adsabs/AstroCLIMB huggingface dataset:
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: A histogram of the cumulative fraction of parameter space points as one accumulates points with increasingly lower relative differences (see, Equation (D3)) between the + polarizations obtained from InspiralESIGMA and the “reduced” version of InspiralESIGMA from which all the eccentric 3PN contributions from the radiative dynamics have been removed. The histogram bins are colored according to the median value of total mass (M) for the parameter space points corresponding to that bin. Furthermore, the opacity of each bin signifies the median eccentricity corresponding to that bin, with a higher opacity signifying a higher median eccentricity.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Realized strength of small-scale dynamo measured by ﹩\left\langle | {B}_{z}| \right\rangle ﹩ and ﹩\left\langle | B| \right\rangle ﹩ as a function of the magnetic flux imbalance ﹩\left\langle Bz\right\rangle ﹩. All quantities are evaluated at the Rosseland mean optical depth unity (τR = 1). Each point corresponds to a different simulation case with different values of ﹩{B}_{h}^{{\rm{in}}}﹩ and ﹩{B}_{{\rm{ave}}}^{z}﹩. Orange-shaded regions indicate typical ranges in the quiet Sun.
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: SGWB spectrum, ΩGW(f), for a population of binaries with (a) circular orbit (e0 = 0) (b) initial eccentricity, e0 = 0.6 at forb = 10−9 Hz. The solid lines represent the median ΩGW(f) obtained from 300 Monte Carlo realizations, while the shaded regions denote the 68% credible intervals.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Dependence of synthesized AIA 193 Å intensity on the vertical magnetic flux imbalance (left) and the rms of the vertical magnetic field (right). The average is taken over the whole horizontal domain and the last 2 hr of each simulation. Two thin gray horizontal lines indicate the typical intensity of the quiet Sun (top) and the coronal hole (bottom).
Paper: An Accurate Modeling of Nano-hertz Gravitational Wave Signal from Eccentric Supermassive Binary Black Holes: An Essential Step Toward a Robust Discovery
Authors: Mohit Raj Sah, Akash Maurya, Suvodip Mukherjee, Prayush Kumar, Vida Saeedzadeh, Arif Babul, Chandra Kant Mishra, Kaushik Paul, Thomas R. Quinn, Michael Tremmel
Figure caption: Normalized spectral covariance matrix CN(f1, f2) (defined in Equation (18)) for a population of binaries with (a) circular orbit (e0 = 0) (b) initial eccentricity, e0 = 0.6 at forb = 10−9 Hz.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Spatial distribution of the true open-field region (determined by tracing magnetic field lines) and coronal holes defined by the synthesized AIA 193 Å intensity with a threshold value of 20 DN s−1 pix−1.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Effects of spatial resolution on coronal hole detection. All quantities are evaluated within 24 × 24 Mm2 horizontal patches. Top left: histogram of coronal hole area. The blue solid line indicates a pixel size of 0.2 × 0.2 Mm2 (original resolution), and the orange dashed line indicates a pixel size of 12 × 12 Mm2 (rebinned). The coronal holes are detected using rebinned maps of the synthesized AIA 193 Å intensity, with a threshold value of 20 DN s−1 pix−1. Gray bars show the histogram of the true open area at the original resolution. Top right: histogram of the total vertical magnetic flux in coronal holes. Gray bars show the histogram of the true open magnetic flux at the original resolution. Bottom left: histogram of the ratio of coronal hole area to the true open area. The open pixels are defined by tracing magnetic field lines in the original resolution. Patches with no open pixels are excluded. Bottom right: histogram of the ratio of coronal hole magnetic flux to the true open magnetic flux.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Time variation of open magnetic flux (top), total area of open-field regions (middle), and total area of coronal holes (bottom). The open magnetic flux in the top panel is estimated from in situ observations of the IMF in the OMNI data (gray solid line) and the PFSS model with source surface heights RSS of 1.3 (blue solid line), 1.8 (orange dashed line), and 2.5R⊙ (green dotted line). The total area of open-field regions (middle) is also estimated from the PFSS model. The total area of coronal holes (bottom) is estimated from the AIA 193 Å intensity with threshold values of 60 (blue solid line), 50 (orange dashed line), and 30 (green dotted line) DN s−1 pix−1.