adsabs/AstroCLIMB huggingface dataset:
Paper: Convective Boundary Mixing Processes
Authors: Evan H. Anders, Adam S. Jermyn, Daniel Lecoanet, J.R. Fuentes, Lydia Korre, Benjamin P. Brown, and Jeffrey S. Oishi
Figure caption: The three processes discussed in Section 1 are shown schematically in the top row. White fluid has the properties of the well-mixed CZ, while purple fluid is the stable RZ. (Left) Convective overshoot occurs when a fluid parcel from the CZ crosses into the RZ; due to a strong positive entropy gradient in the RZ, the parcel is accelerated back into the CZ. (Middle) Motions generated by overshooting fluid parcels drag fluid from the RZ into the CZ in a process called entrainment. (Right) If a region of fluid beyond the convective boundary becomes well-mixed by entrainment, it is a PZ; a non-zero divergence of the radiative flux acts as an internal cooling term, changing the buoyant signature of both upflows and downflows. In the bottom panel, we show the structure of a statistically-stationary convective boundary. The CZ sits below a well-mixed PZ. Above the PZ, the fluid is stable but there is a small OZ where convective overshoot occurs. Above this region is the stable RZ where there are internal gravity waves excited by the convection.
Paper: New Determinations of the Rotational Periods of 78 Vir (A2p SrCrEu) and 52 Her (A1p SiSrCr)
Authors: Richard Monier, and David Mary
Figure caption: Left: Periodogram of the TESS lightcurve of 52 Her, Right: Periodogram for the TESS lightcurve of 78 Vir.
Paper: The Refined Transit Ephemeris of TOI-2180 b
Authors: Paul A. Dalba, Thomas Lee Jacobs, Mark Omohundro, Robert Gagliano, Jay Jursich, Martti H. Kristiansen, Daryll M. LaCourse, Hans M. Schwengeler, Ivan A. Terentev
Figure caption: Top: individual TESS transits in the PDCSAP light curves with the best fit spline. Bottom: stacked transits and best fit EXOFASTv2 model.
Paper: Characteristics of the Permanent Superhumps in V533 Herculis
Authors: McKenna Leichty, Peter Garnavich, Colin Littlefield, Rebecca Boyle, Paul A. Mason
Figure caption: Left: Amplitude spectra of V533 Her from full TESS light curves for each sector. A strong superhump signal is seen varying around a period of 3.8 hr and a weaker orbital peak is detected with a period of 3.537 hr. Center: The dynamical spectra using a moving 5 days window applied to the TESS data. A varying superhump frequency is evident. The apparent oscillations in the orbital period are an artifact resulting from interference with the stronger superhump signal. The vertical white lines on each plot indicate the data download gap in TESS light curves. Right: The superhump peak amplitude is plotted against its frequency for both sectors, clearly showing a positive correlation between frequency and amplitude. A linear fit to the points is shown as a solid line with a slope of 0.74 ± 0.11 in units of amplitude/(cycles day−1). The fractional difference between the superhump and orbital frequencies (ϵ) is displayed at the top of the plot. The value of ϵ in V533 Her varies by 50%, suggesting that long-term monitoring is needed to fully characterize the superhump properties in long orbital period systems.
Paper: The Line Variability of 78 Vir (A2p SrCrEu) in the Far-ultraviolet
Authors: Richard Monier
Figure caption: Left: Line variations of the C I lines and Al II resonance line (FUV maximum SWP 36485 (in black), FUV minimum SWP 30949 (in blue)), Right: Sensitivity of the emergent flux to changes of the carbon and aluminum abundances.
Paper: Light Curve Test of GRB 200716C as a Gravitationally Lensed Echo
Authors: Oindabi Mukherjee, Robert J. Nemiroff
Figure caption: The light curve of GRB 200716C in 16 ms time bins.
Paper: PyExoRaMa: An Interactive Tool in Python to Investigate the Radius–Mass Diagram for Exoplanets
Authors: Amadori Francesco, Damasso Mario, Zeng Li, Sozzetti Alessandro
Figure caption: GUIs of the tool PYEXORAMA.
