adsabs/AstroCLIMB huggingface dataset:
Paper: A New Photoionization Model of the Narrow-line Region in Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Infrared diagnostic diagrams for AGN regions and H II regions. Dusty, isobaric AGN models with different N/O–O/H scaling relations (“NHlow” in solid lines and “NHhigh” in dashed lines), different radiation fields (from top to bottom panels: “Cagn,” ﹩\mathrm{log}{E}_{\mathrm{peak}}=-1.5,-1.25,-1.0﹩) are presented in black grids that consist of constant-metallicity lines (from left to right: ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})=8.00,8.28,8.43,8.70,8.89,9.02,9.26﹩) and constant-ionization-parameter lines (from bottom to top: ﹩\mathrm{log}(U)=-3.8,-3.4,-3.0,-2.6,-2.2﹩) at gas pressure ﹩\mathrm{log}(P/k)=7.4﹩. The black arrow in the upper right corner represents the average effect of gas pressure when it changes from ﹩\mathrm{log}(P/k)=7.4﹩ to ﹩\mathrm{log}(P/k)=8.2﹩. The H II model is shown with a red grid that consists of constant-metallicity lines (from left to right: ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})=7.75,8.15,8.43,8.63,8.76,8.85,8.94,9.00,9.10﹩) and constant-ionization-parameter lines (from bottom to top: ﹩\mathrm{log}(U)=-3.5,-3.25,-3.0,-2.75,-2.5﹩) at gas pressure ﹩\mathrm{log}(P/k)=5.4﹩. The red arrow in the upper right corner represents the average effect of gas pressure when it changes from ﹩\mathrm{log}(P/k)=5.4﹩ to ﹩\mathrm{log}(P/k)=7.4﹩. Infrared spectra for Seyfert 2 galaxies and H II regions are collected from Fernández-Ontiveros et al. (2016) and presented with gray circles and red circles for comparison.
Paper: A New Photoionization Model of the Narrow-line Region in Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Comparison of AGN models built with four different AGN radiation fields on the standard optical diagnostic diagrams. Each model is presented with constant-metallicity lines (from left to right: ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})=8.28,8.43,8.54,8.70,8.80,8.96,9.09,9.16,9.26﹩) and constant-ionization-parameter lines (from bottom to top: ﹩\mathrm{log}(U)=-3.4,-3.0,-2.6,-2.2﹩) at gas pressure ﹩\mathrm{log}(P/k)=7.0﹩. The solid red, green, and blue grids represent AGN models using OXAF ionizing spectra with fixed Γ = 2.0 and p NT = 0.15 and ﹩\mathrm{log}{E}_{\mathrm{peak}}/(\mathrm{keV})=-1.0,-1.25,-1.5﹩, respectively. The solid black grid shows the AGN model built with the CLOUDY default AGN radiation field. The red dashed grid represents the latest version of the H II model (S. L. Li et al. 2023, in preparation) for a complete comparison with the observations. Optical spectra for a large sample of galaxies from SDSS DR16 are presented with gray dots. The mean error bars are shown in the lower right corner. In all three panels, the black solid curves are the Kewley et al. (2001) theoretical maximum starburst lines. In the left panel, the black dashed curve is the Kauffmann et al. (2003) empirical maximum starburst line. The black dashed lines in the right two panels are the Seyfert-LINER separation lines (Kewley et al. 2006).
Paper: A New Photoionization Model of the Narrow-line Region in Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Comparison of dust-free (DF) AGN model (dashed lines) and dust-depleted (DN) AGN model (solid lines) on the standard optical diagnostic diagrams. To isolate the effect from the AGN radiation field, four sets of the dust-free and dusty AGN models are presented in the panels from top to bottom using the CLOUDY default radiation field (called “Cagn”) and the OXAF radiation field with ﹩\mathrm{log}{E}_{\mathrm{peak}}=-1.5,-1.25,-1.0﹩, respectively. Each model is presented with constant-metallicity lines (from left to right: ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})=8.00,8.28,8.43,8.54,8.70,8.80,8.96,9.09﹩) and constant-ionization parameter lines (from bottom to top: ﹩\mathrm{log}(U)=-3.4,-3.0,-2.0﹩) at gas pressure ﹩\mathrm{log}(P/k)=7.0﹩. The optical spectra for a large sample of galaxies from SDSS DR16 are presented with gray dots. The mean error bars are shown in the lower right corner. In all three panels, the black solid curves are the Kewley et al. (2001) theoretical maximum starburst lines. In the left panel, the black dashed curve is the Kauffmann et al. (2003) empirical maximum starburst line. The black dashed lines in the right two panels are the Seyfert-LINER separation lines (Kewley et al. 2006).
