adsabs/AstroCLIMB huggingface dataset:
Paper: Rotation Curve Measurement of Dark Matter Content of a z ∼ 0.5 Galaxy
Authors: Jake Magee, Caitlin M. Casey, Olivia R. Cooper, Alfonso Melendez, Mia Fong, Jeyhan Karltaltepe, Arianna S. Long, Stephanie Urbano Stawinski, Jaclyn B. Champagne, M. C. Cooper, Andreas L. Faisst, Claudia Maraston
Figure caption: (a) (top) Optimally extracted one-dimensional (1D) spectrum of our target in normalized arbitrary flux units. The triangular marks indicate emission lines redshifted to the measured source redshift, and each mark is labeled with its feature's name and rest-frame wavelength (in Angstroms). (bottom) Signal-to-noise two-dimensional (2D) spectrum of our target. (b) LePhare Spectral Energy Distribution (SED) fit to Farmer-extracted photometry for COSMOS ID 106340 from the COSMOS catalog. The vertical dashed line marks where Hα was observed. (c) Rotation curve extracted from the 2D-spectrum, with the spatial offset converted to kiloparsecs. The red curve is an arctangent fit function with r  k  = 19.2 ± 4.3 kpc. (d) RGB image of COSMOS ID 106340 generated from three HST images taken in the F606W, F814W, and F125W bands. The MOSFIRE slit is shown in yellow, and the cyan circle outlines the region on the slit in which the target lies. The dimensions of this cutout are 15″ by 15″.
Paper: New Active Asteroid (588045) 2007 FZ18
Authors: Colin Orion Chandler, William J. Oldroyd, Henry H. Hsieh, Chadwick A. Trujillo, William A. Burris, Jay K. Kueny, Jarod A. DeSpain, Kennedy A. Farrell, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano
Figure caption: (588045) 2007 FZ18 (green dashed arrow) with a pronounced tail (white arrows) in the anti-motion (red −v) direction and a faint tail (white arrow) in the anti-solar (yellow −⊙) direction. This 60 s VR-band image was taken with the DECam on the Blanco 4 m telescope at CTIO (Chile) on UT 2018 February 15 (Program 2014B-0404, PI Schlegel, observer S. G. A. Gontcho). The FOV is about 126″ × 126″.
Paper: New Active Asteroid 2015 VA108: A Citizen Science Discovery
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, William A. Burris, Henry H. Hsieh, Jay K. Kueny, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz
Figure caption: 2015 VA108 (dashed arrow) with a pronounced tail (white arrows) oriented between the anti-motion (−v) and anti-solar (−⊙) directions. These 114 s r-band (left) and 125 s g-band (right) DECam images were captured with the Blanco 4 m telescope (Cerro Tololo Inter-American Observatory, Chile) on UT 2015 October 11 (Program 2014B-0404, PIs Schlegel and Dey, observers D. James, A. Dey, A. Patej).
Paper: The JWST Resolved Stellar Populations Early Release Science Program. III. Photometric Star–Galaxy Separations for NIRCam
Authors: Jack T. Warfield, Hannah Richstein, Nitya Kallivayalil, Roger E. Cohen, Alessandro Savino, Martha L. Boyer, Christopher T. Garling, Mario Gennaro, Kristen B. W. McQuinn, Max J. B. Newman, Jay Anderson, Andrew A. Cole, Matteo Correnti, Andrew E. Dolphin, Marla C. Geha, Karin M. Sandstrom, Daniel R. Weisz, Benjamin F. Williams
Figure caption: Blue stars represent objects classified as stars and orange pluses as galaxies. Gray circles are objects that fit our general S/N cuts, but fail either classification. The top row of plots shows CMDs for each field in the sample. The bottom row shows examples of color–color plots for each field.
Paper: Modeling Star Formation Histories of Post Starburst Galaxies with BAGPIPES
Authors: Dasha L. Crocker, K. Decker French, Akshat Tripathi, Margaret E. Verrico
Figure caption: SFRs computed with BAGPIPES vs. those in Smercina et al. (2018). See Section 3 for more details.(The data used to create this figure are available.)