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Similar to the top panel of Figure 13, but showing the open magnetic flux estimated by the PFSS model linearly scaled to match the open magnetic flux estimated from the OMNI IMF data. The scaling factors are 1.0 for RSS = 1.3R⊙, 1.9 for RSS = 1.8R⊙, and 2.7 for RSS = 2.5R⊙, respectively.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: HMI (top left) and AIA (top right) synoptic maps for CR2098 after preprocessing. The middle and bottom panels show quantities derived from spatially rebinned data: the mean radial magnetic field ﹩\left\langle {B}_{r}\right\rangle ﹩ (middle left), the radial magnetic field strength ﹩{\left\langle {B}_{r}^{2}\right\rangle }^{1/2}﹩ (bottom left), and the mean AIA 193 Å intensity I193 (middle right). The bottom-right panel shows the maximum height of the magnetic field lines extrapolated from the rebinned HMI synoptic map (i.e., middle-left panel) using the PFSS model with a source surface height RSS of 2.5R⊙.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Performance of the magnetic field strength on the photosphere (left) and the maximum height of the magnetic field lines (right) as a binary classifier of the AIA 193 Å intensity. The top panels show the ROC curves with the AUC values. Three binary classifications of the AIA 193 Å intensity with 20, 100, 500 DN s−1 pix−1 are shown. These threshold values correspond to the coronal hole, quiet region, and active region, respectively. The bottom panels show the two-dimensional probability distribution function of the AIA 193 Å intensity and each classifier.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Binary classification of open-field regions by the synthesized AIA 193 Å intensity. Histograms of the open and closed regions (left) and the ROC curves (right) are shown. The estimated AUC is 0.89. The optimal intensity threshold by the Youden’s J statistic is 19.9 DN s−1 pix−1 (shown as a red dashed line in the left panel and a red circle in the right panel).
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: The spatial distribution of open-field region (left) and coronal holes (right). Left panels show the open-field regions defined by the PFSS model with source surface heights of 1.3R⊙ (top), 1.8R⊙ (middle), and 2.5R⊙ (bottom). Right panels show the coronal holes defined by the AIA 193 Å intensity with threshold values of 60 (top), 50 (middle), and 30 DN s−1 pix−1 (bottom).
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Dependence of the magnetic flux ΦCH (left) and area ACH (right) in coronal holes on the spatial resolution. The top panels show the total signed magnetic flux and area of coronal holes above 10°, 30°, and 50°. The bottom panels show the increase of magnetic flux and area relative to the pixel size of 72 Mm near the equator. The threshold value of the AIA 193 Å intensity is set to 20 DN s−1 pix−1.
Paper: What Determines the Brightness of the Magnetically Open Solar Corona?: Insights from Three-dimensional Radiative Magnetohydrodynamic Simulations and Observations
Authors: Haruhisa Iijima
Figure caption: Similar to Figure 11, but showing the dependence on the brightness threshold of AIA 193 Å intensity. The pixel size is set to 7.2 Mm near the equator.
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: Two-dimensional distributions for the Einstein radius θE,defl of G1, the power law density slope of G1 γ, the magnitude of external shear γext, the Einstein radius of S1 θE,s1 and the cosmological distance ratio β12 from the final converged MCMC chains of our best-fit model for AGEL0353. The dark and light-shaded regions represent the 68% and 95% credible regions for each 2D distribution. In each panel along the diagonal from top left to bottom right, the red curve represents the posterior distribution of the corresponding parameter. The shaded region below each parameter’s posterior distribution represents the 1σ credible region. Table (top right) lists the median and 1σ uncertainties for the posterior distributions of each parameter. The posterior distribution for each parameter appears approximately Gaussian except for β12, which ramps toward its upper limit. There appear to be minor correlations between the β12 and θE,defl and the γext and γ distributions. The entire set of model parameters and their 1σ uncertainties can be found in Table A1.
Paper: The Effects of Turbulent Electrical Resistivity on the Response of the Solar Atmosphere to Flare Energy Input. II. Hard X-Ray Spectra, Light Curves, and Spatial Distributions
Authors: A. Gordon Emslie, Joel C. Allred, Meriem Alaoui
Figure caption: As for Figure 6, but for an injected flux ﹩{{ \mathcal F }}_{o}=3\times 1{0}^{11}﹩ erg cm−2 s−1.
