adsabs/AstroCLIMB huggingface dataset:
Paper: Apache Point Observatory Follow-up of ACcelerating Candidate ExopLanet Host Stars (APO ACCELS): Ages for 166 Accelerating Stars in the Northern Hemisphere
Authors: Anne E. Peck, Eric L. Nielsen, Robert J. De Rosa, William Thompson, Bruce Macintosh, William Roberson, Adam J. R. W. Smith, Jessica Klusmeyer, Asif Abbas, Jason Jackiewicz, Jon Holtzman, Hannah Gallamore, Marah Brinjikji, Jennifer Patience, Jayke S. Nguyen, Alex Madurowicz, Dmitry Savransky
Figure caption: We transform Gaia  GBP − GRP color to Johnson B − V using a polynomial fit to a large sample of Gaia-Hipparcos stars (F. van Leeuwen et al. 1997; Gaia Collaboration et al. 2023). We use our derived transformation when calculating median ages and 68% and 95% confidence intervals from BAFFLES (S. A. Stanford-Moore et al. 2020) for stars without precise B − V measurements.
Paper: Microlensing Constraints on the Stellar and Planetary Mass Functions
Authors: Jennifer C. Yee, Scott J. Kenyon
Figure caption: Cumulative distribution functions of planets inferred from ALMA disks from S. Zhang et al. (2018; upper left), G. Lodato et al. (2019; upper right), S. Wang et al. (2021; lower left), and S. Zhang et al. (2023; lower right). The left panel in each pair shows distributions for different assumptions of physics from each study (for S. Zhang et al. 2018 and S. Wang et al. 2021: ﹩A\equiv \,{\mathrm{log}}\,\alpha ﹩, S. Zhang et al. 2023: different limits for the maximum grain size) or, in the case of G. Lodato et al. (2019), different observational samples (see legend). The right panel shows one of those distributions relative to power laws with different indices p, normalized to the points indicated by the vertical dotted lines.
Paper: Discovery of Faint Nebulosity around a Z Camelopardalis–type Cataclysmic Variable in Antlia: Nova Shell or Ancient Planetary Nebula?
Authors: Howard E. Bond, Dana Patchick, Daniel Stern, Jonathan Talbot, John R. Thorstensen
Figure caption: Image of the nebula around ASASSN-19ds, created from 55.4 hr of exposure time in RGB, Hα, and [O III] λ5007 filters as described in the text. Hα is assigned to the red channel, and [O III] to the green and blue channels. Orientation and scale of the image (including a conversion to linear size at the distance of the star) are indicated at the lower right.
Paper: Discovery of Faint Nebulosity around a Z Camelopardalis–type Cataclysmic Variable in Antlia: Nova Shell or Ancient Planetary Nebula?
Authors: Howard E. Bond, Dana Patchick, Daniel Stern, Jonathan Talbot, John R. Thorstensen
Figure caption: SAAO spectrum of ASASSN-19ds, showing strong emission lines of hydrogen and He I and He II, and a feature near λ4640 due to C III and N III. The spectrum confirms that ASASSN-19ds is a cataclysmic variable.
Paper: Discovery of Faint Nebulosity around a Z Camelopardalis–type Cataclysmic Variable in Antlia: Nova Shell or Ancient Planetary Nebula?
Authors: Howard E. Bond, Dana Patchick, Daniel Stern, Jonathan Talbot, John R. Thorstensen
Figure caption: Deep images of the ASASSN-19ds nebula in the light of [O III] λ5007 (top frame) and of Hα (bottom frame).
Paper: Discovery of Faint Nebulosity around a Z Camelopardalis–type Cataclysmic Variable in Antlia: Nova Shell or Ancient Planetary Nebula?
Authors: Howard E. Bond, Dana Patchick, Daniel Stern, Jonathan Talbot, John R. Thorstensen
Figure caption: Seasonal g-band light curves of ASASSN-19ds from data in the ASAS-SN archive. Blue points are for 2021 October 30–2022 July 21, and red points (offset by +2 mag) are for 2022 November 16–2023 August 10. The star shows a “sawtooth” light curve, typical of Z Cam variables, with a variable time interval between successive brightness maxima.
Paper: Discovery of Faint Nebulosity around a Z Camelopardalis–type Cataclysmic Variable in Antlia: Nova Shell or Ancient Planetary Nebula?
Authors: Howard E. Bond, Dana Patchick, Daniel Stern, Jonathan Talbot, John R. Thorstensen
Figure caption: SAAO light curve of ASASSN-19ds on 2 nights in 2025 February, with orbital phases calculated from the ephemeris given on the x-axis label. The star shows an eclipse about 1 mag deep, and rapid flickering outside eclipse.
Paper: Discovery of Faint Nebulosity around a Z Camelopardalis–type Cataclysmic Variable in Antlia: Nova Shell or Ancient Planetary Nebula?
