adsabs/AstroCLIMB huggingface dataset:
Paper: Transit-APP: A Centroid-free Method of Identifying Background Transit False Positives
Authors: Steve Bryson, Michelle Kunimoto
Figure caption: An example of the centroid-free method applied to the known Kepler background false positive KOI-109.01. Upper Left: the scene around the star KOI-109 in quarter 3, with stars from the Gaia DR3 catalog indicated by white stars and their star index and g-magnitudes. The red dot is the star KOI-109. Right: the observed and simulated difference image collections, with the observed difference images Dobs in the first column and each star’s simulated difference images Ds in the other three columns. Only stars 0, 1, and 2 are shown for clarity. The rows are different quarters, with only quarters 1–4 shown for clarity. The orange outline shows the star whose simulated difference images most closely resembles the observed difference images. Lower Left: the expected log pointwise predictive density (ELPD) values and error bars for each star, showing that star 1 is overwhelmingly more likely to be the source of the transit signal than than star 0 (KOI-109) or star 2.
Paper: Apparent Diameters of F- to M-type Main-sequence Stars as Viewed from Habitable Zone Planets
Authors: Shaan D. Patel, Manfred Cuntz, Nevin N. Weinberg
Figure caption: Top: apparent stellar size from a planet located at the inner and outer limits of the respective HZ using MESA (green). Overlaid are the points for the inner/outer HZ of the Sun (blue), along with a point using Sun–Earth distance (purple). Bottom: a subset of MESA-based data points (green) along with data points from calculations based on the models by M. Cuntz & Z. Wang (2018) (purple) and A. W. Mann et al. (2013) (blue).
Paper: Antares: Variability of the Nearby M Supergiant and Core Collapse Type II Supernova Progenitor
Authors: Ed Marici, Edward Guinan
Figure caption: Panel (a) shows the plot of the visual and V-band observations of Antares from 1987 to 2024. The panel adjacent (b) shows the power-spectrum/period analysis showing dominant periods of 348, 850 and 3086 days (8.45 yr). Panel (c) shows the WWZ wavelet analysis displaying the evolution of these periods over time. Panel (d) shows the CLEANest Power spectrum P = 2240 days produced from photoelectric data from 1986 to 2000 made mostly by James Woods.
Paper: Optical Polarimetry of WR 1 Consistent with a CIR and 17 days Rotation
Authors: Nicolaus Steenken, Richard Ignace, Nicole St-Louis, Guillaume Lenoir-Craig
Figure caption: (a) Observed polarization of WR 1 with an amplitude of 0.6% shows three maxima approximately separated by about 17 days. (b) Q − U diagram of observed polarization moving circularly twice during the observation period of 39 days. (c) Observed polarization position angle (PA) in degrees with two maxima. (d) V-band magnitude with two maxima/minima over the 39 days of observation. (e) Delta Q − U diagram of intrinsic polarization after removal of Q interstellar = −5.65%, U interstellar = −0.09%. Numerical labels indicating days since the first observation day 0 until day 17. (f) Intrinsic Q − U diagram for days 21 to 39. For all panels, note that polarization measurements are unfiltered, and error bars are 1σ. Data behind figure available in a machine-readable format in the online Journals and on Zenodo: doi:10.5281/zenodo.14860262.(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. XVIII. HD 53929
Authors: Richard Monier
Figure caption: Left: synthesis of the 4475–4500 Å spectral interval (observed spectrum in black, synthetic spectrum in red). Right: the Hg II line at 5677.10 Å is not detected in the I profile of HD 53929.
Paper: Investigating the Nature of X-Ray Sources in the Andromeda Galaxy Using Chandra and Hubble Data
Authors: Erika Marentes, Blagoy Rangelov
Figure caption: Color–Magnitude Diagrams comparison: closest counterpart to the left and brightness counterpart to the right.
