adsabs/AstroCLIMB huggingface dataset:
Paper: Eta Carinae: The Dissipating Occulter Is an Extended Structure
Authors: Theodore R. Gull, Henrik Hartman, Mairan Teodoro, D. John Hillier, Michael F. Corcoran, Augusto Damineli, Kenji Hamaguchi, Thomas Madura, Anthony F. J. Moffat, Patrick Morris, Krister Nielsen, Noel D. Richardson, Ian R. Stevens, Gerd Weigelt
Figure caption: Sketch of the structures within the Homunculus as seen alone our LOS (not to scale). Is the occulter a portion of the Little Homunculus or a dense clump, like the Weigelt clumps that appear to be within several hundred astronomical units of the binary? In the NUV spectra recorded between 2000 and 2004, multiple, weaker shells at various velocities clustered near −513 km s−1, associated with the Homunculus and the 1840s Great Eruption, were identified (Gull et al. 2006). Additional shells clustered in velocities above and below −146 km s−1 are associated with the Little Homunculus ejected in the 1890s Lesser Eruption. By 2018, signatures of most of the weaker shells had disappeared. For scale, the strongest component of the Homunculus, moving at −513 km s−1 since the 1840s, is about 1.8 × 104 au and the Little Homunculuus, moving at −146 km s−1 since the 1890s, is about 3 × 103 au in front of η Car. The occulter and the interacting winds are associable with or within the Little Homunculus (see Figure 9). The reader may note that the shape and extent of the occulter remains uncertain.
Paper: Eta Carinae: The Dissipating Occulter Is an Extended Structure
Authors: Theodore R. Gull, Henrik Hartman, Mairan Teodoro, D. John Hillier, Michael F. Corcoran, Augusto Damineli, Kenji Hamaguchi, Thomas Madura, Anthony F. J. Moffat, Patrick Morris, Krister Nielsen, Noel D. Richardson, Ian R. Stevens, Gerd Weigelt
Figure caption: [Fe II] shell expansion. The displayed image is the ratio of the [Fe II] λ4815 line recorded at ϕ = 12.516 and 13.004 to enhance the expanding shells caused by the passage of η Car-B through the extended continuous wind of η Car-A. The velocity range is 40 km s−1 centered on −60 km s−1. The three pairs of arrows point to the ends of the three shells found to be expanding outward. These shells do not exist to the NW as the secondary wind has continuously blocked the primary wind throughout the high-ionization state and the FUV radiation from η Car-B has ionized iron to higher ionization states (see Figure 6 in Gull et al. 2016 for additional velocity frames). The + symbol indicates the position of η Car.
Paper: Eta Carinae: The Dissipating Occulter Is an Extended Structure
Authors: Theodore R. Gull, Henrik Hartman, Mairan Teodoro, D. John Hillier, Michael F. Corcoran, Augusto Damineli, Kenji Hamaguchi, Thomas Madura, Anthony F. J. Moffat, Patrick Morris, Krister Nielsen, Noel D. Richardson, Ian R. Stevens, Gerd Weigelt
Figure caption: Sketch of the structures in close proximity to the binary (not to scale). The massive primary, η Car-A, has a very extended wind structure (dark blue) which is modified by the lesser, but faster, wind of η Car-B. Three shells of compressed primary wind, seen in [Fe II] λ4815 (Teodoro et al. 2013), are located beyond the current wind structure of the binary. The occulter has a structure that extends to one side of the binary. The occulter blocked one side of the extended primary wind and strongly blocked the central core, but as the occulter dissipated, our LOS to the core has become increasingly transparent. The leading edge is toward the observer with rotation counterclockwise. On the far side of η Car a dusty structure scatters light from the binary back toward the observer.
Paper: Eta Carinae: The Dissipating Occulter Is an Extended Structure
Authors: Theodore R. Gull, Henrik Hartman, Mairan Teodoro, D. John Hillier, Michael F. Corcoran, Augusto Damineli, Kenji Hamaguchi, Thomas Madura, Anthony F. J. Moffat, Patrick Morris, Krister Nielsen, Noel D. Richardson, Ian R. Stevens, Gerd Weigelt
Figure caption: Low-velocity absorptions attributable to the occulter. Top: Si II λ1309 velocity profile. Two strong absorptions centered at −18 and −32 km s−1 with two weaker components at −50 and +1 kms (foreground cloud). Bottom: C IV λ1551 velocity profile with a strong absorption centered at −39 km s−1 and extending from −20 to −70 km s−1. Observation recorded at ϕ = 13.886.
