adsabs/AstroCLIMB huggingface dataset:
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Spacetime distribution of the accretion rate in the atmospheric region on the lower side (−15H < z < − 4H) for all runs. Black contour shows the region where the accretion rate in the high-altitude region exceeds the averaged accretion rate in the disk region (∣z∣ ≤ 4H). The dotted line represents the gas motion that feels half of the gravity force, −GM/2r, for reference. Note that the cases without the Hall effect do not show any values in this plot.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Comparison of the temperature models of the passively heated disks where the density structure is in vertically isothermal hydrostatic equilibrium. The models are the CG97 two-layer model (dotted), H90 model (solid), and modified two-layer model (dashed). Left: altitude of the irradiation front, normalized by the gas scale height. Middle: irradiation heating rate per unit area, normalized by the stellar radiation flux in the optically thin limit. Right: midplane temperature profiles, with the red line indicating RADMC-3D calculation.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Same as Figure 13, but for FidH+, with firr shown separately for the top and bottom surfaces. The two-layer model with a surface optical depth of τr,irr = 0.4 is also plotted.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Comparison of the simulation temperatures (t = 365 yr) with those calculated from RADMC-3D. Each column represents the simulation runs: FidNoH (left), FidH+ (middle), and FidH− (right). The top panels display the midplane temperature profiles, while the bottom panels show the vertical profile around the midplane at r = 1, 3, 10, 30 au.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Midplane temperature profile around the snowline (T = 170 K), with the time average over 200 yr. The colored solid lines represent the result of the simulation. The gray thin lines represent the temperature of the Static model for comparison.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Vertical temperature profile at r = 5 au and t = 365 in the FidH+ run. The solid line indicates the gas temperature, the dashed line indicates the dust temperature used in the source term, and the dotted line indicates the radiation temperature including the stellar optical irradiation and infrared reemitted radiation.
Paper: Radiative Nonideal Magnetohydrodynamic Simulations of Inner Protoplanetary Disks: Temperature Structures, Asymmetric Winds, and Episodic Surface Accretion
Authors: Shoji Mori, Xue-Ning Bai, Kengo Tomida
Figure caption: Same as the left panels of Figure 14, but for the FidH− run with the snapshots at t = {380, 383, 389, 391} yr. The lines of τr,xuv = 1 (dotted) and τr,irr = 1 (dashed–dotted) are also shown.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: EWLIS vs. EWLyα. Dashed lines with circle markers represent the transmitted (uncorrected for IGM attenuation of Lyα) values reported in A. J. Pahl et al. (2020) and X. Du et al. (2018). These data show a clear correlation with weaker LIS absorption corresponding to stronger Lyα emission. Square and star markers represent values measured from our skewed Gaussian fits. Symbol colors correspond to the redshift of each sample: black (z ∼ 2), blue (z ∼ 3), green (z ∼ 4), orange (z ∼ 5), and red (z ∼ 7). The black arrow shows the effect of correcting for ∼50% IGM attenuation of the Lyα emission as found by M. Tang et al. (2024). We note that for this plot and other figures, negative (positive) EW values correspond to absorption (emission). The full PANCAKEZ composite shows clear deviation from the lower-z trends with overall weaker LIS absorption and suppressed Lyα emission.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: Velocity profiles of Lyα emission (left column), LIS absorption (middle column), and nebular C IV λλ1548, 1551 emission (right column) from our stacked spectra. Each row displays the respective profiles from our non-LAEs (top row), LAEs (middle row), and full PANCAKEZ (bottom row) samples. Bootstrap error spectra (maroon) are shown in each panel along with a dashed black line which represents the relative continuum level. Black tick marks denote the systemic redshift of the spectral features. Note that the Lyα profiles (left column) have different vertical scaling across the three stacks. This figure highlights key spectral differences seen between our full, LAE, and non-LAE stacks. In particular the LAE stack has weaker LIS absorption and stronger C IV emission.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: The overall distribution of MUV and redshifts for the 64 galaxies that make up the PANCAKEZ sample. Lyα emitters (LAEs) are shown in green and non-LAEs are in blue. The full sample is shown with red histograms. (a) The distribution of MUV as a function of redshift. (b) The number distribution of MUV. (c) The number of galaxies in a given redshift bin. For reference, the characteristic UV luminosity is M*UV = −21.15 ± 0.13 at z ≈ 6.8 as reported by R. J. Bouwens et al. (2021).
