adsabs/AstroCLIMB huggingface dataset:
Paper: The Recurrent Nova V745 Sco had a Classical Nova Eruption in 1897 July
Authors: Bradley E. Schaefer
Figure caption: Plate B19719 showing the 1897 eruption of V745 Sco. V745 Sco is indicated with the blue arrow, with the exact position of the nova being 0.″6 away from the middle of the image. Importantly, the V745 Sco image has an eccentricity of 0.27 stretched WNW–ESE, with this being the same ellipticity and orientation as nearby stars. Importantly, the point-spread-function of the V745 Sco image (i.e., a sharp-edged smooth ellipse saturated in the center) is the same as for nearby stars. Five comparison stars are labeled with their B magnitudes from APASS. This close-up from the DASCH scan is 600″ on the sides, with north up and east to the left.
Paper: Spectral Typing with Artificial Intelligence: Classifying Low-resolution Near-infrared Spectra of Standard M/L/T Dwarfs
Authors: Tianxing Zhou, Christopher A. Theissen, Adam J. Burgasser, William M. J. Best, S. Jean Feeser
Figure caption: (Top panels): Classification error as a function of true spectral type for RF (left) and kNN (right) models, defined as true minus predicted classification. The statistics shown are the median (orange lines), mean (green diamond), and 25%–75% quantiles (box). Circles indicate individual outliers (±1.5 times the range of the quantile box). The highlighted gray region indicates ±1 subtype. The numbers in parentheses along the abscissa axis are the number of sources within each subtype group in the test set. (Bottom panel): All standard spectra plotted with feature importance scores, showing the relative importance of each feature (wavelength intervals) in predicting the classification. The gray region indicates telluric absorption regions that were masked out.
Paper: X-Ray Observations of the Zwicky 3146 Galaxy Cluster Reveal a 3.5 keV Excess
Authors: Sunayana Bhargava, Paul Giles, Kathy Romer, Tesla Jeltema, Devon Hollowood, Matt Hilton
Figure caption: Single temperature model fits from XMM-Newton (left) and Chandra (right) spectra for Zw3146 that show a fit improvement above 3σ (blue region) in the energy range of interest (green shaded region). For each plot, the top panel (red line) shows the change in fit statistic ΔC as a function of energy in the range 3–5 keV. The bottom panels (green line) show the fitted normalization of the Gaussian line and corresponding errors. The XMM observation ID is 0605540301 (cleaned exp time 34.1 ks); the Chandra observation is 9371 (cleaned exp time 39.7 ks).
Paper: Exogenous Carbon is Unlikely to be the Source of Methane Microseepage Emissions on Mars
Authors: John E. Moores, Haley M. Sapers, Andrew C. Schuerger
Figure caption: Neither degradation mechanism allows IDPs to supply the needed methane to explain microseepage seepage emissions at Gale. The UV-CH4 model cannot supply sufficient methane even in locations where dust accumulates (panel (A)). Thermal degradation requires too much buried carbon drawn from too large an area or unrealistically high temperatures or both (panel (B)). Map centered on Gale Crater with 10° graduations (Fergason et al. 2018).
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars: Paper I—HD 35548 and HD 89822
Authors: Richard Monier
Figure caption: Left: line synthesis of the Hg II line at 5677.10 Å of HD 35548 (observed spectrum in black, synthetic spectrum in red), Right: same comparison for HD 89822.
Paper: Consolidated Rotation Measure Catalog Update
Authors: Anthony Nuñez, Mehrnoosh Tahani, Susan E. Clark, Enrique Lopez-Rodriguez, Cameron L. Van Eck
Figure caption: The background color shows H I column density obtained by the HI4PI survey (HI4PI Collaboration et al. 2016). The circles and triangles show our corrected RM coordinates and those in the Van Eck et al. (2023) consolidated catalog, respectively. Red (blue) illustrates negative (positive) RM values. Top panel shows the RM observations by Minter & Spangler (1996). Lower panel shows the RM observations by Clegg et al. (1992). One of the RM values is not illustrated on the plot due to large angular separation from the rest of the observations. The differences between the RMs in the lower panel are due to discrepancies between the significant figures used in the Clegg et al. (1992) and Van Eck et al. (2023) catalogs. As a result, different nearby points from Clegg et al. (1992) overlapped and were treated as one point in Van Eck et al. (2023).
Paper: A Lack of Mass-gap Compact Object Binaries in APOGEE
Authors: Meir Schochet, Jamie Tayar, Jeff J. Andrews
Figure caption: We show that our pipeline can identify RV variability from Doppler shifts in previously ((a), Thompson et al.) and newly (b) identified systems. We show the regime (c) where our systems are found and demonstrate that our different mass estimates do not completely agree (d). We show that our detected companions are consistent with expected-trends with mass (e) and metallicity (f).
