adsabs/AstroCLIMB huggingface dataset:
Paper:  FluxCT V2.0: Updates to a Web Tool Identifying Contaminating Flux in Space Telescope Data
Authors: Zilin Dong, Jessica Schonhut-Stasik, Keivan Stassun
Figure caption: Returned plot for TIC 25078304, in the coordinate space R.A. (hour angle) and decl. (degrees). The pink star shows the target source, and the white stars correspond to those found in the Gaia search. Gray dotted lines represent on-sky coordinates; each colored square depicts a pixel. Dark purple represents pixels not included in the original TPA, and lighter shades through white correspond to the source’s TPA, scaled toward white as flux values increase. White lines around the TPA correspond to the smallest possible polygon, with R.A. and decl. values in each corner. TIC 25078304 (magnitude 12.73) has five additional sources within the TPA, with target magnitudes of 15.419, 17.037, 17.04, and 17.055 for the accompanying sources, giving magnitude differences between ∼3 and ∼5. In this case a magnitude cut has been applied so that any stars with a magnitude difference between the source and the target >5 are removed from the analysis. The total flux contamination for this system is 16.2%.
Paper: The Mass–Radius Relation for Planets in Binary Systems
Authors: Eric Gaidos, Catherine A. Clark, Kendall Sullivan
Figure caption: Masses and radii of planets in binaries with projected separations ρ < 500 au. (Filled points have ρ < 200 au.) The shading is a kernel density estimator from 323 planets around single stars with masses more precise than 25%. Model radius–mass relations for sub-Neptunes are labeled by H2/He envelope mass fraction (E. D. Lopez & J. J. Fortney 2014). The empirical relations of J. Chen & D. Kipping (2017) and J. F. Otegi et al. (2020) are shown. The inset compares the sum of the KDE at the locations of the 15 binary-hosted planets (arbitrary units) with the distribution of 3000 Monte Carlo-generated samples of equal size generated from the KDE itself.
Paper: M31N 2013-10c: A Newly Identified Recurrent Nova in M31
Authors: Allen W. Shafter, Kamil Hornoch, Hana Kučáková, Petr Fatka, Jingyuan Zhao, 经 远 赵, Xing Gao, 兴 高, Shahidin Yaqup, 伊丁·亚库普 夏, Tuhong Zhong, 土 红 钟, Ali Esamdin, 力·伊沙木丁 艾, Chunhai Bai, 春海 白, Na Wang, 娜 王, Paul Benni, Aiden Luo, Ilana Yousuf
Figure caption: The lightcurves for the 2013 October (M31N 2013-10c, top panel) and 2023 November (M31N 2023-11f, middle panel) eruptions of the RN M31N 2013-10c. The bottom panel shows both eruptions superimposed after adopting times of maximum of JD 2,456,575.313 and 2,460,276.630 for the 2013 and 2023 eruptions, respectively. The star and the open square in the upper panel corresponds to the photometry reported by the LOSS and N. James, respectively, while the open square in the middle panel shows the unfiltered discovery magnitude of Xu et al. (2023). The open circles in the middle panel represent Sloan r photometry converted to Cousins R as described in the text. The downward-facing triangles represent lower limits from prediscovery images. The dashed line in the lower panel represents the best-fitting two-component line used to estimate 〈t 2(R)〉 = 3.9 ± 1.0 days.(The data used to create this figure are available.)
Paper: Detecting the Undetected: Overcoming Biases in Gravitational-wave Population Studies
Authors: Ryan Raikman, Simone Bavera, Tassos Fragos
Figure caption: Biasing plot—ability of our method to measure the bias caused by removing a certain formation channel from the set of known distributions. Across different values of α CE and χ, we show the sum of estimated branching fractions from known channels against the branching fraction of the unknown channel. The optimal case is the sloped dashed black line, where the branching fraction of the unknown channel is perfectly predicted. The flat dotted black line represents no knowledge of the removed formation channel.
