adsabs/AstroCLIMB huggingface dataset:
Paper: NIRC2 Interferometric Imaging of the HD 34282 Transition Disk’s Small Grain Structure
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Left: the 1σ–5σ contrast limits for HD 34282, as represented by the contours. The diffraction limit is indicated by the black dashed line, and half of the diffraction limit is represented by the blue dashed line. We also indicate the location, in this parameter space, of a 50 MJ companion predicted by G. van der Plas et al. (2017). This demonstrates that this companion would be within the detection limits of this observation; hence, we rule it out and place new, closer-in upper limits on the brown dwarf companion (≳40 MJ at ≳λ/D, or 20 au). Right: the 5σ contrast surface at all position angles and separations. The contrast varies with position angle by ∼0.5–1 mag. We find that the 5σ contrast is deeper than 6.8 mag (the companion candidate contrast) for most position angles, and the 1σ surface contrast is ≳ 6.8 mag at 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 at all position angles (see Section 6.4).
Paper: Spatial Distribution of Secondary Electrons’ Synchrotron Emission: Property and Implication
Authors: Qi-Zuo Wu, Ruo-Yu Liu
Figure caption: Left: energy spectrum for hadronic and leptonic scenario. In γ-ray band, both models satisfy ﹩dN/d{E}_{\gamma }\propto {E}_{\gamma }^{-3}﹩ and F25−100 TeV = 1 × 10−12 erg cm−2 s−1. In the X-ray band, the yellow solid line refers to the synchrotron radiation from primary electrons with Blep = 1 μG. Green-solid, dotted-solid, and dotted lines refer to the synchrotron radiation from secondary electrons with Bhad = 100 μG, 50 μG and 10 μG, respectively. Right: the predicted SBP and photon index profile in 0.5–7 keV with Bhad = 50 μG, Blep = 1 μG. The diffusion coefficient is assumed to D0,had = D0,lep = 1026 cm2 s−1.
Paper: Spatial Distribution of Secondary Electrons’ Synchrotron Emission: Property and Implication
Authors: Qi-Zuo Wu, Ruo-Yu Liu
Figure caption: Normalized electron density distribution (upper panel) and the power-law index profile (lower panel) of secondary electrons in 20–100 TeV. Different colors correspond to the magnetic field B = 10, 50, 100 μG. The purple dashed line corresponds to the normalized primary electron density in the leptonic scenario at 1 μG. The black dotted line corresponds to the normalized distribution of injection rate of secondary electrons Qe at t = 2 Myr. Both the density and injection rate are normalized at r = 0.1 pc.
Paper: Spatial Distribution of Secondary Electrons’ Synchrotron Emission: Property and Implication
Authors: Qi-Zuo Wu, Ruo-Yu Liu
Figure caption: The predicted energy spectrum, SBP, and photon index profile in the hybrid case with Bhybrid = 50 μG and D0,had = D0,lep = 1026 cm2 s−1. The solid, dashed–dotted and dotted lines refer to Kep = 10−2, 10−3 and 10−4.
Paper: NIRC2 Interferometric Imaging of the HD 34282 Transition Disk’s Small Grain Structure
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: The maximum likelihood double-ring model vs. data for closure phases (top) and squared visibilities (bottom). The black line shows that the model follows a near-1:1 fit to the data.
Paper: NIRC2 Interferometric Imaging of the HD 34282 Transition Disk’s Small Grain Structure
Authors: Christina L. Vides, Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Scattered points show (u, v) coverage (the rotation of each baseline with parallactic angle). We obtained ∼103° of sky rotation for the entirety of the half-night.
Paper: Diverse Pathways for Supermassive Black Hole–Galaxy Coevolution
Authors: Bryan A. Terrazas, James Aird, Alison L. Coil
Figure caption: The procedure used for building empirically motivated SMBH growth histories. We begin with z = 0 galaxies from the UniverseMachine empirical galaxy formation model (P. Behroozi et al. 2019), splitting them into five populations based on SFR relative to the main sequence (step 1). We then assign SMBH masses to simulated galaxies based on the observed SMBH mass–stellar mass scaling relations for quiescent and star-forming galaxies at z = 0 from J. E. Greene et al. (2020; step 2). We then assign sBHARs to simulated galaxies based on observationally derived probability functions from J. Aird et al. (2019; step 3) and subtract the estimated amount of SMBH mass grown between two adjacent simulation time steps. We reassign sBHARs at every snapshot based on galaxy SFR and redshift. We then determine SMBH growth histories for each galaxy from z = 2 to z = 0 (step 4). The contours in this last panel indicate the z = 1 distribution of galaxies that are progenitors of the z = 0 star-forming (blue) and quiescent (red) populations. The red and blue lines show the z = 0 (J. E. Greene et al. 2020) relations. The gray line shows an example of a galaxy coevolutionary growth track from z = 0 to 2 from our model.