Paper: Eta Carinae: The Dissipating Occulter Is an Extended Structure
Authors: Theodore R. Gull, Henrik Hartman, Mairan Teodoro, D. John Hillier, Michael F. Corcoran, Augusto Damineli, Kenji Hamaguchi, Thomas Madura, Anthony F. J. Moffat, Patrick Morris, Krister Nielsen, Noel D. Richardson, Ian R. Stevens, Gerd Weigelt
Figure caption: Comparison of the spatial profiles for the spectro-images recorded at ϕ = 10.404 and ϕ = 13.641 (see Figure 4). Left: cross section showing the shifts of the SSE ridge at −0.″5 and the NNW edge at +0.″5. Expansion is notable from the ridge and valley to the SSE and possibly the edge to the NNW. Right: η Car profiles. While the stellar flux in the NUV increased sixfold between 2000 and 2018, the measured FWHM was 0.″11 for both stellar profiles. Note that both plots are in flux units, not normalized.
Paper: Eta Carinae: The Dissipating Occulter Is an Extended Structure
Authors: Theodore R. Gull, Henrik Hartman, Mairan Teodoro, D. John Hillier, Michael F. Corcoran, Augusto Damineli, Kenji Hamaguchi, Thomas Madura, Anthony F. J. Moffat, Patrick Morris, Krister Nielsen, Noel D. Richardson, Ian R. Stevens, Gerd Weigelt
Figure caption: Changes in absorption lines originating from the ground state. Within one orbital cycle strong absorptions in the high-ionization state (left, ϕ = 10.404) increase to even stronger absorptions in the low-ionization state (middle, ϕ = 11.037). Two broad velocity complexes centered on −500 and −150 km s−1 at the star position extend from ≈ − 550 and −200 km s−1 SSE (below the position of η Car) to near 0 km s−1 to the NNW (above the position of η Car). Three orbital cycles later, the absorptions in the high-ionization state have all but disappeared in the SSE (right, ϕ = 13.641) caused by the tenfold increase in FUV radiation. Only one component, −513 km s−1 associated with the Homunculus, remains SSE (bottom) of η Car, but a broader component extending from the star position remains to the NNW which demonstrates that the absorption remains in the walls at lower elevations of the Homunculus foreground lobe. The 0 km s−1 IS absorption lines serve as velocity reference for each of the shell structures. The leftmost absorption line, Mn II λ2577, is described in more detail and in velocity space in Figures 3 and 4.
Paper: Eta Carinae: The Dissipating Occulter Is an Extended Structure
Authors: Theodore R. Gull, Henrik Hartman, Mairan Teodoro, D. John Hillier, Michael F. Corcoran, Augusto Damineli, Kenji Hamaguchi, Thomas Madura, Anthony F. J. Moffat, Patrick Morris, Krister Nielsen, Noel D. Richardson, Ian R. Stevens, Gerd Weigelt
Figure caption: Comparison of changes of Fe II absorption lines originating from the 1.0 eV energy level. As with the ground state absorbers, the absorption increases between the high-ionization state (left, ϕ = 10.404) and the low-ionization state (middle, ϕ = 11.037). The absorptions nearly disappear in the SSE (below the position of η Car), other than the −513 km s−1 component, in the high-ionization state three orbital cycles later (right, ϕ = 13.641). Likewise, the broad absorption remains to the NNW (above the position of η Car) at lower latitudes of the foreground lobe. The right-most absorption line, Fe II λ2757, is presented in more detail and in velocity space in Figures 3 and 4.
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: The Ti/Fe–Mn/Fe (top) and Ti/Fe–Cr/Fe (bottom) mass ratios observed in the Fe-rich ejecta. The faint orange areas are the combination of two of the mass ratios (99% confidence level, Δχ 2 = 6.64). The orange lines indicate the 99% confidence contour for two parameters (Δχ 2 = 9.21). The colored points show the mass ratios in our nucleosynthesis calculations. The color scale indicates the entropy per baryon at the peak temperature in each calculation. The solid and dotted lines indicate the calculations with and without the ν-process, respectively. Here the total neutrino energy is assumed to be 3 × 1053 erg, which corresponds to the binding energy for a neutron star with ∼1.4 M ⊙. The curves plotted with squares show a parameter study for the typical α-rich freeze-out environment (T peak = 6 GK, Y e = 0.499) while changing the initial density from 105.5 to 107.5 g cm−3 (cases a and ﹩{{\rm{a}}}^{{\prime} }﹩). The curves plotted with circles show the same but for a hot (T peak = 10 GK) and proton-rich (Y e = 0.55) environment (cases b and ﹩{{\rm{b}}}^{{\prime} }﹩). In the bottom panel, the curves with and without the ν-process lie mostly on top of each other, except for the proton-rich environment case (circles) at the largest entropy values (which are, anyway, far from the allowed observational range).