Paper: Gnuastro: Visualizing the Full Dynamic Range in Color Images
Authors: Raúl Infante-Sainz, Mohammad Akhlaghi
Figure caption: M51 galaxy group color images from J-PLUS DR3 using the iSDSS, rSDSS, gSDSS (R-G-B), and J0660 (Hα) filters. Top-left: traditional color image, where the background regions become black. Top-right: modified weights of the channels balance to obtain a bluer image. Bottom-left: gray background color image; this is the default mode of astscript-color-faint-gray. The separation between color, black, and gray regions are defined from surface brightness cuts (see text) of the G channel (rSDSS). The use of the gray background colormap reveals diffuse low surface brightness structures that would otherwise remain unveiled. Bottom-right: color image using the Hα narrow band filter (J0660) for the intermediate (G) channel instead of rSDSS. The use of this filter reveals interesting features such as the star-forming regions that are shown in green.
Paper: Variability Census of Legacy Catalogs. II. 6600+ New δ Scuti and γ Doradus Stars 
Authors: Ai-Ying Zhou
Figure caption: Example TESS light curves of newly identified variables. Top 3 rows: six new γ Dor stars; 4th row: two new eclipsing binary systems with γ Dor primary components; 5th–8th rows: four new δ Sct stars. Plots were created during batch processing.
Paper: A Constrained Dust Opacity for Models of Dense Clouds and Protostellar Envelopes
Authors: Klaus M. Pontoppidan, Neal Evans, Jennifer Bergner, Yao-Lun Yang
Figure caption: The KP5 model—Panel (A): The KP5 extinction law compared to the high-extinction measurements from Chapman et al. (2009) and Shirley et al. (2011). The mid-infrared measurements were reported assuming a near-infrared power law slope of β = − 1.6. Panel (B): The size distribution of the silicate and carbon grains (including the ice mantles), parameterized using Weingartner & Draine (2001). The sharp peak in the distribution is due to the constant-thickness ice mantles. Panel (C): The absorption and scattering opacities of the original KP5 compared to a benchmark computed using OpTool, scaled from a silicate density of 3.3–3.8 g cm−3.(The data used to create this figure are available.)
Paper: Virial Velocities for Stellar Flybys with Planetary Disks in Star Formation Regions
Authors: Juan J. Jiménez-Torres, Alvaro Alvarez-Candal
Figure caption: Results of encounters with a 100 au. disk perturbed by a 1 M ⊙ passing star for different velocities from 1.5 to 10 km s−1. These values correspond with the velocities of members in typical star formation regions. The simulations assume an approach distance of 100 au, and impact angles of ϕ = 0°, θ = 45°, and α = 45°. Initial eccentricities and inclinations to the ecliptic of the disk particles are set to 0. Details and references for the structure of stellar impacts with disks can be found in Jiménez-Torres et al. (2011), Jiménez-Torres et al. (2013).
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. II. HD 143807 and HD 16727
Authors: Richard Monier
Figure caption: Left: line synthesis of the Hg II line at 5677.10 Å of HD 143807 (observed spectrum in black, synthetic spectrum in red), Right: the line is not clearly detected at 3σ above the noise in the continuum in the spectrum of HD 16727.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. III. HD 145389 (ϕ  Her) and HD 186122 (46 Aql)
Authors: Richard Monier
Figure caption: Left: Line synthesis of the Hg II line at 5677.10 Å of ϕ Her (coadded spectrum in black, synthetic spectrum in red), Right: The line is not clearly detected at 3σ above the noise in the continuum in the spectrum of 46 Aql.