Paper: Diverse Pathways for Supermassive Black Hole–Galaxy Coevolution
Authors: Bryan A. Terrazas, James Aird, Alison L. Coil
Figure caption: The Eddington fraction (﹩{f}_{{\rm{Edd}}}=\frac{{L}_{{\rm{bol}}}}{{L}_{{\rm{Edd}}}}﹩) as a function of λsBHAR at z = 0 for each SFR classification of simulated galaxies in the UniverseMachine (as indicated by the colors in the legend) following our procedure shown in Figure 1. The top panel shows the derived probability distributions that result from our model (histograms) and the J. Aird et al. (2019) probability distributions we use as constraints (smooth curves). These smooth curves are multiplied by 2 to account for obscured AGN (see Section 2.4). These two sets of data closely match one another by construction according to the procedure we use to build SMBH growth histories. The right panel shows the histograms of fEdd for the different SFR classification bins we use and demonstrates that star-forming galaxies are typically assigned higher Eddington ratios than quiescent galaxies. The horizontal dotted black line denotes the Eddington limit (fEdd = 1), and the dashed black line indicates the nominal scaling between fEdd and λsBHAR adopted by J. Aird et al. (2019).
Paper: The Infrared Complex Refractive Index and Band Strengths of Coronene Thin Films
Authors: J. E. Roser, L. Jovanović, A. Ricca
Figure caption: The measured transmission spectra (black) and the corrected spectra (red) with water and carbon dioxide frost in the MCT detector and baseline distortion at low wavenumbers removed.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Infrared Complex Refractive Index and Band Strengths of Coronene Thin Films
Authors: J. E. Roser, L. Jovanović, A. Ricca
Figure caption: The imaginary part of the index of refraction determined for the experimental spectra using the Kramers–Kronig algorithm of J. E. Roser et al. (2021).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Infrared Complex Refractive Index and Band Strengths of Coronene Thin Films
Authors: J. E. Roser, L. Jovanović, A. Ricca
Figure caption: Sample mean calculations of the real part of the complex index of refraction (left) and the imaginary part of the complex index of refraction (right) for the six spectra of coronene thin films vacuum deposited at 5.1 K.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Infrared Complex Refractive Index and Band Strengths of Coronene Thin Films
Authors: J. E. Roser, L. Jovanović, A. Ricca
Figure caption: The corrected experimental transmission spectra (black) and the spectral baseline transmission as computed using the two thin-film model of J. E. Roser et al. (2021) with parameters given in Table 2.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: A position–velocity map for sight line 4 (Sk−70°115) using H I 21 cm emission data from GASKAP. The left and middle panels are sliced along a ﹩0\mathop{.}\limits^{^\circ }267﹩ region through the sight line’s Galactic latitude and longitude, respectively. The LMC’s disk is prominent between +190 ≲ vLSR ≲ +245 km s−1 (highlighted in gray in the right panel) while the offset material exterior to the disk is located around +260 ≲ vLSR ≲ +310 km s−1 (highlighted in red in the right panel). We caution that the separation between the two H I emission bands for sight line 4 is not the standard among the remaining sight lines. However, we choose to highlight sight line 4 as it is the strongest argument for arm material flowing in this region. We note that the offset gas’s interior edge (side kinematically closer to the LMC’s disk) has a more well-defined boundary than its exterior side, which may suggest the material on leading edge experiences more compression than the trailing gas. The black dashed vertical line is the Galactic latitude or longitude of sight line 4. The vertical green, brown, and purple lines are the velocity ranges from the Voigt fitting analysis of the Fe II, Si II, and S II components, respectively (see Table 3). We intentionally offset the Galactic longitude and latitude of the Fe II and S II components by ﹩+0\mathop{.}\limits^{^\circ }01﹩ and ﹩-0\mathop{.}\limits^{^\circ }01﹩, respectively, for visual clarity. We include the radial velocity of the background star on the left and middle plots as indicated by the star symbol. The right panel has H I 21 cm line emission expressed in terms of column density as a function of velocity from the GASKAP (black) and GASS (cyan) observations. The GASKAP data are rebinned by 1 km s−1. The peaks in the emission-line profile align with the two bands of H I emission in the position–velocity maps.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: Left: projected gas density of a zoomed-in region around the LMC 4 kpc thick overlaid with the gas velocity field in the LMC’s rest frame. This image is rotated with respect to Figure 11 in order to align the angular momentum of the LMC’s disk with the z-axis. The white arrows denote the direction of the LMC’s velocity (labeled “vLMC”), and the direction toward the Sun (labeled “⊙”). The three lines (black, blue, and orange) mark the trajectories for three sight lines along which we measure the radial velocities of the gas in the simulation. Upper right: the radial velocity profiles of the three sight lines. Positive velocities indicate material moving toward the Sun (blueshifted material), while negative velocities indicate redshifted gas. Lower right: the radial velocity profile of the y0 = −5 kpc sight line (black in left and upper right panels) split up based on MW (dark gray) and LMC (light gray) material. The LMC-originating gas is spatially isolated from the MW gas due to the protection of the Magellanic Corona and extends up to ∼3 kpc above and below the plane of the LMC’s disk.