adsabs/AstroCLIMB huggingface dataset:
Paper: How to Become a Mini-moon: Some Hints from 2022 NX1 
Authors: Carlos de la Fuente Marcos, Raúl de la Fuente Marcos
Figure caption: Evolution of the values of the relative mean longitude of 2022 NX1 or difference between the mean longitude of the object and that of Earth, λ r (top panels, see for example Murray & Dermott 1999), its geocentric energy (middle panels), and its motion over the three time intervals that led to temporary captures (negative geocentric energy) in the calculations (bottom panels, ∼1981 in black, ∼2022 in green, and ∼2051 in red). The unit of energy is such that the unit of mass is 1 M ⊙, the unit of distance is 1 au, and the unit of time is one sidereal year divided by 2π. The evolution according to the nominal orbit is shown in the central panels, the left- and righ-hand side panels display results of control orbits with Cartesian vectors separated ± 3σ, respectively, from the nominal values. The trajectories are shown in a frame of reference centered at the Sun and rotating with the Earth, projected on to the ecliptic plane. The output time-step size is 0.1 yr in the top panels and 0.183 day in the rest. The origin of times is epoch 2459800.5 (2022 August 09.0) TDB.
Paper: A Pilot Survey of an M Dwarf Flare Star with Swift’s UV Grism
Authors: Shashank Chavali, Allison Youngblood, Rishi R. Paudel, R. O. Parke Loyd, Karan Molaverdikhani, J. Sebastian Pineda, Thomas Barclay, Laura D. Vega
Figure caption: Swift grism data from the brightest flaring epoch show that AU Mic regularly exceeds the abiogenesis threshold and that the flaring emission is comprised of chromospheric emission lines, Balmer continuum, and possibly blackbody continuum. Left: the average stellar flux from 2000 to 2800 Å is shown as a function of time from the start of Visit 18. The red shaded area shows the abiogenesis threshold level from Rimmer et al. (2018) at 0.31 au (AU Mic’s conservative inner habitable zone edge), and the dashed gray line shows the quiescent stellar flux level. Right: a flare-only spectrum (i.e., the quiescent stellar spectrum is subtracted from the in-flare spectrum) of the brightest data point from the left panel is shown as a black line with the gray shading representing the 1σ uncertainty. Various emission lines and the Balmer continuum are labeled. The colored lines show blackbody curves with temperatures ranging from 5000 to 18,000 K normalized to match the spectrum at 4200 Å.
Paper: Stars on the Verge: From Days to Decades, Studying the Photometric Variations of the Red Supergiant W Persei
Authors: Conor M. Larsen, Edward F. Guinan
Figure caption: Top panel (a): The AAVSO light curve displaying the semi-regular light variations. Middle panel (b): The WWZ plot for W Per. The orange/yellow regions indicate stronger periods. Bottom left panel (c): The CLEANest power spectrum with the four most significant peaks indicated. Bottom right panel (d): The 10 days segment of the TESS pipeline PDCSAP light curve from 2019 mid-November is displayed, showing small (<1 mmag) quasi-periodic light variations on timescales of 0.3 day. Also present is a ∼2 mmag brightness decrease in accord with the downward trend of the AAVSO observations.
Paper: A New Stellar Companion to GJ 1292
Authors: Catherine A. Clark
Figure caption: Left: GJ 1292 and its stellar companion. There is a third, “ghost” peak in the reconstructed image because the phase reconstruction routine was unable to determine the quadrant of the secondary due to low SNR in the bispectrum. Right: Observed and estimated properties for the GJ 1292 system. The uncertainties on the angular separation, position angle, and delta magnitude are from Clark et al. (2022).
Paper: Testing a Galactic Lensing Hypothesis with the Prompt Emission of GRB 221009A
Authors: Joshua S. Bloom
Figure caption: The total magnification of GRB 221009A as a function of correlation timescale Δt for a range of Galactic lens masses at D  l  = 8 kpc. Lines of constant θ  s  are shown in dotted red, labeled in units of milliarcsec. The gray region corresponds to excluded times less than the redshifted timescale associated with a black hole central engine. The vertical lines correspond to the 10% and 50% minimal variability timescale of Fermi events in the 300–1000 keV range from Golkhou et al. (2015) (GRL), corrected to the redshift of GRB 221009A using the median redshift (z GBL = 1.72) of the GRL sample. The horizontal lines labeled at right show the approximate optical depth to massive compact dark matter objects in the Galaxy.
