adsabs/AstroCLIMB huggingface dataset:
Paper: Slow Diffusion is Necessary to Explain the γ-Ray Pulsar Halos
Authors: Li-Zhuo Bao, Kun Fang, Xiao-Jun Bi, Sheng-Hao Wang
Figure caption: The two parts of the γ-ray profile of LHAASO J0621+3755 under the fast-diffusion scenario without (left) and with (right) the PSF convolution.
Paper: Slow Diffusion is Necessary to Explain the γ-Ray Pulsar Halos
Authors: Li-Zhuo Bao, Kun Fang, Xiao-Jun Bi, Sheng-Hao Wang
Figure caption: Relation between the power-law index and the required conversion efficiency to fit the Geminga profile.
Paper: Slow Diffusion is Necessary to Explain the γ-Ray Pulsar Halos
Authors: Li-Zhuo Bao, Kun Fang, Xiao-Jun Bi, Sheng-Hao Wang
Figure caption: Best-fit γ-ray spectrum to the HAWC data.
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Evolution of the midplane pressures in all models. Solid curves show the total pressure and component pressures (thermal, turbulent, and magnetic) for the two-phase (warm+cold) gas, dashed curves show the total pressure of the hot gas, and dotted curves show the estimated dynamical equilibrium pressure. For reference, ΣSFR is also shown, in units 10−5 M ⊙ pc−2 Myr−1 (gray shading).
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Fractional contributions to the total pressure in the warm+cold (“2p”) gas from thermal, turbulent, and magnetic (mean and perturbation) terms, as a function of P DE. Individual points are plotted for each model at intervals of 1 Myr, as well as medians with 25th and 75th percentiles are indicated. Best fit relations are also shown for the thermal and turbulent fractions (see the main text).
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Total vertical pressure P tot ≡ P th + P turb + Πmag in hot gas versus two-phase gas for all models. Midplane-averaged values at intervals of 1 Myr are shown with individual small circles, and medians over the temporal domain shown in Figure 1 are shown as large points with 25th and 75th percentiles indicated. For reference the dotted line shows the identity P tot,hot = P tot,2p.
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Measured total midplane pressure of the warm+cold (two-phase) gas, P tot,2p, versus the measured and estimated weight of gas, ﹩{{ \mathcal W }}_{2{\rm{p}}}﹩ and P DE, for all models. Individual points at intervals of 1 Myr are plotted for each model, as well as medians with 25th and 75th percentiles are indicated, with dotted lines showing the identity relation in each panel and the solid lines showing the best fits (see the main text).
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Thermal pressure versus density for all gas within one scale height of the midplane. Top row shows model R8, and the bottom row shows model LGR4, each at t = t orb. Both the volume-weighted (left) and mass-weighted (right) PDFs are shown. In each panel, an overlay of the equilibrium curve for the instantaneous heating rate is shown.
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Measured weight of warm+cold (two-phase) gas, ﹩{{ \mathcal W }}_{2{\rm{p}}}﹩, versus the estimated dynamical equilibrium weight, P DE, for all models. Individual points at intervals of 1 Myr are plotted for each model, as well as medians with 25th and 75th percentiles are indicated. For reference the dotted line shows the identity ﹩{{ \mathcal W }}_{2p}={P}_{{DE}}﹩ while the solid line shows the best fit (see text).
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Vertical slices showing the thermal pressure P th (top), turbulent pressure ﹩{P}_{\mathrm{turb}}\equiv \rho {v}_{z}^{2}﹩ (middle), and magnetic pressure P mag ≡ ∣ B ∣2/(8π) (middle) in all models (labeled at top) at t = t orb. Axes are in units of the respective scale height for each model.
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Vertical slices showing the hydrogen number density n H and gas temperature T in all models at t = t orb. Axes are in units of the respective scale height H 2p for each model (see Column (13) in Table 2).
Paper: Pressure-regulated, Feedback-modulated Star Formation in Disk Galaxies
Authors: Eve C. Ostriker, Chang-Goo Kim
Figure caption: Evolution of the star formation rate surface density in all models, calculated based on the mass in new stars formed within the previous 1 Myr, and then smoothed over 10 Myr.
