adsabs/AstroCLIMB huggingface dataset:
Paper: Kast Optical Spectra of Unclassified Stars Within 20 pc of the Sun
Authors: Marylin Loritsch, Adam Burgasser, Madison Fierro, Emma Softich, Christopher Theissen, Preethi Karpoor, Chih-Chun Hsu, Roman Gerasimov
Figure caption: (a) Gaia-2MASS color–magnitude diagram for our sample, with symbol colors indicating spectral type. Median errors shown are σG−J = 0.02 and ﹩{\sigma }_{{M}_{G}}﹩ = 0.004. (b) Kast spectrum of UPM J1425+2540 (black line) compared to its best-fit M7 template (magenta line), with main spectral features labeled. (c) Distribution of template spectral classifications in our sample. (d) Template vs. literature classifications for 26 sources. The center line indicates perfect agreement, the dashed lines indicate ±1 subtype difference. (e) Spectral indices CaH2+CaH3 vs. TiO5. Sources with classifications M3–M6 are color-coded by spectral type, other sources are indicated by grey dots. The dotted line shows the solar metallicity trend from S. Lépine et al. (2007); the inset box shows the distribution of ζ values. (f) ﹩\mathrm{log}\left({L}_{{\rm{H\alpha }}}/{L}_{{\rm{bol}}}\right)﹩ as a function of spectral type. Detections are indicated by magenta points, upper limits by downward pointing arrows. LSPM J0540+6417, NLTT 37185, and LSPM J2044+1517 were observed twice, and the smaller values are indicated by black open circles. The median error in ﹩\mathrm{log}\left({L}_{{\rm{H\alpha }}}/{L}_{{\rm{bol}}}\right)﹩ of 0.18 is indicated. A catalog of source properties and Kast spectra obtained for all sources are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. XXVI. HD 173524 B (46 Dra B)
Authors: Richard Monier
Figure caption: Left: Synthesis of the Hg II line at 5677.10 for 46 Dra B (observed spectrum in black, synthetic in red) Right: Synthesis of the Pt II line at 4514.17 Å.
Paper: Detectability of Dust and Ion Tails of Interstellar Comet 3I/ATLAS by Europa Clipper
Authors: Hsiang-Wen Hsu, Jan Deca, Mihaly Horanyi, Sascha Kempf, Corey J. Cochrane, Xianzhe Jia, Cynthia B. Phillips
Figure caption: Simulated dust and pickup ion tails of interstellar comet 3I/ATLAS at various epochs along its trajectory (panels (a) and (b)). The views from the Earth (c) and the Europa Clipper (d) on 2025 November 5th are generated for future comparison with actual observations. The orbits of Mars, the Europa Clipper, and Jupiter are shown in red, blue, and orange curves, respectively. The syndynes of the cometary dust tails are color-coded by the dust β values. Our results suggest that the Clipper spacecraft is in a favorable position to detect pickup ions from 3I. On the other hand, the dust tails will not encounter Mars, the Clipper spacecraft, nor the Jovian system.
Paper: Tracking the Activity of the Interstellar Object 3I/ATLAS through Its Perihelion
Authors: T. Marshall Eubanks, Craig E. DeForest, Kevin J. Walsh, Simon Porter, Thomas Lehmann, Bruce G. Bills, Adam Hibberd, W. Paul Blase, Andreas M. Hein, Robert G. Kennedy, Adrien Coffinet, Pierre Kervella, Carlos Gomez de Olea Ballester
Figure caption: 3I/ATLAS magnitude data from a variety of sources, together with the November 6th prediction models in Equations (3) and (4).
Paper: An SMA Survey of UV-driven Chemical Tracers in Transition Disks
Authors: Shantanusinh Parmar, Charles J. Law
Figure caption: Top: disk-integrated spectra extracted using Keplerian masks. Bottom: violin plots of distance-normalized CN and HCO+ fluxes sub-divided by the presence and radial size of dust cavities. Points are individual measurements from our SMA data and the literature. Black bars show the interquartile range, and violin widths are kernel density estimations.
Paper: Evidence for No Orbital Decay in the Hot Jupiter XO-3b from Transit-timing Analysis
Authors: Jinyi Zhou
Figure caption: Transit time deviation plot of XO-3b with data from all sources (left) and Spitzer and TESS only (right), with quadratic and linear fit models.
Paper: High-spectral Resolution, Multi-wavelength Center-to-limb Observations of the Sun
Authors: Meetu Verma, Carsten Denker, Alexander G. M. Pietrow, Robert Kamlah, Dominique J. M. Petit dit de la Roche
Figure caption: GONG Hα full-disk image obtained at 10:49:11 UT. The grayscale insert is an Hα line-core VTT drift scan image taken at 10:48:53 UT (top-left). Spectroheliograms were taken at seven positions along the Hα line, and the labels to the right indicate the wavelength offset from the line center (top-right). The Hα quiet-Sun spectra are shown as a function of the cosine of the heliocentric angle ﹩\mu =\cos \theta ﹩ in the interval [0.2, 1.0] in steps of dμ = 0.1. The thick black curve represents an FTS atlas reference profile (bottom).
Paper: Further Identification of δ Scuti, γ Doradus Stars, and Eclipsing Binaries with TESS
Authors: Ai-Ying Zhou
Figure caption: Examples of newly identified δ Sct, γ Dor stars and hybrid pulsators.
Paper: Variability Census of Legacy Catalogs. IV. 3600+ New δ Scuti and γ Doradus Stars
Authors: Ai-Ying Zhou
Figure caption: Example TESS light curves and periodograms of newly identified: γ Dor stars (top two rows: HD 49152, HD 52087), δ Sct-γ Dor hybrid (rows 3–4: TYC 1854-93-1, HD 281579), eclipsing binaries with δ Sct (rows 5–6: HD 355359, HD 292868A) and γ Dor (bottom row: HD 337051, HD 290580) primary components.
Paper: IAU CPS Satellite Optical Brightness Recommendation: Rationale
Authors: Aaron C. Boley, Richard Green, Meredith L. Rawls, Siegfried Eggl
Figure caption: Comparison between (1) the IAU CPS recommendation based on the altitude ratio approximation and (2) the full expression using rates. The approximation is favored for the recommendation due to its simplicity.
Paper: Observations and Characterization of the New Active Centaur 2023 RS61
Authors: Eva Lilly, Charles A. Schambeau, Audrey Thirouin, Peter Jevčák, Robert Weryk, Richard J. Wainscoat
Figure caption: Left: cropped archival Pan-STARRS1 images taken on (Top) 2017 September 21 in w-band recalibrated against G/Gaia-DR2 with brightness G  ∼ 23.5, and on (Bottom) 2017 October 10 in i-band, with G  ∼ 19.1 during an apparent outburst. Right blue panels display data taken on 2025 January 2 with LDT in SDSS ﹩{r}^{{\prime} }﹩-band, where the lower panel is a zoomed-in view of the top. The projected skyplane directions for the Sun and RS61’s velocity are indicated by the yellow and red arrows, respectively.
Paper: Prediction and Observation of a Stellar Occultation by Haumea’s Satellite Namaka
Authors: Flavia L. Rommel, Benjamin C. N. Proudfoot, Bryan J. Holler, Jose L. Ortiz, Estela Fernández-Valenzuela
Figure caption: Predictions of the stellar occultations by (a) Haumea and (b) Namaka. Solid blue lines denote the estimated diameters of the objects and dashed red lines show the 1σ uncertainties. Panel (c) presents the normalized occultation light curve, and panel (d) presents the on-sky projection of the chords for Haumea and Namaka.