Paper: The Intermediate Polar FO Aquarii Has Not Been the Same Since Recovering from a Series of Low States
Authors: Peter Garnavich, Colin Littlefield, Rebecca S. Boyle, Mark Kennedy
Figure caption: Left Column: Light curves of FO Aqr from 2014 (K2, top) and 2021 (TESS, middle). Each plot displays two consecutive binary orbits with each minimum corresponding to partial eclipse and inferior conjunction of the secondary star. Light curves from two nights in 2022 August are shown at the bottom of the left column. Right Column: The full ASAS-SN light curve of FO Aqr covering 2012–2022 (top). The red band shows the average brightness of FO Aqr excluding the low states. middle: The dynamic power spectrum of the K2 photometry in 2014 and TESS photometry in 2021. A signal at approximately twice the spin frequency appears between orbital phases 0.6 and 0.9. bottom: The flux from FO Aqr as a function of orbital phase and spin phase. For the TESS data, the diagonal feature seen around spin phase of 0.5 is the beat pulse that is not detectable in the K2 photometry.
Paper: Flickering Returns as RS Oph Reestablishes Quiescent Conditions Following its 2021 Nova Outburst
Authors: Ulisse Munari, Fulvio Tabacco
Figure caption: Upper panels: flickering of RS Oph and the five check stars for two of the observing dates. The ordinate scale is the same in all panels. The values for B, B−V, and σ are in magnitudes. Lower-left panel: ANS Collaboration B-band light-curve of RS Oph during the 2021 nova outburst. Two levels of B-band brightness in quiescence are indicated (median values from the ANS Collaboration long-term monitoring): B = 12.24 mag characterizing the first 10 years following the 2006 eruption, and B = 11.94 mag for the last 5 years preceding the 2021 outburst. Lower-right panel: summary of the results of our observations in search for flickering in RS Oph following its emergence from Solar conjunction.
Paper: Signs of Emissions of Alkali Metals Na I, Li I, and K I During First Minutes After DART Probe Crash on Dimorphos
Authors: Shestakova L. I., Serebryanskiy A. V., Krugov M. A., Aimanova G. K., Omarov Ch. T.
Figure caption: Spectra of Didymos & Dimorphos double asteroid taken on 2022 September 26 during DART impact event.
Paper: Measures of Variance on Windowed Gaussian Processes
Authors: Daeyoung Lee, Charles F. Gammie
Figure caption: The mean and variance of ﹩{\sigma }_{T}^{2}﹩ and M  T  for a damped random walk, along with the covariance and correlation of these measurements on consecutive windows, as functions of the window length T/τ, averaged over 107 realizations with σ = 0.24 and μ = 2.4. Analytic results, where available, are shown in red. The means are normalized by σ 2 and σ/μ, respectively, and the variance and covariance are normalized by σ 4 and (σ/μ)2.
Paper: Scant Evidence for the Gangotri Wave
Authors: T. M. Dame
Figure caption: The upper figure (a) is a reproduction of Figure 1 from Veena et al. using the CO survey of Dame et al. (2001) this map has slightly lower angular resolution (8′ vs. 5′), but a wider latitude range. Deviations from the plane here look smaller than those in the Venna et al. map because they stretched latitude relative to longitude by a factor of ∼2.7. The lower figure (b) is a similar map of CO in the 4th Galactic quadrant, but shifted lower in velocity by 20 km                 s −1  (−75 to −55 km s−1). To first order, both maps simply show the Galactic plane, not giant filaments, and both are quite similar in terms of vertical thickness and “ripples” above and below b = 0°. (The Galactic plane in the bottom map should be somewhat thicker because it covers emission at lower velocities and consequently nearer distances.)