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: (a) Asymmetric ejecta distribution in the Cassiopeia A SN remnant. Red and blue highlight Fe- and O-rich emission regions, respectively. The Chandra ratio map of the Si/Mg band is shown in green, where the jetlike structures can be seen in the northeastern and southwestern directions (e.g., Hwang et al. 2004; Laming et al. 2006; Ikeda et al. 2022). In the southeastern region, it has been proposed (Hughes et al. 2000; Wongwathanarat et al. 2017; Orlando et al. 2021; Sato et al. 2021) that the apparent overturning of ejecta layers was produced by plumes from rising bubbles in the neutrino-driven convection layer during the SN explosion. (b) X-ray spectrum (black data) from the Fe-rich region. The red curve shows the best-fit thermal model without Cr and Mn emissions. In the 5.5–5.9 and 6.0–6.3 keV photon energy bands (denoted with faint gray and yellow regions), X-ray line features from shocked Cr and Mn are clearly identified.
Paper: Examining Neutrino–Matter Interactions in the Cassiopeia A Supernova
Authors: Toshiki Sato, Takashi Yoshida, Hideyuki Umeda, John P. Hughes, Keiichi Maeda, Shigehiro Nagataki, Brian J. Williams
Figure caption: The Ti/Fe and Mn/Fe mass ratios observed in the Fe-rich ejecta (same as the top panel of Figure 2) compared with models that have values of Y e varying from 0.51 to 0.58. The colored curves show a parameter study for hot and proton-rich ejecta (T peak = 10 GK, Y e > 0.5) while changing the initial density from 105.5 to 107.5 g cm−3. We used the thermodynamic trajectory taken from the innermost region of our 1D SN model (Z = 0.5 Z ⊙ and ﹩{E}_{\exp }=3\times {10}^{51}﹩ erg) to calculate these models. The high explosion energy for the Cassiopeia A SN has been supported by some previous studies (e.g., Hwang & Laming 2012; Laming & Temim 2020; Sato et al. 2020).
Paper: As Simple as Possible but No Simpler: Optimizing the Performance of Neural Net Emulators for Galaxy SED Fitting
Authors: Elijah P. Mathews, Joel Leja, Joshua S. Speagle, 佳士 沈, Benjamin D. Johnson, Justus Gibson, Erica J. Nelson, Katherine A. Suess, Sandro Tacchella, Katherine E. Whitaker, Bingjie Wang, 冰洁 王
Figure caption: The emulation precision of each emulator trained in this work as a function of filter effective wavelength, where the precision is expressed in terms of ﹩\mathrm{arsinh}﹩ magnitudes (the native outputs of the emulator, as defined in Section 2.1). Emulation precision generally doubles (i.e., σ decreases by a factor of 2) as network width doubles, except for filters in the far-IR and for extremely wide networks, which see diminishing returns. Solid lines denote architectures deemed sufficiently accurate and precise for SED fitting in this work, while dashed–dotted lines denote emulators deemed marginally sufficient and dotted lines denote emulators deemed insufficient.
Paper: As Simple as Possible but No Simpler: Optimizing the Performance of Neural Net Emulators for Galaxy SED Fitting
Authors: Elijah P. Mathews, Joel Leja, Joshua S. Speagle, 佳士 沈, Benjamin D. Johnson, Justus Gibson, Erica J. Nelson, Katherine A. Suess, Sandro Tacchella, Katherine E. Whitaker, Bingjie Wang, 冰洁 王
Figure caption: Execution time of ANN emulators (on a CPU) as a function of the width of the network (i.e., the number of nodes per layer). The solid black line denotes the median execution time among all benchmark trials evaluated with a given architecture, while the shaded region encompasses the  ±1σ quantiles of those trials. The dashed gray line near the top of the plot denotes the execution time of FSPS with the settings used for our physical model. The colored points denote the network widths used for the emulators trained in this work. For network widths N ≥ 256, the execution time scales approximately as N 2.01±0.01.