Paper: The Effect of Metallicity on the Formation of Massive Black Holes through Stellar Collisions in Young Massive Star Clusters
Authors: Riya Shrivastava, Kyle Kremer
Figure caption: Panel (a) shows the distribution of black hole masses across different initial conditions. As a blue (green) background, we show the assumed range of mass-gap black holes (IMBHs). Panels (b) and (c) show the number of massive black holes and PISNe in each model for different initial conditions (numbers on the horizontal axes denote independent models). Colored text denotes the average number across all ten models for each set of initial conditions.
Paper: Plaskett’s Star and Its Environment
Authors: T. J. Davidge
Figure caption: (Panel a) Proper motion measurements of objects within 1500″ of PS that have G ≤ 16 and parallaxes that fall within 1σ of the PS parallax, referred to in the text as the baseline sample. The regions used to extract the PS (green circle) and comparison (red circle) samples are indicated. PS is marked with a solid green square. (Panel b) The locations of objects on the sky. Objects in the PS sample are indicated with green squares, while those in the comparison sample are red squares and those in the baseline sample are black crosses. PS is plotted as a solid green square. The majority of sources in the PS sample fall to the south of PS, while the majority of sources in the comparison sample are more uniformly distributed. In addition, all but one of the sources in the PS sample to the north of PS fall along a distinct sequence centered near α = 99.°35. (Panel c) The (G, BP − RP) CMD of objects plotted in panel a, with the same identifications as in panel b. The brightest blue sources are in the PS sample, while the comparison sample contains two objects that are possible red supergiants.
Paper: An Early Assessment of the Forecast by the Solar Cycle 25 Prediction Panel
Authors: V. M. S. Carrasco, J. M. Vaquero
Figure caption: (Top panel) Evolution of solar cycles from 1 to 25 according to its smoothed monthly sunspot number provided by SILSO. (Lower panel) Comparison between the forecast by the SC25PP (blue) and the smoothed monthly sunspot number values available by SILSO (red). Blue shadow is the smoothed monthly sunspot number range predicted by the SC25PP.
Paper: The Behavior of HgMn Stars in the Far UV-Paper 11: HD 53929 and HD 172044
Authors: Richard Monier
Figure caption: Left: Absence of variations in SWP 34110 ans SWP 34118 for HD 172044 separated by one day, Right: The strong resonance lines of Ga II at 1414.40 Å and Ga III at 1495.05 Å for HD 172044
Paper: An Update on the Future Flyby of Gliese 710 to the Solar System Using Gaia DR3: Flyby Parameters Reproduced, Uncertainties Reduced
Authors: Raúl de la Fuente Marcos, Carlos de la Fuente Marcos
Figure caption: Future perihelion passage of Gliese 710 as estimated from Gaia DR3 input data and the N-body simulations discussed in the text. The distribution of times of perihelion passage is shown in the top-left panel and perihelion distances in the top-right one. The blue vertical lines mark the median values, the red ones show the 5th and 95th percentiles. The bottom panels show the times of perihelion passage (bottom-left) and the distance of closest approach (bottom–right) as a function of the observed values of the radial velocity of Gliese 710 and its distance (randomly generated using the mean values and standard deviations from Gaia DR3), both as color coded scatter plots of the distribution in the associated top panel. Histograms have been produced using the Matplotlib library (Hunter 2007) with sets of bins computed using Numpy (Harris et al. 2020) by applying the Freedman and Diaconis rule; instead of considering frequency-based histograms, we used counts to form a probability density so the area under the histogram will sum to one. The colormap scatter plot has also been produced using Matplotlib.
