adsabs/AstroCLIMB huggingface dataset:
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Wavelength-dependent flux variations between Epoch 2018 and Epoch 2020. Left: spectra of VHS 1256 b in Epoch 2018 (blue) and Epoch 2020 (yellow). The solid lines are for the median spectra, and the dashed lines are for the extrema spectra. The shaded regions show the range of spectral variability. Right: representative spectral variability curves. The solid lines show the ﹩{F}_{\max }/{F}_{\min }﹩ flux ratios between the Epoch 2020 maximum and the Epoch 2018 minimum (green), as well as between the Epoch 2020 minimum and the Epoch 2018 minimum (red). For reference, flux ratio curves derived using the extrema of the same epochs are shown in dashed lines (blue for Epoch 2018; yellow for Epoch 2020).
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Comparisons of the observed wavelength-dependent amplitudes and atmospheric model predictions. The spectral variability patterns of the sine waves fall into two categories: Wave 1, Wave 2, and the linear trend match well with the prediction of a partly cloudy model; Wave 3 is better fit with a model involving thermal profile anomalies.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Fitting the multiple-sinusoidal model to light curves integrated in representative bandpasses. The three bandpasses represent the 1.4 μm water absorption band (F139M, middle column) and the continuum (F127M, left column; F153M, right column). The markers are identical to those in Figure 3. The top row shows the comparisons between the model and observed light curves, and rows 2–4 illustrate the individual components. In each row, the y-axis scale is kept consistent for all columns, allowing crude visual comparisons between light curves (e.g., the F127M light curve has a steeper slope and high Wave 1 and 2 amplitudes; the F139M light curve has the highest Wave 3 amplitude).
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Light curves of VHS 1256 b integrated in four representative bandpasses obtained in the 2020 observations: the G141 broad band (black), the F127M filter (blue), the F139M filter (green), and the F153M filter (red). High amplitude brightness modulations are detected in every light curve.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Posterior distributions of the three-sine-wave parameters in a corner plot.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Distribution of the best-fitting periods of a 36 hr light curve segment obtained from a period-recovery test. In this test, a single sine wave is fit to 10,000 random 36 hr segments of VHS 1256 b’s evolving light curve, which is assumed to be the multiple-sinusoidal model that we found in the Epoch 2020 data. We show the results with a histogram that is normalized so that an integral of the probability density equals to 1. The distribution peaks at 17 hr, the average period of Waves 1 and 2. It also has a long tail extending toward long periods, suggesting a nonnegligible probability to detect a signal with period P fit ≥ 22 hr. Two embedded panels show examples of light curve segments fit by models with different periods. Based on this result, we can at least partially attribute the apparent discrepancy in period measurements between the HST and Spitzer observations to the limited observing windows.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Thermal profile of VHS 1256 b and pressure levels probed by various bandpasses. The black solid line is the T-P profile of the best-fitting atmospheric model found by Zhou et al. (2020                      ; T eff = 1000  K, ﹩\mathrm{log}g=3.2﹩, f sed = 1.0, 80% cloud optical depth of the fully cloudy model). The green, blue, and orange horizontal bands/lines mark the pressure levels probed by the WFC3/G141 continuum (λ < 1.30 μm or λ > 1.50 μm), the 1.4 μm H2O band, and the Spitzer 4.5 μm channel, respectively. These pressure levels are mapped from the observed brightness temperatures based on the thermal profile. The lower pressure levels probed by the Spitzer band compared to those by WFC3/G141 may contribute to the difference in period measurements between the two bands.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Alternative decompositions of the broadband light curves. Left: a model composed of three variable spots; right: a model composed of two waves and a variable bright spot. The solid lines, representing the best-fitting models, fit the data reasonably well. The dashed lines show individual model components. The fitting solutions are not unique due to parameter degeneracy. We show additional examples in the Appendix.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Two-spot light curve decomposition.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Two waves + one spot light curve decomposition.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: One wave (k  =  2) + two spots light curve decomposition.