Paper: Disk Material Inflates Gaia RUWE Values in Single Stars
Authors: Shannon Fitton, Benjamin M. Tofflemire, Adam L. Kraus
Figure caption: (a) Confirmed single and binary systems in our sample. (b) RUWE distribution for single stars, with 95th percentile indicator for disk-bearing, single-stars sample. (c) CDF of disk-bearing and disk-free stars, with the vertical line indicating the KS test value.
Paper: Introducing MEGASIM: Multitudinous Earth Greek/Trojan Asteroid SIMulation 
Authors: Travis Yeager, Nathan Golovich
Figure caption: Stacked maps of ETAs from the WHFast integrated simulation. Positions are of all remaining ETAs every 100 kyr for 1 Gyr beginning at 100 kyr integration time. The left panel shows the cumulative positions projected onto the ecliptic sky coordinates as viewed from Earth. The Sun is at position (0, 0), the black dot is L4 at (0, 60°) and the red cross indicates the location of highest density. The right panel shows the view from above onto the Ecliptic. The Sun is at (0, 0) and the concentric black circles starting nearest the Sun are the approximate orbits of Mercury, Venus, Earth and Mars.
Paper: Applying Random Forest Classification to Ultracool Dwarf Discovery in Deep Surveys. II. Color Classification with PanSTARRS, 2MASS, UKIDSS, and WISE Photometry
Authors: Eduardo Gauna Gutierrez, Arantxa Mendiola Maytorena, Zijie Gong, Adriana Nava Vega, Carlos Verdaguer, Christian Aganze, Christopher Danner, Adam J. Burgasser
Figure caption: Assessment of RF classification for ultracool dwarfs. (a) Confusion matrix for the UCD/non-UCD classifier. Diagonal elements indicate number of correct classifications, off-diagonal elements indicate number of mis-classifications. (b) Confusion matrix for UCD spectral group classification. (c) Feature importance plot indicating the relative importance of various colors in determining UCD spectral group classifications. (d) Comparison of actual and predicted UCD spectral types based on the RF regressor model.
Paper: A Linear Divider Between the Blue Sequence and Red Sequence in Color–Magnitude Space
Authors: Derrick James, Barbara S. Ryden
Figure caption: Color–magnitude diagram (u − r vs. M  r ) for the SDSS galaxy sample. Blue dots are the optimal 〈u − r〉 for each absolute magnitude bin. Cyan line is the linear color divider.
Paper: Using Stellar Rotation to Identify Tidally Stripped Members of the Praesepe Open Cluster
Authors: Jessica McDivitt, Stephanie T. Douglas, Jason Lee Curtis, Mark Popinchalk, Alejandro Núñez
Figure caption: (Left) Color–period diagram for Praesepe showing that the majority of our newly identified rotators (black stars) are consistent with the P rot distribution of the cluster core (gray points). We can conclude that these stars were probably once members of the Praesepe core. Four stars are outliers; three of these become consistent with the cluster core if we double their periods (blue stars). (Right) Color–magnitude diagram for Praesepe, showing the locations of candidate tidal tail members with (colored stars) and without (open stars) measured P rot. Core cluster members with measured rotation periods are also shown (gray points). The 92 target rotator data is available as the data behind the Figure.(The data used to create this figure are available.)
Paper: HIPPI-2 Commissioned at MIRA
Authors: Daniel V. Cotton, Jeremy Bailey, Jeff Larson, Wm. Bruce Weaver, Jean Perkins, Glenn Henderson
Figure caption: HIPPI-2's performance on MIRA's 36 inch telescope. Colors denote effective wavelength. Panel (a) shows the scatter in repeat ﹩g^{\prime} ﹩ observations of bright stars compared to their means (α Boo [10.2, 0.1], α Aql [−3.6 , 0.9], α Cep [−43.3, −17.0]); plotted with internal measurement errors only. Panel (b) shows TP observations and band means. Panel (c) plots the bandpass-derived fit and the resulting match (colored symbols) to broadband observations (open symbols) of standards. Panel (d) shows the projected instrument performance based on these data.