Paper: Can LISA Resolve Black Hole Binaries in the M87 Globular Clusters?
Authors: Donavon Evans, Kyle Kremer
Figure caption: Estimate of LISA source counts in globular clusters at various distances. In black is the LISA sensitivity curve. Blue curves show the characteristic strain vs. frequency for a fiducial 30 + 30 M ⊙ BH binary at four distances, d, representative of clusters in the Milky Way, M31, M87, and near the LISA detection threshold for stellar BHs. Labeled as R are the total BH merger rates in the cluster populations enclosed within each distance. Vertical dashed lines show characteristic GW inspiral times at various frequencies. In accordance with our CMC simulations, we predict zero sources will be resolved by LISA in the M87 clusters while a few to tens of sources may be resolved in more distant galaxies near the detection limit.
Paper: Ultracool Dwarf Absolute Magnitude versus Spectral Type Relations for JWST NIRCam Filters
Authors: Aniket Sanghi, Michael C. Liu, William M. Best, Trent J. Dupuy, Robert J. Siverd, Zhoujian Zhang
Figure caption: Absolute magnitudes derived for our sample of 1054 ultracool dwarfs as a function of their spectral type (SpT) in various JWST NIRCam filters. Field objects, low gravity objects, and young moving group members are marked by gray, cyan, and blue points respectively. Random scatter in the x direction with amplitude 0.3 SpT is applied to avoid overlapping points. Due to the large number of points, uncertainties in individual measurements are not shown. The median uncertainty in absolute magnitude is 0.055 mag. The black solid and dashed lines are the best-fit polynomial relations for the field and young objects, respectively. The shaded blue and orange regions represent the rms scatter about the field and young object fits, respectively.
Paper: Constraints on the Bright Meyer Group Comet C/2023 F2 (SOHO)
Authors: Quanzhi Ye, 泉 志 叶, Qicheng Zhang, Cristian Guiñez, Vicente Maldonado, Patricio Rojo, James M. Bauer, Karl Battams, Matthew M. Knight
Figure caption: Mosaics of the search images taken by the Danish 1.54 m telescope on 2023 April 4 and 5 UT and made by SWarp (Bertin 2010). The orbital “clones” at 3σ level, computed using the published astrometric points, are shown in red dots over the mosaics.
Paper: Evolution of Circumstellar Disks around T Tauri Stars as a Function of Stellar Age
Authors: L. Prato, M. Simon
Figure caption: Kiel Diagram: mass tracks are in increments of 0.1 M ⊙ beginning with ∼0.9 M ⊙. Isochrones, from updated magnetic models of Feiden (2016), are for 1, 1.5, 2, 3, 4, 5, 6, 7, 8, 9, 10, 12, 14, and 20 Myr. Red circles and violet stars represent Class II and Class III objects, respectively. LV21 values used for this plot, with corrected uncertainties (see text) available via Data behind the Figure.(The data used to create this figure are available.)
Paper: Abundances of Helium, Neon, Magnesium and Phosphorus in the Atmosphere of the Bp He-weak Star HD 175156
Authors: Richard Monier
Figure caption: Left: Synthesis of the Mg II triplet at 4481.0 Å and two weak S II lines (observed spectrum in black, synthetic spectrum in red). Right: Synthesis of 3 P II and 2 Ne II lines from 6000 to 6100 Å
Paper: SN 2023ixf—Temporal Development of Hα Emission
Authors: M. Koenig
Figure caption: Synopsis of all seven spectra from SN 2023ixf. In all spectral profiles the continuum was removed, and all were normalized using the value range of 490–520 nm. The spectra were arranged vertically using offsets to show the temporal development of spectral features. The observation dates are listed in the legend. The color of the date defines the color of the associated spectrum. By stacking 15 minutes exposures, exposure times of 2–3 hr were be achieved for each spectrum.(The data used to create this figure are available.)
