adsabs/AstroCLIMB huggingface dataset:
Paper: The Advanced Spectral Library: The Evolution of Chromospheric Wind Characteristics from Noncoronal to Hybrid Giant Stars 
Authors: Krister E. Nielsen, Vladimir S. Airapetian, Kenneth G. Carpenter, Gioia Rau
Figure caption: Nonthermal velocity, ξ (diamonds), and ion sound speed, v  s  (circles), of the high-ionization diagnostics observed in γ Dra as a function of formation temperature, T. The plot uses the core line width for C IV (at log T = 5.0) and N V (at log T = 5.2). The green and red lines are polynomial fits to the respective data sets. They are included to show the reader the general trend of the nonthermal velocity and sound speed with temperature, as discussed in the text.
Paper: The Advanced Spectral Library: The Evolution of Chromospheric Wind Characteristics from Noncoronal to Hybrid Giant Stars 
Authors: Krister E. Nielsen, Vladimir S. Airapetian, Kenneth G. Carpenter, Gioia Rau
Figure caption: Top: mass-loss rates calculated for γ Dra using the ASTRAL Fe II spectrum (circles). Filled diamonds are values from the O I and Mg II resonance lines. Bottom: comparison of the mass-loss rates calculated for noncoronal γ Cru using the GHRS (plus signs) and ASTRAL (circles) Fe II spectra. Filled diamonds are from the Mg II resonance lines.
Paper: The Advanced Spectral Library: The Evolution of Chromospheric Wind Characteristics from Noncoronal to Hybrid Giant Stars 
Authors: Krister E. Nielsen, Vladimir S. Airapetian, Kenneth G. Carpenter, Gioia Rau
Figure caption: Plasma flow velocity measurement for the self-reversed lines in γ Cru. The figure shows how the emission (top) and two absorptions (bottom) vary with atmospheric height. The emission is centered at rest velocity, while the absorption components are linearly changing with atmospheric height. The circles represent the ASTRAL measurements, and the plus signs are for the GHRS measurements.
Paper: The Advanced Spectral Library: The Evolution of Chromospheric Wind Characteristics from Noncoronal to Hybrid Giant Stars 
Authors: Krister E. Nielsen, Vladimir S. Airapetian, Kenneth G. Carpenter, Gioia Rau
Figure caption: Intensity plots for γ Cru (top) and γ Dra (bottom). The Fe II lines are normalized to their peak intensity in the chosen velocity range, and the flux for the opacity between the observed Fe II lines has been calculated by interpolation. Many of the Fe II features are blended; hence, the unwanted intensity peaks in the velocity range give an uneven appearance. The intensity is normalized to the peak intensity. The measured Fe II lines are marked on the right side of the plot.
Paper: The Advanced Spectral Library: The Evolution of Chromospheric Wind Characteristics from Noncoronal to Hybrid Giant Stars 
Authors: Krister E. Nielsen, Vladimir S. Airapetian, Kenneth G. Carpenter, Gioia Rau
Figure caption: Plasma flow velocity measurement for the self-reversed lines in γ Dra. The figure shows how the emission (top) and absorption (bottom) vary with atmospheric height. Both components are centered at rest velocity with a slight departure for the stronger lines.
Paper: Improved Measurements of the IXPE Crab Polarization
Authors: Josephine Wong, Roger W. Romani, Jack T. Dinsmore
Figure caption: IXPE X-ray polarization measurements, after leakage correction, compared with optical values. Optical q=Q/I and u=U/I from off-pulse subtracted OPTIMA observations are shown as black dots (with the optical light curve shown in green for phase reference). The average OPTIMA q and u fluxes will be zero in the dashed line-delimited off-pulse region. Red error bars show the IXPE measurement uncertainties. Phase bins whose PD exceeds 3σ significance are circled in blue, those exceeding 2σ are circled in dark green. Note that while optical and X-ray q values at the second peak are consistent, there are substantial differences for the other peak polarizations.
Paper: Improved Measurements of the IXPE Crab Polarization
Authors: Josephine Wong, Roger W. Romani, Jack T. Dinsmore
Figure caption: On-off and simultaneous fits for nebula polarization from a simulated 100ks Crab observation. The left-hand column includes the model maps of Stokes q = Q/I and u = U/I. Their color bar is common to all panels. Beside each reconstructed map (middle and right-hand columns) is a histogram of the uncertainties of the polarization values. Note that simultaneous fitting produces maps that more cleanly resemble the model with smaller uncertainties.