Paper: A Multiwavelength Study of the Ongoing Changing-look AGN AT2021fxu
Authors: Yukta Ajay, Muryel Guolo, Dheeraj Pasham
Figure caption: (a) Optical spectrum of the host galaxy in 2001 (black), and the optical spectrum post-outburst in 2022 May (blue) showing the appearance of BELs and a strong blue continuum; (b) Unfolded spectra and models for Swift/XRT data between 2011–2012 (before the optical outburst), and Swift/XRT and NICER between 2022 June and August (post-outburst); (c) Optical and UV light curves from Swift/UVOT; (d) Swift/XRT and NICER X-ray light curves, zoomed in plot shows short-term X-ray variability.(The data used to create this figure are available.)
Paper: Synthetic Color–Magnitude Diagrams for the Globular Cluster 47 Tucanae
Authors: Tianxing Zhou, Angelica Whisnant, Roman Gerasimov, Adam J. Burgasser
Figure caption: Theoretical isochrones of 47 Tucanae calculated in this study for HST Advanced Camera for Surveys (Left) and JWST NIRCam (Right). The nominal chemical abundances are shown in the middle panel. The inferred intrinsic scatter is indicated for selected elements, shown in green. Data from Kalirai et al. (2012) are overplotted with the HST isochrones for comparison. The two boundary condition (BC) schemes described in text are represented with red and black curves. An equivalent isochrone for solar abundances is shown in blue.(The data used to create this figure are available.)
Paper: Light Curve Analysis of Nine Algol (EA) Eclipsing Binaries Discovered During the Dauban Survey
Authors: David H. Hinzel
Figure caption: Light Curves for V242, V243, V244, and V247.
Paper: Quick-look Pipeline Light Curves for 5.7 Million Stars Observed Over the Second Year of TESS’ First Extended Mission
Authors: Michelle Kunimoto, Evan Tey, Willie Fong, Katharine Hesse, Avi Shporer, Michael Fausnaugh, Roland Vanderspek, George Ricker
Figure caption: Left: the celestial coordinates of targets with QLP light curves from the northern ecliptic hemisphere (Sectors 40, 41, and 47–55) and ecliptic (Sectors 42–46), with sector numbers annotated over the centers of Camera 1. Targets are color-coded by the number of observed sectors, either 1 (red), 2 (orange), 3 (yellow), 4–10 (green), or 11 (blue). Right: 1 hr photometric precision of 16,000 randomly selected light curves from each orbit across Sectors 40–55. The 50th and 10th percentiles of the precision binned every ΔT = 0.1 mag are shown in orange and red, respectively.
Paper: Planetary Line-to-accretion Luminosity Scaling Relations: Extrapolating to Higher-order Hydrogen Lines
Authors: Gabriel-Dominique Marleau, Yuhiko Aoyama
Figure caption: Fit coefficients of the planetary L acc–L line relation (Equation (1)) for Lyman (n f = 1) to Brackett (n f = 4) lines. Circles: direct fits of L acc–L line (A021 and see text). Black lines: our fit of a and b (Equation (2)). Golden squares: Alcalá et al. (2017) for Balmer lines.
Paper: Light Curve Analysis of Nine Algol (EA) Eclipsing Binaries Discovered During the Dauban Survey-additional Data
Authors: David H. Hinzel
Figure caption: Light Curves for V239, V240, V241, V245, and V246.
Paper: Re-evaluation of the Effect of Brown Dwarfs’ Viewing Geometry using a Bayesian Framework
Authors: Mateo E. Guerra Toro, Yifan Zhou, Brendan P. Bowler
Figure caption: Newly obtained inclination distributions for two brown dwarfs, 2M0103+19 (top left) and SIMP0136 (top right). The distributions obtained by the MCMC and the MC methods of 2M0103+19 and SIMP0136 are shown in red and black, respectively. For 2M0103+19, the distributions of ﹩\cos i﹩ are similar, but for SIMP0136, the MCMC and MC results are significantly different. We derive new linear correlations between variability amplitude and inclination (bottom left), and between color anomaly and inclination (bottom right). The dark and light swashes represent the 1σ and 2σ ranges of the distributions of the linear correlations. Regressions derived from the published inclinations from Vos et al. (2017) are presented with red and blue lines for comparison.