Paper: No UV-bright Eruptions from SN 2023ixf in GALEX Imaging 15–20 yr Before Explosion
Authors: Nicholas Flinner, Michael A. Tucker, John F. Beacom, Benjamin J. Shappee
Figure caption: Left Panels: ﹩1^{\prime} \times 1^{\prime} ﹩ cutouts centered on the location of SN 2023ixf. Insets are shown for both filters and are averaged over all ≈15,000 s of exposure time. The red circle represent the aperture and the yellow circles represent the background. Right Panels: NUV (top) and FUV (bottom) light curves of single-pointing (open symbols) and the weighted averages of observations separated by >0.1 yr and shifted 0.1 yr for visual clarity (filled symbols). The solid lines are the weighted average of all single-pointing luminosities and the shaded bands represent 1σ scatter.
Paper: Cometary Activity Discovered on Vacationing Centaur 2019 OE31
Authors: William J. Oldroyd, Colin Orion Chandler, Chadwick A. Trujillo, Sam Deen, Henry H. Hsieh, Kennedy A. Farrell, Jarod A. DeSpain, Jay K. Kueny, William A. Burris, Scott S. Sheppard, Nima Sedaghat, Mark Jesus Mendoza Magbanua, 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: Images of faint activity (white arrows) on 2019 OE31 (green dashed arrows). Activity is primarily in or between the on-sky anti-motion (red and black arrows) and the anti-solar (yellow arrows) directions. Images are oriented North up and East left, have a FOV of 60″ × 60″, and were taken with the Dark Energy Camera on the 4 m Blanco telescope at Cerro Tololo Inter-American Observatory in Chile. (a) 90 s g-band image, prop. ID 2019A-0305, PI: Drlica-Wagner, observers: Mitch McNanna and Allison Hughes. (b) 90 s i-band image, prop. ID 2019A-0305, PI: Drlica-Wagner, observers: Ting Li and Kiyan Tavangar. (c) 90 s i-band image prop. ID 2019B-1014, PI: Olivares, observers: Felipe Olivares and Ignacio Sanchez.
Paper: New Active Jupiter Family Comet 2008 QZ44: a Discovery with Citizen Science
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, Henry H. Hsieh, Nima Sedaghat, Jay K. Kueny, William A. Burris, Jarod A. DeSpain, Kennedy A. Farrell, 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: 2008 QZ44 is at center, with North up and East left. The anti-solar (yellow arrow) and anti-motion (black outlined red arrow) directions are indicated. (a) UT 2008 November 20: 9 (3 g-band, 4 r-band) co-added 120 s CFHT MegaPrime exposures (PI Hoekstra, observers “QSO Team”). A tail is seen oriented towards the anti-solar direction. The FOV is 126″ × 126″. (b) UT 2017 November 12: 71 s r-band DECam exposure (prop. ID 2014B-0404, PI Schlegel, observers C. Stillman, J. Moustakas, M. Poemba). A faint tail is seen oriented towards the 2 o’clock position, between the anti-solar and anti-motion vectors. The FOV is 32″ × 32″.
Paper: CO and Atomic Line Emission from the Young Stellar Object V1331 Cygni
Authors: Richard J. Rudy, Ray W. Russell, Michael L. Sitko
Figure caption: 0.7–5.2 μm spectrum of V1331 Cyg from 2023 May 15. The top three panels highlight the atomic emission lines, particularly those from elements heavier than oxygen, which are extremely rare at these strengths in emission line sources. The bottom panel displays the observed spectral segment that includes the fundamental and first overtone emission from carbon monoxide (CO). Overplotted in blue is the a model for the CO emission with temperature 3000 K and an optical depth of 100 (in the strongest transition of the CO fundamental). The dashed lines represent the first overtone and fundamental plotted on top of an estimated continuum.(The data used to create this figure are available.)
Paper: Hidden Companions to Intermediate-mass Stars. XIV. Discovery of a 1.8 M ⊙, 0.3 au Companion to Ascella = Zeta Sagittarii A 
Authors: Idel Waisberg, Ygal Klein, Boaz Katz
Figure caption:  ζ Sgr VLTI/GRAVITY interferometric data in the science fiber for one of the three files taken on 2023 May 17 (UTC 07:23). Each baseline/triangle is plotted in a different color and the best fit triple star model is shown in black.