Paper: Improved Measurements of the IXPE Crab Polarization
Authors: Josephine Wong, Roger W. Romani, Jack T. Dinsmore
Figure caption: On-off and simultaneous fits for pulsar polarization from a simulated 100ks Crab observation. The black line represents the polarization model. The light curve is displayed in the background (gray) with the off-pulse phase region shaded in purple. By definition, Q pulsar = U pulsar = 0 in these phase bins for on-off analysis.
Paper: Improved Measurements of the IXPE Crab Polarization
Authors: Josephine Wong, Roger W. Romani, Jack T. Dinsmore
Figure caption: IXPE Crab pulsar PD-PA contour plots showing 1σ, 2σ, and 3σ (red, green, and blue) contours for simultaneous-fitted bins around the two peaks. Phases with greater than 5σ detection are the brightest in color and fade for the >2σ bins. Numbers correspond with the phase bins numbered in Figure 3. For P1, a CCW sweep can be inferred; P2 requires more bins to show a polarization pattern.
Paper: Improved Measurements of the IXPE Crab Polarization
Authors: Josephine Wong, Roger W. Romani, Jack T. Dinsmore
Figure caption: IXPE Crab pulsar Stokes Q/I and U/I, after leakage correction, from on-off and simultaneous fitting. Statistically significant detections (>3σ) are circled red and blue, respectively. With simultaneous fitting, due to the extra signal we extract from the data, we can afford to use finer (and more) phase bins, which helps us to capture the polarization sweep. Both methods have >5σ detection at the first peak. The X-ray light curve is displayed in gray.
Paper: Improved Measurements of the IXPE Crab Polarization
Authors: Josephine Wong, Roger W. Romani, Jack T. Dinsmore
Figure caption: IXPE Crab nebula polarization map after leakage correction. The green lines indicate magnetic field direction (perpendicular to the electric field PA) and the tiles’ color indicates PD. Contour intensity levels (red) derived from the contemporaneous CXO Crab observation (OBSID 23539), both displayed in the background, are included for reference; the pulsar’s position is marked with a red cross.
Paper: HOW-MHD: A High-order WENO-based Magnetohydrodynamic Code with a High-order Constrained Transport Algorithm for Astrophysical Applications
Authors: Jeongbhin Seo, Dongsu Ryu
Figure caption: Power spectra of the density, P  ρ (k) (left panels), the kinetic energy, ﹩{P}_{{E}_{K}}(k)﹩ (middle panels), and the magnetic energy, ﹩{P}_{{E}_{B}}(k)﹩ (right panels), in the ISM turbulence with M turb ≈ 10 and β  p  = 0.1 (top panels) and the ICM turbulence with M turb ≈ 0.5 and β  p  = 106 (bottom panels). See the main text for the setup of the turbulences. The results from simulations with 256 × 256 × 256 grid cells using the WENO codes with CT6, CT4, and CTorg and also using the TVD code are shown. The spectra are averaged over the saturated period. To avoid overlap, the spectra with the codes with CT6 and CTorg are multiplied by factors of 2 and 1/2, respectively. For comparison purposes, the results from a lower-resolution simulation with 128 × 128 × 128 grid cells using the WENO code with CT6 are shown with dashed lines. The short black lines draw the slope of the Kolmogorov spectrum.
Paper: HOW-MHD: A High-order WENO-based Magnetohydrodynamic Code with a High-order Constrained Transport Algorithm for Astrophysical Applications
Authors: Jeongbhin Seo, Dongsu Ryu
Figure caption: Results of the 2D MHD rotor test. See the main text for the setup. The computational domain consists of [–0.5, 0.5] × [–0.5, 0.5] with 400 × 400 grid cells in the x-y plane. (a−d) The distributions of ρ, v 2, B 2, and P. The results of a simulation at t = 0.125 using the code with CT6 are shown. (e, f) The line profiles of B  y  along the x-axis (y = 0, dotted line in panel (c)) and B  x  along the y-axis (x = 0, dashed line in panel (c)). The results of simulations using the codes with CT6 and CTorg are shown. The solid lines draw the results of a higher-resolution simulation with 1024 × 1024 grid cells using the code with CT6 for comparison.
