adsabs/AstroCLIMB huggingface dataset:
Paper: Siena Galaxy Atlas 2020
Authors: John Moustakas, Dustin Lang, Arjun Dey, Stéphanie Juneau, Aaron Meisner, Adam D. Myers, Edward F. Schlafly, David J. Schlegel, Francisco Valdes, Benjamin A. Weaver, Rongpu Zhou
Figure caption: Optical mosaics of 42 galaxies from the SGA-2020 sorted by increasing angular diameter from the top left to the bottom right. Galaxies are chosen randomly from a uniform (flat) probability distribution in angular diameter. The horizontal white bar in the lower left corner of each panel represents ﹩1^{\prime} ﹩, and the mosaic cutouts range from ﹩3\buildrel{\,\prime}\over{.} 2﹩ to ﹩13\buildrel{\,\prime}\over{.} 4﹩. This figure illustrates the tremendous range of galaxy types, sizes, colors, and surface-brightness profiles, internal structure, and environments of the galaxies in the SGA.
Paper: Siena Galaxy Atlas 2020
Authors: John Moustakas, Dustin Lang, Arjun Dey, Stéphanie Juneau, Aaron Meisner, Adam D. Myers, Edward F. Schlafly, David J. Schlegel, Francisco Valdes, Benjamin A. Weaver, Rongpu Zhou
Figure caption: Distribution of 531,677 galaxies in the SGA-2020 parent sample in an equal-area Mollweide projection in equatorial coordinates, binned into 3.4 deg2 healpix pixels (Zonca et al. 2019). The dark gray curve represents the Galactic plane. Note the significant variations in galaxy surface density, which we attribute to surface-brightness incompleteness and heterogeneity in the aggregate HyperLeda catalog.
Paper: Siena Galaxy Atlas 2020
Authors: John Moustakas, Dustin Lang, Arjun Dey, Stéphanie Juneau, Aaron Meisner, Adam D. Myers, Edward F. Schlafly, David J. Schlegel, Francisco Valdes, Benjamin A. Weaver, Rongpu Zhou
Figure caption: Like Figure 5, but for PGC 193192, the second-largest member of the PGC 193199 Group.
Paper: Wavelengths and Energy Levels of the Upper Levels of Singly Ionized Nickel (Ni II) from 3d 8(3 F)5f to 3d 8(3 F)9s 
Authors: Christian P. Clear, Juliet C. Pickering, Gillian Nave, Peter Uylings, Ton Raassen
Figure caption: Diagram showing (a) the subconfigurations of the singly excited (normal) system 3d 8(3 F)nl of Ni II and (b) only the high-lying subconfigurations. The height of the boxes indicate the maximum energy range of the levels in each subconfiguration. The f, g, and h levels are each split into three groups by the J  c  values of the Ni III parent core (J  c  = 2, 3 or 4).
Paper: Nonequilibrium Ionization Effects on Synthetic Spectra in the AWSoM Solar Corona
Authors: J. Szente, E. Landi, B. van der Holst
Figure caption: Plasma emission calculated assuming EI (left), NEI (center) and showing the nonequilibrium/equilibrium ratio (right) for ions: Si X (253.790 Å, ﹩\mathrm{log}T=6.15﹩), S X (264.230 Å, ﹩\mathrm{log}T=6.17﹩), Si XI (303.325 Å, ﹩\mathrm{log}T=6.22﹩), and Si XII (520.665 Å, ﹩\mathrm{log}T=6.29﹩).
Paper: Nonequilibrium Ionization Effects on Synthetic Spectra in the AWSoM Solar Corona
Authors: J. Szente, E. Landi, B. van der Holst
Figure caption: Plasma emission in terms of the nonequilibrium/equilibrium ratio for ions (top to bottom): O VI (1031.912 Å, ﹩\mathrm{log}T=5.5\,{\rm{K}}﹩) and Ne VIII (770.428 Å, ﹩\mathrm{log}T=5.8\,{\rm{K}}﹩).
Paper: Nonequilibrium Ionization Effects on Synthetic Spectra in the AWSoM Solar Corona
Authors: J. Szente, E. Landi, B. van der Holst
Figure caption: Electron temperature (left) and radial speed (right) on magnetic field lines. The solar surface is colored with the contour of the magnetic field strength.