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: The measured LIS absorption velocity centroid (vcen,LIS) for our full z ∼ 7 composite compared with z = 2–5 samples. The top panel shows measured values from our best-fit skewed Gaussian models while the bottom panel shows the values measured from our best-fit symmetric models. Overall we see that the z ∼ 7 stack has a considerably lower LIS velocity offset compared to the lower-z stacks.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: The redshift trend of average EWLIS from z = 2–5 samples (square markers) and our z ∼ 7 composite (star marker). EWLIS values are measured from skewed Gaussian profile fits applied consistently to all composite spectra. Plotted redshifts represent the average for each composite spectrum (or the reported median redshift in the case of A. J. Pahl et al. 2020). The black dashed line represents the best-fit linear relation, illustrating the overall trend of weaker EWLIS at higher redshifts.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: Top: the full composite spectrum of the 64 zspec ≥ 6 galaxies. Middle: the number of spectra combined at each wavelength, shown for each filter individually. Bottom: the average redshift calculated at each wavelength of the combined galaxies. Black represents the weighted average. Overall our fiducial stack probes a consistent sample of galaxies across a broad wavelength range in each filter composite, and across the full wavelength range of the weighted average. The majority of rest-frame UV ISM features used in this work are captured entirely by the G140M filter, while rest-frame optical emission lines are predominantly covered by the G395M filter.
Paper: Investigating the Sulfur Mystery in Protoplanetary Disks through Chemical Modeling
Authors: Becky J. Williams, L. Ilsedore Cleeves, Rachel E. Gross, Jackson Baker
Figure caption: Disk-averaged column densities of CS, SO, and C2S in our models, compared to observational data. The top plot is the average from 1 to 100 au, and the bottom plot is the average from 10 to 100 au. Model runs are listed in Table 2. The blue shaded region shows the 1σ detected CS column densities from R. Le Gal et al. (2021), and the dashed orange and mint green lines show the upper limits of SO and C2S, respectively, also from R. Le Gal et al. (2021). These upper limits are the values for the disk around IM Lup, chosen because IM Lup is the most similar in age and stellar mass to our modeled disk.
Paper: Investigating the Sulfur Mystery in Protoplanetary Disks through Chemical Modeling
Authors: Becky J. Williams, L. Ilsedore Cleeves, Rachel E. Gross, Jackson Baker
Figure caption: Variations in the abundance of CS and SO for different volatile sulfur abundances. The first two plots compare mid1 to low1 (S/H = 10−8–10−9), and the second two plots compare high1 to mid1 (S/H = 10−7–10−8). We only plot regions where the abundance of the shown molecule is greater than 10−15 relative to H2.
Paper: Investigating the Sulfur Mystery in Protoplanetary Disks through Chemical Modeling
Authors: Becky J. Williams, L. Ilsedore Cleeves, Rachel E. Gross, Jackson Baker
Figure caption: Physical environment of the 2D model, showing gas density, gas temperature, ultraviolet radiation, and X-ray radiation.
Paper: Investigating the Sulfur Mystery in Protoplanetary Disks through Chemical Modeling
Authors: Becky J. Williams, L. Ilsedore Cleeves, Rachel E. Gross, Jackson Baker
Figure caption: Abundance of sulfur species over time at R = 40 au, Z = 8 au (Z/R = 0.2), for run mid8, where sulfur begins in the form S8 ice. Sulfur allotropes are destroyed around 104–105 yr, as simpler sulfur forms (S, SO2 ice, OCS ice, and SO ice) become the dominant sulfur carriers.
Paper: Investigating the Sulfur Mystery in Protoplanetary Disks through Chemical Modeling
Authors: Becky J. Williams, L. Ilsedore Cleeves, Rachel E. Gross, Jackson Baker
Figure caption: Abundances of four ice species, H2S, SO2, OCS, and SO, for the four models where we varied the initial sulfur form (mid1: CS and SO, mid7: H2S, mid8: S8 ice, and mid9: S). For more specifics on the model runs, refer to Table 2.
Paper: Investigating the Sulfur Mystery in Protoplanetary Disks through Chemical Modeling
Authors: Becky J. Williams, L. Ilsedore Cleeves, Rachel E. Gross, Jackson Baker
Figure caption: Log of the CS/SO ratio as C/O ratio increases from 0.36 to 1.40 (see Table 2). The light gray contour lines show where the CS/SO ratio equals the C/O ratio for that run. For each plot, we only plot regions where the abundance of at least one molecule is greater than 10−15 relative to H2.