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: The best-fit model for AGEL0353. The observed image of AGEL0353 in HST’s WFC3 F200LP filter is displayed in the top left panel, the reconstructed image produced by the lens model is in the top middle, and the normalized residual map between the observed and reconstructed images is displayed in the top right. The projected source reconstructions of S1, S2a, and S2b are shown in the bottom left panel with caustics (with respect to S2a’s source plane) overlaid in green. The convergence map representing the projected lensing surface mass density of the system with respect to S2a is displayed in the bottom middle panel. The arc-like structures represent the projected convergence of S1, lensed by G1. The projected magnification with respect to S2a is shown in the bottom right panel. Similarly to the convergence, the arc-like structures represented the projected magnification of S1, lensed by G1. The model accurately reproduces the locations and overall shapes of the lensed images, which agree with their corresponding source-plane reconstructions.
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: Color composite of AGEL0353 in the F200LP (blue) and F140W (red) filter bands from HST’s Wide Field Camera 3 (WFC3) with sides of 6″. The cyan triangle marks the center of G1. The yellow lines encircle the pair of images corresponding to S1. The pink lines encircle the arc created by S2a. The dashed white lines outlined the pair of images corresponding to S2b. The measured redshifts for G1, S1, and S2a are annotated in corresponding colored texts. We assume the redshift of S2b to be equal to zS2.
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: Schematic diagram of a double-source-plane lens (DSPL) based on Figure 12 of P. Schneider et al. (2006). Yellow rays show the path of light from source 1, deflected by the deflector toward the observer. Pink rays show the path of light from source 2, deflected by source 1, and the deflector toward the observer. The dashed line represents the line of sight through the center of the deflector. Angular diameter distances D are displayed at the bottom by double-headed arrows, where the subscripts d, s1, and s2 denote the deflector, source 1, and source 2. θ1, θ2, and θ3 denote the angular positions of source 2 in the deflector plane, in the first source plane, and true position in the second source plane. The angles ﹩{\hat{{\boldsymbol{\alpha }}}}_{{\bf{1}}}﹩ and ﹩{\hat{{\boldsymbol{\alpha }}}}_{{\bf{2}}}﹩ represent deflection by the deflector and source 1.
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: Median image of AGEL0353 from KCWI’s medium slicer and blue low-resolution grating. The cutout is 12 × 23 spatial pixels corresponding to a field of view of 8﹩\mathop{.}\limits^{\unicode{x02033}}﹩4 × 6﹩\mathop{.}\limits^{\unicode{x02033}}﹩9 with a spatial pixel size of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩7 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩3. The solid blue and yellow outlined regions indicate which pixels were integrated over to obtain the 1D spectra for G1 and S1 shown in Figure 3. The dashed pink and yellow outlined regions are overlaid to highlight the relative image positions of S2a and S1 from the HST imaging in Figure 2.
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: PDF of Ωm under the assumption of a flat ΛCDM cosmology given β12 sampled from our lens model. The red, blue, and orange lines represent the individual PDFs for AGEL0353, AGEL1507, and J0946. The green line shows the combined PDF from all three DSPLs. The colored shaded regions represent the 68% credible interval for each PDF. The green dotted line indicates the median of the combined PDF.
Paper: Constraining Cosmology with Double-source-plane Strong Gravitational Lenses from the AGEL Survey
Authors: Duncan J. Bowden, Nandini Sahu, Anowar J. Shajib, Kim-Vy Tran, Tania M. Barone, Keerthi Vasan G. C., Daniel J. Ballard, Thomas E. Collett, Faith Dalessandro, Giovanni Ferrami, Karl Glazebrook, William J. Gottemoller, Leena Iwamoto, Tucker Jones, Glenn G. Kacprzak, Geraint F. Lewis, Haven McIntosh-Lombardo, Hannah Skobe, Sherry H. Suyu, Sarah M. Sweet
Figure caption: Rest-frame spectra for (from left to right) G1, S1 and S2a of AGEL0353. The integrated spectra of G1 and S1 used to measure redshifts of zdefl = 0.617 and zS1 = 1.460 were obtained using KCWI integral field spectroscopy. The spectrum of S2a used to measure a redshift of zS2 = 1.675 was obtained using NIRES. The green vertical lines display the emission (dashed) and absorption (solid) lines used in determining each redshift.
