adsabs/AstroCLIMB huggingface dataset:
Paper: Hidden Companions to Intermediate-mass Stars. XXVIII. Uncovering a 0.62 M⊙, 0.18 au Companion to Lambda Aquilae 
Authors: Idel Waisberg, Ygal Klein, Boaz Katz
Figure caption: VLTI/GRAVITY interferometric data (colored) of Lambda Aquilae. The best fit binary model is shown in solid black lines and the expected values for a single unresolved star in dashed lines.
Paper: Carbon Monoxide Emission from the 1998 Outburst of the Recurrent Nova V2487 Ophiuchi
Authors: Richard J. Rudy, David K. Lynch, R. C. Puetter
Figure caption: Infrared spectra of the recurrent nova V2487 Ophiuchi. The top panel shows the clear presence of emission from the first overtone of carbon monoxide on 1998 June 19 (plotted in black) and its absence on June 22 (plotted in blue). To enhance the comparison, the 1998 June 22 data, taken from D. K. Lynch et al. (2000), are scaled and plotted with an offset. The top panel also illustrates other spectral changes that occurred along with the disappearance of the CO, notably the increase in the He II lines and the fading of the He I lines (D. K. Lynch et al. 2000). The locations of the stronger H I Pfund series lines are marked since they overlap the CO emission and should be present in the June 19 data, although at a very small level. The bottom panel shows an enlargement of the CO spectral region for the June 19 data together with our model for the CO first overtone emission (plotted, for clarity, with an offset in the flux level). The model is for a CO temperature of 4500 K and 13C/12C = 1.5.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Avoiding (photo-z) Catastrophe
Authors: A. J. Battisti, E. da Cunha, S. Jin, J. A. Hodge
Figure caption: Upper panel : MAGPHYS+photo-z best-fit solutions for three filtersets: F090W − F1800W (green), MIPS24 − VLA1.4 GHz (orange), and all filters (black). Lower panel: Likelihood distributions for zphot (median and 1σ listed) and a few galaxy properties (some uncorrected for lensing magnification, μ). ﹩{E}_{b}^{{\prime} }﹩ describes the 2175 Å feature strength (A. J. Battisti et al. 2019). For JWST-only filters (green), there is a degeneracy where the F090W upper-limit can be interpreted as either a Lyman break or a moderate 2175 Å dust absorption feature, resulting in two zphot peaks (first panel, second row). For filters longer than JWST (orange), the zphot solution is very broad but single-peaked at low-z. Combining all filters (black) provides the tightest constraint on zphot.
Paper: On the Origin of the X-Ray Emission Surrounding PSR B0656+14 in the eROSITA Cal-PV Data
Authors: Alena Khokhriakova, Werner Becker, Peter Predehl, Jeremy S. Sanders, Michael Freyberg, Axel Schwope
Figure caption: The X-ray spectrum of the diffuse emission in the (4–6)﹩{}^{{\prime} }﹩ annulus around PSR B0656+14 fitted with the pulsar’s spectral model, consisting of two blackbody components and a power-law. The solid blue line shows the total source model, while the dashed green and magenta dashed–dotted lines indicate the first and second blackbody components, respectively. The power-law component is not shown, as its contribution is negligible; only an upper limit on its normalization could be derived.
Paper: The Effect of Photometric Errors on the Measured Width of the Main Sequence in Star Clusters
Authors: Steven R. Spangler
Figure caption: The simulated pdf of the residual magnitude Δm with superposed Gaussian errors corresponding to expected noise. The ordinate is the number of simulated stars per bin. The red curve represents the analytic expression, Equation (7).