Paper: Nonequilibrium Ionization Effects on Synthetic Spectra in the AWSoM Solar Corona
Authors: J. Szente, E. Landi, B. van der Holst
Figure caption: Plasma emission in terms of the nonequilibrium/equilibrium ratio for ions (left to right): Mg VII (276.154 Å, ﹩\mathrm{log}T=5.8\,{\rm{K}}﹩), Mg VIII (772.260 Å, ﹩\mathrm{log}T=5.9\,{\rm{K}}﹩), Mg IX (706.060 Å, ﹩\mathrm{log}T=6.0\,{\rm{K}}﹩), and Mg X (624.941 Å, ﹩\mathrm{log}T=6.1\,{\rm{K}}﹩).
Paper: Nonequilibrium Ionization Effects on Synthetic Spectra in the AWSoM Solar Corona
Authors: J. Szente, E. Landi, B. van der Holst
Figure caption: Plasma emission in terms of the nonequilibrium/equilibrium ratio for ions (left to right): Si VII (275.361 Å, ﹩\mathrm{log}T=5.8\,{\rm{K}}﹩), Si VIII (316.218 Å, ﹩\mathrm{log}T=5.9\,{\rm{K}}﹩), and Si IX (290.690 Å, ﹩\mathrm{log}T=6.1\,{\rm{K}}﹩),
Paper: Wavelengths and Energy Levels of the Upper Levels of Singly Ionized Nickel (Ni II) from 3d 8(3 F)5f to 3d 8(3 F)9s 
Authors: Christian P. Clear, Juliet C. Pickering, Gillian Nave, Peter Uylings, Ton Raassen
Figure caption: Determination of the ionization energy of Ni II using the 3d 8(3 F)5g, 3d 8(3 F)6g, and 3d 8(3 F)6h levels. The intercept for each configuration is ﹩{IE}-\alpha {R}_{{\rm{Ni}}}{Z}_{c}^{2}\langle {r}^{-4}{\rangle }_{{nl}}﹩.
Paper: Wavelengths and Energy Levels of the Upper Levels of Singly Ionized Nickel (Ni II) from 3d 8(3 F)5f to 3d 8(3 F)9s 
Authors: Christian P. Clear, Juliet C. Pickering, Gillian Nave, Peter Uylings, Ton Raassen
Figure caption: Comparison between the revised energy levels of this work and values previously published by Sugar & Corliss (1985). The newly revised values minus the previously published values are plotted against the newly revised energies with error bars in red for previously published values and in black for our new energy levels.
Paper: Nonequilibrium Ionization Effects on Synthetic Spectra in the AWSoM Solar Corona
Authors: J. Szente, E. Landi, B. van der Holst
Figure caption: Plasma emission ratios of plasma assuming NEI vs. EI for iron ions Fe VIII to Fe XII. The peak formation temperatures for the lines presented in this figure can be found in Table 1.
Paper: HAFFET: Hybrid Analytic Flux FittEr for Transients
Authors: Sheng Yang, Jesper Sollerman
Figure caption: As shown in the lower-left panel of Figure 7, we fit the Arnett and tail functions to the Lyman-inferred bolometric luminosity LC of SN 2020bcq (ZTF20aajcdad) as an example. The marginalized parameter distributions are shown as corner plots in this figure. In the left panel, we fit the Arnett model by using the explosion epoch from our earlier power-law fits, while in the middle plot we treat the explosion epoch as a free parameter in the Arnett model. The predicted rise time from the Arnett model, i.e., the time between the estimated explosion epoch to peak, is 13.93 days, which is comparable to the estimate from the power-law fits (13.14 days). The slight difference in the explosion epoch does not change the nickel mass estimate but modifies τ  m  from 9.6 to 10.6 days. The marginalized parameter distributions of the tail fitting are shown as corner plots to the right. The best-fit nickel mass is 0.04 solar masses, which is roughly half that inferred from the Arnett model.
Paper: HAFFET: Hybrid Analytic Flux FittEr for Transients
Authors: Sheng Yang, Jesper Sollerman
Figure caption: Various models fit to the bolometric LC of SN 2020bcq (the open circles). The realization with the best-fit Arnett and tail models are shown by models 1 and 2 (the solid cyan and red lines; see also the lower-right panel of Figure 7). From model 1, we obtain the posterior distributions of M Ni and τ  m , which can be translated into M Ej and E Kin together with a velocity measurement (∼10,000 km s−1). We use the parameters obtained from model 1 to reproduce a tail bolometric, model 3 (the brown line). We adapted its γ trapping opacity (model 4, κ  γ  from 0.027–0.05 cm2 g−1) or photospheric velocity (model 5, V ph from 10,000–5000 km s−1) so that the tail can be brighter to match the observed data.