Paper: A New Photoionization Model of the Narrow-line Region in Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Comparison of AGN models built with different N/O–O/H scaling relations (solid blue for “NHlow” and red dashed for “NHhigh”) on the standard optical diagnostic diagrams. Each model is presented with constant-metallicity lines (from left to right: ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})=8.28,8.43,8.54,8.70,8.80,8.89,8.96,9.02﹩) and constant-ionization parameter lines (from bottom to top: ﹩\mathrm{log}(U)=-3.8,-3.4,-3.0,-2.6,-2.2,-1.0﹩) at gas pressure ﹩\mathrm{log}(P/k)=7.4﹩. Both AGN models are dusty models with isobaric structures, nonuniform abundance sets, and the ﹩\mathrm{log}{E}_{\mathrm{peak}}=-1.25﹩ OXAF radiation field calculated by MAPPINGS V. Optical spectra for a large sample of galaxies from SDSS DR16 are presented with gray dots. The mean error bars are shown in the lower right corner. In all three panels, the black solid curves are the Kewley et al. (2001) theoretical maximum starburst lines. In the left panel, the black dashed curve is the Kauffmann et al. (2003) empirical maximum starburst line. The black dashed lines in the right two panels are the Seyfert-LINER separation lines (Kewley et al. 2006).
Paper: A New Photoionization Model of the Narrow-line Region in Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Dusty ﹩\mathrm{log}{E}_{\mathrm{peak}}=-1.25﹩ isobaric AGN models with different gas pressure ﹩\mathrm{log}(P/k)\,=﹩ 5.0, 7.0, 7.8, 8.6 shown in yellow, red, green, and blue grids on the standard optical diagnostic diagrams. Each model is presented with constant-metallicity lines (from left to right: ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})\,=﹩ 8.28, 8.43, 8.70, 8.89, 9.02) and constant-ionization parameter lines (from bottom to top: ﹩\mathrm{log}(U)=-3.8,-3.4,-3.0,-2.2﹩). The “NHlow” nitrogen scaling relation is adopted in these models. The optical spectra for a large sample of galaxies from SDSS DR16 are presented with gray dots. The mean error bars are shown in the lower right corner.
Paper: A New Photoionization Model of the Narrow-line Region in Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Comparison of ﹩\mathrm{log}{E}_{\mathrm{peak}}=-1.5﹩ dusty AGN models using radiation-pressure-dominated isobaric and isochoric structures. Each model is presented with constant-metallicity lines (from left to right: ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})=8.28,8.43,8.54,8.70,8.80,8.89,8.96,9.02﹩) and constant-ionization parameter lines (from bottom to top: ﹩\mathrm{log}(U)=-3.8,-3.4,-3.0,-2.6,-2.2,-1.8﹩) at gas pressure ﹩\mathrm{log}(P/k)=7.0﹩ (isobaric model, in solid blue) or at hydrogen density n H = 1000 cm−3 (isochoric model, in red dashed). The “NHlow” nitrogen scaling relation is adopted in these models. The optical spectra for a large sample of galaxies from SDSS DR16 are presented with gray dots. The mean error bars are shown in the lower right corner.
Paper: A New Photoionization Model of the Narrow-line Region in Active Galactic Nuclei
Authors: Peixin Zhu, Lisa J. Kewley, Ralph S. Sutherland
Figure caption: Same as Figure 8 but adopting [Ne III]/[O II] as the ionization parameter diagnostic.
Paper: Interplay between Anisotropy- and Skewness-driven Whistler Instabilities in the Solar Wind under the Core–Strahlo Model
Authors: Bea Zenteno-Quinteros, Pablo S. Moya, Marian Lazar, Adolfo F. Viñas, Stefaan Poedts
Figure caption: Upper and lower panels: whistler-mode dispersion relation, parallel cuts of the CS distribution function, and contours of the eVDF considering η  s  = 0.1, β ∥s  = 0.1, A  s  = 1.0, and A  c  = 1.6 (top) or A  c  = 2.5 (bottom). The different colors represent different values of the skewness parameter, namely: δ = 0.00 (green), 0.10 (blue), 0.20 (red), and 0.25 (black).