Paper: New Spectroscopic Redshift Places PEARLSDG in a Group at ∼124 Mpc
Authors: Timothy Carleton, Steven P. Willner, Timothy Ellsworth-Bowers, Rogier A. Windhorst, Seth H. Cohen, Christopher J. Conselice, Jose M. Diego, Adi Zitrin, Haylee N. Archer, Isabel McIntyre, Patrick Kamieneski, Rolf A. Jansen, Jake Summers, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Rafael Ortiz, Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Benne W. Holwerda
Figure caption: Top: comparison of the Lowell Discovery Telescope (LDT) spectra of PEARLSDG of Carleton et al. (2024, light blue) and new MMT/Hectospec observations of 2024 April 10 (dark orange) and 2024 June 11 (green). The dashed lines mark Hδ, Hγ, Hβ, and Hα absorption at the updated redshift of 0.02809. Middle: a zoom-in of those regions showing the continuum-normalized spectra as observed and as modeled for an old, metal-poor stellar population. The dashed and solid curves are for the previously reported and new redshifts of 0.008 and 0.02809, respectively. The new, higher S/N spectra more robustly establish the redshift of PEARLSDG. Bottom: an illustration of the updated environment of PEARLSDG (shown as the teal star). Nearby galaxies from the NASA Sloan Atlas are shown as circular dots with sizes that correspond to the galaxy’s stellar mass (Blanton et al. 2011). With the updated redshift, PEARLSDG appears associated with a group of galaxies at ∼124 Mpc.
Paper: Constrained Wave-telescope Technique
Authors: T. Broeren, K. G. Klein
Figure caption: We apply the two different proposed constraint matrices ( C  − and  C  +) to a simulation of a divergence-free wave with added (non divergence-free) 15% Gaussian noise. We compare the results of a wave-telescope scan through wavevector direction space to a wave-telescope scan done using no constraint matrix.
Paper: How Reliable are Rotation Period Determinations from TESS Data?
Authors: Mariel Lares-Martiz, Derek Buzasi, Terry Oswalt, Krystian Confeiteiro, Ahnika Gee, Luca Guida, Ryan Reynolds, Melinda Walls
Figure caption: Comparison between detected rotation period and x-position periods. Red dashed lines mark the 2:1, 1:1, and 0.5:1 period ratios. Filled orange circles are the number of apparent rotation periods identified by the Lomb–Scargle algorithm that match periodicities found in the x-positions.
Paper: The Abundances of the Noble Gases Neon and Xenon in the Atmosphere of 53 Tau (HD 27295)
Authors: Richard Monier
Figure caption: Left: line synthesis of the Ne I line at 6402.05 Å computed for the solar neon abundance (observed spectrum in black, synthetic spectrum in red), Right: line synthesis of the Xe II line at 5292.22 Å.
Paper: Assessing the Evolution of Solar Cycle 25: A Weak-moderate Cycle
Authors: V. M. S. Carrasco, J. M. Vaquero, A. J. P. Aparicio
Figure caption: Solar cycles from 1 to 25 according to the 13 months smoothed sunspot number provided by SILSO starting in the minimum of each cycle (https://www.sidc.be/silso).
Paper: Deep HST Imaging Favors the Bulgeless Edge-on Galaxy Explanation for the Hypothetical Stellar Wake Created by a Runaway Supermassive Black Hole
Authors: Mireia Montes, Jorge Sánchez Almeida, Ignacio Trujillo
Figure caption: Top: RGB image of the linear feature, including the field where the putative counter wake to be produced by the second pair of SMBHs is expected. Bottom left: zoom-in of the box marked in the top panel, where the bow shock from the motion of the SMBH on the circumgalactic medium was expected. Bottom right: UV emission (F200LP − F350LP color) along the feature averaged ±1 kpc from its centroid. It is aligned with the image in the top panel. The plot also includes the UV F200LP − F350LP emission to be expected from single stellar population models (without internal dust attenuation) corresponding to various ages as labeled. The distances are referred to the dynamical center determined from the position–velocity curve in Sánchez Almeida et al. (2023). The vertical dashed lines, included to guide the eye, mark ±20 and ±40 kpc from the center of the edge-on galaxy. The blue–black knots scattered throughout the image set the background noise level.
Paper: No Significant Redshift Evolution in the Intrinsic Scatter of the M •–M ⋆ Relation for Overmassive Black Holes
Authors: Carl Audric Guia, Fabio Pacucci
Figure caption: Standard intrinsic scatter as a function of the median redshift for all our data sets in various redshift regimes. Typical values are within the range of 0.45–0.65 dex. No statistically significant redshift evolution is observed.
