. Cordes (1993; solid lines) and arm n.2 from E. S. Levine et al. (2006; dashed line).
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: The distribution of 695 Cepheids within the distance range 2–5 kpc in Galactic coordinates, for which both dS24 and dGaia are available. The color represents the expected value of RGaia estimated from the distance difference (dS24 − dGaia) assuming that dS24 distances are correct. To be compared with Figure 2 from X. Zhang & G. M. Green (2025).
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Position of the Cepheids in the Galactic plane. The Sun’s position is shown by a black circle, and the Galactic center is shown by a black plus sign. Stars are color coded by their height above/below the Galactic plane Z (left panel) and age (right panel).
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: The difference in Cepheid distances from this study (S24) and based on Gaia (optical) Wesenheit magnitudes as a function of Galactic longitude, for 2910 classical Cepheids. The mean offset is 179 ± 1293 pc.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Color–color distribution G − W1 vs. GBP − GRP of 8723 dwarfs color coded by metallicity. Lines with different colors represent the photometric transformation of Equation (A1) for [M/H] = 0 (black), [M/H] = +0.4 (violet), and [M/H] = −0.9 (blue).
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Differences in the distances from this study and based on Gaia (optical) Wesenheit magnitudes, as a function of G magnitude (top) and G − W1 color (bottom).
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Ages of 3424 Cepheids in our sample estimated from the period–age relation derived by R. I. Anderson et al. (2016). The median age is 132 Myr.
Paper: The Milky Way as Seen by Classical Cepheids. I. Distances Based on Mid-infrared Photometry
Authors: Dorota M. Skowron, Ronald Drimmel, Shourya Khanna, Alessandro Spagna, Eloisa Poggio, Pau Ramos
Figure caption: Test sample: distribution of the residuals between W1U and the value computed from Equation (A1) vs. fracflux. Red lines show the median and the 16th and 84th percentiles.
Paper: FArSide Trained Active Region Recognition (FASTARR): A Machine Learning Approach
Authors: Amr Hamada, Mitchell Creelman, Kiran Jain, Charles Lindsey
Figure caption: FASTARR-AR temporal stability on the target map for 2014 June 17, 12:00 UT (first row), with the two preceding maps at a 12 hr cadence: 2014 June 17, 00:00 UT and 2014 June 16, 12:00  UT. First column ((a), (e), and (i)): the input far-side helioseismic phase maps. Second column ((b), (f), and (j)): the FASTARR output probability maps, showing the likelihood of AR presence. Third column ((c), (g), and (k)): FASTARR’s AR masks, where the ARs from the prior 12 and 24 hr are labeled with cyan and magenta boxes, respectively. Fourth column ((d), (h), and (l)): the far-side EUV/304 Å maps, where the black and blue contours represent the ground truth and predicted ARs, respectively. For the target phase map (a), the output ARs (c) are labeled with green boxes if they overlap with other ARs from both of the prior two maps at the same location. Yellow-labeled ARs represent those that overlap with only one of the prior two maps at the same location. Red-labeled ARs represent those with no overlap with any of the ARs from the prior maps at the same location.