adsabs/AstroCLIMB huggingface dataset:
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: Radial profiles of (a) density and (b) temperature of the AGN disk during relaxation, with colors indicating different times. Panel (c) shows the time evolution of the disk’s total energy. Gray circles represent simulation data, while the black solid line indicates the expected quasi-steady energy loss rate, estimated from the viscous heating rate Qvisc (Equation (12)). The red vertical line marks t ≈ 80 days, when viscous heating becomes nearly balanced by radiative cooling. The red arrow in panel (c) indicates t ≈ 90 days, at which the disk is considered to be relaxed and the corresponding profiles are adopted as the initial condition.
Paper: Tidal Disruption Events in Active Galactic Nuclei: on Orbital Inclination and Schwarzschild Apsidal Precession
Authors: Minghao Zhang, 铭浩 张, Wenda Zhang, 文达 张, Hongping Deng, 洪平 邓, Hengxiao Guo, 恒潇 郭, Jingbo Sun, 静泊 孙
Figure caption: A sketch map illustrating the inclined stellar orbits adopted in this work. Each orbit is color-coded according to its inclination angle, with an arrow indicating the orientation of motion. The direction of rotation of the accretion disk is marked with a black arrow for reference.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: The dark matter densities at 150 pc for the three dSphs. The black stars and green diamonds represent results in J. I. Read et al. (2019) and K. Hayashi et al. (2020). The magenta filled circles represent our results using the combined member star sample from DESI observations and M. G. Walker et al. (2023), based on the best constrained chemodynamical model. The results of the single-population model are very similar (see Figure 7) and thus are not shown. The blue filled circles are measurements based on DESI-observed member stars only. For UMi, the magenta filled circle overlaps the blue filled circle. We also repeat our analysis for Sextans and UMi using the same member star samples as K. Hayashi et al. (2020), and the results are shown by the hollow magenta triangles.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: The mean LOSV (﹩{v}_{{z}^{{\prime} }}﹩) and the LOSV dispersion (﹩{\sigma }_{{z}^{{\prime} }}﹩) profiles along major (two left columns) and minor (two right columns) axes of three dSphs: (a) Draco, (b) Sextans, and (c) UMi. The green dots and black stars represent the binned data within sectors of ±45° relative to the corresponding axes. The number of stars in each bin is the same for a given galaxy but varies between different systems. The x-errors represent the bin width while the y-errors represent the 1σ scatters. The yellow and black curves represent best-fit model profiles along the projected major and minor axes, respectively. Solid and dashed curves represent best-fit model profiles and corresponding 1σ uncertainties. The velocity dispersions of both the data and the best-fit model include observational uncertainties. They are not intrinsic velocity dispersions deconvolved with errors.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: The spatial, metallicity, and velocity distributions for the metal-rich (red) and metal-poor (blue) populations recovered by the chemodynamical model. Each subplot has five panels. Top histogram: the spatial distributions of the two populations. Middle-left scatter panel: [Fe/H] vs. the projected radius ﹩{R}^{{\prime} }﹩. Middle-right histogram: metallicity distributions of the two populations. Bottom-left scatter panel: the LOSV (﹩{v}_{z}^{{\prime} }﹩) of each star vs. the projected radius ﹩{R}^{{\prime} }﹩. Bottom-right histogram: the global velocity distributions of the two populations. The division of the two populations is based on Equation (17), with metal-rich and metal-poor populations having this probability greater than 0.5. The histogram distributions in the two right panels are for the data, while the solid smooth curves with the same colors are the model predictions. Gray dashed horizontal lines denote the hard cuts in metallicity to create the red and blue spatial templates.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: The dark matter densities at 150 pc (y-axis) vs. the stellar-to-halo mass ratios (x-axis) for dwarf galaxies in a few previous studies. The black filled squares and stars denote the results in J. I. Read et al. (2019) for dwarf irregular galaxies and dSphs, respectively. The green symbols represent the results in K. Hayashi et al. (2020). The magenta filled circles represent the results in our main analysis using the combined member star sample from DESI observations and M. G. Walker et al. (2023), based on the best constrained chemodynamical model in this work. No obvious correlation is observed.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: As in Figure 8, but only for the velocity moment profiles along major axes of different stellar populations in the three dSphs. The two left and two right columns are the mean LOSV and LOSV dispersion profiles binned along the major axis for the metal-poor (blue dots) and metal-rich (red dots) populations, respectively. We do not show results along the minor axis, as the main trends and comparisons are very similar. In each panel, the green and magenta solid curves are the best model predictions (see the legend), with the two dashed curves on both sides showing the 1σ confidence regions. The number of stars in each bin is the same for a given population in one galaxy, but varies between populations and among dSphs.