Paper: Investigating the Sulfur Mystery in Protoplanetary Disks through Chemical Modeling
Authors: Becky J. Williams, L. Ilsedore Cleeves, Rachel E. Gross, Jackson Baker
Figure caption: Abundances of 15 sulfur-bearing species in a generic disk for the standard case (mid1). The total sulfur abundance is S/H2 = 2 × 10−8, C/O = 0.36, and the initial sulfur form is gas-phase CS and SO.
Paper: Investigating the Sulfur Mystery in Protoplanetary Disks through Chemical Modeling
Authors: Becky J. Williams, L. Ilsedore Cleeves, Rachel E. Gross, Jackson Baker
Figure caption: Column density as a function of radius for all model runs. Each column is a different molecule, and each row is a different set of model runs. See Table 2 for the parameters of each run.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: Stacked LIS absorption profiles from A. E. Shapley et al. (2003, blue), T. Jones et al. (2012, green), A. J. Pahl et al. (2020, orange), and this work (red). Solid lines show the respective mean LIS absorption and the dashed lines represent the best-fit skewed Gaussian model. Note that individual spectra are shifted vertically in increments of 0.5 for display purposes. The averaged LIS absorption from our z ∼ 7 stack displays a smaller velocity offset (i.e., less blueshifted) along with overall weaker absorption strength compared to the lower-z studies.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: The composite spectrum continuum SNR as a function of the number of galaxies combined to create the stack. The color of each symbol represents the minimum continuum SNR (“SNR Threshold,” or SNRthresh) that individual galaxies must achieve in order to be included. As expected for our methodology, the highest composite SNR (≈6.3) is achieved by combining galaxies with relatively high individual SNR, but at the cost of having a small sample size (N = 20 out of the parent sample of 131). Conversely, combining galaxies with low individual continuum SNR results in having a lower SNR in the stacked composite spectrum (yellow circle). The star marker indicates the fiducial N = 64 PANCAKEZ sample, which balances the desires of a large representative sample and good continuum SNR.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: The full PANCAKEZ composite spectrum for each JWST grating: G140M (blue), G235M (orange), and G395M (green). The filter composites are constructed by averaging normalized individual spectra in units of fν (Section 3). Prominent spectral features are labeled with names and dotted vertical lines. Closely separated doublets are marked with “λλ.” The bootstrap error spectrum for each filter stack is shown in maroon under the composite, subtracted uniformly by one for clarity. This figure showcases the quality of our composite spectrum constructed from our fiducial sample of 64 z > 6 galaxies.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: The rest-frame UV composite spectra from A. E. Shapley et al. (2003, blue), T. Jones et al. (2012, green), and A. J. Pahl et al. (2020, orange) overlaid on our full 64 galaxy PANCAKEZ composite (red). All spectra are consistently normalized at rest-frame 1450–1500 Å. Black dotted lines in the upper panel mark various spectral features of interest: H I λ1216 (Lyα), Si II λ1260, O I λ1302, Si II λ1304, C II λ1334, Si II λ1526, and C IV λλ1548, 1550. Overall the PANCAKEZ composite shows a continuum shape and spectral features similar to the lower-z studies, although LIS absorption lines and Lyα emission are weaker in the PANCAKEZ z ∼ 7 composite.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: Stacked Lyα emission profiles from A. E. Shapley et al. (2003, blue), T. Jones et al. (2012, green), A. J. Pahl et al. (2020, orange), and this work (red). Skewed Gaussian models are shown as a dashed line superimposed on the respective stack. A gray dashed line is drawn at the rest-frame wavelength of Lyα. Individual spectra are shifted vertically in increments of two for display purposes. The Lyα emission from our z ∼ 7 stack is significantly weaker than in the lower-z studies, which we attribute to suppression due to neutral H I in the IGM at z ∼ 7.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: The rest-frame UV composite spectra produced from the full 64 galaxy PANCAKEZ sample (red), our bin of 12 LAEs (green), and our bin of 52 non-LAEs (blue). The top panel displays all three composites plotted directly top of each other while the bottom panel has them vertically separated by increments of two. Black dotted lines denote various spectral features of interest (see Figure 3): H I λ1216 (Lyα), Si II λ1260, O I λ1302, Si II λ1304, C II λ1334, Si II λ1526, and C IV λλ1548, 1550.