Paper: Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere
Authors: Yifan Zhou, Brendan P. Bowler, Dániel Apai, Tiffany Kataria, Caroline V. Morley, Marta L. Bryan, Andrew J. Skemer, Björn Benneke
Figure caption: Three-spot light curve decomposition.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: Left: HST aperture in black with simulated subapertures on top in white. Right: the corresponding baselines (at 1.7 μm), color-coded by the number of distinct pairs of subapertures that contribute to the point. The 104 subapertures sample 258 spatial frequencies and generate 206 kernel phases.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: Similar to Figure 2, but for 2MASS J1221+0257, a brown dwarf with no companion. Top left: HST/NICMOS NIC1 image (fourth root scaling). Bottom row: Fourier amplitude (left), and Fourier phase (right). Gray circles show the spatial frequencies sampled by the model aperture shown in Figure 1. Top right: Histogram of measured kernel phases. A point source would have kernel phases of 0° (with some noise), as is the case with this target.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: The progression from image to kernel phase for an observation of 2MASS J0147-4954, a brown dwarf with a companion at ∼140 mas ( ∼ 1λ/D) and 2:1 contrast in F170M. Top left: HST/NICMOS NIC1 image (fourth root scaling). Bottom row: Fourier amplitude (left), and Fourier phase (right). Gray circles show the spatial frequencies sampled by the model aperture shown in Figure 1. Top right: Histogram of measured kernel phases. A point source would have kernel phases of 0° (with some noise), which is clearly not the case.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: Histogram of Bayes factors (median value for the five calibrators) for the 117 observations in our sample, color-coded by the assessment from our scramble-and-fit detection method. True (unbinned) positions are indicated with dashes under the histogram. Individual targets are discussed in Section 5.3.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: Stacked 5σ detection limits as a function of separation for all sources in the survey. Filled circles indicate the positions of detected companions, the diamond is our one marginal detection, and Xs indicate literature values for nondetections. Points are color-coded by type of detection and are outlined in the legend. Black symbols indicate companions previously found by PSF fitting. Blue and orange symbols indicate the “significant” and “marginal” detections from Pope et al. (2013), respectively. Green Xs indicate the literature contrast values of the two sources (one in each filter) that we only detected in one filter. Red points indicate the positions of “spurious” detections (see Section 4.3), with dotted lines to gray Xs indicating the literature values. Purple symbols indicate the position of 2MASS 0518-2828 (see Section 4.4). Two sources were extremely wide and were not recovered, due to strong aliasing; they are shown by gray arrows, at a separation given by the labeled text. The survey detection limits in both filters, in units of number of sources, are available as the data behind the figure.(The data used to create this figure are available.)
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: Both filter and dither position images of 2M 0024-0158. The location of the primary is indicated by a black circle, and the location of the best-fit “companion” is shown by a white circle. The locations of bad pixels are indicated with red Xs. Note that, in both dither positions, there is a bad pixel at almost exactly the same location relative to the target—and that in F170M, the bad pixel is located in the first dark ring, while in F110W, it is located in the first bright ring. Our bad-pixel rejection imperfectly replaced the bad pixel on the dark ring and yielded a spurious faint detection in F170M.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: The difference in sensitivity between F110W and F170M (given in units of the number of observations our analysis was sensitive to out of a total of 117) as a function of separation and contrast. F110W is more sensitive at close separations, where the diffraction limit dominates, while F170M is more sensitive globally, because aberrations are smaller with respect to the longer wavelength.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: Similar to Figure 4, but for 2MASS 0024-0158. Large red Xs over the 1D and 2D histograms indicate no detection in the F110W filter. This fit locked onto the signal produced by a bad pixel.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: Similar to Figure 4, but for 2MASS 2204-5646. Our binary model did not recover the true values of the wide companion in this low-S/N observation.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: Similar to Figure 4, but for the spurious fit to 2MASS 0205-1159. This source is a triple system and thus is not well-fit with a binary model.