Paper: The JWST Resolved Stellar Populations Early Release Science Program. I. NIRCam Flux Calibration
Authors: Martha L. Boyer, Jay Anderson, Mario Gennaro, Marla Geha, Kristen B. Wingfield McQuinn, Erik Tollerud, Matteo Correnti, Max J. Brenner Newman, Roger E. Cohen, Nitya Kallivayalil, Rachel Beaton, Andrew A. Cole, Andrew Dolphin, Jason S. Kalirai, Karin M. Sandstrom, Alessandro Savino, Evan D. Skillman, Daniel R. Weisz, Benjamin F. Williams
Figure caption: M92 CMDs, plotted with different zero-points and color-coded by NIRCam SW detectors. Inset in each panel is a histogram of the F090W–F150W color between the dotted lines, offset in panel (C) to account for the different absolute calibration. The zero-points used to make these CMDs are available in a table behind the figure. Panel (A): Zero-points currently in the JWST pipeline (pmap959), derived with Commissioning data (PID 1074). Several distinct (and overlapping) branches are visible, caused by detector flux offsets. Panel (B): Plotted using the latest NIRCam zero-points, not yet in the JWST pipeline. Panel (C): Zero-points from G. Brammer, derived from LMC data and bootstrapped to the NIRISS flux calibration. Panel (D): 1D luminosity function correction derived from M92 data, normalized to detector B1. Panel (E): 2D KDE correction derived from M92 data normalized to detector B1. Panel (F): Offsets derived from LMC data in the archive, normalized to detector B1.(The data used to create this figure are available.)
Paper: A Significant Sudden Ionospheric Disturbance Associated with Gamma-Ray Burst GRB 221009A
Authors: Laura A. Hayes, Peter T. Gallagher
Figure caption: The VLF amplitude over the full day is shown in (a), with a zoom-in between the vertical lines shown in (b). The X-ray and γ-ray signatures of the GRB from STIX and the GBM (NAI-7) are shown in (c) and (d), respectively. The STIX time is adjusted for the light-travel time of the GRB between Earth and Solar Orbiter (∼15 s)
Paper: Update on Global Helioseismic Observations of the Solar Torsional Oscillation
Authors: Rachel Howe, W. J. Chaplin, J. Christensen-Dalsgaard, Y. P. Elsworth, J. Schou
Figure caption: Rotation residuals from 2dRLS inversions of GONG, MDI, and HMI rotational splitting data, at a target depth of 0.99 R ⊙.
Paper: A Visually Classified Spectroscopic Object Catalog for SDSS-IV MaNGA
Authors: Joshua L. Steffen, Hai Fu
Figure caption: A example of our identification and classification pipeline for a single MaNGA field (Plate-IFU: 12512-12702). The top row shows SDSS pseudocolor images for the MaNGA field. The image on the left shows the 40″ field with SDSS’s PHOTOOBJ catalog overlaid in blue circles and SDSS’s spectroscopic catalog overlaid in red squares. The white hexagon represents MaNGA’s field-of-view. The image in the middle shows the same field but with the cleaned catalog in green circles. The numbers above the green circles are object IDs. The right image shows the same object with a wider field (160″ across). The bottom three rows show the spectra for each object. The black spectra represents the extracted spectra from MaNGA’s data cubes, the red spectra is SPFIT’s best-fit model spectra, and the blue spectra are the best-fit emission lines. In the top left corner of each spectra plot shows the object ID and our spectral classification.
Paper: [Eu/Ba]: Clock and r-process Indicator
Authors: Charles R. Cowley, Robert E. Stencel
Figure caption: [Eu/Ba] vs. Age. Red plus signs: BD18, black dots: DM19. Circled outliers are all metal-rich planet hosts (NASA Exoplanet Archive). See text for blue dot.
Paper: Deriving Median Disk Lifetimes from Disk Lifetime Distributions
Authors: Susanne Pfalzner
Figure caption: Distribution of disk lifetimes assuming an initial disk fraction of 100%. The left panel illustrates the method, the right panel shows the scatter taking the error bars into account panel.