Paper: Discovery of 128 New Saturnian Irregular Moons
Authors: Edward Ashton, Brett Gladman, Mike Alexandersen, Jean-Marc Petit
Figure caption: Rose diagram of the irregular moons of Saturn. For the 122 previously known irregular moons each circle represents the time-averaged inclination and semimajor axis of a moon, with the size of the circle indicating the relative size of the moon. Additionally, each moon has a line that goes from the time-averaged pericentre to the time-averaged apocentre. Color has been used to split six specific regions; the Gallic group (yellow), the Inuit group (green), the low-i (<151∘) Norse members (cyan), Kari subgroup (blue), the Mundilfari subgroup (magenta), and the Phoebe subgroup (red) (E. Ashton et al. 2025). The osculating orbits of the 83 new moons with multiyear arcs are indicated with black crosses.
Paper: The Calm Before the Storm: The Impact of Radiative Cooling on Magnetic Field Amplification
Authors: Nicholas Anthony Proietti, Meg Georgina Blackburn, Ryan Jeffery Farber
Figure caption: Evolution of the mean magnetic-field strength of gas with 2Tcold < T < Thot/2 over a 7 Myr interval for three simulation setups: adiabatic (red), with radiative cooling (blue), and a reduced temperature floor of 400 K maintaining Thot = 106 K (cyan). Solid, dashed, and dotted lines respectively denote resolutions of 32 × 32 × 64, 64 × 64 × 128, and 128 × 128 × 256.
Paper: The Early Infrared Spectrum of the Fe II Nova V1310 Scorpii
Authors: Richard J. Rudy, Ray W. Russell, David K. Lynch, Michael L. Sitko
Figure caption: 0.8–5.2 μm spectrum of the Fe II-type nova V1310 Scorpii, obtained 11 days after peak brightness. The top three panels break the spectrum into shorter segments to allow for identification of the many emission lines that are seen frequently in Fe II novae early in their spectral development. The bottom panel is a comparison with the Fe II nova V1663 Aql (plotted with a slight offset in flux to minimize the overlap between the spectra) from R. J. Rudy et al. (2025), to which V1310 Sco is remarkably similar. V1310 Sco displays the expected H I emission, with lines from four series (Paschen, Brackett, Pfund, and Humphreys) being present. It also has a very rich N I spectrum, the lines of which are labeled in blue. The excellent atmospheric transmission at the time of the observation reveals the strength of the N I line complex at 1.36 μm. Fe II lines, which are fluorescently excited (see text), are also plentiful and are denoted by green labels. He I lines are just starting to emerge and, in the case of lines at 1.0830 and 2.0587 μm, display P-Cygni profiles. The O I lines at 0.8446 and 1.12890 μm, which are fluorescently excited by Lyβ, are the strongest lines in the spectrum.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Persistent Periodic Signals from 51 Peg in TESS Lightcurves
Authors: Eric Gaidos, Douglas Caldwell, Stefan Dreizler
Figure caption: Periodograms and phased lightcurves of TESS photometry of 51 Peg during Sectors 56 (top) and 83 (bottom) showing the persistent signal at 4.55 days, well above the FAP = 0.001 level (horizontal line) and distinct from systematics produced by the spacecraft momentum wheels and orbit (dotted vertical lines). Points in the phased lightcurve are the median of data binned by phase, with uncertainties from sampling with replacement, and the red curve is the generalized Lomb–Scargle sine wave fit. Phase is with respect to the TESS time zero-point of BJD = 2457000.
Paper: Discovery of 12 New Orbital Periods for Classical Novae
Authors: Bradley E. Schaefer
Figure caption: The folded light curve for all 12 new orbital periods. The red squares are the phase averaged light curve for all the TESS sectors, with either 25 or 50 phase bins. The horizontal axis is the phase from 0.0 to 1.0, and then doubled to 2.0. The phase is calculated with the quoted period (always in days) and epoch (BJD). The vertical axis is the nova brightness as measured in flux in electrons s−1. The photometry apertures are either 1 × 1 or 3 × 3 in pixels, with each TESS pixel being 21 arcsec square. These large apertures contain many nearby stars and skylight, with this background light being largely unknowable, and certainly provides almost all of the recorded flux. In this situation, the observed amplitude in flux cannot be usefully converted into an amplitude in magnitudes.