Paper: Frequency-resolved Lag Predictions of the Corona-heated Accretion-disk Reprocessing Model Agree Well with the UV/Optical Reverberation Mapping of Mrk 817
Authors: Jie Chen, Mouyuan Sun, Shuying Zhou
Figure caption: Simulated frequency-resolved lags in Mrk 817. The frequency range is 0.008–0.999 day−1. The purple curves represent the median lags in the 512 CHAR simulations. Black dots with error bars are the frequency-resolved lags and their 1σ uncertainties from C. Lewin et al. (2024). The simulated frequency-resolved lags for Mrk 817 from the CHAR model without free parameters are well consistent with observations.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. VIII. HD 175640
Authors: Richard Monier
Figure caption: Left: synthesis of the Hg II line at 5677.10 Å (observed spectrum in black, synthetic spectra in red (+4.00 dex) and blue (+4.40 dex)) Right: emission lines of Ti II at 6106.48 and 6102.55 Å.
Paper: GHOST Reduced Data Products for the Gemini Observatory Community and Beyond
Authors: Vinicius M. Placco, David Herrera, Brian M. Merino, Paul Hirst, Kathleen Labrie, Chris Simpson, James Turner, William D. Vacca, Emily Deibert, Ruben Diaz, Jeong-Eun Heo, Venu Kalari, Henrique Reggiani, Cinthya Rodriguez, Roque Ruiz-Carmona, Joanna Thomas-Osip
Figure caption: GHOST raw science (standard resolution, 2 × 4 binning—first row) and calibration (flat field and arc lamp—second row) data. Bottom panels: blue and red DRAGONS-reduced spectra used for quality assessment (_dragons.fits files).
Paper: GRANDMA Observations of SN 2023wrk, a Luminous Type Ia Supernova with Significant Unburned Carbon in the Outer Ejecta
Authors: Cristina Andrade, Pierre-Alexandre Duverne, Jialian Liu, Felipe Navarete, Abdelaziz E. Abdelaziz, Mohamed Abdelkareem, Ilmah Abdi, Mohamed Aboueisha, Christophe Adami, Shabnam Agayeva, Vova Aivazyan, Leandro de Almeida, Dalya Akl, Sarah Antier, Yvan Arnaud, Saad A. Ata, Wageeh A. Badawy, Chunhai Bai, Reda Bendary, Zouhair Benkhaldoun, Kevin Borrot, Eric Broens, Yongzhi Cai, Olivier Clerget, Wagner Corradi, Michael W. Coughlin, Nicolas Delaunoy, Franky Dubois, Jean-Grégoire Ducoin, Eslam Elhosseiny, Thomas M. Esposito, Ali Esamdin, Pascal Foulon, Roland Foulon, Michael Freeberg, Charles Galdies, Priyadarshini Gokuldass, Bruno Guillet, Gamal M. Hamed, Bruno Haremza, Patrice Hello, Yasser Hendy, Patrick Huth, Raguli Inasaridze, Abdusamatjan Iskandar, Aziz Kaeouach, Tarek M. Kamel, Sergey Karpov, Raymond Kneip, Nino Kochiashvili, Petri Kuossari, Liping Li, Xin Li, Jinzhong Liu, Markus Lorber, Raouf H. Mabrouk, Denis Marchais, Elisabeth Maris, Isabel Márquez, Martin Mašek, Roger Ménard, Nicola Meneghelli, Mike Mitchell, Kanthanakorn Noysena, Mohammad Odeh, Wataru Ono, Gérard Parent, Bruce Parker, Julien Peloton, Adam Popowicz, Thierry Pradier, Stephen Price, Oleksandra Pyshna, Yodgor Rajabov, Fadi Saibi, Sophie Saibi, Denis Saint-Gelais, Nelio Sasaki, Marc Serrau, Masao Shimizu, Ahmed Shokry, Andrii Simon, Oleksii Sokoliuk, Ali Takey, Manasanun Tanasan, Yusuf Tillayev, Giuseppe Di Tommaso, Iara Tosta e Melo, Damien Turpin, Xiaofeng Wang, Zhenyu Wang, Ibrahim Zead, Jujia Zhang
Figure caption: The left panel shows the UV/Optical photometric lightcurves obtained by GRANDMA and kilonova-Catcher. The plots also includes the Swift observations of SN 2023wrk. The right panel corresponds to the various spectra obtained by GRANDMA OHP and TNG facilities along with the KNC observations.