Paper: HAFFET: Hybrid Analytic Flux FittEr for Transients
Authors: Sheng Yang, Jesper Sollerman
Figure caption: As shown in the upper panel of Figure 7, we fit the multiband LCs following analytic models of Bazin et al. (2009) with SN 2020bcq (ZTF20aajcdad) as an example. Such fits can be done in different routines, and in this plot we compare the fitting results between them. The parameter distributions from MCMC on r-band LCs are shown as corner plots. The vertical dashed lines in the marginalized parameter histograms represent the 16th and 84th percentile of all burn-in samples, which correspond to the 1σ posterior parameter distributions from the scipy minimize routine (the green box).
Paper: HAFFET: Hybrid Analytic Flux FittEr for Transients
Authors: Sheng Yang, Jesper Sollerman
Figure caption: Magnetar model fitting on SN 2015bn via HAFFET. We construct the bolometric LC of SN 2015bn with g and r magnitudes with the analytic bolometric correction for stripped-envelope SNe derived in Lyman et al. (2014). They are shown as black and blue open circles. As shown, they are quite similar to the one from Nicholl et al. (2016), i.e., the red circles. The cyan dashed lines are reproduced with the fitted magnetar model samplings. The parameter contours are shown to the right, which is similar to the estimates of Nicholl et al. (2016, their Figure 4).
Paper: HAFFET: Hybrid Analytic Flux FittEr for Transients
Authors: Sheng Yang, Jesper Sollerman
Figure caption: Comparison of M Ni between Arnett fits and fits to the radioactive decay tail. The ZTF SNe Ibc (the subset of SNe in Paper I that clearly shows a tail) are shown with black dots, while the sample from Afsariardchi et al. (2021; a selection from the literature, including 27 stripped-envelope SNe) is shown with red dots. The blue dashed line is the one-to-one relation. As shown, the Arnett inferred M Ni is systematically higher than those from the tails.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The intraday periodic results calculated by the the REDFIT program, where the black lines stand for the signal, the colored lines stand for the Gaussian fitting, and the colored dotted lines stand for the theoretical red-noise spectra of 80%, 90%, 95%, and 99% significance levels, respectively.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The ΔT and Δm distributions at the gri bands. The black, red, and green lines stand for the values from the g band, r band, and i band, respectively. The cyan lines stand for the Gaussian fitting.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The IDVs at the g band. The black dots stand for the lightcurves, the red dots stand for the magnitude difference between two comparison stars, and the colored lines stand for the different stages.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The IDVs at the i band. The black dots stand for the lightcurves, the red dots stand for the magnitude difference between two comparison stars, and the colored lines stand for the different stages.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The g, r, and i fitting results of the four comparison stars. The black solid dots stand for U, B, V, R, and I data, the red solid dots stand for g, r, and i data, and the red lines stand for the least-square fitting curves.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The g, r, and i lightcurves. The black solid dots stand for the g lightcurve, the red solid dots stand for the r lightcurve, and the green solid dots stand for the i lightcurve.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The distributions of the time rates of the IDVs at the gri bands. The black, red, and green lines stand for the values from the g band, r band and i band, respectively.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The IDVs at the r band. The black dots stand for the lightcurves, the red dots stand for the magnitude difference between two comparison stars, and the colored lines stand for the different stages.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The correlation relations between the flux densities (F  gri ) and spectral indices (α), where the light red area stands for the 95% confidence band, and the dark red area stands for the 95% prediction band.
Paper: Optical Monitoring and Intraday Variabilities of BL Lacertae
Authors: Y. H. Yuan, G. J. Du, J. H. Fan, Y. Liu, J. H. Yang, G. Z. Ding, Z. Y. Pei
Figure caption: The correlation between the g magnitude (m  g ) and color index (m  g  − m  i ), where the colored dots stand for distributions of different stages, the green lines stand for the linear fitting, and the rectangular boxes mark the time range of observations (JD +2459000).
Paper: Statistical Analysis of Long GRBs’ Prompt Emission and X-Ray Flares: Multivariate Clustering and Correlations
Authors: Joseph Saji, Shabnam Iyyani, Kratika Mazde
Figure caption: (a) α  P  is plotted against α  F . (b) F  P,peak is plotted against F  F,peak. (c) The ratio of F  P,peak to F  F1,peak and F  F2,peak is plotted against T  P,100 as black circles and blue squares, respectively. (d) The ratio of F  F1,peak to F  F2,peak is plotted against T  P,100 as blue circles and the ratio of F  F2,peak to F  F3,peak as red circles. (e) F  P,peak is plotted against T  P,100. (f) F  F,peak is compared against T  F,100. (g) F  P,peak is plotted against T  P,var. (h) F  F,peak is compared against T  F,var. (i) F  P,peak is plotted against T  q . (j) F  F,peak is compared against T  q . The linear fit modeling the correlations in (h) and (j) is shown as red solid lines. The parameters of flares occurring during the plateau phase of the afterglow are highlighted as green unfilled circle and square markers for the first and second episodes of the flares, respectively.