Paper: Limits to Star Formation in Post Starburst Galaxies from Type II Supernovae
Authors: Laetile Makoko, Roberto De Propris
Figure caption: Volumetric supernova rates from X. Ma et al. (2025) and our results vs. Hubble type. Upper limits are indicated by the downward facing arrows and identified in the figure (to the left of each arrow). Error bars from X. Ma et al. (2025) are omitted.
Paper: Growing Pains: Binaries Suppress Planetary Systems at a Young Age
Authors: Zach Werber
Figure caption: Distribution of host star median masses and ages (left) and my calculated binary fractions compared to the literature (right). The vast majority of my sample are solar mass, allowing me to use field binary rates calculated in D. Raghavan et al. (2010) as a comparison against my sample of young systems. β Pic Moving Group binary fractions come from R. A. Lee et al. (2024), while the range of Young Moving Group binary fractions comes from M. Kounkel et al. (2019) and N. Susemiehl & M. R. Meyer (2022). The upper limits on my error bars in binary fraction represent if all RUWE binaries are within 50 au. By assuming the separation of the RUWE binaries is ﹩\sim 0\mathop{.}\limits^{^{\prime\prime} }3﹩ (median points), my results are in agreement with A. L. Kraus et al. (2016). Studies of binary fraction for planet-hosting stars (starred points) have lower rates than the field or young moving groups, meaning that binaries suppress the occurrence of planets.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Relationship Between Eddington Ratio and Column Density in U/LIRG AGN
Authors: Jaya Nagarajan-Swenson, George C. Privon, Aaron S. Evans, Loreto Barcos-Muñoz, Claudio Ricci, Anne M. Medling, Vivian U, Alejandro Saravia, Kara N. Green, Makoto Johnstone, Gabriela A. Meza
Figure caption: GOALS systems in the NH–λEdd plane. Colored symbols show U/LIRG AGN, and light grey contours show BASS AGN (C. Ricci et al. 2022). Sources cycle clockwise in this plane, from (1) an accretion event to (2) an obscured phase, (3) a blowout phase, and (4) an unobscured phase. Dark grey lines delimiting the blowout region from the obscured phase show hypothetical Eddington limits for dusty gas (see C. Ricci et al. 2021, for details), and the horizontal line at NH = 22 represents the maximum possible contribution of a host galaxy to NH.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Color–Magnitude Diagram in the DDO Photometric System
Authors: Graeme H. Smith
Figure caption: Photometric diagrams for the MF81-DR3 overlap sample of field stars. Upper-left panel: the DDO C(45–48) vs. C(42–45) two-color diagram. Upper-right panel: a hybrid Gaia-DDO color (m48 − G) vs. (42–25). Lower-left panel: a color–magnitude diagram in the DDO system, wherein the absolute 48 mag is plotted vs. C(42–45). Lower-right panel: a Gaia-based color–magnitude diagram for the overlap sample.
Paper: Polarimetric Variability Hints at Long-term Structural Changes in CV Ser
Authors: Emma P. Lieb, Jennifer L. Hoffman, Noel Richardson, Anthony F. J. Moffat, Kenneth H. Nordsieck
Figure caption: Polarimetric variations of CV Ser. (a) Spectrum of CV Ser from the RSS data set on 2020 September 9 (gray shaded) with polarization data from the same date (green) and 2018 August 21 (purple) overplotted, binned to 10 Å. (b) Comparison of V-band data in Stokes q − u space, with linear fits to each data set overplotted. The larger, darker point in each cloud represents the error-weighted mean of that data set. We have not removed any interstellar polarization estimates. (c) Same points as in (b), but with shaded regions depicting the 1σ–3σ population statistics of both data sets. RSS error bars represent precision uncertainties obtained by comparing sequential measurements.