Paper: Carbon Monoxide Emission in the Early Spectrum of the Nova V7993 Sagittarii
Authors: Richard J. Rudy, John P. Subasavage
Figure caption: Optical and infrared spectroscopy of the nova V7993 Sgr eleven days after peak brightness. The top panel shows the characteristic Fe II lines as well exceptionally strong emission from the Ca II “infrared” triplet. The second and third panels from the top illustrate the richness of the C I line spectrum and the large intensity of it’s peak lines. Infrared Fe II features are present as well although their intensities are unexceptional. The third panel down shows the emission from the first overtone of carbon monoxide (CO). An enlarged view of the CO spectral region is shown in the bottom panel together with a model for the CO emission. The CO model is for a gas temperature of 4000 K and 13C/12C value of 0.8. For clarity, the model is offset vertically from the observations. The 2–0 bandhead of 12C16O is blended with the C I line at 2.2913 μm.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: TIC 318249571.01: A New Hot-Jupiter Transiting Planet Candidate from TESS Data
Authors: Mariana S. Bittencourt, Stela Ishitani Silva, Clécio R. Bom, Greg Olmschenk, Veselin Kostov, Diogo P. L. Carvalho, Helem Salinas, Gabriel Teixeira, Richard K. Barry
Figure caption: (a) SPOC FFI Sector 38 lightcurve; (b) Sector 65 DAVE centroid analysis: mean difference image (upper left), mean out-of-transit image (upper right), mean in-transit image (lower left), and signal-to-noise ratio of the mean difference image (lower right); (c) Sector 38 DAVE output for the flux (ppm) per phase for odd and even transits; (d) Phase-folded lightcurve with best-fit MCMC model in orange; (e) Corner plot with results of the MCMC exploration for the fitted parameters: periastron ω (radians), orbital eccentricity e, planet radius Rp (Jupiter radii), impact parameter b, mid-transit t0 (days) and orbital period (days).
Paper: Meet Arjuna 2025 PN7, the Newest Quasi-satellite of Earth
Authors: Carlos de la Fuente Marcos, Raúl de la Fuente Marcos
Figure caption: The top panels show the time evolution of the relative mean longitude with respect to Earth, λr, for Cardea, Kamo‘oalewa, 277810, 2013 LX28, 2014 OL339, 2023 FW13, and 2025 PN7. The origin of time is the epoch 2460800.5 JD Barycentric Dynamical Time (2025 May 05.0 00:00:00.0 TDB), which is the epoch of the orbit, and the output step is 15 days. The bottom panel maps the known quasi-satellites within the dynamic context of the Arjuna asteroid belt: Cardea (gold point), Kamo‘oalewa (red), 277810 (orange), 2013 LX28 (yellow), 2014 OL339 (violet), 2023 FW13 (pink), and 2025 PN7 (lime). The median value of λr in the year interval (2000, 2050) is displayed as ﹩{\lambda }_{{\rm{r}}}^{* }﹩, the equivalent value for the semimajor axis is a*. Error bars correspond to the 16th and 84th percentile values of the distributions. The two red dashed vertical lines show the Hill radius, the black horizontal line shows the angle 0°and the blue ones signal ±60°. Data source: JPL’s Horizons and SBDB.
Paper: Ks-band Photometry of the Extreme T Subdwarf CWISE J221706.28−145437.6 
Authors: Jerry J.-Y. Zhang, 俊䶮 章, Nicolas Lodieu, Eduardo L. Martín
Figure caption: WISE2217’s field (the small panel), photometry (red diamonds and magnitude values), with those of the benchmark esdT WISE1810 (blue circles) and its spectrum (black). The relative photometry of the two objects is aligned in the J band. WISE2217’s absolute photometry (yellow diamonds) is also scaled to WISE1810’s J-band photometry. The uncertainty of the absolute photometry is mainly from the parallax uncertainty.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å. XXIII. HD 90264 B (L Car)
Authors: Richard Monier
Figure caption: Left: synthesis of the Hg II line at 3983.93 Å of HD 90264 B (observed spectrum in black, synthetic spectrum in red), Right: synthesis of the Hg II line at 5677.10 Å.
Paper: Mass- and Metallicity-dependent Changes in Stellar Hydrogen Luminosity after Low-mass Brown Dwarf Engulfment
Authors: Pranav Siddineni, Parker Johnson
Figure caption: Log of stellar hydrogen luminosity over time, from the start of the simulation, for each brown dwarf mass and stellar metallicity.