Paper: On the Spatial Distribution of Polarization and Color of a Distant Comet C/2017 K2 (PanSTARRS)
Authors: Evgenij Zubko, Gorden Videen
Figure caption: Six examples of the agglomerated debris particles (top) and results of modeling polarimetric observations of Comet C/2017 K2 (PanSTARRS) at heliocentric distance ∼7 au.
Paper: Identifying Ultracool Binary Systems using Machine Learning Methods
Authors: Malina Desai, Juan Diego Draxl Giannoni, Camille Dunning, Luke McDermott, Christian Aganze, Christopher A. Theissen, Adam J. Burgasser
Figure caption: (Top panels) Distribution of spectral types (left) and S/Ns (right) for our initial template set. (Bottom left) Construction of a binary template (in black) from flux-calibrated L2 primary (magenta) and T4 secondary (green) components. A single L4 template (blue, offset by +1) is shown for comparison. (Bottom right) Feature importance (FI) plot for the high-S/N RF model (bottom panel) compared to the L2+T4 binary template (blue line) and regions sampled by the Bardalez Gagliuffi et al. (2014) indices (magenta bands).
Paper: The Effect of Multiple Low-mass Flybys Can Preserve the Orbit of Neptune-like Objects in Slightly Perturbed Orbits in Star Formation Clusters
Authors: Juan J. Jiménez-Torres
Figure caption: Top: Histogram adapted for an illustrative star formation region of 20,000 members following the prevalence ratios of newborn stars of Kroupa (2002) and Salpeter (1955). Bottom: Resultant orbits after the impact of low-mass flybys and a single massive encounter. Chi-squared calculations and probability levels for the resultant orbits of the Neptune-like particle confronted to the orbit of Neptune.
Paper: Resolved Binaries with Late-M and L Dwarf Companions Identified in Gaia eDR3
Authors: Tianxing Zhou, Delilah Jacobsen, Brigette Vazquez-Segovia, Chih-Chun Hsu, Christopher A. Theissen, Adam J. Burgasser
Figure caption: Gaia CMDs (upper panels) and reported spectral type distributions (lower panels) for primaries (left) and secondaries (right). For the CMDs, the full 400 pc sample is indicated by gray dots; sources with literature spectral types are indicated by colored dots scaled to spectral type; white dwarf primaries with/without literature classifications are indicated in dark/light magenta dots. Spectral type distributions for our 400 and 100 pc samples are shown in blue and orange, respectively, with classified white dwarf primaries (11 out of 128 sources) labeled in magenta.(The data used to create this figure are available.)
Paper: Comet-like Activity Discovered on Quasi-Hilda Asteroid 2009 DQ118
Authors: William J. Oldroyd, Colin Orion Chandler, Chadwick A. Trujillo, William A. Burris, Jay K. Kueny, Henry H. Hsieh, Kennedy A. Farrell, Jarod A. DeSpain, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano
Figure caption: Images of 2009 DQ118 (green arrow) with a comet-like tail (white arrows) in the direction of the on-sky anti-motion (−v) and anti-solar (− ⊙ ) vectors. Images were taken with DECam on the 4 m Blanco telescope at CTIO. Left: 300 s VR band image taken on UT 2016 March 8 (Prop. ID 2016A-0189; PI Rest; observers A. Rest, DJJ). Right: 200 s r band image taken UT 2016 March 9 (Prop. ID 2015A-0121; PI von der Linden; observer A. von der Linden).
Paper: Calibration Target Selection for the SPARCS Satellite
Authors: Alexandra Frymire, David Ardila
Figure caption: All 10 stars analyzed can be used as SPARCS calibrators. Top: Target variability compared with the SPARCS requirement. Only two 120 s gPhoton observations were available in the FUV for GJ 754.1A and WD 2027+068. Only two GALEX Archive observations were available in the NUV for WD 2027+068. Bottom: WDs in the plots above. All 10 stars are of spectral type DA, DB, or DO.