Paper: A Stellar Stream around the Spiral Galaxy Messier 61 in Rubin First Look Imaging
Authors: Aaron J. Romanowsky, David Martínez-Delgado, Giuseppe Donatiello, Juan Miró-Carretero, Seppo Laine
Figure caption: M61 in Rubin. (a): 50 kpc stream extends Northward. (b): Zoom-in on plume North-end, showing complex structure. (c): Image-stretch highlighting lower-SB features. Apparent plumes ∼20–30 kpc out on the disk-periphery (arrows) will require confirmation with the full data set. Image credit: RubinObs/NOIRLab/SLAC/NSF/DOE/AURA.
Paper: Prospects for the Crossing of Comet 3I/ATLAS’s Ion Tail
Authors: Samuel R. Grant, Geraint H. Jones
Figure caption: (Upper) Impact parameters for Europa Clipper relative to comet 3I/ATLAS for purely radial SW velocities 200, 450 and 900 km s−1. The minima for the three curves fall between 2025 October 30 and November 6. (Lower) Simulation of 3I/ATLAS’s ion tail on 2025 November 1 assuming a 460 km s−1 radial flow. Positions of Europa Clipper, Sun, Hera, and 3I/ATLAS are shown in a frame where the Sun–Europa Clipper line is fixed. The plane represents that of the ecliptic, with grid lines spaced at 0.1 au. The comet’s position is shown every 6 hr, with legs showing its position north of the ecliptic. Europa Clipper is also north of the ecliptic by 0.069 au. Earth and Mars’s mean orbital distances are included for scale.
Paper: DDO Photometry and the NASA ExEP Star List (2023 Version) for the Habitable Worlds Observatory Mission
Authors: Graeme H. Smith
Figure caption: DDO color–magnitude and two-color diagrams for the NASA ExEP-HWO 2023 listing of main sequence stars. In the right-hand panels symbols are used to designate metallicity: filled triangles for [Fe/H] < − 0.20, filled squares for −0.20 ≤ [Fe/H] < 0.00, open squares for 0.00 ≤ [Fe/H] ≤ 0.20, and open triangles for [Fe/H] > 0.20. Left-hand panels incorporate symbols that designate chromospheric activity level as follows: filled circles (﹩{\mathrm{log}}_{10}\,R{{\prime} }_{{\rm{HK}}}\leqslant -4.80﹩), open circles (﹩-4.80\lt {\mathrm{log}}_{10}\,R{{\prime} }_{{\rm{HK}}}\leqslant -4.50﹩), open pentagons (﹩{\mathrm{log}}_{10}\,R{{\prime} }_{{\rm{HK}}}\gt -4.50﹩). Solid and dashed lines show model colors for a metallicity of [A/H] = 0.0 and +0.5 dex, respectively, from M. Tripicco & R. A. Bell (1991).
Paper: Symmetric Tidal Tails of Galactic Open Clusters
Authors: Songmei Qin, 松梅 秦, Friedrich Anders, Lola Balaguer-Núñez, Yueyue Jiang, 悦悦 蒋, Jing Zhong, 靖 钟, Li Chen, 力 陈, Jinliang Hou, 金良 侯
Figure caption: Leading and tailing tail comparison of 156 OCs within 1 kpc. Left: number of members in the trailing tail versus that in the leading tail (the dashed line indicates identity). Middle: distribution of tail number difference (leading minus trailing). Right: distribution of the normalized asymmetry parameter ϵ.
Paper: Supernova Code Comparison: FLASH and Athena
Authors: Breyton Ambler, Ryan Jeffrey Farber
Figure caption: The first 3 rows show the supernova remnant radius vs. time (left) and respective difference between codes (right). The first row varies resolution. The second row shows simulations with constant 10243 resolution and varies γ = 5/3 and 7/5. The third row varies the initial density of the interstellar medium. The fourth row compares simulations to the analytical solution and a powerlaw fit (left) and respective relative error vs. analytical (right).
Paper: Identification of δ Scuti, γ Doradus Stars and Eclipsing Binaries with TESS
Authors: Ai-Ying Zhou
Figure caption: Examples of newly identified TESS hybrid δ Sct-γ Dor pulsators.