Paper: As Simple as Possible but No Simpler: Optimizing the Performance of Neural Net Emulators for Galaxy SED Fitting
Authors: Elijah P. Mathews, Joel Leja, Joshua S. Speagle, 佳士 沈, Benjamin D. Johnson, Justus Gibson, Erica J. Nelson, Katherine A. Suess, Sandro Tacchella, Katherine E. Whitaker, Bingjie Wang, 冰洁 王
Figure caption: Covariance matrices for the 32 node-per-layer emulator (left) and 1024 node-per-layer emulator (right), normalized by the emulation precision in the relevant filters (i.e., plotted is  σ  ij /(σ  i  σ  j )). Note the differing color bar scales between the two plots. Compared to the 32 node-per-layer emulator, the 1024 node-per-layer emulator provides covariances that are both smaller in scale and less spectrally widespread (i.e., they are limited to filters with similar effective wavelengths).
Paper: As Simple as Possible but No Simpler: Optimizing the Performance of Neural Net Emulators for Galaxy SED Fitting
Authors: Elijah P. Mathews, Joel Leja, Joshua S. Speagle, 佳士 沈, Benjamin D. Johnson, Justus Gibson, Erica J. Nelson, Katherine A. Suess, Sandro Tacchella, Katherine E. Whitaker, Bingjie Wang, 冰洁 王
Figure caption: Illustration of the neural network architecture used in this work. At the far left, a vector   θ  of physical parameters is taken as input, from which a precomputed mean is subtracted and standard deviation divided to normalize the inputs. Then, a set of L − 1 hidden layers (where L = 6 for the entirety of this work), each of which has N fully connected nodes using the GELU activation function as described in Section 2.2. The final fully connected layer, layer L, has linear activation and a number of nodes equal to the number of predicted photometric filters (137 in this work). Finally, the output has a precomputed mean readded (the precomputed standard deviation is fixed to 1), which represents the predicted photometry.
Paper: As Simple as Possible but No Simpler: Optimizing the Performance of Neural Net Emulators for Galaxy SED Fitting
Authors: Elijah P. Mathews, Joel Leja, Joshua S. Speagle, 佳士 沈, Benjamin D. Johnson, Justus Gibson, Erica J. Nelson, Katherine A. Suess, Sandro Tacchella, Katherine E. Whitaker, Bingjie Wang, 冰洁 王
Figure caption: The difference in behavior between ordinary logarithmic magnitudes (e.g., AB magnitudes) and the ﹩\mathrm{arsinh}﹩ magnitude system used in the emulators in this work. For logarithmic magnitudes significantly brighter than  μ 0, the ﹩\mathrm{arsinh}﹩ system behaves identically to the logarithmic system. However, for logarithmic magnitudes  ≥μ 0, the ﹩\mathrm{arsinh}﹩ system asymptotically approaches a constant value μ 0 (equal to 35 in this work).
Paper: As Simple as Possible but No Simpler: Optimizing the Performance of Neural Net Emulators for Galaxy SED Fitting
Authors: Elijah P. Mathews, Joel Leja, Joshua S. Speagle, 佳士 沈, Benjamin D. Johnson, Justus Gibson, Erica J. Nelson, Katherine A. Suess, Sandro Tacchella, Katherine E. Whitaker, Bingjie Wang, 冰洁 王
Figure caption: The distribution of absolute test set residuals (i.e.,  ∣emulated − actual∣) for each emulator, evaluated for the Mayall Mosaic U, Keck LRIS R  s , JWST NIRCam F277W, and Spitzer MIPS 24 μm filters. The thin vertical dotted lines denote the residual corresponding to the distribution’s  ∼68th percentile.
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Mass-loss rate ﹩\dot{M}﹩ (top), kinetic power ﹩{E}_{K}=(W-1)\dot{M}﹩ (center), where W is the Lorentz factor, and ﹩\dot{M}﹩-weighted average specific entropy s (bottom) of the outflows through a spherical surface of radius r = 60 km, as a function of time since magnetic field initialization. For all models, no-B (black, ×), lo-B (blue circles), and hi-B (red triangles), these quantities are shown across the full 4π solid angle. For model hi-B (red), we show separately the isotropic-equivalent mass-loss rate as well as the kinetic power, and the average entropy across a solid angle at high latitudes close to the poles (θ = 0°–45° and θ = 135°–180°; dotted line) and near the equatorial plane (θ = 45°–135°; solid line).