Paper: HOW-MHD: A High-order WENO-based Magnetohydrodynamic Code with a High-order Constrained Transport Algorithm for Astrophysical Applications
Authors: Jeongbhin Seo, Dongsu Ryu
Figure caption: 2D oblique MHD shock-tube test, the same test shown in Figure 2 of Ryu et al. (1995). See the main text for the setup. The computational domain covers the x-y plane of [0, 1] × [0, 1] with 256 × 256 grid cells. The results of a simulation at ﹩t\,=\,0.2\times \sqrt{2}﹩ using the code with SSPRK and CT6 are shown with blue circles. For comparison, the results using the code with RK4 and CT6 are also shown with orange stars. The numerical solutions are along the diagonal line of x = y and compared to the exact solution of Ryu & Jones (1995) drawn with solid lines.
Paper: HOW-MHD: A High-order WENO-based Magnetohydrodynamic Code with a High-order Constrained Transport Algorithm for Astrophysical Applications
Authors: Jeongbhin Seo, Dongsu Ryu
Figure caption: Results of the 3D MHD blast wave test. See the main text for the setup. The computational domain consists of [–0.5, 0.5] × [–0.5, 0.5] × [–0.5, 0.5] with 200 × 200 × 200 grid cells. (a−d) The 2D slice images of ρ, v 2, B 2, and P through z = 0. The results of a simulation at t = 0.02 using the code with CT6 are shown. (e, f) The line profiles of B 2 and P along the diagonal line of x = y at z = 0 (dotted lines in panels (c) and (d)). The results of simulations using the codes with CT6 and CTorg are shown. The solid lines draw the results of a higher-resolution simulation with 400 × 400 × 400 grid cells using the code with CT6 for comparison.
Paper: HOW-MHD: A High-order WENO-based Magnetohydrodynamic Code with a High-order Constrained Transport Algorithm for Astrophysical Applications
Authors: Jeongbhin Seo, Dongsu Ryu
Figure caption: Results of the 2D magnetic reconnection test in the x-y domain of [−1, 1] × [ − 0.5, 0.5]. See the main text for the setup of the current sheet. Left panel: the 2D distributions of the gas pressure, P, in simulations with 128 × 64 grid cells, using the codes with CT6, CT4, and CTorg, at t = 30. Right panel: the time evolution of the magnetic energy in the entire computational domain, normalized to the initial magnetic energy, in the same simulations shown in the left panel. The result of a higher-resolution simulation with 512 × 256 grid cells is also shown for comparison.
Paper: HOW-MHD: A High-order WENO-based Magnetohydrodynamic Code with a High-order Constrained Transport Algorithm for Astrophysical Applications
Authors: Jeongbhin Seo, Dongsu Ryu
Figure caption: 2D slice images of the magnetic energy in the ISM turbulence with M turb ≈ 10 and β  p  = 0.1 (top panels) and the ICM turbulence with M turb ≈ 0.5 and β  p  = 106 (bottom panels), from simulations with 256 × 256 × 256 grid cells using the TVD code (left panels) and the WENO code with CT6 (right panels), at the end of simulations. See the main text for the setup of the turbulences.
Paper: HOW-MHD: A High-order WENO-based Magnetohydrodynamic Code with a High-order Constrained Transport Algorithm for Astrophysical Applications
Authors: Jeongbhin Seo, Dongsu Ryu
Figure caption: Time evolution of the maximum value of ∇ ·  b , normalized with the initial magnetic field and the cell size, B 0/Δx, in the 2D MHD rotor test with 400 × 400 grid cells using the codes with CT6, CT4, and CTorg. The values of ∇ ·  b  are calculated with Equation (29) using Equation (27) for the cases of CT6 (ν = 6) and CT4 (ν = 4) and using a second-order FD for CTorg, matched with the order of the CT algorithms.