Paper: A Grid-constrained Fourier Neural Operator for Magnetic Field Extrapolation of the Solar Corona
Authors: Hao Yang, Zhenhua Liu, Pingbing Zuo, Peng Zou, Ruize Zhang, Yanshi Huang
Figure caption: Comparison of SDO/AIA observations and model extrapolations for AR 11158. Top panels show the EUV 171 and 94 Å observations, middle panels display GC-FNO results, and bottom panels show PINO results.
Paper: A Grid-constrained Fourier Neural Operator for Magnetic Field Extrapolation of the Solar Corona
Authors: Hao Yang, Zhenhua Liu, Pingbing Zuo, Peng Zou, Ruize Zhang, Yanshi Huang
Figure caption: Overview of the GC-FNO architecture and training process. The yellow box indicates the FNO, and the red box represents the loss functions. NLFFF data are displayed using color maps, while the FNO output is shown in grayscale. Training proceeds in two steps, separated by a dashed black line.
Paper: A Grid-constrained Fourier Neural Operator for Magnetic Field Extrapolation of the Solar Corona
Authors: Hao Yang, Zhenhua Liu, Pingbing Zuo, Peng Zou, Ruize Zhang, Yanshi Huang
Figure caption: Computed MAE and cosine similarity between neighboring height slices in the NLFFF data set. The red line denotes cosine similarity, with values closer to 1 indicating stronger agreement, and the blue line represents MAE between the two slices.
Paper: A Grid-constrained Fourier Neural Operator for Magnetic Field Extrapolation of the Solar Corona
Authors: Hao Yang, Zhenhua Liu, Pingbing Zuo, Peng Zou, Ruize Zhang, Yanshi Huang
Figure caption: Generalization test results of the GC-FNO on AR 11158. The model is trained using NLFFF data from 2011 February 14 20:36:00 UT and generates 3D magnetic fields within a ±3 hr window centered on this time. The three metrics from top to bottom are CWsin, 〈∣fi∣〉, and the magnetic energy ratio to potential field. The black line corresponds to NLFFF results, the blue line to the FNO, and the red line to the GC-FNO.
Paper: A Grid-constrained Fourier Neural Operator for Magnetic Field Extrapolation of the Solar Corona
Authors: Hao Yang, Zhenhua Liu, Pingbing Zuo, Peng Zou, Ruize Zhang, Yanshi Huang
Figure caption: Comparison between the GC-FNO generalization results and SDO/AIA observations for AR 11158. Panel (a) and (c) show the observations in the EUV 171 and 304 Å channels at 2011 February 14 17:36:00 UT, and panel (e) presents the extrapolation results from the GC-FNO at that time. Panels (b), (d), and (f) show the observations in the EUV 171 and 304 Å channels and the GC-FNO extrapolation results at 2011 February 14 23:36:00 UT.
Paper: A Grid-constrained Fourier Neural Operator for Magnetic Field Extrapolation of the Solar Corona
Authors: Hao Yang, Zhenhua Liu, Pingbing Zuo, Peng Zou, Ruize Zhang, Yanshi Huang
Figure caption: Comparisons of the extrapolation results of the GC-FNO and NLFFF from 2011 February 14 22:00:00 UT to 2011 February 15 03:24:00 UT. From top to bottom, the four panels show the magnetic field force freeness, magnetic field divergence, magnetic energy, and magnetic free energy. The black and red solid lines represent the NLFFF and GC-FNO results, respectively. The start and end times (2011 February 15 01:44:00 UT and 2011 February 15 02:06:00 UT) of flare are indicated by black dashed lines, and the peak time (2011 February 15 01:56:00 UT) is indicated by a blue dashed line.
Paper: A Grid-constrained Fourier Neural Operator for Magnetic Field Extrapolation of the Solar Corona
Authors: Hao Yang, Zhenhua Liu, Pingbing Zuo, Peng Zou, Ruize Zhang, Yanshi Huang
Figure caption: Comparison of preflare coronal magnetic configurations reconstructed by the GC-FNO and NLFFF at 2011 February 15 01:36:00 UT in AR 11158. The green and blue lines are the configuration for tether-cutting reconnection. The pink lines are the part of the sigmoid structure.