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: A comparison of the FWHM, center velocity, and offset from 30 Doradus for each sight line’s absorption components. We choose to show each sight line’s offset from 30 Doradus rather than display a linear increase on the top x-axis (all following offset plots are arranged in this layout). We prefer this labeling as sight lines 5–7 are located at similar angular offsets and a linear spacing would align the three sight lines on top of each other. The kinematic boundary of the LMC’s disk and offset gas along these sight lines are highlighted in gray and red, respectively. Six ion species are placed on this figure: S I in purple, C I in white with horizontal hatches, Fe II in dark gray, Si II in tan, S II in white with diagonal black hatches, and Al III in green. The height of the rectangles corresponds to the FWHM of each component, where ﹩\mathrm{FWHM}=2\sqrt{\mathrm{ln}(2)}b﹩. Saturated components have a thicker yellow outline around them and a “‡” symbol on top. We label the velocity ranges of arm B and arm E (S. Kim et al. 2003; L. Staveley-Smith et al. 2003) along each sight line by the horizontal purple and orange dotted lines, respectively. From left to right, the sight lines are arranged in order of increasing angular offset from 30 Doradus.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: A plot stack of various ion transitions for sight line 4. Top panel: GASS H I emission in terms of column density as a function of velocity. Lower panels: low and intermediate ion transitions. The MW is located around 0 km s−1. The gray shaded region is the kinematic boundary of the LMC’s disk and in red is the kinematic extent of the offset gas as determined from the H I emission (see Table 2). Both shaded regions were determined through assessing the reliability of the Gaussian fits from the Gaussian decomposition technique on the H I emission. We also label the predicted velocity ranges of arm B and arm E from the H I channel maps of S. Kim et al. (2003) and L. Staveley-Smith et al. (2003) by the purple and orange rectangles above the flux and H I emission, respectively. Each panel is labeled with the ion transition, wavelength in angstrom, and oscillator strength. The flux of the spectra is normalized and has a 1σ error envelope. The light tan line outlines the total Voigt profile while the individual components are outlined by the black dashed lines.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: Top panel: total integrated column densities for the offset absorbers of Ni II (tan), P II (green), Fe II (purple), and Si II (brown) for each of the sight lines. The upward arrows on the data points indicate saturated components that are lower limits. The two circle data points for Si II and P II along sight line 4 are integrated between the velocity of the right edge of the disk boundary and the last offset UV absorber of the offset gas. We include these data points because there are UV absorbers kinematically located between the determined H I boundaries of the disk and offset gas. Bottom panel: total integrated column densities for the offset absorbers of Al III. The gray envelope is the 3σ prediction interval of the linear regression fit. We highlight the Kendall’s τ coefficient and p-value of the fit in the top right corner. The sight lines are arranged in order of increasing angular offset from 30 Doradus from left to right.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: The deviation velocity range of the redshifted absorbers from the high-velocity edge of the LMC’s H I disk as a function of offset from 30 Doradus (offset increasing from bottom to top). We emphasize that the right y-axis displaying the offset of each sight line from 30 Doradus is not linearly spaced. Rather, it labels the measured offset of each sight line recorded in Table 1. The deviation (vDev) is found from vDev = voffset gas − vLMC right bound where voffset gas is the center velocity of the redshifted absorbers and vLMC right bound is the red velocity boundary of the LMC’s disk as determined from the H I emission (see Table 2). We perform the subtraction for each absorber and then identify the minimum and maximum values as the deviation range. We note the deviation can be below zero for components blended with the LMC’s disk.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: A moment 1 (emission-weighted mean velocity; see Equation (1)) map of the LMC from the GASS survey. The locations of the eight sight lines are marked with a star symbol. Each sight line is color coded based on the star’s radial velocity (see Table 1). The star marker labeled as “5–7” contains three different colors that correspond to the radial velocities of sight lines 5–7. As sight line 2 does not have a measured radial velocity, we mark with a black star. The pathways of arm B (dashed black line) and arm E (dotted black line) from the D. L. Nidever et al. (2008) Gaussian decomposition of the LAB survey are highlighted.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: The electron density measurements across all our sight lines. Data points with upward arrows are lower limits. The error bar for the data point associated with BI184 extends below 0 cm−3 and we indicate this with a downward arrow. We order the sight lines from left to right with increasing angular offset from 30 Doradus.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: The cooling rate per nucleon measurements across all our sight lines. Data points with upward arrows are lower limits. Sight lines are arranged from left to right with increasing angular offset from 30 Doradus.