Paper: Pre-maximum Evolution of the Classical Nova YZ Reticuli
Authors: Mariko Kato, Hideyuki Saio, Izumi Hachisu
Figure caption: (top) List of our models. From left to right, the WD mass, mass accretion rate in the quiescent phase, the mass fraction of additional carbon, recurrence period, duration of X-ray flash τ X, maximum nuclear burning rate ﹩{L}_{\mathrm{nuc}}^{\max }﹩, ignition mass, and time of the optical maximum since the onset of shell flash t peak. We assumed the chemical composition of the accreted matter to be X = 0.7, Y = 0.28, and Z = 0.02, except for model J. In model J, the accreting matter is already enriched by carbon, i.e., X = 0.7, Y = 0.18, C = 0.1, and Z = 0.02. (a) τ X against t peak. (b) τ X against ﹩{L}_{\mathrm{nuc}}^{\max }﹩. (c) t peak against ﹩{L}_{\mathrm{nuc}}^{\max }﹩. The red symbols correspond 1.3 M ☉ WD model, while the black symbols 1.35 M ☉ WD. The shaded region indicates t peak > 4.1 days and dashed line denotes t peak = 2.8 days.
Paper: Estimating Aerodynamic Properties of Planetary Surfaces using Drone Attitude
Authors: Brian Jackson
Figure caption: (a) Field set-up. The four anemometers measuring wind speeds at various heights are in the background. The drone is hovering flush with the uppermost anemometer. (b) Drone telemetry (curves) and wind speed (purple dots) collected by the uppermost anemometer (in m s−1). The dashed blue curve shows the drone altitude (in m), the solid orange curve shows the tilt (in degrees), and the dashed–dotted green curve shows the yaw (in degrees azimuth). The gray shaded regions show when the drone settled at a fixed altitude and attitude, allowing determination of an average tilt (shown by the horizontal solid black lines). (c) Inferred wind speeds at each altitude (blue dots), along with uncertainties estimated by combining in quadrature the uncertainties on the drone tilt and on the tilt-wind speed relationship. The dashed, orange line shows the model fit, and wind profile parameters with uncertainties are indicated.
Paper: Extension of the Asfgrid for Correcting Asteroseismic Large Frequency Separations
Authors: Dennis Stello, Sanjib Sharma
Figure caption: Grid points in Mass and [Fe/H] of the original grid from Sharma et al. (2016) (black) and our new extension (red).
Paper: Evolutionary Status of Selected Post-AGB Single and Binary Stars in Gaia DR3
Authors: M. Parthasarathy, Marina Kounkel, Keivan G. Stassun
Figure caption: (top) HR Diagram positions of the sample stars, and (bottom) RUWE values vs. ﹩\mathrm{log}{L}_{\mathrm{bol}}﹩. Post-AGB stars are shown with open symbols, post-AGB binary stars are shown with filled symbols.
Paper: Polar Upwelling at Three Sunspot Minima
Authors: Roger K. Ulrich, Tham Tran, John E. Boyden
Figure caption: Comparison of the latitude and time dependence of the rotation rate deviation δ ω (Top plot) to the line-of-sight velocity offset δ V (Bottom plot). For δ V poleward flow is positive in both hemispheres. Times of sunspot minima are shown by the arrows below the figure and by the vertical lines through the figure.
Paper: VVV J165507.19-421755.5: A Nearby T Dwarf Hidden in the Galactic Plane
Authors: Noah Schapera, Dan Caselden, Aaron M. Meisner, Adam J. Burgasser, Adam C. Schneider, Austin Humphreys, Chih-Chun Hsu, Emma Softich, Leigh C. Smith, Philip W. Lucas, J. Davy Kirkpatrick, Federico Marocco, Jacqueline K. Faherty, Marc J. Kuchner, Michael C. Cushing
Figure caption: Figure 1.1: Smoothed NIRES spectrum of J1655−4217 (green line), compared to low-resolution T4, T5 and T6 spectral standards (blue, purple, and brown lines, respectively; data from Burgasser et al. 2004). T5 provides the best match. Measured and inferred properties of this object are summarized in the upper right. Figure 1.2: VVV K-band images of J1655−4217 in 2010 and 2015. The red circle highlights the 2010 position (left) and the blue circle highlights the 2015 position (right).