Paper: NICMOS Kernel-phase Interferometry. I. Catalogue of Brown Dwarfs Observed in F110W and F170M
Authors: Samuel M. Factor, Adam L. Kraus
Figure caption: Similar to Figure 4, but for the marginal detection of 2MASS 2028+0052. Red Xs indicate no detection in F170M.
Paper: A Search for Predicted Astrometric Microlensing Events by Nearby Brown Dwarfs 
Authors: Judah Luberto, Emily C. Martin, Peter McGill, Alexie Leauthaud, Andrew J. Skemer, Jessica R. Lu
Figure caption: The distribution of parallaxes (upper left), π, magnitudes of proper motion (upper right), μ mag, and stellar densities (lower left), σ bg for our sample of 1905 objects. This distribution is used in the random sampling of the motion of an average hypothetical brown dwarf to calculate the probability of an event per year for a hypothetical brown dwarf. Brown dwarfs with high parallax, proper motion, or star density were cut from the plot to show significant data. For the star densities, we computed each data point using a 5′ radius circle. The number of events per year (bottom-right) is calculated for 5000 hypothetical brown dwarfs. For each brown dwarf, π, μ mag, and σ bg were randomly sampled from the known distributions of each observable. This plot is used in comparison to Cushing et al. (2014), who found the probability of events per year for a brown dwarf in the Galactic plane to be near 0.05, instead of our calculated distribution’s trend of <0.0001 events per year. The data above 0.00006 events / year were cut to plot only significant data.
Paper: A Search for Predicted Astrometric Microlensing Events by Nearby Brown Dwarfs 
Authors: Judah Luberto, Emily C. Martin, Peter McGill, Alexie Leauthaud, Andrew J. Skemer, Jessica R. Lu
Figure caption: The maximum separation in milliarcseconds required for an event to yield a given mass uncertainty in M Jup using Equation (4). This is calculated for a brown dwarf with a median parallax from our sample (50.35 mas). Several astrometric uncertainties are plotted, δΔθ = 0.2 mas is inline with current HST capabilities (e.g., Kains et al. 2017). δΔθ = 0.05 mas represents the effective precision a large observing campaign may achieve by taking multiple epoch of data (Sahu et al. 2017; Zurlo et al. 2018) or future space-based astrometric missions (e.g., WFIRST Astrometry Working Group et al. 2019).
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: Cycles 1 and 3 TESS light curves for HD 35833. We show both the Sector 6 (left) and Sector 32 (right) 2-minute cadence data. From top to bottom: SAP (green), PDCSAP (pink), and custom pixel level decorrelation (PLD)-detrended (blue; Sector 32 only). The photometric analysis herein makes use of the PDCSAP reduction (RMS CDPP ≈ 60 ppm) for Sector 6, and the PLD-detrended reduction (RMS CDPP ≈ 100 ppm) for Sector 32. The Sector 32 detrended light curve is available as the data behind the figure.(The data used to create this figure are available.)
Paper: A Search for Predicted Astrometric Microlensing Events by Nearby Brown Dwarfs 
Authors: Judah Luberto, Emily C. Martin, Peter McGill, Alexie Leauthaud, Andrew J. Skemer, Jessica R. Lu
Figure caption: Distribution of δ M L calculated by using a Monte Carlo sampling of α, δ, π, μ  α , and μ δ. The motion and respective uncertainties were the average brown dwarf motions used in this paper. The minimum separation was 12 mas and the mass uncertainty calculated in this fashion is δΔM  L  = 5.88 ±3.28 M jup.