Paper: New Interpretation for the Orientation of the LMC’s Gaseous Arms B and E Using ULLYSES 
Authors: April Horton, Suraj Poudel, Kathleen A. Barger, Scott Lucchini, David L. Nidever, Erica Chwalik, Frances H. Cashman, Andrew J. Fox, Nicolas Lehner, Dhanesh Krishnarao, Naomi McClure-Griffiths, Elena D'Onghia, Jason Tumlinson, Jo Vazquez, Lauren Sdun, Stone Gebhart, Katherine Anthony, Bryce Cole, Jacco Th. van Loon, John M. Dickey, Callum Lynn, Hiep Nguyen, Min-Young Lee
Figure caption: Plot stacks for sight lines 1–3 and 5–8. We include four additional ionization species for sight line 4 not highlighted in Figure 6. The H I boundaries of the LMC’s disk and the offset gas from Table 2 are shaded in with gray and red, respectively. The individual Voigt fits are outlined by the black dashed lines. The total Voigt fit profile is highlighted in tan. The predicted velocities of arm B and arm E are labeled above each spectra. Each ionization species is labeled in the panel with its corresponding oscillator strength. The target name and ID are given in the H I emission panel.
Paper: A Gigaparsec-scale Hydrodynamic Volume Reconstructed with Deep Learning
Authors: Cooper Jacobus, Roger de Belsunce, Solène Chabanier, Peter Harrington, J. D. Emberson, Zarija Lukić, Salman Habib
Figure caption: The three-dimensional power spectrum (P3D) of the Lyα forest for four different simulations shown as a function of Fourier wavenumber, k, and the cosine of the angle with the line of sight, μ = k∥/∣k∣: (i) low-resolution 960 h−1 Mpc box in purple; (ii) the reconstructed 960 h−1 Mpc box in blue; (iii) the high-resolution input 80 h−1 Mpc simulation in black dashed; and (iv) EFT fits to the ACCEL2 simulation in pink with a box of length L = 160 h−1 Mpc (S. Chabanier et al. 2024; R. de Belsunce et al. 2025a). The panels show the 3D power spectrum divided into four separate μ bins. The generative deep learning model is able to reconstruct the angular evolution for the 960 h−1 Mpc box and an overall agreement at the ∼20% level.
Paper: A Gigaparsec-scale Hydrodynamic Volume Reconstructed with Deep Learning
Authors: Cooper Jacobus, Roger de Belsunce, Solène Chabanier, Peter Harrington, J. D. Emberson, Zarija Lukić, Salman Habib
Figure caption: (Top) The PDFs of the predicted density and temperature fields (dark blue lines) compared against the reference distributions from a target high-resolution simulation (dotted lines). (Bottom) The density–temperature phase distribution of the gas in our model prediction compared against the reference distributions from the low-resolution and high-resolution simulations. For each output, we plot the best-fit power-law relationship between density and temperature; our model presents an improvement in the slope of this power-law, γ, when compared against the low-resolution simulation but produces a much broader distribution.
Paper: A Gigaparsec-scale Hydrodynamic Volume Reconstructed with Deep Learning
Authors: Cooper Jacobus, Roger de Belsunce, Solène Chabanier, Peter Harrington, J. D. Emberson, Zarija Lukić, Salman Habib
Figure caption: Comparison of the quality of the EFT fits to the 3D power spectra of the three simulations. Left panel: low-resolution box; middle panel: reconstructed box; and right panel: high-resolution input box as a function of angular bin μ. In each bottom panel, we show the residuals and guide the eye with a 2% error band shown in gray. We use a maximum wavenumber of ﹩\,{k}_{{\rm{\max }}}=1\,{\rm{h}}\,{{\rm{Mpc}}}^{-1}﹩ for the large simulations and ﹩\,{k}_{{\rm{\max }}}=2\,{\rm{h}}\,{{\rm{Mpc}}}^{-1}﹩ for the small volume.