Paper: ASKAP-EMU Discovery of New Galactic SNR Candidate: Unicycle (G312.65+2.87)
Authors: Zachary J. Smeaton, Miroslav D. Filipović, Bärbel S. Koribalski, Sanja Lazarević, Rami Z. E. Alsaberi, Werner Becker, Kristen C. Dage, Yjan Gordon, Andrew M. Hopkins, Roland Kothes, Denis Leahy, Ana Mitras̆inović
Figure caption: RGB composite image where the 944 MHz ASKAP image is in red and blue and WISE 12 μm infrared image is in green. All images use linear scaling.
Paper: The Gravitational Wave AfterglowPy Analysis (GWAPA) webtool
Authors: R. A. J. Eyles-Ferris, H. van Eerten, E. Troja, P. T. O'Brien
Figure caption: The user interface for GWAPA, built using the Bokeh package.
Paper: Predicting Stellar Masses of the First Galaxies Using Graph Neural Networks
Authors: Vincent A. Horvath, Snigdaa S. Sethuram, John H. Wise
Figure caption: Stellar masses from the Skinner & Wise (2020) simulation (left) and our GNN (middle) vs. simulated DM halo mass. The right panel compares our GNN-predicted results with the simulated masses.
Paper: Validating Gaia DR3 Pulsating Variable Classifications with TESS: Building Reliable δ Scuti and γ Doradus Stars Catalogs (In Progress) 
Authors: Ai-Ying Zhou
Figure caption: Example TESS light curves of ten newly identified variables not DSCT∣GDOR∣SXPHE types. Top left: a new RRab star; Top right: EA+flare; 2nd and 3rd rows: four new heartbeat stars; 4th row left: a new rotating ellipsoidal variable star; Right, a candidate planetary transit; 5th rows: two new eclipsing binaries with pulsating γ Dor primary components.
Paper: Initial Entropy and Potential Delayed Formation of the Directly Imaged Exoplanet AF Lep b
Authors: Zhoujian Zhang, 周健 张
Figure caption: Panel (a): Inferred initial entropy and age of AF Lep b based on its dynamical mass and bolometric luminosity. The 1σ/2σ (dark/light) confidence intervals are shown in orange. The upper x-axis denotes the potential delayed formation timescale of AF Lep b, derived from two BPMG age estimates. Panels (b) and (c): Inferred properties of AF Lep b using a different luminosity (blue), or different masses (purple and green), following the format as Panel (a).
Paper: Minimum Mars Climate Sounder Retrieval Altitudes Reveal Cloud Altitudes at Aphelion and Stranded High-altitude Dust Following the MY34 Global Dust Storm on Mars
Authors: Alex C. Innanen, John E. Moores, Margaret E. Landis, Victoria Concepcion
Figure caption: (A) cut-off altitudes for MCS retrievals over Gale Crater. (B) Normalized frequencies of cut-off altitudes during the clouds season and (C) dust season. (D) Cut-off altitudes for Mars year 34, with the decay phase fitted with an exponential decay curve (solid red line).
Paper: A Report on Stellar Companion Mass Estimates within Our Solar Neighborhood
Authors: Sangeeta Kumar, Maïssa Salama
Figure caption: Distribution of estimated masses from the empirical and orvara methods. Plots (a) and (b) show the primary and companion masses, respectively, as a function of the companion’s projected separation. Plot (c) compares the different methods of estimating individual component masses. Data behind this figure(Gaia IDs, separations, and mass estimates) are available in the electronic version.(The data used to create this figure are available.)