Paper: Galaxy Alignments with Surrounding Structure in the Sloan Digital Sky Survey
Authors: Dhvanil D. Desai, Barbara S. Ryden
Figure caption: Average alignment angle 〈Φ〉 as a function of target galaxy absolute magnitudes M  r  for blue and red subsamples, using the color divider of James & Ryden (2022). (a) Blue target galaxies with surrounding galaxies out to r  p  = 3.0 Mpc; (b) red target galaxies with surrounding galaxies out to r  p  = 0.5 Mpc; (c) red target galaxies with surrounding galaxies out to r  p  = 3.0 Mpc; (d) red target galaxies with surrounding galaxies out to r  p  = 7.5 Mpc.
Paper: Galaxy Alignments with Surrounding Structure in the Sloan Digital Sky Survey
Authors: Dhvanil D. Desai, Barbara S. Ryden
Figure caption: Average alignment angle 〈Φ〉 as a function of maximum projected surrounding radius r  p  = 0.1→ 7.5 Mpc for the four subsamples of target galaxies.
Paper: Galaxy Alignments with Surrounding Structure in the Sloan Digital Sky Survey
Authors: Dhvanil D. Desai, Barbara S. Ryden
Figure caption: Definition of the alignment angle Φ of the target galaxy (filled red ellipse) relative to the distribution of surrounding galaxies (fitted by the open blue ellipse).
Paper: Galaxy Alignments with Surrounding Structure in the Sloan Digital Sky Survey
Authors: Dhvanil D. Desai, Barbara S. Ryden
Figure caption: Normalized distribution of alignment angle Φ for the four subsamples of target galaxies. The best linear fit is shown as the red line in each panel. The gray lines indicate the range of slopes that yield P ks > 0.1 in a Kolmogorov–Smirnov test.
Paper: A Reliable Calibration of H II Galaxies Hubble Diagram with Cosmic Chronometers and Artificial Neural Network
Authors: Jian-Chen Zhang, 建臣 张, Kang Jiao, 康 焦, Tingting Zhang, Tong-Jie Zhang, 杰 张同, Bo Yu, 波 于
Figure caption: Left: reconstructions of c/H(z) using the Gaussian process (blue) and artificial neural network (orange). The solid central lines represent the reconstructed values, whereas the shaded regions represent the 1σ confidence intervals. The black error bars are the 32 OHD that are used as the basis in our reconstructions. Right: the corresponding reconstructions of the comoving distances, while 1σ regions are calculated based on the upper and lower bounds of the c/H(z) in the left panel.
Paper: A Reliable Calibration of H II Galaxies Hubble Diagram with Cosmic Chronometers and Artificial Neural Network
Authors: Jian-Chen Zhang, 建臣 张, Kang Jiao, 康 焦, Tingting Zhang, Tong-Jie Zhang, 杰 张同, Bo Yu, 波 于
Figure caption: Hubble diagrams of HIIGx and JLA SNe Ia samples. Error bars represent the calibrated distance modulus of the HIIGx and JLA sample and their corresponding 1σ uncertainties, labeled by the sample names and calibration methods, with calib1 and calib2 standing for using the Gaussian process (GP) and artificial neural network (ANN) reconstructed data respectively. The blue (orange) solid curves and shaded regions are the GP (ANN) reconstructed ﹩{\mu }_{{\rm{H}}\,\mathrm{II}}^{\mathrm{rec}}﹩ and their corresponding 1σ confidence regions at the redshift of JLA sample.
Paper: A Reliable Calibration of H II Galaxies Hubble Diagram with Cosmic Chronometers and Artificial Neural Network
Authors: Jian-Chen Zhang, 建臣 张, Kang Jiao, 康 焦, Tingting Zhang, Tong-Jie Zhang, 杰 张同, Bo Yu, 波 于
Figure caption: 68 and 95% confidence contours for the parameters involved in calibrating the HIIGx Hubble diagram with OHD. Results from the fit of not assuming a flat universe are show in blue and orange contours for using the GP and ANN reconstructed μ OHD data respectively, whereas the red and violet contours are that from assuming a flat universe.
Paper: A Reliable Calibration of H II Galaxies Hubble Diagram with Cosmic Chronometers and Artificial Neural Network
Authors: Jian-Chen Zhang, 建臣 张, Kang Jiao, 康 焦, Tingting Zhang, Tong-Jie Zhang, 杰 张同, Bo Yu, 波 于
Figure caption: 68% and 95% confidence contours for the parameters involved in calibrating the SNe Hubble diagram with calibrated HIIGx data. Blue (orange) contours result from the fit of using the GP (ANN) reconstructed μ H II data and the full JLA sample.