Paper: Interplay between Anisotropy- and Skewness-driven Whistler Instabilities in the Solar Wind under the Core–Strahlo Model
Authors: Bea Zenteno-Quinteros, Pablo S. Moya, Marian Lazar, Adolfo F. Viñas, Stefaan Poedts
Figure caption: Growth rates of the whistler mode for A  c  = 1.0, A  s  = 1.5, and different values of the skewness parameter: δ = 0.0 (black lines), δ = 0.05 (green lines), δ = 0.15 (red lines), and δ = 0.25 (blue lines). Also, each panel shows a different combination of the strahlo density ratio and beta parameter, namely: (a) η  s  = 0.05 and β ∥s  = 0.05; (b) η  s  = 0.1 and β ∥s  = 0.05; (c) η  s  = 0.05 and β ∥s  = 0.1; and (d) η  s  = 0.1 and β ∥s  = 0.1.
Paper: Interplay between Anisotropy- and Skewness-driven Whistler Instabilities in the Solar Wind under the Core–Strahlo Model
Authors: Bea Zenteno-Quinteros, Pablo S. Moya, Marian Lazar, Adolfo F. Viñas, Stefaan Poedts
Figure caption: (a) Whistler-mode dispersion relation for η  s  = 0.1, β ∥s  = 0.1, δ = 0.0, A  c  = 1.0, and different values of the strahlo anisotropy A  s . (b) Parallel cuts of the CS distribution function. (c) Contours of the eVDF. In all panels, the colors represent different values of A  s : namely, A  s  = 0.8 (green), 1.0 (blue), 1.2 (red), and 1.3 (black).
Paper: Interplay between Anisotropy- and Skewness-driven Whistler Instabilities in the Solar Wind under the Core–Strahlo Model
Authors: Bea Zenteno-Quinteros, Pablo S. Moya, Marian Lazar, Adolfo F. Viñas, Stefaan Poedts
Figure caption: (a) Whistler-mode dispersion relation for η  s  = 0.1, β ∥s  = 0.1, δ = 0.0, A  s  = 1.0, and different values of the core anisotropy A  c . (b) Parallel cuts of the CS distribution function. (c) Contours of the eVDF. In all panels, the colors represent different values of A  c : namely, A  c  = 1.0 (green), 2.0 (blue), 2.5 (black), and 3.0 (red).
Paper: Interplay between Anisotropy- and Skewness-driven Whistler Instabilities in the Solar Wind under the Core–Strahlo Model
Authors: Bea Zenteno-Quinteros, Pablo S. Moya, Marian Lazar, Adolfo F. Viñas, Stefaan Poedts
Figure caption: (a) Whistler-mode dispersion relation for η  s  = 0.1, β ∥s  = 0.1, δ = 0.2, A  s  = 1.0, and different values of the core anisotropy A  c . (b) Parallel cuts of the CS distribution function. (c) Contours of the eVDF. In all panels, the colors represent different values of A  c : namely, A  c  = 0.5 (green), 1.0 (blue), 2.0 (red), and 3.0 (black).
Paper: Interplay between Anisotropy- and Skewness-driven Whistler Instabilities in the Solar Wind under the Core–Strahlo Model
Authors: Bea Zenteno-Quinteros, Pablo S. Moya, Marian Lazar, Adolfo F. Viñas, Stefaan Poedts
Figure caption: Left panels: whistler-mode dispersion relation for η  s  = 0.1, β ∥s  = 0.1, δ = 0.2, A  c  = 1.0, and different values of the strahlo anisotropy A  s . Middle panels: parallel cuts of the CS distribution function. Right panels: contours of the eVDF. In all panels, the colors represent different values of A  s : namely, A  s  = 0.8 (green), 1.0 (blue), 1.2 (red; upper panels) and A  s  = 1.0 (green), 2.0 (blue), 3.0 (red; lower panels).