Paper: Statistical Analysis of Long GRBs’ Prompt Emission and X-Ray Flares: Multivariate Clustering and Correlations
Authors: Joseph Saji, Shabnam Iyyani, Kratika Mazde
Figure caption: (a) T  F,100 is plotted against T  P,100. The black circles, blue squares, and red triangles represent the first, second, and third X-ray flaring episodes, respectively. The same color code and markers are used hereafter. The green dashed line represents when T  P,100 = T  F,100. (b) T  F,var is plotted against the corresponding T  P,var. (c) T  F,var is plotted against T  F,100. The linear fit in the log space is shown by the red solid line. The shaded red and blue regions correspond to the 1σ and 2σ deviations of the data from the fit. The color code represents the same contours hereafter. (d) T  P,100 is plotted against T  P,var. (e) T  q  is plotted against T  F,100. (f) T  q  is plotted against T  P,100. Note that the gray diamonds, which represent GRBs with quiescent periods equal to zero, are not included in the modeling of the correlation. The parameters of flares that occur during the plateau phase of the afterglow are marked as green unfilled circles and squares for the first and second episodes of the flares, respectively.
Paper: Statistical Analysis of Long GRBs’ Prompt Emission and X-Ray Flares: Multivariate Clustering and Correlations
Authors: Joseph Saji, Shabnam Iyyani, Kratika Mazde
Figure caption: (a) A schematic representation of the GRB prompt emission and afterglow light curves including the late-time X-ray flares. The temporal parameters, T  P,100, T  F,100, and the quiescent period T  q , are marked. (b) Residual plot of GRB 170705A showing polynomial fit in the rise and decay phases of the X-ray flare. The points at which the fit coincides with the residual = 0 line are marked with blue squares. The afterglow (black) and its corresponding model (blue solid line) of the same GRB are shown in the embedded plot.
Paper: Statistical Analysis of Long GRBs’ Prompt Emission and X-Ray Flares: Multivariate Clustering and Correlations
Authors: Joseph Saji, Shabnam Iyyani, Kratika Mazde
Figure caption: The distributions obtained for the prompt (red) and flare (orange for first flare episode and blue for second flare episode) temporal parameters are shown. The vertical bars represent the histograms and the respective KDE curves are shown as color-filled curves. The distributions of (a) T  P,100, (b) T  F,100, (c) T  q , (d) T  P,var, (e) T  F,var, (f) α  P , (g) α  F , (h) Fluence P , (i) Fluence F , (j) F  P,peak, and (k) F  F,peak are shown.
Paper: Statistical Analysis of Long GRBs’ Prompt Emission and X-Ray Flares: Multivariate Clustering and Correlations
Authors: Joseph Saji, Shabnam Iyyani, Kratika Mazde
Figure caption: (a) The PCA circle of correlation showing the relationships between all the prompt and X-ray flare parameters is shown. The percentage of the total contribution of each parameter to the PCA axes is represented by the color coding. (b) The Pearson correlation matrix of the various parameters of the prompt emission and the first (blue) and second (green) X-ray flare episodes is shown. Markers representing the p-values of the obtained correlations are shown in each cell representing the statistical significance of the correlation.
Paper: Statistical Analysis of Long GRBs’ Prompt Emission and X-Ray Flares: Multivariate Clustering and Correlations
Authors: Joseph Saji, Shabnam Iyyani, Kratika Mazde
Figure caption: (a) The K-means clustering results are visualized in a principal component plot. Black cross and red square markers represent GRBs that possess multiple flares and GRBs with zero quiescent period, respectively. The yellow triangle markers represent GRBs with flares in the plateau region of the afterglow. (b) The KDE distributions of the various flare properties of clusters B and D are shown.