Paper: AstroLLaMA-Chat: Scaling AstroLLaMA with Conversational and Diverse Datasets
Authors: Ernest Perkowski, Rui Pan, Tuan Dung Nguyen, Yuan-Sen Ting, Sandor Kruk, Tong Zhang, Charlie O'Neill, Maja Jablonska, Zechang Sun, Michael J. Smith, Huiling Liu, Kevin Schawinski, Kartheik Iyer, Ioana Ciucă
Figure caption: Demonstration of AstroLLaMA-Chat’s Capabilities. While general large language models like GPT-4 continue to exhibit robust reasoning and Q&A abilities, even in specialized domains such as astronomy, our study highlights the benefits of continual pre-training on a dedicated astronomy corpus from arXiv, enriched with the latest data. This approach gives AstroLLaMA-Chat an edge in two specific areas. The top example illustrates its performance in a highly specialized topic within astronomy. AstroLLaMA-Chat demonstrates a better understanding of the complexities involved in studying the dimensionality of elemental abundance in stars, reflecting the true chemical yield channels. It also outlines prevalent methods in this specialized area. In contrast, GPT-4 and the LLaMA-2-7b model, from which AstroLLaMA is derived, often provide responses that lack depth in understanding this field. The bottom panel illustrates AstroLLaMA-Chat’s adeptness in addressing contemporary and dynamic research areas, notably the burgeoning field of parity violation studies in cosmology. While it captures some of the latest directions in the field (though with occasional detail inaccuracies), both GPT-4 and LLaMA-2 tend to diverge into broader implications and detection methods, failing to encapsulate the current focus of the field.
Paper: 2016 UU121: An Active Asteroid Discovery via AI-enhanced Citizen Science
Authors: Nima Sedaghat, Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, William A. Burris, Henry H. Hsieh, Jay K. Kueny, Kennedy A. Farrell, 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: 2016 UU121 (at center) of the 63″ × 63″ (north up, east left) FOV with a tail oriented in the anti-motion (red-bordered black arrow) directions as projected on sky. Also indicated is the anti-solar direction (yellow arrow). All images were 120 s VR-band exposures acquired with the Dark Energy Camera (DECam) on the Blanco 4 m telescope at Cerro-Tololo Inter-American Observatory, Chile (Prop. ID 2019A-0337, PI Trilling). (a) UT 2021 September 10 (observer Edward Lin). (b) UT 2021 September 11 (observer David Gerdes).
Paper: Modeling the Light Curve of HD 222925's Progenitor Kilonova
Authors: Ian P. A. Johnson, Erika M. Holmbeck
Figure caption: Top: semi-analytical bolometric light curves associated with HD 222925's progenitor kilonova for two models that successfully replicate its abundance pattern: a constrained Y  e  distribution (dark green) and a different nuclear mass model (light green). Bottom: fractional difference in bolometric luminosity between the two models. Also shown are the approximate time-dependent uncertainties (±ΔL/L int) on the bolometric luminosity of the GW170817 kilonova, AT2017gfo, from Waxman et al. (2018). Note that these data stop at 16.5 days.(The data used to create this figure are available.)
Paper: The Late-epoch, Intermediate Excitation Spectrum of the Nova V612 Scuti
Authors: Richard J. Rudy, John P. Subasavage, Jon C. Mauerhan
Figure caption: Combined optical and optical-infrared spectra of the nova V612 Scuti from 1116 and 1593 days after discovery. The top panel combines the UV/optical data (unique to the observations of the first epoch) with infrared data (unique to the second epoch) to highlight the numerous [Fe VI] (labeled in black) and [Fe VII] (labeled in blue) emission lines. Lines from other ions are identified in green. The middle panel shows the remainder of the observations from the first epoch. The weak lines of [Fe V], which are discussed in the text, are highlighted in red. The very weak feature at 0.9930 μm that is notated with a question mark in the bottom panel is unidentified. Overall, the emission line spectrum is very rich, with features present from numerous elements and a broad range of ionization states.(The data used to create this figure are available.)
Paper: GRB 230911A: The First Discovery of a Fermi GRB Optical Counterpart with the Gravitational-wave Optical Transient Observer (GOTO)
Authors: S. Belkin, B. P. Gompertz, A. Kumar, K. Ackley, D. K. Galloway, F. Jiménez-Ibarra, T. L. Killestein, D. O'Neill, K. Wiersema, D. B. Malesani, A. J. Levan, J. Lyman, M. J. Dyer, K. Ulaczyk, D. Steeghs, V. S. Dhillon, P. O'Brien, G. Ramsay, K. Noysena, R. Kotak, R. P. Breton, L. K. Nuttall, E. Pallé, D. Pollacco, S. Awiphan, U. Burhanudin, P. Chote, A. Chrimes, E. Daw, C. Duffy, R. Eyles-Ferris, B. Godson, T. Heikkilä, P. Irawati, L. Kelsey, M. R. Kennedy, S. Littlefair, L. Makrygianni, T. Marsh, D. Mata Sánchez, S. Mattila, J. Maund, J. McCormac, D. Mkrtichian, J. Mullaney, M. Patel, J. Rana, E. Rol, U. Sawangwit, E. Stanway, R. Starling, P. A. Strøm, B. Warwick
Figure caption: GOTO L-band light curve of GRB 230911A with a single power-law (SPL) model fit. Inset: GOTO-North image of the GRB 230911A first detection.