Paper: HOW-MHD: A High-order WENO-based Magnetohydrodynamic Code with a High-order Constrained Transport Algorithm for Astrophysical Applications
Authors: Jeongbhin Seo, Dongsu Ryu
Figure caption: Results of the 3D MHD jet launching test. See the main text for the setup. The 2D slice images of ρ, ﹩\mathrm{log}({\beta }_{p})﹩, B, and P through y = 0 from a simulation using the code with CT6 are shown. The computational domain consists of [–12, 12] × [–12, 12] × [–12, 12] with 480 × 480 × 480 grid cells, and the images are at the end of the simulation, t = 5.
Paper: HOW-MHD: A High-order WENO-based Magnetohydrodynamic Code with a High-order Constrained Transport Algorithm for Astrophysical Applications
Authors: Jeongbhin Seo, Dongsu Ryu
Figure caption: Volume rendering images of ﹩{B}^{2}/{B}_{0}^{2}﹩, the normalized magnetic energy of the inclined, cylindrical magnetic loop advecting across a diagonal direction in the 3D domain of 1 × 1 × 2 volume with 64 × 64 × 128 grids. The test results using the codes with CT6, CT4, and CTorg at t = 20 are displayed.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Measured dust laws and the transmission curves of the three Swift NUV filters. SMC/LMC (green and yellow respectively) from Gordon et al. (2003), MW (black) from Cardelli et al. (1989), and starburst (SB; blue) from Calzetti et al. (2000). Filter transmission curves of the three NUV Swift UVOT filters taken from the SVO Filter Profile Service (Rodrigo & Solano 2020) are overlaid on the measured dust laws (gray dashed lines). The UVM2 filter covers the 2175 Å bump and the UVW1 and UVW2 filters are on either side, allowing us to measure the UV SED better and constrain the UV attenuation law. Note: the MW extinction law and other galaxy attenuation laws are not directly comparable.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: The three SFH parameterizations used during our fitting. From top to bottom, exponential (red), double power law (green), and piecewise (blue). This plot shows 500 realizations of the SFH for M101 from our SED fitting. The exponential and double-power-law forms are the most rigid in their assumed forms but are used due to the ease of computation. The piecewise SFH is nonparametric in that no rigid shape is imposed on the SFH and is thought to be better at producing a more physically realistic SFH. However, it has the most parameters and therefore is more computationally demanding. The photometric data do not constrain the earliest epochs of star formation and these are more dependent on the priors and shape of the chosen SFH.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Swift/UVOT UVW1 photometry measurements for NGC 7793. Left: source brightness as a function of aperture size, which clearly asymptotes at large radii. Right: count rate as a function of rate of change of flux accumulation. Following Gil de Paz et al. (2007), we calculate the asymptotic flux by determining the count rate where the rate of change of the count rate with respect to the radius equals zero. This calculation is done only at large radii where very little flux is still being accumulated as the aperture increases. The blue line is the best-fit line, where the intercept is used as the asymptotic flux measurement.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: An example SED of NGC 628 (M74) showing the flux observed in each bandpass. The inset in the upper left shows the additional UV coverage provided by Swift/UVOT in red. The error bars on the fluxes are shown but are negligible in most cases. These data are then used as the input for our SED fitting.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Comparison of the piecewise and double-power-law fits using standardized t-scores for stellar mass, δ, and E  b . We find less scatter in stellar mass compared to the dust law parameters for every possible pair of SFHs. This means that parameters such as stellar mass are much less sensitive to the chosen SFH.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: Example output corner plot for MCSED for NGC 3267 and the piecewise SFH (Foreman-Mackey 2016). This figure summarizes the parameter distributions. The posterior probability distributions of the different parameters can be seen in the lower left. The best-fit spectrum, SFH, and attenuation law are shown in the upper right. This plot allows a quick check to see if the fit was successful in modeling the emission from the given galaxy and if there are any degeneracies between parameters.
Paper: Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry
Authors: Alexander Belles, Marjorie Decleir, William P. Bowman, Lea M. Z. Hagen, Caryl Gronwall, Michael H. Siegel
Figure caption: False color images of select SINGS/KINGFISH galaxies using Swift UVOT (UVW2, UVM2, and UVW1 filters). From left to right, NGC 1566, NGC 3031 (M81), NGC 4594 (M104), NGC 5194 (M51), and NGC 6946.