Paper: Stacking PANCAKEZ: Spectroscopic Analysis with NIRSpec Stacks in the Epoch of Reionization. Weak Interstellar Medium Absorption and Implications for Ionizing Photon Escape at z ∼ 7
Authors: Kelsey S. Glazer, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Maruša Bradač, Anthony J. Pahl, Alice E. Shapley, Richard S. Ellis, Michael W. Topping, Naveen A. Reddy
Figure caption: The reddening-corrected O32 vs. R23 diagram for the PANCAKEZ sample (red stars), compared with low-redshift SFGs from the Sloan Digital Sky Survey (SDSS; C. A. Tremonti et al. 2004) shown in gray scale. The cyan dashed line marks the median ridgeline of the SDSS sample within the high-ionization/excitation tail. Also shown are recent JWST composites from A. J. Cameron et al. (2023), R. L. Sanders et al. (2023), and G. Roberts-Borsani et al. (2024; color coded by redshift). The PANCAKEZ sample, with its high ionization/excitation, lies on the extreme tail of the low-z galaxy distribution and is representative of typical galaxies at z > 6.
Paper: Monte Carlo Simulations of Polarized Radiative Transfer in Neutron Star Atmospheres
Authors: Hoa Dinh Thi, Matthew G. Baring, Kun Hu, Alice K. Harding, Joseph A. Barchas
Figure caption: Angular distributions for intensity (left panel) and linear polarization degree, ﹩{{\rm{\Pi }}}_{l}=\sqrt{{Q}^{2}+{U}^{2}}/I=\left|Q/I\right|﹩ (right panel), as functions ﹩\cos {\theta }_{z}﹩ from the MAGTHOMSCATT simulation (black histograms). Note that U = 0 due to the integration over azimuthal angles around the zenith. The simulation was performed for ω/ωB = 1000, τeff = 10, ﹩{{ \mathcal N }}_{{\rm{rec}}}=1{0}^{11}﹩, and θB = 0°. The distributions are binned at a θz resolution of 0.0625°. The red dashed lines present the analytical fit functions in Equation (19), while the traces with green diamonds and blue crosses, respectively, correspond to results from S. Chandrasekhar (1960) and R. A. Sunyaev & L. G. Titarchuk (1985) for nonmagnetic Thomson transport. The intensities (left panel) in S. Chandrasekhar (1960; green diamonds) and in R. A. Sunyaev & L. G. Titarchuk (1985; blue crosses) are scaled by factors of 2 and 2.54, respectively.
Paper: Monte Carlo Simulations of Polarized Radiative Transfer in Neutron Star Atmospheres
Authors: Hoa Dinh Thi, Matthew G. Baring, Kun Hu, Alice K. Harding, Joseph A. Barchas
Figure caption: Simulated intensity pulse profiles from the MAGTHOMSCATT simulation displayed for two rotational cycles for three different frequency ratios: ω/ωB = 0.003 (dots), ω/ωB = 0.01(solid lines), and ω/ωB = 0.03 (dashed lines). Emissions are from two identical antipodal polar caps, extending from the respective magnetic poles to colatitudes of θcap = 15° (top row) and θcap = 30° (bottom row); all photons are propagated through a general relativistic magnetosphere. Two values of inclination angles are considered: α = 30° (left column) and α = 60° (right column). Each panel shows the pulse profiles for three selected viewing angles: ζ = 10° (orange), ζ = 50° (black), and ζ = 90° (blue).
Paper: Monte Carlo Simulations of Polarized Radiative Transfer in Neutron Star Atmospheres
Authors: Hoa Dinh Thi, Matthew G. Baring, Kun Hu, Alice K. Harding, Joseph A. Barchas
Figure caption: Angular distributions of intensity (top row) and Q/I (bottom row) obtained with the standard AP protocol (black solid lines), where ﹩{n}_{{\rm{scat}},{\rm{\min }}}=1﹩ for all θi and θB, in comparison with those obtained with the AP* protocol, where ﹩{n}_{{\rm{scat}},{\rm{\min }}}﹩ is given by Equation (20), for ω/ωB = 0.03. The results are displayed for three selected θB values: θB = 0° (left column), θB = 20° (middle column), and θB = 60° (right column). The results at convergence in the AP* protocol are shown in red dashed lines. In panels (b) and (c), we also present for the AP* protocol distributions at three τeff values smaller than the convergence one.
Paper: Monte Carlo Simulations of Polarized Radiative Transfer in Neutron Star Atmospheres
Authors: Hoa Dinh Thi, Matthew G. Baring, Kun Hu, Alice K. Harding, Joseph A. Barchas
Figure caption: Same as Figure 11, but for the linear polarization degree.