Paper: The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor
Authors: Hao Yang, Wenting Wang, Ling Zhu, Ting S. Li, Sergey E. Koposov, Jiaxin Han, Songting Li, Rui Shi, Monica Valluri, Alexander H. Riley, Arjun Dey, Constance Rockosi, Carles G. Palau, Jessica Nicole Aguilar, Steven Ahlen, David Brooks, Todd Claybaugh, Andrew Cooper, Axel de la Macorra, Peter Doel, Simone Ferraro, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma Xochitl Gonzalez Morales, Gaston Gutierrez, Julien Guy, Klaus Honscheid, Mustapha Ishak, Dick Joyce, Robert Kehoe, Theodore Kisner, Namitha Kizhuprakkat, Anthony Kremin, Ofer Lahav, Martin Landriau, Laurent Le Guillou, Gustavo E. Medina, Aaron Meisner, Ramon Miquel, Nathalie Palanque-Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Measured J (top) and D (bottom) factors for the three dSphs. Green and magenta symbols denote those from K. Hayashi et al. (2020) and this work.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: Top: Bias-weighted luminosity density as a function of redshift for the four spectral features considered in the SPHEREx case from our model (Section 4). Bottom: Bias-weighted intensity as a function of observed wavelength, derived from the bias-weighted luminosity density shown in the top panel using Equation (16).
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: The autopower spectrum ﹩{C}_{\ell ,\lambda \lambda }^{{\rm{clus}}}﹩—i.e., the diagonal elements of the power spectrum matrix shown in Figure 7—for the lowest and highest ℓ bins centered at ℓ = 601 and ℓ = 16,631 in the PHI/FIRESS case (blue and orange). The dark and light-colored lines show the autopower spectra for PHI and FIRESS, respectively. The brown and gray dots show the noise power spectrum ﹩{C}_{\ell }^{n}﹩ (Equation (8)) for each channel (R = 20 and R = 100) for PHI and FIRESS, respectively.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: Top: Bias-weighted luminosity density as a function of redshift for the four spectral features considered in the PRIMA case from our model (Section 4). Bottom: Bias-weighted intensity as a function of observed wavelength, derived from the bias-weighted luminosity density shown in the top panel using Equation (16).
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: The autopower spectrum ﹩{C}_{\ell ,\lambda \lambda }^{{\rm{clus}}}﹩—i.e., the diagonal elements of the power spectrum matrix shown in Figure 6—for the lowest and highest ℓ bins centered at ℓ = 55 and ℓ = 317 in the SPHEREx case (blue and orange). The brown and gray dots show the noise power spectrum ﹩{C}_{\ell }^{n}﹩ (Equation (8)) for each channel in the deep-fields and the all-sky survey, respectively.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: The bias-weighted luminosity density of the four features in the SPHEREx case. Solid lines show the signal from all sources in the fiducial case, as presented in Figure 4. Dashed and dotted lines represent the cases where sources individually detectable in the SPHEREx deep-fields and all-sky survey, respectively, have been removed.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: The clustering power spectrum matrix ﹩{C}_{\ell }^{{\rm{clus}}}﹩ (Equation (7)) at the lowest ℓ mode, centered at ℓ = 601, for the PHI (top)/FIRESS (bottom) case.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: The clustering power spectrum matrix ﹩{C}_{\ell }^{{\rm{clus}}}﹩ (Equation (7)) at the lowest ℓ mode, centered at ℓ = 55, for the SPHEREx case.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: The S/N for constraining the bias-weighted luminosity density in Δz = 0.1 bins of redshifts for each feature in the SPHEREx case. Solid/dashed lines with filled/open circles represent the deep-fields/all-sky cases, respectively. The total S/N of each feature summed over all redshift bins (Equation (12)) for the deep-fields/all-sky cases is provided in the legend.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: The S/N for constraining the bias-weighted luminosity density in Δz = 0.5 bins of redshifts for each feature in the fiducial PHI (top) and FIRESS (bottom) case. The total S/N of each feature summed over all redshift bins (Equation (12)) is provided in the legend.