Paper: Updated Spectral Type Polynomials for Ultracool Dwarfs with CatWISE Photometry
Authors: S. Jean Feeser, William M. J. Best, Aniket Sanghi, Michael C. Liu
Figure caption: Polynomial fits for absolute magnitude as a function of spectral type for M6–Y1 field objects with parallax measurements and CatWISE photometry (solid line). We find these are consistent with the previous work of Feeser & Best (2022, dashed line). We provide the rms about the fit for five spectral types ranges: <L0, L0–L4, L4.5–L8, L8.5–T4, ≥T4.5 along the bottom (with colors corresponding to the data); and for the total rms about the fit over all spectral types, indicated in the upper right corner.
Paper: Gaia Astrometry Challenges the High Central Oxygen Abundance Claimed for the Pulsating Helium-Atmosphere White Dwarf KIC 08626021
Authors: Keaton J. Bell
Figure caption: The seismic radius constraint for the pulsating helium-atmosphere white dwarf KIC 08626021 from Giammichele et al. (2018) is >6σ discrepant with the radius constraint from Gaia DR3 astrometry. The asteroseismic measurement is displayed with 1σ error bars. The shaded region corresponds to the 14th and 86th percentile distances from Bailer-Jones et al. (2021) and the solid line to the median.
Paper: TrExoLiSTS: Transiting Exoplanets List of Space Telescope Spectroscopy
Authors: Nikolay K. Nikolov, Aiden Kovacs, Catherine Martlin
Figure caption: Example of the current version of the TREXOLISTS catalog for A: HST WFC3 and B: JWST.
Paper: Hα and Continuum Sizes with the HST/WFC3 G141 GRISM: Outside-in Quenching for z = 1.0–1.4 Fast Quenchers
Authors: Gaël Noirot, Marcin Sawicki
Figure caption: (a) 2D G141 grism data and 1D Hα (blue) and continuum (red) spatial profiles. (b) Age–τ diagram, color-coded by the galaxy size-ratios. Galaxies move with time to the right along lines of constant τ (dashed lines). The green shaded area approximates the transition region between the blue cloud and the red sequence, as determined in N22. (c) Size evolution as a function of time since peak SFR.
Paper: A Meteor Spectroscopic Survey in the Nullarbor
Authors: Hadrien A. R. Devillepoix, Juraj Tóth, Pavol Matlovič, Martin Cupák, Martin C. Towner, Eleanor K. Sansom, Leonard Kornoš, Tomáš Paulech, Pavol Zigo
Figure caption: (a) map of meteor observatories in the Nullarbor. Blue: DFN+AMOS stations. Red: other DFN observatories. Yellow: Ground track of the fireball (finishing South-West toward the ocean). White circles: locations of orbital meteorites recovered by the DFN. (b) photograph of the fireball from the Mundrabilla DFN observatory. (c) stack of the video spectrum recorded by AMOS-Spec-HR at Forrest airport. (d) section of the calibrated spectral profile of the fireball with identified main emission features.
Paper: Keck NIRES Spectral Standards for L, T, and Y Dwarfs
Authors: Christopher A. Theissen, Adam J. Burgasser, Emily C. Martin, Michael C. Cushing, Quinn M. Konopacky, Ian S. McLean, Chih-Chun Hsu, Daniella C. Bardalez Gagliuffi, Adam C. Schneider, Marc J. Kuchner, Jacqueline K. Faherty, Charles A. Beichman, Brittany Miles, Andy Skemer, Sarah E. Logsdon, Aaron M. Meisner, J. Davy Kirkpatrick
Figure caption: NIRES spectral standards (solid colored lines). Low-resolution NIR spectra of the same sources from the SPL are overplotted as dotted gray lines, with the exception of the Y0 standard (HST/WFC3 data from Schneider et al. 2015). Each NIRES spectrum has been shifted to the rest frame wavelength, and NIRES order has been scaled to the low-resolution spectrum and offset by a constant value. Each low-resolution spectrum has been normalized to its median flux between 1.2–1.25 μm. Spectra have also been shifted to the rest frame (see text). Regions of strong telluric absorption have also been masked. Flux zero-points are indicated with the dashed gray lines. The Y dwarf has been downsampled to half its resolution for clarity. Source names, corresponding spectral types, and radial velocities are listed on the right. Key atomic and molecular features are labeled. Subplots highlight features in the 1.1–1.3 μm (top right) and 1.60–1.73 μm regions (bottom right).(The data used to create this figure are available.)