Paper: Transiting Exoplanet Yields for the Roman Galactic Bulge Time Domain Survey Predicted from Pixel-level Simulations
Authors: Robert F. Wilson, Thomas Barclay, Brian P. Powell, Joshua Schlieder, Christina Hedges, Benjamin T. Montet, Elisa Quintana, Iain Mcdonald, Matthew T. Penny, Néstor Espinoza, Eamonn Kerins
Figure caption: The luminosity function (LF) for the bulge population in our simulated catalog compared to observations. The top row of figures shows the empirical completeness-corrected luminosity function (squares) from Terry et al. (2020), the LF from the default BGM1612 model catalog (gray), the LF after correcting for binarity and dust (purple), and our final adopted catalog LF, which corrects for binarity, dust, and the bulge IMF (teal). The bottom row of panels shows the star counts from the default BGM1612 catalog (gray), our catalog after correcting for dust and binarity (purple), and our adopted catalog (teal) divided by the empirical luminosity function. The error bars were calculated assuming Poisson uncertainties from the empirical LF, adjusted for catalog completeness and proper motion selection efficiency. For the residuals, the empirical LF uncertainties were added in quadrature with the Poisson uncertainties from the generated catalog. The BGM1612 model underpredicts NIR star counts below the main-sequence turn-off (i.e., J ≳ 18.5, H ≳ 18), even after adjusting for dust (purple), which necessitates the amended bulge IMF in our final adopted catalog (teal). The turnover at H > 23 is likely too early and a result of the BGM1612 model excluding very low-mass dwarfs (M ⋆ < 0.15M ⊙) in the bulge population.
Paper: Transiting Exoplanet Yields for the Roman Galactic Bulge Time Domain Survey Predicted from Pixel-level Simulations
Authors: Robert F. Wilson, Thomas Barclay, Brian P. Powell, Joshua Schlieder, Christina Hedges, Benjamin T. Montet, Elisa Quintana, Iain Mcdonald, Matthew T. Penny, Néstor Espinoza, Eamonn Kerins
Figure caption: The distribution functions for the fraction of flux contributed by neighboring stars within circular apertures of varying radii, for different magnitude ranges. Each panel shows a specific magnitude range, and each color denotes a different aperture radius. The distribution marked by the solid black line shows the crowding in the aperture that optimized the signal-to-noise ratio of the injected signal, measured via the multiple-event statistic (MES), and this is the crowding distribution that we adopt to build our noise model. The vertical solid and dashed lines show the median and mean crowding, respectively, in the optimized aperture.
Paper: Statistical Analysis of Long GRBs’ Prompt Emission and X-Ray Flares: Multivariate Clustering and Correlations
Authors: Joseph Saji, Shabnam Iyyani, Kratika Mazde
Figure caption: The afterglow light curves of (a) GRB 060223A and (b) GRB 180602A represent cases with no data during the decay and rise phases of the flaring episode, respectively. (c) GRB 100805A and (d) GRB 130803A represent cases that have few observational points during flare emission. (e) GRB 160408A and (f) GRB 160624A represent cases where underlying afterglow emission is absent or not enough data points are available for proper modeling. (g) GRB 130427A and (h) GRB 090404 represent cases that are avoided due to their very low S/N. The red shaded portion represents the flare duration as identified by the Swift-XRT team. The afterglow light curves of (i) GRB 170705A and (j) GRB 150626B possessing a single flare are shown. (k) GRB 140206A and (l) GRB 150911A represent afterglows with double flaring episodes, while panels (m) and (n) show the light curves of GRB 190926A and GRB 050822, which have three flaring episodes each. Panels (o) and (p) present the light curves of GRB 161219B and GRB 091029 with a full and partial flare, respectively, within the plateau region of the afterglow. The blue shaded region represents the flare duration as identified in this study. The red dotted line shown in all the plots represents the afterglow model obtained after excluding the flare region.
Paper: Transiting Exoplanet Yields for the Roman Galactic Bulge Time Domain Survey Predicted from Pixel-level Simulations
Authors: Robert F. Wilson, Thomas Barclay, Brian P. Powell, Joshua Schlieder, Christina Hedges, Benjamin T. Montet, Elisa Quintana, Iain Mcdonald, Matthew T. Penny, Néstor Espinoza, Eamonn Kerins
Figure caption:  RImTimSim generates images that yield photometry with realistic uncertainties. The circles show the measured RMS scatter from white-noise light curves generated from simulated images of isolated point sources, assuming a constant aperture. The total expected noise, estimated from Equation (2), is shown by the black line, and the dashed lines show the contributions from individual noise components. The gray shaded region shows the range of noise floors expected for stars with one or more nearly saturated pixels in their aperture. This floor varies based on the location of the point source relative to the center and edges of a pixel. The structure in the RMS scatter at F146 ≲ 18 is due to semisaturation effects, which are exacerbated by the relatively small aperture used to make this figure.