Paper: Detecting Novel Damped Lyα Absorbers in the Intergalactic Medium
Authors: Katherine C. Lee
Figure caption: (A) Example of artificial data generation, starting with raw spectrum cropped, continuum fitting and normalization, insertion of the Voigt profile, and final product after noise generation. (B) Example of a newly found DLA (J003001.62+275458.8). (C) Example of Voigt profile fitting for column density measurements (green: weighted points). (D) Example of normalization with continuum fitting.
Paper: No Missing Flare in OJ 287
Authors: Mauri J. Valtonen
Figure caption: The optical light curve of OJ 287 during 2005 in V-band mJy units, in averaged data points. The dashed-line curve gives the general outline. If the disk levels and the impact distances were the same in 2005 and in 2022, one can draw an upper scale for the expected light curve in 2022 (M. J. Valtonen et al. 2021).
Paper: Additional Doppler Monitoring Corroborates HAT-P-11c as a Planet
Authors: Samuel W. Yee, Erik A. Petigura, Howard Isaacson, Andrew W. Howard, Sarah Blunt, Paul A. Dalba, Fei Dai, Benjamin J. Fulton, Steven Giacalone, Stephen R. Kane, Molly Kosiarek, Teo Močnik, Malena Rice, Ryan Rubenzahl, Nicholas Saunders, Dakotah Tyler, Lauren M. Weiss, Jingwen Zhang
Figure caption: Top: RVs of HAT-P-11 after subtracting the best-fitting model for the inner transiting planet b and a linear correlation with the S HK index. Data collected after Y18 are shown as squares. Error bars include a jitter term added in quadrature to the measurement uncertainties. The blue line shows the best-fit model for the stellar reflex motion due to planet c. Middle: Residuals to the best-fit two-planet model. Bottom: S HK time series for HAT-P-11, which does not show a coherent long-term periodicity. The data and best-fit model parameters are available as 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. X. HD 221507 (β Scl)
Authors: Richard Monier
Figure caption: Left: synthesis of the Hg II line at 5677.10 Å (observed FEROS spectrum of β Scl in black, synthetic spectra in red) Right: synthesis of the same wavelength range for the UVES spectrum of β Scl.
Paper: Spatially Resolved Stellar Populations of z = 3–6 Lyα-emitting Galaxies with CEERS JWST NIRCam Imaging
Authors: Turaba Rahman, Intae Jung, Abdurro'uf, Henry C. Ferguson, Fabio Pacucci, Nimish P. Hathi, Anton M. Koekemoer
Figure caption: (a): A sample 2D maps of properties (Galaxy ID = 70583) with centers marked as red crosses. (b): SFR vs. M* of our sample galaxies. The color coding illustrates redshift grouping. Solid lines show SFMS relation, corresponding to different redshifts as marked by red, blue, and green colors. (c): Radial profiles of sample galaxies. Multi-colored lines represent individual galaxies, thick black lines represent the median trends, light gray lines represent 1σ errors of the medians, thick blue and magenta lines represent the median trends of the galaxies above/on and below SFMS lines, respectively.
Paper: V1663 Aquilae: A Fast Fe II-type Nova that Formed Dust and Coronal Lines
Authors: Richard J. Rudy, Ray W. Russell, David K. Lynch, R. C. Puetter
Figure caption: Optical and infrared spectra of the nova V1663 Aquilae. The July spectrum, from 36 days after maximum brightness, is shown in blue while the November spectrum, from 157 days, is in black. The top panel compares the two epochs to highlight the change in the spectral continuum produced by dust emission. The middle panel presents a portion of the July spectrum illustrating the prevalence of lines from neutral species, a signature Fe II feature, the dominance of the fluorescently excited O I lines at 0.8846 μm and 1.1290 μm (in red), and a single forbidden line, [N I] 1.0405 μm. The bottom panel displays the infrared portion of the November spectrum, emphasizing the coronal lines (labeled in green) and the clear rise in the continuum toward longer wavelengths produced by emission from hot dust. He I 1.0830 μm, weakly present in the July spectrum, is the dominant emission line feature in November. O I lines are much diminished but still detectable.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Far-ultraviolet Spectrum of FU Ori South
Authors: Adolfo S. Carvalho, Gregory J. Herczeg, Kevin France, Lynne A. Hillenbrand
Figure caption: The UV spectrum of FU Ori S, compared with that of BP Tau. Emission lines commonly seen in the spectra of accreting T Tauri stars are marked in vertical solid light blue lines. The dotted line shows the location of the feature at 2775 Å. Between 1400 and 1550 Å the H2 emission lines are marked by cyan vertical lines, some of which are almost as bright as the C IV doublet at 1548/1550 Å.