Paper: A Search for Predicted Astrometric Microlensing Events by Nearby Brown Dwarfs 
Authors: Judah Luberto, Emily C. Martin, Peter McGill, Alexie Leauthaud, Andrew J. Skemer, Jessica R. Lu
Figure caption: The path of WISE 0413-4750 from 2022-2042 plotted over a Legacy Survey data release 9 image. The cyan line is the astrometric path of the brown dwarf and the green arrow near the brown dwarf’s path indicates the direction of the brown dwarf, beginning in the bottom left and moving toward the top right. The brown dwarf has a minimum separation in 2031 December of 0.″07 ± 0.″03. While no measurable astrometric microlensing event occurs in this system, it is useful to note that this background star is not found in GDR2, demonstrating the power of deep photometric surveys for providing additional background sources.
Paper: A Search for Predicted Astrometric Microlensing Events by Nearby Brown Dwarfs 
Authors: Judah Luberto, Emily C. Martin, Peter McGill, Alexie Leauthaud, Andrew J. Skemer, Jessica R. Lu
Figure caption: Sky coverage in Galactic coordinates of the Legacy Survey, the upcoming Legacy Survey of Space and Time by the Vera C. Rubin Observatory (VRO), as well as the positions of the brown dwarfs from Kirkpatrick et al. (2021) and Best et al. (2020a; black dots). The Legacy Survey is in purple, VRO is in green, and the overlap is in gray. The Legacy Survey (used in this paper) covers most of the northern hemisphere, while VRO covers the southern hemisphere and the Galactic plane.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: Cycle 4 TESS light curve for HD 35833. We show both the 2-minute cadence data for Sectors 43, 44, and 45. From top to bottom: SAP (green) and PDCSAP (pink). The photometric analysis herein makes use of the PDCSAP reduction (RMS CDPP ≈ 60 ppm) for the combined light curve.
Paper: A Search for Predicted Astrometric Microlensing Events by Nearby Brown Dwarfs 
Authors: Judah Luberto, Emily C. Martin, Peter McGill, Alexie Leauthaud, Andrew J. Skemer, Jessica R. Lu
Figure caption: The mass uncertainty of an astrometric microlensing event of WISE 0413-4750 as predicted using a Monte Carlo simulation. 5000 samples were used, using the uncertainty of the motions and positions of the brown dwarf and the background star. The mass uncertainty is δ M  L  = 32.04 ± 14.76M jup.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: Power spectral density for HD 35833 TESS Sector 6 (top), Sector 32 (middle), and the Cycle 4 data (bottom), with fine sampling in light gray and a boxcar-smoothed power spectrum in black. For Sectors 6 and 43–45, we show the individual oscillation (orange), granulation (green), and white noise (gray horizontal line) components as fit by pySYD as well as the sum of these components (blue). For Sector 32, we show the fitted granulation and white noise components, as well as injected oscillation signals with frequencies set by the signal detected in the Cycle 4 data and amplitudes scaled by 1.23 × (dashed line) and 1.70 × (dotted line) for the 50% and 99% detection limits, respectively.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The relative difference between the predicted and observed values of ﹩{\nu }_{\max }﹩, Δν, A phot, and A RV for grids of possible stellar parameters for HD 35833. The dark swaths indicate regions of parameter space for which the predicted values would be consistent with observations. The T eff and ﹩\mathrm{log}g﹩ values (M ⋆ and R ⋆ values for Δν) given in Table 1 are shown as a white circle (black for A RV), with error bars for the formal uncertainties. We note that the observed values are consistent with predictions for ﹩{\nu }_{\max }﹩ and Δν, and <5σ discrepant for A phot. But there is no reasonable set of stellar parameters that is simultaneously compatible with the aforementioned values as well as with the observed value of A RV.
Paper: Detection of p-mode Oscillations in HD 35833 with NEID and TESS
Authors: Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: Predicted (orange) and observed, decomposed (black) residual amplitude for the decomposed p-mode oscillation signal in the NEID RVs for HD 35833. While the shapes are the same, the amplitude of the observed signal is suppressed relative to predictions by a factor of 2.58 (blue). We also indicate the predicted value of ﹩{\nu }_{\max }^{-1}﹩ as a gray vertical line.