Paper: The “Super-Active” Accretion Phase of T CrB has Ended
Authors: Ulisse Munari
Figure caption: Spectral and photometric changes prior to and during the “super-active” accretion phase of T CrB. The bottom panel shows the B-band light-curve of T CrB collected by ANS Collaboration. The panels above plot the integrated flux of selected emission lines measured on low-resolution spectra, all obtained with the Asiago 1.22 m + B&C (and 300 ln mm−1 grating). While Hβ is discernible in emission at all epochs, higher excitation/ionization lines turned on only during the “super-active” accretion phase (the arrows point to missing-line epochs).
Paper: Comparing the Photometric Calibration of DESI Imaging and Gaia Synthetic Photometry
Authors: Rongpu Zhou, Arjun Dey, Dustin Lang, John Moustakas, Edward F. Schlafly, David J. Schlegel
Figure caption: Maps of the magnitude offset between LS DR9 and the Gaia synthetic photometry in grz bands. The offset is the median value of the magnitude difference, m LS − m Gaia,synth, for stars in each HEALPix (Nside = 128) pixel. We separate North and South at decl. = +32.375 in the North Galactic Cap (i.e., only showing northern offsets at decl. > +32.375). The LS photometry is tied to PS1 north of decl. = −29.°25 and calibrated using ubercal south of this boundary.
Paper: A Simple Code for Rotational Broadening of Broad Wavelength Range High-Dispersion Spectra
Authors: Adolfo Carvalho, Christopher M. Johns-Krull
Figure caption: Results from rotationally broadening spectra using the two methods, direct integration and convolution. Left: A 5500 K PHOENIX (Husser et al. 2013) atmosphere model, broadened to 30 km s−1 using the two methods and assuming a limb darkening coefficient of 0.6. We show a small piece of spectrum to better distinguish the individual line profiles. The wavelength ranges (Δλ) and mean wavelengths (﹩\bar{\lambda }﹩) of each spectrum are given in the legend. Notice the “fast” convolution matches the direct integration almost perfectly when the wavelength range is small and the region of interest is near the center of that range. In that case, the result is the same as using the “slow” method. However, for the larger wavelength range, where we are now far from the mean central wavelength, the broadening accuracy is much worse. The direct integration case is computed on the Δλ = 2800 Å case. Right: The times for the two broadening method as a function of the length of the array being broadened. Notice the rapid increase in time for the convolution method compared to integration. The spectra shown are sampled at d λ ∼ 0.01, so Δλ = 1000 is a 105 element array. The grid used for the integration has N  r  = 10 and N  θ  = 100, the default values for our function.
Paper: The Recent Mass Loss History of the Hypergiant RW Cep
Authors: Terry Jay Jones, Dinesh Shenoy, Roberta Humphreys
Figure caption: Left panel: SED and DUSTY model; Right panel: Extended 11.9 μm emission around RW Cep. The contours are in Jy/sq arcsec.
Paper: Spectroscopic Follow-up of Two Star-forming Objects in the M101 Field 
Authors: Ray Garner, Steven Janowiecki, J. Christopher Mihos
Figure caption: Top: the spectrum of N5474-3-1. Bottom: the spectrum of N5486-2-1. In both panels, several lines are identified. The gray areas show the masked parts of the spectra, i.e., those areas affected by sky residuals.
Paper: New Post-DART Collision Period for the Didymos System: Evidence for Anomalous Orbital Decay
Authors: Taylor Gudebski, Elisabeth Heldridge, Brady McGawn, Elle O Hill, Jonathan J. Swift, Henry Zhou
Figure caption: (top panel) Phase folded photometric measurements of (65803) Didymos used to derive a Fourier model of the rotational modulation to the light curve (dashed black line). (bottom panels) Light curves of (65803) Didymos from 2022 October 30 and 31 corrected for rotational modulation and showing the best fit primary eclipse model using our derived ΔP = − 34.2 minutes.
Paper: Baked before Breaking into Bits: Evidence for Atira-type Asteroid Splits
Authors: Carlos de la Fuente Marcos, Raúl de la Fuente Marcos
Figure caption: Mutual nodal distances as a function of the distance to the node (top panel) and as a function of the angular separation of the perihelia (bottom panel) for the 32 known Atiras. The first percentil of the distribution is shown as an orange line (solid or dashed). The pink vertical bars show Venus’ perihelion and aphelion, the brown vertical bars display those of Mercury (top panel). The error bars are the result of the evaluation of 104 sets of synthetic elements compatible with the uncertainties and generated using a Monte Carlo process. The black squares in the panels correspond to pairs that include 2023 WK3.