Paper: On the Dynamical Erasure of Initial Conditions in Multi-planetary Systems
Authors: Kevin Marimbu, Eve J. Lee
Figure caption: Under merger events, the orbital period distribution flattens over ∼10–100 Myr. The immediate loss of planets inside ∼10 days is likely unphysical from our neglect of general relativistic precession and tidal circularization. Similarly, the period ratio distribution broadens over time reaching a broad peak near 3:2.
Paper: Validating Gaia DR3 Pulsating Variable Classifications with TESS. II. 360+ Eclipsing Binaries with δ Scuti and γ Doradus Components
Authors: Ai-Ying Zhou
Figure caption: Examples of newly identified Algol-type (detached) eclipsing binary systems containing pulsating components of types δ Sct, γ Dor and SPB. All graphs were generated during automated batch processing.
Paper: No Pulsar Timing Noise from Brownian Motion of the Sun
Authors: James M. Cline
Figure caption: Angular correlation function of pulsar timing frequency residuals for random choices of the velocity perturbation  V . Left:  V  is allowed to vary over 4π. Right:  V  is restricted to the plane of decl. zero, roughly aligned with the ecliptic. Legend shows relative contribution of quadrupole vs. dipole in best fit.
Paper: NICER Observes the Full Z-track in GX 13+1
Authors: Mohamad Ali Kaddouh, Malu Sudha, Renee M. Ludlam
Figure caption: HIDs of all the observation sets over-plotted on the full track from the one observation set shown in panel (d). Panel (h) shows the PDS with the peaked noise component seen in the highlighted portion of panel (b).
Paper: Identifying Uncertainties in Stellar Evolution Models Using the Open Cluster M67
Authors: Susan Byrom, Jamie Tayar
Figure caption: (a), (b), (c), and (d) are Kiel diagrams of the open cluster M67. Isochrones generated at [M/H] = 0.00 are shown for 4, 5, and 6 Gyr. Stars from M67 were treated as field stars to estimate their ages, which are shown by the colorbar. (e) shows age as a function of surface gravity for all four models. Vertical dashed lines indicate the approximate boundary between main sequence, subgiant, and red giant stars. The age estimates for each model are fitted with LOWESS non-parametric smooth curves. Notably, the GARSTEC red giant age estimates are near the predicted age of M67, and all models have similar behavior on the subgiant branch. In subfigure (f), model-generated mass estimates for M67 red giants are compared to D. Stello et al. (2016) asteroseismic mass estimates for red giants.
Paper: Citizen Scientists Discover “Asteroid in a Cometary Orbit” 2010 MK43 has a Comet Tail
Authors: Jay K. Kueny, Colin Orion Chandler, Maxwell K. Frissell, William J. Oldroyd, Chadwick A. Trujillo, William A. Burris, Kennedy A. Farrell, Nima Sedaghat, Henry H. Hsieh, Jarod A. DeSpain, 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: 2010 MK43 (center) in these r-band DECam images. The FOV is 63″ × 63″, with North up and East left; anti-motion (yellow arrow) and anti-solar (red-outlined black arrow) directions are shown. All images acquired with DECam on the 4 m Blanco telescope at the Cerro Tololo Inter-American Observatory (CTIO) in Chile as part of Prop. ID 2024A-755342, PI Shen. Each image shown is a co-addition of 1 × 175 s g-band + 1 × 150 s g-band + 1 × 200 s i-band. In both images a short, diffuse tail is clearly visible oriented toward roughly 11 o’clock. (a) UT 2024 February 12 (observer M. Verrico). (b) UT 2024 February 18 (observer Kevin Luhman).
Paper: Examining the Rotation of the Planet-hosting M Dwarf GJ 3942
Authors: Andrew Fonseca, Sarah Dodson-Robinson
Figure caption: Top left: The Fisher-transformed magnitude-squared coherence estimate from RV and Hα has peaks at frequencies 1/32 day−1 and 1/16 day−1. Top right: TESS PDCSAP photometry of GJ 3942 from Sector 52 shows evidence for rotational modulation. Lower left: Average periodogram from seven TESS light curves. Vertical lines indicate local maxima that may correspond to rotation harmonics. Lower right: ﹩| d\overline{{ \mathcal P }}/df| ﹩ calculated from average TESS periodogram with probable rotation harmonics indicated by red dots.