Paper: Using Bayesian Deep Learning to Infer Planet Mass from Gaps in Protoplanetary Disks
Authors: Sayantan Auddy, Ramit Dey, Min-Kai Lin, Daniel Carrera, Jacob B. Simon
Figure caption: Top panels: the distributions of the predicted planet masses at the three identified gaps in HL Tau, obtained using DPNNet-Bayesian. The mean values along with the standard deviations of the predicted planet masses at 10 au, 30 au, and 80 au are 86.0 ± 5.5 M ⊕, 43.8 ± 3.3 M ⊕, and 92.2 ± 5.1 M ⊕, respectively. Bottom panel: the distributions of the predicted masses for the two identified gaps in AS 209 for the given disk parameters and gap widths. The mean predicted planet masses along with the standard deviations are 20.6 ± 2.2 M ⊕ and 36.3 ± 2.5 M ⊕ at 9 au and 99 au, respectively.
Paper: Using Bayesian Deep Learning to Infer Planet Mass from Gaps in Protoplanetary Disks
Authors: Sayantan Auddy, Ramit Dey, Min-Kai Lin, Daniel Carrera, Jacob B. Simon
Figure caption: The distributions of the predicted planet masses for sample disk features selected randomly from the test data set. Left panel: the distribution captures the EP associated with DPNNet due to lack of data and/or variations of the model parameters. Middle panel: the distribution represents the AL that arises due to errors/variations inherent in the data. Right panel: the distribution captures the combined uncertainty in the predicted planet mass due to both EP and AL. The red dashed line represents the mean planet mass in each of the plots.
Paper: Using Bayesian Deep Learning to Infer Planet Mass from Gaps in Protoplanetary Disks
Authors: Sayantan Auddy, Ramit Dey, Min-Kai Lin, Daniel Carrera, Jacob B. Simon
Figure caption: Correlation between the simulated and predicted mass in units of M ⊕. The vertical error bars give the standard deviation associated with each predicted value, obtained using the BNN. The r2 score indicates the goodness of the fit.
Paper: Using Bayesian Deep Learning to Infer Planet Mass from Gaps in Protoplanetary Disks
Authors: Sayantan Auddy, Ramit Dey, Min-Kai Lin, Daniel Carrera, Jacob B. Simon
Figure caption: The radial profiles of the azimuthally averaged gas and dust surface densities at the beginning of the simulation and after 1000P 0. The steady-state profile is maintained with little evolution, in the absence of an embedded planet.
Paper: A Magnetogram-matching Method for Energizing Magnetic Flux Ropes Toward Eruption
Authors: V. S. Titov, C. Downs, T. Török, J. A. Linker
Figure caption: The evolution of the free magnetic energy W (its scale is shown at the axis on the left) of our pre-eruptive configuration (see Figure 1) during the energization by our helicity-pumping method (solid lines). The distribution of α in the central cross section of the configuration is shown at the beginning or end of each cycle to show how the current structure evolves during this process. For comparison, the dashed brown curve presents the decay of the free energy during the initial relaxation of the optimized RBSL MFR configuration toward the pre-eruptive configuration. The relaxation phase of the third cycle is prolonged from t ≈ 0.37 to t ≈ 0.55 to prove that the preliminary last cycle (dotted line) is indeed destabilizing. Small circles connected by dotted lines show a stepwise increase of the relative helicity H (its scale is shown at the axis on the right) in our energization procedure.
Paper: A Magnetogram-matching Method for Energizing Magnetic Flux Ropes Toward Eruption
Authors: V. S. Titov, C. Downs, T. Török, J. A. Linker
Figure caption: Side (panel (a)) and top (panel (c)) views of the magnetic field structure during the W evolution presented in Figure 2, shown here at t = 0.64. The shown magnetic surfaces that bound the MFR and its “arms” and the quasi-separators QS1 and QS2 are derived from the Q-map (b) in the central cross section of the configuration (see., Figure 1(e)).
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption: Unfolded Chandra (orange and red), XMM-Newton (purple and magenta), and NuSTAR (blue and cyan) 0.6–50 keV combined spectra of NGC 7479 modeled with MYTorus. The best-fit model is plotted with a solid green line, while the individual model components are plotted in black. Line-of-sight emission: solid line; reflection component: 90° reflection is plotted with dashed line, while the 0° reflection with a dashed–dotted–dashed line; scattering component: dashed–dotted; apec: dotted line.