Paper: Synthesis of the 4400–4600 Å Spectral Range for the A2.5V star HD 176687 (ζ Sagitarii A)
Authors: Richard Monier
Figure caption: Synthesis of the 4400–4600 spectral window (observed spectrum in black, synthetic spectrum in red).
Paper: A New Stellar Companion to GJ 835
Authors: Catherine A. Clark, Elliott P. Horch, James W. Davidson
Figure caption: Reconstructed images of the newly triple system GJ 835. From left to right, the UT 2017 October 20 observation at 880 nm, and the UT 2023 September 4 observations at 692, 880, and 1500 nm are shown. Each image has a slightly different pixel scale, which we have not adjusted here. In the images, north is upwards and east is to the left. The new tertiary moved ∼150° in position angle in the six years between epochs of observation.
Paper: Optical Observations of the Type Ia Supernova 2022hrs
Authors: Sophia Risin, Cooper Jacobus, Ivan Altunin, Thomas G. Brink, Kishore C. Patra, WeiKang Zheng, Yi Yang, Neil Pichay, Michael Fitzgerald, Grady Boyce, Pat Boyce, Alexei V. Filippenko
Figure caption: (A) Light curve of SN 2022hrs in four filters over 35 days. (B) B − V color evolution. (C) Line-of-sight velocity evolution of SN 2022hrs. (D) Top: Kast spectral evolution of SN 2022hrs spanning −4.8 to 81.2 days relative to peak brightness. Bottom: late-time spectra of SN 2022hrs taken with Lick/Kast and Keck/DEIMOS. Vertical lines denote the rest wavelengths of several known features.(The data used to create this figure are available.)
Paper: Galactic ChitChat: Using Large Language Models to Converse with Astronomy Literature
Authors: Ioana Ciucă, Yuan-Sen Ting
Figure caption: The GPT-4 model responses to expert-level questioning in no-context vs. multi-document context settings. No-context responses may lack recent findings and sometimes hallucinate details. For example, Belokurov et al. (2018) did not use GALAH data. The in-context GPT-4 instance performs well in summarisation, study comparisons, and idea generation. For example, the model accurately identifies that it only has access to Kawata et al. (2018), as shown in Comparative Analysis III.
Paper: The 23.01 Release of Cloudy
Authors: Chamani M. Gunasekera, Peter A. M. van Hoof, Marios Chatzikos, Gary J. Ferland
Figure caption: A contour plot of H Lyα line intensity predicted by C23.01 relative to the same quantity from C23.00, for the baseline model Orion_hii_open.in in the CLOUDY test suite. The ratio of ionizing photon flux ϕ(H) to hydrogen density n(H) is effectively the ionization parameter U. The lower-right corner of the panels corresponds to high U, and the upper-left corner is low U.
Paper: A Fully Explicit Integrator for Modeling Astrophysical Reactive Flows
Authors: Parker Johnson, Michael Zingale, Eric T. Johnson, Alexander Smith, Kyle E. Niemeyer
Figure caption: Number of node hours and carbon mass as a function of time for the different integrators and time-integration method on CPU/GPU.
Paper: New Pulsating Variable Stars and Eclipsing Binaries in NGC 6871 
Authors: Ai-Ying Zhou
Figure caption: Examples of newly identified variable stars. Top two rows: two new δ Sct stars HD 191025 (=TIC 41189624) and HD 227647 (=TIC 40831024); 3rd–5th rows: four new γ Dor stars TIC 1966186334, TIC 90463595, TIC 91105923, and TIC 89119933 (=HD 227505); 6th and 7th rows: four new eclipsing binaries, TIC 91111661, TIC 90349599, TIC 90461796 with a pulsating or rotating component, TIC 104914249 being double eclipsing binary systems of quadruple objects (Zasche et al. 2023).