Authors: Howard E. Bond, Dana Patchick, Daniel Stern, Jonathan Talbot, John R. Thorstensen
Figure caption: Phase-binned light curves of ASASSN-19ds from TESS (top panel), ATLAS (middle panel), and ASAS-SN (bottom panel).
Paper: Discovery of Faint Nebulosity around a Z Camelopardalis–type Cataclysmic Variable in Antlia: Nova Shell or Ancient Planetary Nebula?
Authors: Howard E. Bond, Dana Patchick, Daniel Stern, Jonathan Talbot, John R. Thorstensen
Figure caption: Hα image of the nebula around ASASSN-19ds. Height of frame is ﹩1{8}^{{\prime} }﹩; north is at the top, east on the left. Magenta lines mark the cataclysmic variable.
Paper: Distributions of Wide Binary Stars in Theory and in Gaia Data. II. Reconstruction of Sample Probability Density of True Orbit Sizes
Authors: Valeri V. Makarov
Figure caption: Left: the differential function Φ(l) (Equation (7)) related to the power index γ(l) in the tail of PDF(a) reconstructed by the direct mapping technique. The dashed red line shows the linear fit for the interval l ∈ [3, 5]. Right: the empirical function Φ(λ) estimated from the actual histogram of ﹩\lambda ={{\mathrm{log}}}_{10}\,(s)﹩. The dashed red line is the same linear fit as in the left panel, for reference.
Paper: Distributions of Wide Binary Stars in Theory and in Gaia Data. II. Reconstruction of Sample Probability Density of True Orbit Sizes
Authors: Valeri V. Makarov
Figure caption: Numerically reconstructed probability density of orbit sizes a and apparent separation s per decibel using the IF method. Left: the orange line is a fit given by Equation (12), and the green curve is a kernel smoothing result of the actual reconstructed PDF, which is shown with the gray line. Right: the observed (blue) and reconstructed (red) histograms of ﹩{{\mathrm{log}}}_{10}\,(s)﹩.
Paper: Distributions of Wide Binary Stars in Theory and in Gaia Data. II. Reconstruction of Sample Probability Density of True Orbit Sizes
Authors: Valeri V. Makarov
Figure caption: Distribution (histogram in green) of the logarithms of semimajor axes between the components of resolved binary systems in Gaia DR3 from the catalog by K. El-Badry et al. (2021) by direct Monte Carlo mapping. The orange line is the numerically fitted analytical distribution given by Equation (5).
Paper: Distributions of Wide Binary Stars in Theory and in Gaia Data. II. Reconstruction of Sample Probability Density of True Orbit Sizes
Authors: Valeri V. Makarov
Figure caption: Monte Carlo-simulated histograms of f, which is the fractional projection factor given by Equation (3), for three cases of power-law eccentricity distributions, ﹩{\alpha }^{{\prime} }=-1﹩ (left), ﹩{\alpha }^{{\prime} }=+0.15﹩ (center), and ﹩{\alpha }^{{\prime} }=+1﹩ (right).
Paper: Distributions of Wide Binary Stars in Theory and in Gaia Data. II. Reconstruction of Sample Probability Density of True Orbit Sizes
Authors: Valeri V. Makarov
Figure caption: The differential function Φ(l) (Equation (7)) related to the power index γ(l) in the tail of PDF(a) reconstructed by the IF technique. The dashed red line shows the same linear fit for the interval l ∈ [3, 5] as in Figure 3, for reference.
Paper: Distributions of Wide Binary Stars in Theory and in Gaia Data. II. Reconstruction of Sample Probability Density of True Orbit Sizes
Authors: Valeri V. Makarov
Figure caption: Survival functions (1 − CDF(l)) of the probability density of orbit sizes ﹩l={{\mathrm{log}}}_{10}\,(a)﹩ for the widest binaries reconstructed by direct Monte Carlo mapping for two input sources of resolved pairs. The black curve represents the original smaller sample with a cut at angular separation below 2″, while the green curve shows the result for a larger sample without this cut.
Paper: Down But Not Out: The Case of Long-period Comet C/2021 O3 (Panstarrs)
Authors: David Jewitt, Jing Li, Michael Jaeger, Yoonyoung Kim
Figure caption: (Upper:) Observing geometry as viewed from Earth as a function of observation date. rH (solid blue curve) and Δ (dashed red curve) are the heliocentric and geocentric distances, respectively, while α (dashed–dotted orange curve) is the phase angle. The shaded region shows the range of dates on which observations were acquired. (Lower:) Same quantities as in the upper panel but for observations from STEREO-A.
Paper: Down But Not Out: The Case of Long-period Comet C/2021 O3 (Panstarrs)
Authors: David Jewitt, Jing Li, Michael Jaeger, Yoonyoung Kim
Figure caption: Postperihelion appearance of C/2021 O3 on UT 2022 May 17 (DOY 502), when rH = 0.80 au, with cardinal directions and a 100″ scale bar. This is a cleaned composite of 12 images selected to avoid contaminating stars.