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption: Unfolded Chandra (orange and red), XMM-Newton (purple and magenta), and NuSTAR (blue and cyan) 0.6–50 keV combined spectra of NGC 7479 modeled with UXCLUMPY. The best-fit model is plotted with a solid green line, while the individual model components are plotted in black. Reflection component: dashed line; scattering component: dashed–dotted; apec: dotted line.
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption: Unfolded Chandra (orange and red), XMM-Newton (purple and magenta), and NuSTAR (blue and cyan) 0.6–50 keV combined spectra of NGC 7479 modeled with borus02. The best-fit model is plotted with a solid green line, while the individual model components are plotted in black. Line-of-sight emission: solid line; reflection component: dashed line; scattering component: dashed–dotted; apec: dotted line.
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption: Line-of-sight hydrogen column density variability of NGC 7479 between 2001 and 2020. We note how the N H,av of the torus is higher with respect to the N H,los for all models. For clarity purposes, we added 50 days to the date of the second Chandra observation (Chandra-b in Table 1).
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption: cosθ  i  vs. CAGN (left), and cosθ  i  vs. Γ (right—upper) and log(N H,av) (right—bottom) multidimensional confidence contour plots obtained with borus02 model for all observations. In this case, the degeneracy between the parameters is broken in all scenarios.
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption: NGC 7479's torus representation based on best-fit parameters obtained during the modeling.
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption:  N H,los—C2 multidimensional confidence contour plots for Chandra-a (left), and Chandra-b (right) observations obtained with the three physically motivated models used in this work.
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption: Unfolded NuSTAR (blue and cyan), XMM-Newton (purple and magenta), and Chandra (orange and red) 0.6–50 keV single-epoch spectra of NGC 7479 modeled with borus02. The best-fit model is plotted with a solid green line, while the individual model components are plotted in black. Line-of-sight component: solid line; reflection component: dashed line; scattering component: dashed–dotted; apec: dotted line.
Paper: A Multiepoch X-Ray Study of the Nearby Seyfert 2 Galaxy NGC 7479: Linking Column Density Variability to the Torus Geometry
Authors: A. Pizzetti, N. Torres-Albà, S. Marchesi, M. Ajello, R. Silver, X. Zhao
Figure caption:  N H,los vs. cosθ  i , (left), and N H,los vs. Γ (right), multidimensional confidence contour plots obtained with the borus02 model for all observations. In both cases we see how all parameters are constrained within 1σ.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: Comparing the azimuthally averaged radial profile of the CO optical depth, τ 0, in black, with the azimuthally averaged radial profiles of the integrated intensities of the CO and CS emission, dark and light blue, respectively. The uncertainty shown on τ 0 is dominated by the statistical uncertainty associated with the fitting of the line profile rather than azimuthal scatter.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: Rotation profiles using the new parameterization to model non-Keplerian components. The top row shows the v  ϕ  in km s−1, while the bottom row shows them relative to a purely Keplerian rotation profile. Panels (a) and (d) show the impact of changing M disk, while panels (b) and (e) show the impact of changing γ. Panels (c) and (f) demonstrate how a negative M disk in this parameterization can be used to model sub-Keplerian rotation in the outer disk.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: The accuracy to which the parameters of a Gaussian profile can be fit to noisy data for a given sampling rate, R, and signal-to-noise ratio, S/N. Each column represents a different parameter, each row represents a different τ 0: 5, 3, 1, and 0, from top to bottom.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: Moment maps of the CS emission. The v 0 and ΔV panels are shown on the same scaling as CO in Figure 11. Only regions where I 0 > 3σ, where σ = 0.3 mJy beam−1, are shown.
Paper: Mapping the Complex Kinematic Substructure in the TW Hya Disk
Authors: Richard Teague, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Jane Huang, Cristiano Longarini, David Wilner
Figure caption: Moment maps of the CO emission. Only regions where I 0 > 5σ, where σ = 0.7 mJy beam−1, are shown.