Paper: Asymptotic Giant Branch Mass-loss Rates and Metal Yields from Scaled Mixing-length and Mass-loss Parameters
Authors: Ezra Huscher, Kristian Finlator, Jason Jackiewicz
Figure caption: Top: the initial mass of our models as a function of the final mass they reach. For comparison, observations are included from J. S. Kalirai et al. (2009) of this relation in white dwarfs residing in nearby Milky Way globular clusters. Bottom: time-averaged luminosities of our 2M, 2.5M, and 3M models throughout the TPAGB as a function of their initial metal mass fraction. These masses encompass most of the carbon stars that would exist in a population such as the one studied by C. Abia et al. (2022) and show good agreement with the average luminosity for their carbon star population, which is the horizontal blue line with the associated error.
Paper: Asymptotic Giant Branch Mass-loss Rates and Metal Yields from Scaled Mixing-length and Mass-loss Parameters
Authors: Ezra Huscher, Kristian Finlator, Jason Jackiewicz
Figure caption: Mass-loss rates of the MESA models as a function of the AGB star’s age, calculated by integrating the mass-loss rate during pulsing and dividing by the duration. For each initial metal mass fraction (i.e., Z = 0.015), the mass-loss rates are interpolated in initial stellar mass to provide rates at a fine series of stellar ages. The top axis indicates the initial stellar mass which would pass through the AGB phase at the corresponding stellar age. The mass-loss rates found by M. A. T. Groenewegen & G. C. Sloan (2018) for carbon stars in the Local Group are represented by the gray dotted line (average) and dark gray area (range).
Paper: Asymptotic Giant Branch Mass-loss Rates and Metal Yields from Scaled Mixing-length and Mass-loss Parameters
Authors: Ezra Huscher, Kristian Finlator, Jason Jackiewicz
Figure caption: Lines are the mass ratios of the total yields as a function of initial stellar mass after the last thermal pulse at Z = 0.0001 (dotted–dashed purple), Z = 0.015 (dashed teal), and Z = 0.03 (solid gold). Open circles are the ratio of the final surface mass fractions after the last thermal pulse.
Paper: Asymptotic Giant Branch Mass-loss Rates and Metal Yields from Scaled Mixing-length and Mass-loss Parameters
Authors: Ezra Huscher, Kristian Finlator, Jason Jackiewicz
Figure caption: A comparison between different studies of the surface C/O ratio at the end of the AGB phase at (top) Z = 0.0001, (second) Z = 0.005, (third) Z = 0.015, and (bottom) Z = 0.03. Dashed lines are the result of MESA models from MIST (J. Choi et al. 2016), dotted lines are the results of Monash models from A. I. Karakas & M. Lugaro (2016), and solid lines are our models. The points where they rise above the thick gray horizontal lines (C/O = 1) are the stellar masses that become carbon stars.
Paper: Asymptotic Giant Branch Mass-loss Rates and Metal Yields from Scaled Mixing-length and Mass-loss Parameters
Authors: Ezra Huscher, Kristian Finlator, Jason Jackiewicz
Figure caption: The AGB phase in a Hertzsprung–Russell diagram for the model with an initial mass of 2 M⊙ and an initial metal mass fraction of 0.002. The progression of thermal pulsing leads to increased carbon at the star’s surface.
Paper: Asymptotic Giant Branch Mass-loss Rates and Metal Yields from Scaled Mixing-length and Mass-loss Parameters
Authors: Ezra Huscher, Kristian Finlator, Jason Jackiewicz
Figure caption: A comparison between the existing input tables for simulations such as EAGLE and TECHNICOLOR DAWN on the left and our results on the right, all weighted by a Chabrier IMF (G. Chabrier 2003). Top: instantaneous mass-loss rates of AGB stars as a function of their age and initial metallicity, normalized by the stellar mass formed. Bottom: same, but instantaneous carbon mass fraction of the outflowing gas from the AGB stars.