Paper: A Weak-moderate Solar Cycle 25 is Confirmed
Authors: M. C. Gallego, A. J. P. Aparicio, V. M. S. Carrasco, J. M. Vaquero
Figure caption: Comparison of the temporal evolution of the last 25 observed solar cycles. The thick black line represents Solar Cycle 25, based on the observed 13 months smoothed monthly values of the sunspot number. All other solar cycles are overlaid and aligned at their respective starting points to facilitate comparison.
Paper: A Case of the Lensed AGN ULAS J081621.49+213442.65 at z ∼ 7.45 Confused with an Asteroid
Authors: Ekaterina Koptelova, Chorng-Yuan Hwang
Figure caption: (a) 88″ × 44″ UKIDSS J-band leavstack cutout from 2008 November 28. The positions of the moving object MObjHK2008-11-27 are marked with crosses. (b) Corresponding difference image between the UKIDSS J-band images of 2008 and 2007. The newly identified object is labeled MObjJ2008-11-28. (A FITS file of the full analyzed region is available as the data behind the figure.) (c) UKIDSS Y and J-band cutouts from 2008 November 28 (upper panels) in comparison with the UKIRT K-band 90-s cutouts from 2024 February 10 (lower panels) during brightening at the same positions. (d) Astrometry of J0816+2134 A1, A2, B, and C (magenta). Overplotted with blue and green are the UKIDSS positions in the Y- and J-band data of 2008, respectively. The positions of the intensity peaks in the sequence of single-exposure UKIDSS J-band frames (green data points) are connected by a red line, illustrating the corresponding astrometric shifts. Similar shifts along the A1A2 arc were measured in the K band on 2024 February 10 (black data points). The relative positions of the lensed components of J0816+2134 in panel (c) are marked with crosses. In all panels, north is up and east is to the left.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: No Turnover Found in Giant-Planet Occurrence Within 3 au Around Low-mass Stars
Authors: Katherine L. Gonglewski, Galen J. Bergsten, Ilaria Pascucci, Renu Malhotra, Gijs D. Mulders, Jamie Dietrich, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Remo Burn, Christoph Mordasini
Figure caption: Occurrence rate of GPs, defined as ﹩dN/d{\rm{ln}}\,a﹩ (number of planets per star per unit ﹩{\rm{ln}}a﹩), as a function of semimajor axis a, in astronomical units. Left: IDEM rates and NGPPS population-synthesis predictions. Right: Median joint occurrence model (black, ﹩\frac{dN}{d{\rm{ln}}a}\propto {a}^{\beta }﹩) with posterior samples (grey) fit to the Kepler, K2, and CLS planet populations. Shaded bands mark the sensitivity regimes for Gaia astrometry and direct imaging (DI), along with corresponding model-predicted occurrence rates.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. XV. HD 79158 (36 Lyncis)
Authors: Richard Monier
Figure caption: Left: Comparison of the observed NARVAL I profile of 36 Lyncis in the range 4420–4500 Å (observed profile in black, synthetic spectrum in red), Right: Same comparison in the range 4510–4560 Å.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. XVI. HD 33904 (μ Lep)
Authors: Richard Monier
Figure caption: Left: synthesis of the Hg II line at 5677.10 Å (observed FEROS spectrum of μ Lep in black, synthetic spectra in red) Right: synthesis of the the same line in a HARPS spectrum of μ Lep.
Paper: Palomar and Apache Point Spectrophotometry of Interstellar Comet 3I/ATLAS
Authors: Matthew Belyakov, Christoffer Fremling, Matthew J. Graham, Bryce T. Bolin, Mukremin Kilic, Gracyn Jewett, Carey M. Lisse, Carl Ingebretsen, M. Ryleigh Davis, Ian Wong
Figure caption: Left: Palomar and Apache Point imaging and spectroscopy. 3I/ATLAS has a red spectrum in the visible that becomes more neutral at longer wavelengths. Right: comparison between our combined and binned 3I/ATLAS spectrum and 1I from A. Fitzsimmons et al. (2018) and 2I from J. de León et al. (2020). 3I/ATLAS appears roughly consistent with 2I/Borisov. Area used to normalize spectra shown as faint dotted lines. All error bars are 1σ.