Paper: Erratum: “Effect of Electrical Resistivity on the Damping of Slow Sausage Modes” (2020, ApJ, 897, 120)
Authors: Michaël Geeraerts, Tom Van Doorsselaere, Shao-Xia Chen, Bo Li
Figure caption: Damping time-to-period ratio as a function of the magnetic Reynolds number for the resistive mode obtained with our analytical model, which lies closest to the global mode obtained with the code of Chen et al. (2018) but for a boundary layer width l = 0.01, for different values of the longitudinal wavenumber k  z  and in the range of R  m  relevant for a photospheric pore. The dotted lines represent the numerical results from the code, whereas the solid lines are obtained through our analytical model. The red and magenta curves are for k  z  a = 0.7, the green and yellow curves are for k  z  a = 2.0, and the blue and cyan curves are for k  z  a = 4.3. Here [v si, v se, v Ae] = ﹩\left[0.5,0.75,0.25\right]{v}_{\mathrm{Ai}}﹩ and ﹩{\rho }_{0{\rm{e}}}={\rho }_{0{\rm{i}}}\left(\tfrac{{v}_{\mathrm{si}}^{2}}{\gamma }+\tfrac{{v}_{\mathrm{Ai}}^{2}}{2}\right)/\left(\tfrac{{v}_{\mathrm{se}}^{2}}{\gamma }+\tfrac{{v}_{\mathrm{Ae}}^{2}}{2}\right)﹩ with γ = 5/3. The values of B 0z  are determined by ﹩{v}_{{\rm{A}}}={B}_{0z}/\sqrt{{\mu }_{0}{\rho }_{0}}﹩.
Paper: GRB 190829A—A Showcase of Binary Late Evolution
Authors: Yu Wang, J. A. Rueda, R. Ruffini, R. Moradi, Liang Li, Y. Aimuratov, F. Rastegarnia, S. Eslamzadeh, N. Sahakyan, Yunlong Zheng
Figure caption: The ongoing accretion process onto the νNS and the NS companion, as simulated in Becerra et al. (2019). The νNS is located at the center of the dark blue spot, and is accreting the surrounding material. The SN ejecta are also being accreted by the NS companion, which is located at the center of the green spot. We also notice that the expansion of the SN ejecta is distorted by the companion NS and that some of the SN ejecta are flowing back to the νNS. This process creates a unique feature of BdHNe: the fallback accretion onto the νNS is enhanced, creating a second peak of accretion at about an orbital period of time after the SN explosion (see, e.g., Figure 5 in Becerra et al. 2019 for more details).
Paper: Erratum: “Effect of Electrical Resistivity on the Damping of Slow Sausage Modes” (2020, ApJ, 897, 120)
Authors: Michaël Geeraerts, Tom Van Doorsselaere, Shao-Xia Chen, Bo Li
Figure caption: Logarithm of the modulus of the dispersion function. The left panel shows a global view of the region where the slow modes lie, whereas the right panel focuses on the region marked by the black rectangle in the left panel, around ω Ci = 0.313. Here [v si, v se, v Ae] = [0.5, 0.75, 0.25]v Ai, k  z  a = 0.7, R m = 3 × 104, and ﹩{\rho }_{0{\rm{e}}}={\rho }_{0{\rm{i}}}\left(\tfrac{{v}_{\mathrm{si}}^{2}}{\gamma }+\tfrac{{v}_{\mathrm{Ai}}^{2}}{2}\right)/\left(\tfrac{{v}_{\mathrm{se}}^{2}}{\gamma }+\tfrac{{v}_{\mathrm{Ae}}^{2}}{2}\right)﹩ with γ = 5/3. The values of B 0z  are determined by ﹩{v}_{{\rm{A}}}={B}_{0z}/\sqrt{{\mu }_{0}{\rho }_{0}}﹩.
Paper: The Long Stare at Hercules X-1. I. Emission Lines from the Outer Disk, the Magnetosphere Boundary, and the Accretion Curtain
Authors: P. Kosec, E. Kara, A. C. Fabian, F. Fürst, C. Pinto, I. Psaradaki, C. S. Reynolds, D. Rogantini, D. J. Walton, R. Ballhausen, C. Canizares, S. Dyda, R. Staubert, J. Wilms
Figure caption: RGS spectra (stacked for visual purposes) from observation 0865440501 around the excluded 22.25–24 Å region. Two spectral models are shown, and the most important model features are denoted with labels. The green model includes the problematic region while the blue model ignores it. The green model clearly overpredicts the broadening of the medium-width O VIII and N VII features. The position of the possible instrumental feature is indicated by the arrow.