Paper: Asymptotic Giant Branch Mass-loss Rates and Metal Yields from Scaled Mixing-length and Mass-loss Parameters
Authors: Ezra Huscher, Kristian Finlator, Jason Jackiewicz
Figure caption: The ejected 12C, 14N, 16O, 19F, 20Ne, and 24Mg yields as a function of initial stellar mass for three initial metallicities: nearly metal free (0.0001), solar (0.014 or 0.015), and supersolar (0.03), with A. I. Karakas & M. Lugaro (2016)’s results shown for comparison. Yields between the two models match reasonably well with the exception of 24Mg.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: The S/N for constraining the bias-weighted luminosity density in Δz = 0.1 bins for each feature in the fiducial case without masking detected sources (solid lines with filled circles), and in the case where all detected sources in the deep fields (top)/all sky (bottom) are masked.
Paper: Synthetic Ca II 8542 Å Stokes Profile Associated with Chromospheric Magnetic Reconnection in a Simulated Active Region
Authors: Xinyu Zhou, Takaaki Yokoyama, Haruhisa Iijima, Takuma Matsumoto, Shin Toriumi, Yukio Katsukawa, Masahito Kubo
Figure caption: x–λ maps for (a) Stokes I, (b) Q, (c) V, with 2D maps for simulation data on (d) density, (e) Bx, (f) Bz, (g) Vz, (h) temperature, and (i) normalized current density around the reconnection event 1 at t = 1966 s. The colored contour lines of Stokes I at I = 0.2Ic (orange) for absorption features and I = 0.4Ic (red) for emission features are shown on every map for Stokes signals. The blue arrows in panels (a), (b), and (c) indicate the Stokes features from the reconnection current sheet. The vertical yellow dotted line on each panel indicates the location of Figure 5. Besides the lime contour line of the surface of mean optical depth τ = 1 in the spectrum core on the panels showing simulation data, orange and gold contour lines are added for the wavelength range λ0 − 0.5 Å to −1.0 Å, and λ0 + 0.5 Å to +1.0 Å, respectively.
Paper: Synthetic Ca II 8542 Å Stokes Profile Associated with Chromospheric Magnetic Reconnection in a Simulated Active Region
Authors: Xinyu Zhou, Takaaki Yokoyama, Haruhisa Iijima, Takuma Matsumoto, Shin Toriumi, Yukio Katsukawa, Masahito Kubo
Figure caption: Temperature distribution at different stages: (a) initial setup; (b) magnetic flux imposed in the convection zone; (c) magnetic flux emerging into the chromosphere. The black contour lines indicate the magnetic field lines. The lime contour lines indicate the surface of mean optical depth τ = 1 in the wavelength range λ ∼ λ0 ± 0.25 Å.
Paper: Synthetic Ca II 8542 Å Stokes Profile Associated with Chromospheric Magnetic Reconnection in a Simulated Active Region
Authors: Xinyu Zhou, Takaaki Yokoyama, Haruhisa Iijima, Takuma Matsumoto, Shin Toriumi, Yukio Katsukawa, Masahito Kubo
Figure caption: An example of a synthetic Stokes profile at x = 3.95 Mm from the snapshot at t = 2 s (yellow dotted line in Figure 1(b)).
Paper: Synthetic Ca II 8542 Å Stokes Profile Associated with Chromospheric Magnetic Reconnection in a Simulated Active Region
Authors: Xinyu Zhou, Takaaki Yokoyama, Haruhisa Iijima, Takuma Matsumoto, Shin Toriumi, Yukio Katsukawa, Masahito Kubo
Figure caption: A λ−t map for Stokes I and Q at x = 0.72 Mm. The colored contour line is the same as in Figure 4. The ”white” horizontal line at t = 1922 s represents missing data due to a failure in Stokes profile synthesis. The horizontal yellow dotted line in each panel indicates the time of Figure 4.