Paper: Updated Mutual Inclination Measurement for 14 Her b and c
Authors: Guang-Yao Xiao, Fabo Feng
Figure caption: Panel (a): Best-fit to RVs of various instruments. Panel (b): RV residuals. Panel (c): Best-fit to Hipparcos, Gaia DR2 and DR3 astrometry. The black thick line denotes the optimal orbit of 14 Her, while the arrow indicates its direction of motion. Panel (d): Zoom in on the rectangle region of panel (c) where depicts the best fit to Gaia GOST data. Panel (e): Residuals of Hipparcos abscissa. The brightness of points gradually increases with observation time. Panel (f): Best-fit to JWST data. 50 orbits are randomly drawn from the MCMC chain. Panel (g): Posterior distribution of ψ between the orbits of 14 Her b and c, compared to the prior, G. F. Benedict et al. (2023) (Benedict2023) and D. C. Bardalez Gagliuffi et al. (2025) (BG2025). Panel (g): PMa significance map between Gaia DR2 and DR3. The short-scale astrometric variation induced by 14 Her b is very significant.
Paper: Peculiar Stellar Ages of the Peculiar Dwarf Galaxy NGC 5474
Authors: Liv Moody, Ray Garner
Figure caption: Top left: the broadband B image of NGC 5474 (J. C. Mihos et al. 2013). Top right: the narrowband continuum-subtracted Hβ image; white indicates emission and black indicates absorption. In both panels, the blue circle defines the bulge, the inner green circle defines the main disk and the outer circle defines the outer disk, both centered on the kinematic center (B. K. Rownd et al. 1994). Bottom left: the Hβ and [O II] EWs of the main disk and bulge. The main disk is colored by radial distance from the kinematic center. The lines are different modeled SFHs (see text). Bottom right: same as the bottom left, but with density contours in three radial ranges and the bulge. Characteristic errors are given to the left in each panel.
Paper: XRISM Observations of the Cooling Flow Cluster A2029 Support Heating by Mixing
Authors: Noam Soker
Figure caption: A temperature map with radio contours of A2029 adapted from T. E. Clarke et al. (2004). The temperature scale is by the color bar in keV; 1″ corresponds to 1.45 kpc. I draw the approximate distance to which the turbulence can carry hot gas within one (black) and two (red) cooling times, where τcool(0) = 6 × 107 yr.
Paper: Discovery of Photodissociation Region in Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Kyle W. Cook, William C. Keel, Rogier A. Windhorst
Figure caption: Top left: the AV map of the PDR. Top right: the ﹩{R}_{\widetilde{VI}}﹩ (see Equation (2)) map. Bottom left: the JWST F356W image of the PDR, circled in gold. Bottom right: the ICA map from the JWST F356W and F444W filters. On the AV and ICA maps, the HST F336W intensity is overlaid as a contour where: cyan = 0.003 counts (photons) per second (cps) and the magenta = 0.007 cps. The bottom panel is illustration of the use of the available HST and JWST data on the PDR.