Paper: StarStream: Automatic Detection Algorithm for Stellar Streams
Authors: Yingtian Chen, Oleg Y. Gnedin, Adrian M. Price-Whelan, Colin Holm-Hansen
Figure caption: Distribution of S/N in the color–magnitude diagram for actual members of the mock stream in Figure 1. The signal and noise densities are estimated using a similar KDE method in Sections 2.1 and 2.2, respectively. We multiply the stream kernel width by a factor of 3 to account for the lower number density of stars that do not sample the parameter space as well as simulated tracers. The same 104 background stars as in Figure 1 are also shown for reference.
Paper: StarStream: Automatic Detection Algorithm for Stellar Streams
Authors: Yingtian Chen, Oleg Y. Gnedin, Adrian M. Price-Whelan, Colin Holm-Hansen
Figure caption: Same as Figure 3, but with the alternative isochrone model ﹩{\mathtt{PARSEC}}﹩ (left column) and three alternative Galactic potential models (right column): (1) the base potential model scaled down by 20% (dotted curves), (2) the base potential model scaled up by 20% (dashed curves), and (3) the MilkyWayPotential2022 model from gala. We show the interquartile ranges for the base case for comparison.
Paper: StarStream: Automatic Detection Algorithm for Stellar Streams
Authors: Yingtian Chen, Oleg Y. Gnedin, Adrian M. Price-Whelan, Colin Holm-Hansen
Figure caption: Same as Figure 3, but including dust extinction from the SFD map. We also show the original cases (no extinction) as thin curves for comparison.
Paper: StarStream: Automatic Detection Algorithm for Stellar Streams
Authors: Yingtian Chen, Oleg Y. Gnedin, Adrian M. Price-Whelan, Colin Holm-Hansen
Figure caption: Same as Figure 4, but including dust extinction from the SFD map.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Surface brightness maps (top row) and line ratio maps (bottom row) for [O III] λ5007, [O II] λλ3727, 3729, and Hα. Surface brightnesses are shown in units of 10−16 erg cm−2 s−1 arcsec−2, and the line ratio maps display [O III]/Hα, [O II]/Hα, and [O III]/[O II] across the CGM. All maps are aligned onto a common spatial grid. Points “A” and “B” mark regions at projected distances of 9 kpc and 16 kpc, respectively, selected to probe the inner and outer boundaries of the counterrotating CGM. Two filamentary structures with extended emission are marked as “Filament 1” and “Filament 2,” both showing coherent features across multiple emission lines. We note faint Hα emission between Filament 1 and Filament 2 that lacks corresponding [O III]/[O II] at the adopted threshold. While a possible weak [O III] counterpart appears when lowering the SNR threshold (Figure 4), the feature remains marginal and disconnected from the main CGM structures, and is therefore not analyzed further. These regions are analyzed in Sections 5.2.4 and 5.2.5 using photoionization modeling.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Surface brightness, velocity, and velocity dispersion maps for Hβ, [O III] λ4959, λ5007, Hα, and [N II] λ6583 using a 3D mask with optimal central wavelengths and line widths for each spaxel (see the text). The surface brightness maps closely resemble the middle columns of Figure 5, where summation occurs over 4 Å around the systemic line center. Most emission exhibits a velocity shift of −150–150 km s−1 (blueshifted relative to J0910b), consistent with Figure 3. The velocity dispersion is typically within 200 km s−1 and forms a shell-like structure around the galaxy continuum. Although dispersion appears lower at greater distances, this may result from low SNR in those regions. The black contour near J0910b marks the ISM–CGM boundary (95% stellar continuum light; see Figure 15), and is overplotted on all panels for reference.
Paper: Kinematically Complex Circumgalactic Gas Around a Low-mass Galaxy: Filamentary Inflow and Counterrotation in J0910b
Authors: Zeren Lin, D. Christopher Martin, Mateusz Matuszewski, James D. Neill, Drew M. Miles, Vincent Picouet, Nikolaus Z. Prusinski, Keri Hoadley, Rosalie McGurk
Figure caption: Narrowband images (4 Å) centered on Hβ (5325–5329 Å), [O III] λ4959 (5432–5436 Å), [O III] λ5007 (5484–5488 Å), Hα (7188–7192 Å), and [N II] λ6583 (7211–7215 Å), after adaptive smoothing (SNR threshold of 2.5) and denoising (see the text). Continuum sources are masked similarly to Figures 2 and 3, except that J0910b remains unmasked for adaptive smoothing. The left and right columns show narrowband images with central wavelengths ±10 Å from the middle column, except for Hα, where the redder side is summed over 7168–7172 Å to exclude [N II] λ6548. Note that all panels cover the same region on the sky (i.e., same R.A. and decl. range); differences in the displayed fields of view (dark gray rectangles) reflect slight variations in the pointing and dither pattern between KCWI-blue and KCWI-red exposures.