Paper: The Infrared Spectrum of the Stellar Merger V1309 Scorpii One Month After Outburst
Authors: Richard J. Rudy, Ray W. Russell, David K. Lynch, Michael L. Sitko
Figure caption: 0.8–5.1 μm spectrum of V1309 Scorpii from 32 days after discovery. The top panel shows the entire spectrum. The continuum is very similar to that of a late-type M-supergiant. The stronger absorption features are labeled in blue with identifications from M. C. Cushing et al. (2005) and J. T. Rayner et al. (2009). The center and bottom panels focus on the atomic lines in the spectrum. The H I lines, which are purely emission are labeled in black as is the strong Ca II infrared triplet. The Ti I (emission) and Sr II (absorption) features, which are rarely seen, are coded in red and green, respectively. He I emission lines at 1.0830 and 2.0587 μm are present and are also labeled in black. The bandheads of the first overtone of carbon monoxide (12C16O) are marked in blue.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Validation of Two Earth-mass Planets Orbiting GJ 1002
Authors: Paula Andrea Castro Nieva, Sarah Dodson-Robinson, Victor Ramirez Delgado
Figure caption: Top left: Welch’s RV power spectrum estimate from CARMENES and ESPRESSO data. Top right: Welch’s power spectrum estimate from temperature-corrected FWHMs. Bottom left: Welch’s pseudowindow at fb. Bottom right: Results of Monte Carlo period search experiment.
Paper: Notes on Compact Obscured Nuclei. I. The Evolutionary Context
Authors: William A. St. John, John S. Gallagher
Figure caption: Left: mass, distance, and luminosity distributions are displayed for our samples of LIRGs, CT-AGN, and CON-LIRGs. The star marks the location of the uncertain bolometric luminosity of the NGC 1068 Seyfert-2 galaxy, an example of a nearby CT-AGN sharing some properties of CONs. Right: flowchart illustrating possible evolutionary connections between the galaxy samples. The box connects galaxies with similar stellar masses. Although the CON-LIRGs are more luminous than the CT-AGN, arrows show potential evolutionary relationships between CONs, LIRGs, and CT-AGN among galaxies with similar basic characteristics.
Paper: Disentangling the Effects of Temperature, Clouds, and Gravity on K I Doublet in L Dwarfs
Authors: Alexandra J. Baldelli, Genaro Suárez, Kelle L. Cruz, Jacqueline K. Faherty, Austin Rothermich
Figure caption: Top Left: pseudo-Voigt fits (black dashed lines) to the K I doublet at 1.17 μm from Sonora Diamondback model spectra convolved to R ≈ 1000 (green solid lines). Top Middle and Right: average FWHM vs. gravity (middle plot) and average maximum depth vs. fsed (right plot) for model spectra with Teff = 1600 K (L5 spectral types). The Pearson correlation coefficient is shown in the bottom right corner. Bottom: average maximum depth vs. average FWHM for the K I doublet. The colors of “x” indicate temperature, and the circle shades indicate gravity. Dotted lines connect points of the same temperature (by color) and the same gravity (by shade).
Paper: WTP 21aaeuqd: NEOWISE Discovery and Keck Confirmation of a Heavily Reddened, Optically Missed Galactic Nova
Authors: Padmalakshmi Ramesh, Kishalay De, Danielle Frostig
Figure caption: (Left) Discovery images and difference photometry light curves for the transient WTP 21aaeuqd for all data until the 2023 NEOWISE data release. Filled colored squares and circles detections (see legend), while inverted triangles indicate upper limits in the corresponding bands. The inset shows the triplet NEOWISE images corresponding to the peak of the outburst in W2 band, with the science (left panel), reference (middle panel) and difference (right panel) image. (Right) The reduced NIR spectrum of WTP 21aaeuqd, with gray and black lines showing the unbinned and binned spectra respectively. Prominent emission lines identified are marked in the figure.