Paper: SPHEREx Discovery of Strong Water Ice Absorption and an Extended Carbon Dioxide Coma in 3I/ATLAS
Authors: C. M. Lisse, Y. P. Bach, S. Bryan, B. P. Crill, A. Cukierman, O. Doré, B. Fabinsky, A. Faisst, P. M. Korngut, G. Melnick, Z. Rustamkulov, V. Tolls, M. Werner, M. L. Sitko, C. Champagne, M. Connelley, J. P. Emery, Y. R. Fernandez, B. Yang
Figure caption: (a) SPHEREx 0.75–5.0 μm 2 pixel radius aperture spectrophotometry (left) and solar spectrum corrected reflectance (right) for 3I. Red arrows denote possible significant background contamination due to known background sources. The arrows start at the measured flux+1σ. For the reflectance, the NASA-IRTF/SpeX 0.7–2.5 μm spectrum (green) is overlaid. The two sets of measurements are consistent, and characterized by a slightly rising slope from 0.7 to 1.0 μm, a flat regime from 1.0 to 1.5 μm, a shallow absorption at 1.5 and 2.1 μm, and a strong falloff starting at 2.4 μm. The SPHEREx spectrophotometry stays low from 2.5 to 5.0 μm, with a huge uptick at 4.3 μm due to CO2 gas emission. Also overlaid for comparison is the average “cliff” KBO spectrum of N. Pinilla-Alonso et al. (2025) (pink). (b): Stacked 1.0–1.5 μm SPHEREx geometry- and solar flux-corrected image of 3I. Assuming the reflectance is flat across these wavelengths, this median stacking produces a deep image of the nucleus + dust scattered light continuum flux from 3I. There is no significant extension found in the stacked image beyond a stellar point source in a SPHEREx 6﹩\mathop{^{\prime\prime} }\limits_{.}﹩15 pixel. (c)–(e): SPHEREx images centered at the H2O/CO2/CO coma gas wavelengths of 3.0/4.26/4.7 μm, respectively. 3I is undetected in H2O and CO, with 2 pixel radius preliminary conservative upper limits of 0.45 and 0.99 mJy. By contrast, a bright CO2 coma with central PSF flux = 33 mJy that extends out to at least 30 pixel (348,000 km) was found. This observed minimum size for the CO2 coma corresponds to ∼700,000 s mean lifetime at vgas = 0.48 km s−1. The reported photodissociation lifetime for CO2 at 1 au is 135 hr = 486,000 s (W. Huebner et al. 1992), which scales by ﹩1/{r}_{h}^{2}﹩ to ∼ 4,670,000 s at 3.2 au. (f): Azimuthally averaged radial profile for the SPHEREx 3I CO2 coma. The observed falloff with projected distance is steeper than 1/ρ, closer to 1/ρ3/2, which is consistent with a near-nucleus source of CO2 coupled with photodissociation + charge exchange ionization processing of free-flying molecules in the coma.
Paper: Mapping Gamma-Ray Bursts: Distinguishing Progenitor Systems Through Machine Learning
Authors: Sharleen N. Espinoza, Nicole M. Lloyd-Ronning, Michela Negro, Roseanne M. Cheng, Nicoló Cibrario
Figure caption: (a) Top left: GRBs with known radio afterglow classification; radio-bright GRBs are shown in gold, radio-dark in navy. (b) Top right: low-luminosity GRBs (llGRBs) with L < 1049 erg s−1, overlaid in purple (c) Bottom: continuous gradient of T90 durations for all 2511 GRBs; the longest duration GRBs appear to cluster in a distinct region in the head.
Paper: A Refined Orbital Ephemeris for the Intermediate Polar FO Aquarii and Evidence for a Period Derivative
Authors: Peter Garnavich, Jordan Tweddale, Colin Littlefield
Figure caption: Left: The dark points show one of the recent light curves of a FO Aqr obtained from the SLKT. This light curve covers approximately one binary orbit, while the rapid modulation results from the spinning white dwarf. The solid line plotted on the points is a light curve model constructed from L–S analysis. The difference between the data and model is plotted as a solid line below the light curve. The vertical line marks the measured time of the eclipse in the residual light curve. Right: The difference between the observed time of eclipse and the time calculated from the updated linear ephemeris in Equation (1). The K2 and TESS timings are shown with star symbols. The solid line displays a quadratic fit to the residuals that implies the orbital period of FO Aqr is increasing.