Paper: Solar Calibration of the Convective Mixing Length for Use with the ÆSOPUS Opacities in MESA
Authors: Giulia C. Cinquegrana, Meridith Joyce
Figure caption: Two 3M ⊙, solar metallicity models are compared: one with α MLT = 1.931 (continuous line) and one with α MLT = 2.0 (dashed line). The left panel shows the stellar tracks of the two models. The right panels shows the variance of the helium burning luminosity and radius as the models approach the thermally pulsing AGB.
Paper: The Behavior of HgMn Stars in the Far UV-3: 53 Tau and HD 35548
Authors: Richard Monier
Figure caption: Left: The mean spectral energy distribution of 53 Tauri, Right: The TESS lightcurve of 53 Tauri.
Paper: A Deep Dimming and Abrupt Recovery of a YSO Candidate in MonR2
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Time Series Photometry and Images of [CMD97]-1031: Top—Lightcurve from Gaia G (blue squares), ATLAS o-band with SNR >5 (orange squares), PTF and ZTF r-band (red squares), and ZTF upper limits where image data exist but no photometry was calculated (magenta triangles). Lower Left—Two successive zooms of the lightcurve. Upper panel shows the ATLAS-o data shifted by −0.622 mag in order to match the median brightness with the ZTF-r data, and a Gaussian fit for the dip assuming that the fade starts immediately after an observing season, in the data gap. The resulting fit has amplitude of 2.56 mag, mean JD = 58365, and standard deviation of 60 days. Lower panel highlights the epochs (green circles) for which ZTF images are shown. Lower Right—ZTF images corresponding to 8 different dates, with MJD indicated.
Paper: Evolutionary Status of Selected Post-AGB Stars Based on Gaia DR3
Authors: M. Parthasarathy, Marina Kounkel, Keivan G. Stassun
Figure caption: HR Diagram positions of the sample stars.
Paper: Assessment of the Roche and the Darwin–Radau Approximations for Rotating Astrophysical Objects
Authors: Shin'ichirou Yoshida
Figure caption: Comparison of the rotational angular frequency ω computed by the two analytic formulae. The ratio of the rotational frequency computed by the Roche approximation ω R to the rotational frequency of the self-consistent model (HSCF model) ω 0 is plotted in black. The ratio of the Darwin–Radau frequency ω DR to ω 0 is plotted in gray. The solid curves, the dotted curves, and the dashed–dotted curves correspond to the polytropic indices of N = 1.5, N = 1.0, and N = 3.0, respectively. The dashed curve is produced by fixing the dimensionless moment of inertia which is equal to the value of non-rotating N = 1.5 polytrope. The rightmost point on each curve is the mass-shedding limit point for each polytropic index, which is highlighted by the vertical dotted line.
Paper: The Closest Past Flyby of a Known Star to the Solar System: HD 7977, UCAC4 237-008148 or WISE J072003.20-084651.2?
Authors: Raúl de la Fuente Marcos, Carlos de la Fuente Marcos
Figure caption: Top panels: Past perihelion passage of WISE J072003.20-084651.2 as estimated from input data from Dupuy et al. (2019) and the N-body simulations discussed in the text. The results for UCAC4 237-008148 and HD 7977 are shown in the middle and bottom panels, respectively. The distributions of times of perihelion passage are shown in the left panels and perihelion distances in the right panels. The blue vertical lines mark the median values, the red ones show the 5th and 95th percentiles. Histograms have been produced using the Matplotlib library (Hunter 2007) with sets of bins computed using Numpy (Harris et al. 2020) by applying Freedman and Diaconis’ rule and using counts to form a probability density such as the area under the histogram will sum to one.