Paper: Sudden Dimming of the Symbiotic Mira HM Sge
Authors: Steven R. Goldman, Ravi Sankrit, Nathan Wolthuis, Sean Garner, Carlo Gualdoni, Simone Bolzoni
Figure caption: The brightness of HM Sge in BVIR filters over the past 20 yr and the recent dimming in B, R, and I filters. While the sinusoidal pattern in the I-band is linked to the AGB pulsation, the recent drop in brightness appears independent of this variability; this figure includes only a subset of the available AAVSO data.
Paper: Ten-micron Emission in a Color–magnitude Diagram of M Giant Variables
Authors: Graeme H. Smith
Figure caption: Color–magnitude diagrams and a period-magnitude relation for M giant stars from Noguchi (1990). In all three panels, filled and open circles denote the presence or absence, respectively, of 10 μm emission as recorded in IRAS spectrometry. The top panel shows the (M  Ks , J − K  s ) diagram from 2MASS photometry, while a M  K,IRC vs. (I − K)IRC diagram derived from TMSS photometry is given in the middle panel. Dashed lines in these two panels designate a proposed boundary in the CMD to the location of most M giants with 10 μm emission. Bottom panel shows period (in days) vs. absolute K  s  magnitude; the dashed line indicates ﹩\mathrm{log}P(\mathrm{days})=1.7﹩.
Paper: Smallest Scale Clumpy Star Formation in Stephan’s Quintet Revealed from UV and IR Imaging
Authors: P. Joseph, K. George, S. Subramanian, C. Mondal, A. Subramaniam
Figure caption: Clockwise from the top-left panel: (a) RGB image of SQ created by assigning red (JWST F200W band), green (JWST F150W band) and blue (UVIT F148W+F169M band) colors to the filter passband images. (b) RGB image of SQ created by assigning red (JWST F770W band), green (JWST F200W band) and blue (UVIT F148W+F169M band) colors to the filter passband images. (c) Distribution of the size of segments (diameter in arcsec and pc).
Paper: VLT/CRIRES Science Verification Observations: A hint of C18O in the Young Brown Dwarf 2M0355
Authors: Yapeng Zhang, Ignas A. G. Snellen, Matteo Brogi, Jayne L. Birkby
Figure caption: Panel (a): K-band (2.32–2.37 μm) spectrum of the brown dwarf 2M0355 taken with VLT/CRIRES. The orange line shows the best-fit model obtained through the retrieval analysis. The blue and green lines are the template spectra of 13CO and C18O. The observational residuals (namely, observations minus the model with main isotopes only) are shown in gray. Panel (b): Cross-correlation functions of the observational residuals with the 13CO or C18O template. Panel (c): Posterior distribution of the carbon isotope abundance ratio constrained by the retrieval. The vertical dashed lines denote the 1σ interval. Panel (d): Same as panel (c), but for the oxygen isotope ratio.
Paper: Kepler K2 Observations of the Faint, Understudied Polar SDSS J092122.84+203857.1
Authors: Bradley O'Brien, Sierra Sanne, Colin Littlefield
Figure caption: Top: Representative half-day segment of the light curve of J0921. The orbital profile is difficult to distinguish from noise. Middle: Power spectrum of J0921. The orbital frequency (Ω) is labeled at 17.099 cycles day−1, as are its 2Ω and 3Ω harmonics. Spurious frequencies (Baran 2013) are marked with a green “X.” Bottom: Phase-averaged orbital light curve of J0921.
Paper: Prediction of an Earth-sized Planet Formed in the Habitable Zone of the SPECULOOS-2 System
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: Top: Probability distributions of predicted exoplanet periods (green) and HZ evolution (blue) for SPECULOOS-2. Bottom: HZ evolution for TRAPPIST-1. TRAPPIST-1e forms interior to the HZ, while PxP-3 likely formed within the HZ.