Paper: Comparison of Australasian Tektites with Australasian Microtektites and BeLaU Spherules Recovered from the Ocean
Authors: Eugenia Hyung, Emma Levy, Loralei Cook, Stein B. Jacobsen, Abraham Loeb, Jayden Squire, Juraj Farkas
Figure caption: Panel (a) Primitive-mantle normalized (using W. F. McDonough & S. S. Sun 1995 values) elemental compositions of Australasian tektites compared to the UCC (R. L. Rudnick & S. Gao 2014), arranged in order of most incompatible to most compatible elements. Panel (b): The UCC-normalized elemental patterns of the individual tektites (red, green, blue, and orange) and the average of the four specimens (white symbols, black line). The number “1” represents the UCC (dark symbols), plotted alongside the average BeLaU abundance pattern (white symbols, gray line) normalized with respect to the UCC. Panel (c): Australasian-tektite normalized elemental compositions of BeLaU (white circles) and microtektites (gray squares; L. Folco et al. 2018). Here, the number “1” (black circles) represents the average of the Australasian tektites measured in this study.
Paper: JAM 1: Discovery of a New Candidate Evolved Planetary Nebula in Deep [O III] and Hα Imaging
Authors: J. A. Manuel, D. Jones, M. Santander-García
Figure caption: Discovery images of the candidate planetary nebula JAM 1.
Paper: Modeling Supernova 2023ixf: Lightcurve Degeneracies and Morphological Differences
Authors: Shannon Forde, Jared A. Goldberg
Figure caption: Left: Families for SN 2023ixf: Mej(top), Menv(middle), and ﹩{E}_{{\rm{\exp }}}﹩(bottom) as a function of R, shading the 11% modeling uncertainty (GBP19). The GB20 stellar model grid is overlaid, with color indicating MZAMS from 10 to 25M⊙ (lighter colors = lower MZAMS). Upper Right: Lightcurve for the explosion of an MZAMS = 11M⊙ model taken from the Mej grid, compared to SN 2023ixf’s bolometric lightcurve (E. A. Zimmerman et al. 2024, purple). Lower Right: Lightcurves for MZAMS = 23M⊙ models with different wind efficiency parameters. The gray shaded region indicates the circumstellar-interaction phase, where we do not expect agreement between these models and observations.
Paper: SKYSURF-7: Exploring PSF Contamination in Diffuse Sky Measurements with HST
Authors: Logan R. Conrad, Rosalia O'Brien, Delondrae Carter, Alex Pigarelli, Rogier A. Windhorst, Timothy Carleton, Seth H. Cohen, Rolf A. Jansen, Rafael Ortiz
Figure caption: Comparison of the difference between recovered and input sky-SB as a function of the sky-SB level for a modeled Gaussian PSF, and an empirical HST PSF. Each data point represents a single image. The blue triangles represent realistic HST PSF data, and the red squares represent the modeled data. We calculate the PSF leak by using the difference in measured sky value and input value. Assuming a retrieved value of 0 has no contamination, the average values would represent the average contamination from a PSF. The result in total contamination of 0.00054 MJy sr−1. A portion of this value is noise, so we compare it to the modeled Gaussian PSF .
Paper: Upper Limits on GeV Gamma-Ray Flux from the Ultra-long Period Neutron Star PSR J0901−4046
Authors: Anne Duerr, Henrike Fleischhack, David Kieda
Figure caption: The gamma-ray luminosity vs. spin-down power of PSR J0901−4046 (upper limit) and the third Fermi pulsar catalog (D. A. Smith et al. 2023).
Paper: Apparent Change in Comet 103P/Hartley 2’s Rotation Period During 2023/2024 Measured via Aperture Photometry
Authors: Thomas Lehmann
Figure caption: Top: Calibrated apparent magnitude in a 5000 km radius aperture using the green filter. The size of points approximately corresponds to the average uncertainty of a magnitude estimate (2σ level). The line represents a model curve ﹩m=14.2+5{\rm{log}}(\Delta )+4.5\ast 2.5{\rm{log}}({r}_{{\rm{H}}})﹩ where Δ is geocentric distance (au) and rH is heliocentric distance (au). The photometry covering epochs a to d in this figure is available as Data behind the Figure. Middle: Lomb–Scargle periodograms for the subsets of data labeled a to d in the top panel, with the most probable period indicated at the top of the plot. Bottom: Phase plots corresponding to the date range and best period in the periodogram above, with zero phase set to the time of perihelion. The point colors are the same in the top and bottom panels. The legend gives telescope IDs (see Section 2).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)