Paper: 9-yr Deep Sky unWISE Coadds
Authors: Aaron M. Meisner, Dustin Lang, Edward F. Schlafly, David J. Schlegel
Figure caption: Comparison of Spitzer GLIMPSE360 imaging (Benjamin et al. 2003) vs. our 9 yr static sky unWISE coadds, near the Galactic anticenter. Top: Spitzer ch1 (3.6 μm) compared to W1 (3.4 μm). Bottom: Spitzer ch2 (4.5 μm) compared to W2 (4.6 μm). Spitzer offers ∼3–4× better angular resolution than WISE, but nevertheless our nine-year unWISE coadds are similarly deep. The field center is (α, δ) = (86.°935, 29.°159), (l gal, b gal) = (180.°050, 0.°511) and the field of view is 3.′1 by 2.′7. North is up and east is left.
Paper: Dealing with Large Gaps in Asteroseismic Time Series
Authors: Timothy R. Bedding, Hans Kjeldsen
Figure caption: The top panel shows 15 months of Kepler short-cadence data for KIC 11137075 (Quarters 7–11). The other panels show the power spectra in narrow (2.5 μHz) regions centered on four of the strongest modes (see text). The vertical dashed lines mark the frequencies measured from the full Kepler time series by Tian et al. (2015).
Paper: The Behavior of HgMn Stars in the Far-UV—Paper 15: HD 216494
Authors: Richard Monier
Figure caption: Left: The mean SWP spectral energy distribution of HD 216494 (the resonance lines of Ga II, Ga III and Hg II are depicted as vertical lines); Right: The TESS lightcurve of HD 216494.
Paper: Witnessing a Galaxy Cluster Merger with JWST and a Chandra X-Ray Temperature Map
Authors: Brian C. Alden, Jack O. Burns
Figure caption: Combined ACB X-ray temperature map and JWST infrared image across 6 bands. White contour lines represent the X-ray surface brightness from Chandra X-ray Observatory. The logarithmic contour lines shown begin at 3× the rms background of the image and ascend to just below the peak surface brightness. The cooler region in the north just right of center provides evidence of an infalling subcluster. The coolest portion near the center of the cluster is approximately 5.3 ± 0.6 keV. The heated region opposite of it alludes to a shock front from this merger and has a peak temperature of 10.0 ± 2.1 keV. While more data is necessary to make the claim that a shock is present, the current evidence points in that direction.
Paper: Gangotri Wave—A High Density Gas Ripple in the Inner Galaxy
Authors: V. S. Veena, P. Schilke, Á. Sánchez-Monge, M. C. Sormani, R. S. Klessen, F. Schuller, D. Colombo, T. Csengeri, M. Mattern, J. S. Urquhart
Figure caption:  13CO(2–1) integrated intensity map in the velocity range (a) −55 to −35 km s−1, (b) −75 to −55 km s−1 and (Bottomc) −95 to −75 km s−1 (Gangotri wave). Images resolution is 1′. (d) 3D map of 13CO(2–1) emission overlaid with Gangotri wave (red). (e) 3D map of H I emission from SGPS survey. The red and yellow curves correspond to approximate locations of the Norma and 3 kpc arms.
Paper: Estimation of the Number of Stellar Encounters on a Cross-sectional Area containing a Planetary Disk in Birth Clusters of Stars
Authors: Juan J. Jiménez-Torres
Figure caption: Results of Monte Carlo runs for Equation (1). The first and second frames show the distributions of the number of encounters N  T  vs. the variables v and ρ, respectively. The third frame shows the histogram for the number of encounters. The total number of Monte Carlo runs is 10,000.
Paper: A SuperWASP Light Curve Displaying a Single Long-duration Transit: A Jupiter Size Exoplanet in a Very Distant Orbit?
Authors: Andrew J. Norton, Hugh J. Dickinson, Adam McMaster, Matthew Middleton, Richard G. West
Figure caption: (Upper panel) The SuperWASP light curve of 1SWASP J182438.34 + 302546.0 spanning 8 yr. (Lower panel) A zoom-in to ∼60 days of the light curve during 2004 showing the transit-like event, over-layed with a best-fit transit model.