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: Observed interferometric visibilities for HCN, CH3OH, and CH3CN, with the best-fitting models overlaid. The observations and model data have been (spatially) averaged within 10 m uv bins and (spectrally) averaged over all line emission channels for each species, including 13 lines for CH3OH and five lines for CH3CN. The zero-spacing data points (at uv = 0) were taken from the ALMA autocorrelations (observed simultaneously with the interferometric data). The preferred best-fitting visibility models are shown with solid lines, while dashed and dotted curves show models that are ruled out based on a poorer quality of fit (or other criteria; see text).
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: Variation of the 46P coma kinetic temperature with radius in the sunward (jet) and antisunward (ambient) coma regions, derived from modeling the CH3OH J = 5–4 data. Shaded regions indicate the ±1σ error envelopes.(The data used to create this figure are available.)
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: Spectrally integrated ALMA emission maps of HCN, CH3OH, and CH3CN, centered on their respective emission peaks. Beam size (FWHM of a Gaussian fit to the PSF) is shown in the lower-left corner. Insets show the molecular spectra on a cometocentric velocity scale, integrated within a 5″ diameter aperture centered on the brightness peak. The (sky-projected) direction of the comet’s orbital trail and comet–Sun vector are shown for CH3CN in the lower-right corner. Five times the rms noise level (5σ) is indicated on the color bar for each species (﹩\sigma (\mathrm{HCN})=5.0﹩, σ(CH3OH) = 7.1, and ﹩\sigma ({\mathrm{CH}}_{3}\mathrm{CN})=2.1﹩ mJy km s−1).
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: Same as Figure 1 but for H2CO, CS, and HNC. The H2CO and HNC maps are centered on the position of the HCN emission peak relative to the phase center, while the CS map is centered on the CH3OH peak. In the inset spectrum, the H2CO data have been binned over eight spectral channels for display. The rms noise level (σ) is indicated on the color bar for each species (σ(H2CO) = 3.0, σ(CS) = 0.5, and σ(HNC) = 1.6 mJy km s−1).
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: Same as Figure 6 but for H2CO, CS, and HNC.
Paper: Gas Sources from the Coma and Nucleus of Comet 46P/Wirtanen Observed Using ALMA
Authors: M. A. Cordiner, N. X. Roth, S. N. Milam, G. L. Villanueva, D. Bockelée-Morvan, A. J. Remijan, S. B. Charnley, N. Biver, D. C. Lis, C. Qi, B. P. Bonev, J. Crovisier, J. Boissier
Figure caption: ALMA autocorrelation (total power) spectra in the rest frame of the comet. The spectra have been baseline-subtracted and corrected for the nominal ALMA beam efficiency (see text). The CH3OH spectrum is the mean of the five strongest unblended lines.
Paper: Systematic Multiepoch Monitoring of LkCa 15: Dynamic Dust Structures on Solar System Scales
Authors: Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Comparison of observed reconstructed images in combined data sets from each band (top row) to expectations for best-fit three-point-source (middle row) and polar Gaussian ring models (bottom row). From left to right, the columns show the 2019-01 H-band, 2015-02 K  s -band, and 2014–2020 combined ﹩{L}^{{\prime} }﹩-band data. As fits to the combined multiepoch ﹩{L}^{{\prime} }﹩ data set, the geometric models used here are the static models from Figure 5. Similar to Figure 5, we add Gaussian noise to each simulated observation to match the scatter in the real data. The simulated reconstructions shown here are affected by both the Fourier coverage and noise levels of the mock observations. See the Appendix for example simulated reconstructions where these effects are isolated.
Paper: Systematic Multiepoch Monitoring of LkCa 15: Dynamic Dust Structures on Solar System Scales
Authors: Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Color composite image of selected, previously published LkCa 15 data sets and companion candidate positions. Red shows ALMA 1.3 mm observations from Facchini et al. (2020) that led to the identification of annular substructures. Green shows SPHERE J-band polarized-light imaging from Thalmann et al. (2016). Blue scattered points show the positions of the three companion candidates in Sallum et al. (2015a), which, when compared to the three companion signals in Kraus & Ireland (2012), exhibited apparent position angle changes along the orbits marked in white (in the direction indicated by the white arrow). The detection of polarized light due to scattering by disk material (Thalmann et al. 2016) and follow-up observations that were inconsistent with three distinct companion orbits (Currie et al. 2019) suggested that a ∼20 au, small-grain disk could be at least partially responsible for the companion candidate signals.