Paper: Faint Comet Detection with Unistellar eVscopes
Authors: Ariel Graykowski, Samantha Hemmelgarn, Thomas M. Esposito, Franck Marchis, David Koster, Darren Rivett, Masao Shimizu
Figure caption: Unistellar eVscope images. Comet 12P (Left) is centered in a 60 minutes stack of images. Comet C/2023 A3 (Right) is centered in a 40 minutes stack of images.
Paper: The Far Ultraviolet Light Curve of 78 Vir (A2p SrCrEu)
Authors: Richard Monier
Figure caption: Left: the FUV light curve of 78 Vir at 1500 Å, Right: the corresponding variations of the FES counts.
Paper: The Once-canceled Habitable-zone Super-Earth Gliese 581d Might Indeed Exist!
Authors: Manfred Cuntz, Scott G. Engle, Edward F. Guinan
Figure caption: Top: Photometry of Gliese 581, starting in 2006 May; the star has been observed for 9 seasons. Individual measures (3–5 per night) were binned into nightly means before running the period analyses. Blue data points were obtained using the 0.75 m Four College Automated Photoelectric Telescope at Fairborn Observatory. Green and pink data points were obtained with the 1.3 m Robotically Controlled Telescope at Kitt Peak National Observatory, but with different CCD cameras. Lower Left: the GLS power spectrum, as implemented by astropy, is shown. FAPs of 10%, 1%, and 0.1%, are plotted as red, green, and blue dashed lines, respectively. The most prominent period is P rot = 148.7 ± 0.8 days. The one-year aliasing effect causes the weaker, evenly spaced spikes seen along the periodogram. Lower Right: the phased light curve of Gliese 581, using the likeliest period returned from the GLS algorithm, is shown; it employs the same coloring scheme as in the plot at the top of the figure. A coherent, sinusoidal pattern is visible in the data when phased to a period of 148.7 days.
Paper: Multiwavelength Catalog of 10,000 4XMM-DR13 Sources with Known Classifications
Authors: Yichao Lin, Hui Yang, Jeremy Hare, Igor Volkov, Oleg Kargaltsev
Figure caption: A screenshot from the interactive visualization tool, available at https://yichaolin-astro.github.io/4XMM-DR13-XCLASS/, shows HR1 vs. F X/F o, with an LM-STAR source selected. One can see LM-STAR and AGN are two separate clusters while other source classes show some overlapping, thus requiring using different pairs of source properties for distinction.
Paper: CO and C I Emission in the Early Spectrum of the Nova V1391 Cassiopeiae
Authors: Richard J. Rudy, Ray W. Russell, Michael L. Sitko, Hideyo Kawakita
Figure caption: The 0.69–5.2 μm spectrum of V1391 Cas from six days after maximum brightness. Colored labels are used to distinguish among lines of different neutral species and to highlight the numerous C I line present. Dashed lines below the spectral segments in the top, and bottom two panels denote the locations of H I lines from the Paschen, Brackett, and Humphreys series, respectively. Lines whose presence is uncertain are marked with a question mark; unknown lines are labeled with the measured wavelength in magenta. The spectrum is very low excitation: the He I lines at 1.0830 μm (second panel) and 2.0587 μm are very weak if present at all. The locations of both the 12C16O and 13C16O bandheads are marked in the third panel while the bottom panel shows the carbon monoxide model plotted in blue over the observations.(The data used to create this figure are available.)