Paper: AI-enhanced Citizen Science Discovers Cometary Activity on Near-Earth Object (523822) 2012 DG61
Authors: Colin Orion Chandler, Nima Sedaghat, William J. Oldroyd, Maxwell K. Frissell, Chadwick A. Trujillo, William A. Burris, Henry H. Hsieh, Jay K. Kueny, Kennedy A. Farrell, Gennady V. Borisov, Jarod A. DeSpain, Pedro H. Bernardinelli, Jacob Kurlander, Mark Jesus Mendoza Magbanua, Scott S. Sheppard, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes
Figure caption: (523822) 2012 DG61 is centered in each image. The field of view is 126″ × 126″ (a), (c) or 420″ × 420″ (b), with North up, East left. On-sky projected anti-motion (red arrow) and anti-solar (yellow arrow) directions are marked; in all images, an anti-solar oriented tail is evident. (a) UT 2018 April 16, 118.14 s g-band exposure via the 90prime camera on the Steward Observatory 2.3 m Bart Bok telescope (Kitt Peak National Observatory, Arizona). Prop. ID 2015A-0801, PI Xiaohui Fan; observers X. Peng, T. Zhang, Y. Ning. (b) UT 2015 May 14, 14-image co-addition, acquired with a 0.3 m telescope at MARGO Observatory (Crimea-Nauchnij); observer G. Borisov. (c) UT 2024 April 18, co-addition of 4 × 50 s r-band DECam (4 m Blanco telescope, Cerro Tololo Inter-American Observatory, Chile). Prop. ID 2023B-809270, PI Kleyna; observer Wilson Liu.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. XIII. HR 6000 (HD 144667)
Authors: Richard Monier
Figure caption: Left: Absence of the Hg II line at 5677.10 Å (observed UVES spectrum of HR 6000 in black), Right: Synthesis of the 4480–4510 Å range (observed UVES spectrum in black, synthetic spectrum in red).
Paper: Exploring Spica's Apsidal Motion: Insights from Feature Engineering and Machine Learning with MESA
Authors: Hannah C. Woodruff, Dumindu Samaraweera, Jason P. Aufdenberg
Figure caption: (a) Two 1σ (dark) and 2σ (light) observational constraints on Spica A's effective temperature and aspidal motion constant, k2, compared to predictions. The model track from A. P. Odell (1974) (purple, zero-age main sequence near the top of the figure with core hydrogen exhaustion, and beyond, near the bottom) is not consistent with observational parameters from D. Herbison-Evans et al. (1971) (pink), which motivated those models, while the MESA (r7385) model track from A. Claret (2019) (green) is consistent with observational parameters from A. Tkachenko et al. (2016) (gray) including the luminosity and age. A portion of our MESA grid (H. C. Woodruff 2024, yellow), constrained by effective temperature and luminosity uncertainties from A. Tkachenko et al. (2016), shows a spread of predictions due to a range of values for convection mixing length (α) and convective overshooting (fov). (b) Summary of machine learning (ML) and deep learning (DL) methods, including performance metrics: Mean Standard Error (MSE), Root Mean Squared Error (RMSE), goodness-of-fit measure (R2) and Mean Absolute Error (MAE). Random Forrest (RF) and Recurrent Neural Network (RNN) predict MESA output best. The feature importance of parameters in the full MESA grid for predicting k2 are shown as SHapley additive exPlanations (SHAP) values for (c) ML/RF and (d) DL/RNN methods.
Paper: Spurious Oscillatory Signal in Kepler Eclipsing Binary Light Curves
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Eric S. Perlman
Figure caption: Phased Kepler (left) and averaged (right) light curves of KIC 8690104. The oscillatory pattern is evident in both light curves.
Paper: Crossmatching the TESS Eclipsing Binary Catalog with Kepler
Authors: Anirvan Banerjee, Andrej Prša
Figure caption: Left: phase-folded light curves for the 21 Kepler EBs missing from the TESS catalog observed in the first two years of TESS’s operation. Note the varying y-axis scale of normalized flux due to the different eclipse depths. Many different signal types can be seen, with the single shallow eclipse type being most prevalent. Right: list of target TIC IDs and their respective epochs and orbital periods.