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Change in the energy contained within the volume extending from r = 15 km to an outer radius r between t ≈ 15 ms and t ≈ 55 ms following the initialization of the magnetic field for model hi-B. Left: polar component, averaged azimuthally and over polar angles θ = 0°–45° and 135°–180°. Right: equatorial component, averaged azimuthally and over polar angles θ = 45°–135°. The energies are defined as follows: kinetic energy ﹩{E}_{K}\,=\int (W-1)\rho W\sqrt{\gamma }\,{d}^{3}x﹩ (blue); thermal energy ﹩{E}_{\mathrm{th}}=\int \epsilon \rho W\sqrt{\gamma }\,{d}^{3}x﹩ (green); electromagnetic energy ﹩{E}_{\mathrm{EM}}=\int {n}_{\mu }{n}_{\nu }{T}_{\mathrm{EM}}^{\mu \nu }\sqrt{\gamma }\,{d}^{3}x﹩ (black); and net integrated neutrino heating ﹩{Q}_{\mathrm{net}}=\int \int {\dot{q}}_{\mathrm{net}}\rho W\sqrt{\gamma }\,{d}^{3}x\,{dt}﹩ (red). Here, ﹩{T}_{\mathrm{EM}}^{\mu \nu }﹩ is the electromagnetic stress–energy tensor, n  μ  is the four-velocity of the Eulerian observer, W is the Lorentz factor associated with the total four-velocity, and γ is the determinant of the three-metric. The specific net neutrino-heating rate ﹩{\dot{q}}_{\mathrm{net}}﹩ is integrated over the time interval; all other quantities are evaluated at the final and initial times, with their difference plotted.
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Radial profiles of the poloidal magnetic field strength B P for models lo-B and hi-B, taken from a slice through the magnetic dipole axis (y = 0), angle averaged in the polar region from θ = 0° to θ = 45°. Solid lines show B P time averaged from t ≈ 0–5 ms after the magnetic field is activated, while dashed lines represent B P time averaged from t ≈ 25–35 ms. To guide the eye, thick solid lines show power laws of r −2 (blue) and r −3 (green). Both models approach the split-monopole solution (∝r −2) in the polar region.
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Snapshots of the outflow properties as a cross section through the magnetic dipole axis (y = 0 plane) at t ≈ 55 ms after B-field initialization for models lo-B (left) and hi-B (right). Colors show the rest-mass density ρ, with the magnetic field line geometry overlaid in white. The neutrinosphere (﹩{\tau }_{{\bar{\nu }}_{e}}=1﹩ surface) is shown with a red contour. The field lines have been nearly completely torn open radially in the weakly magnetized model, while an equatorial belt of closed field lines persists in the strongly magnetized case.
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Snapshots of the radial velocity v  r  in the y = 0 magnetic dipole axis plane for models lo-B and hi-B. The top panel shows the moment the magnetic field is initialized (t ≈ 0 ms), while the middle and bottom panels are at t ≈ 31 ms and t ≈ 55 ms, respectively. A cyan contour represents the α-particle formation surface (Xα = 0.5) around which r-process seed nuclei begin to form, while the red contour represents the neutrinosphere surface (﹩{\tau }_{{\bar{\nu }}_{e}}=1﹩). The lower velocities of matter in the equatorial closed zone region, particularly in the first two snapshots, are apparent.
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Same as Figure 7, but for specific entropy s. The effect of the enhanced heating of matter in the equatorial closed zone is apparent.
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Same as Figure 6, but for magnetic-to-fluid pressure ratio β −1.
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Same as Figure 7, but for Y  e .
Paper: Three-dimensional General-relativistic Simulations of Neutrino-driven Winds from Magnetized Proto–Neutron Stars
Authors: Dhruv K. Desai, Daniel M. Siegel, Brian D. Metzger
Figure caption: Same as Figure 7, but for temperature T.
Paper: The Gamma-Ray Pulsar Phenomenology in View of 3D Kinetic Global Magnetosphere Models
Authors: Constantinos Kalapotharakos, Zorawar Wadiasingh, Alice K. Harding, Demosthenes Kazanas
Figure caption: The separatrix zone model is schematically presented. Top panel: The polar-cap region around a magnetic pole is denoted by the point P. The polar-cap rim is the origin of the last open magnetic-field lines, i.e., those that do not cross the LC. The separatrix zone is the region along all the magnetic-field lines that originate at the red zone. The width, w, of the red zone is measured as a fraction of the polar-cap radius, r pc. In simulations, the polar-cap rim, i.e., r pc(θ pc), is identified (at every time step) as the origin of the field lines that reach the LC. Bottom panel: The FF magnetosphere structure on the poloidal magnetic dipole moment—angular velocity, ( μ –Ω), plane. The red region denotes the separatrix zone, while the blue and white regions denote the zones of the open and closed magnetic-field lines, respectively. The orange region that emanates from the tip of the separatrix zone denotes the ECS region.