Paper: Interplay between Anisotropy- and Skewness-driven Whistler Instabilities in the Solar Wind under the Core–Strahlo Model
Authors: Bea Zenteno-Quinteros, Pablo S. Moya, Marian Lazar, Adolfo F. Viñas, Stefaan Poedts
Figure caption: Growth rates of the whistler mode for A  c  = 1.0, δ = 0.25, and different values of the strahlo anisotropy: A  s  = 0.8 (black lines), A  s  = 0.9 (orange lines), A  s  = 1.0 (green lines), A  s  = 1.1 (red lines), and A  s  = 1.2 (blue lines). Also, each panel shows a different combination of the strahlo density ratio and beta parameter, namely: (a) η  s  = 0.05 and β ∥s  = 0.05; (b) η  s  = 0.1 and β ∥s  = 0.05; (c) η  s  = 0.05 and β ∥s  = 0.1; and (d) η  s  = 0.1 and β ∥s  = 0.1.
Paper: Interplay between Anisotropy- and Skewness-driven Whistler Instabilities in the Solar Wind under the Core–Strahlo Model
Authors: Bea Zenteno-Quinteros, Pablo S. Moya, Marian Lazar, Adolfo F. Viñas, Stefaan Poedts
Figure caption: (a) Whistler-mode dispersion relation for η  s  = 0.1, β ∥s  = 0.1, A  s  = 1.5, A  c  = 1.0, and different values of the skewness parameter δ. (b) Parallel cuts of the CS distribution function. (c) Contours of the eVDF. In all panels, the colors represent different values of δ: namely, δ = 0.0 (green), 0.1 (blue), and 0.2 (red).
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: Two-σ diagram: σ out/σ hot(M *) vs. σ in/σ hot(M *). For QCCs, it is σ out/σ hot(M q) vs. σ in/σ hot(M q). The small circles show the results for FQGs (top-left), QCCs (top-middle-left), PQGs (top-middle-right), FSGs (top-right), optical AGN host galaxies (bottom-left), radio galaxies (bottom-middle-left), and barred galaxies (bottom-middle-right). In the top-middle-right panel, PQGs are shown with color-coded circles according to their ﹩{\bar{f}}_{{\rm{q}}}﹩. In the bottom-right panel, contour lines for FQGs (red), PQGs (green), and FSGs (blue) are shown. The inclined dashed lines show 1:1 relation. The horizontal and vertical dashed lines are those used to define horizontal and vertical sequences as discussed in Section 4. Contour lines with different colors correspond to different galaxies/objects as labeled in the corresponding panels. We show two contour levels, which enclose 40% and 80% of the galaxies/objects, respectively.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: Schematic Two-σ diagram. The arrows illustrate possible evolutionary tracks (see the text for details). We also show the SDSS images of several representative galaxies located at different places along the horizontal and vertical sequences. Red, green, and blue square frames indicate the images for FQGs, PQGs, and FSGs, respectively. The orange and yellow frames indicate the sketches for optical and radio AGNs.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: Galaxy activity along the horizontal sequence (﹩\mathrm{log}({\sigma }_{\mathrm{out}}/{\sigma }_{\mathrm{hot}})\lt -0.5﹩). FSGs, PQGs, and FQGs are shown in blue, green, and red, respectively. Left panel: sSFR as a function of ﹩\mathrm{log}({\sigma }_{\mathrm{in}}/{\sigma }_{\mathrm{hot}})﹩. Right panel: similar to the right panel of Figure 13 but for optical AGN fraction (f AGN) as a function of ﹩\mathrm{log}({\sigma }_{\mathrm{in}}/{\sigma }_{\mathrm{hot}})﹩. The vertical dashed lines show ﹩\mathrm{log}({\sigma }_{\mathrm{in}}/{\sigma }_{\mathrm{hot}})=-0.3﹩.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: Galaxy structure along the horizontal sequence (﹩\mathrm{log}({\sigma }_{\mathrm{out}}/{\sigma }_{\mathrm{hot}})\lt -0.5﹩). FSGs, PQGs, and FQGs are shown in blue, green, and red, respectively. Left panel: Sérsic index n as a function of ﹩\mathrm{log}({\sigma }_{\mathrm{in}}/{\sigma }_{\mathrm{hot}})﹩. Middle panel: ﹩\mathrm{log}[{R}_{{\rm{e}}}/{R}_{\mathrm{FQG}}({M}_{* })]﹩ as a function of ﹩\mathrm{log}({\sigma }_{\mathrm{in}}/{\sigma }_{\mathrm{hot}})﹩, where R FQG(M *) is the best fit for the mass–size relation of FQGs shown in Figure 7. Right panel: barred galaxy fraction (f bar) as a function of ﹩\mathrm{log}({\sigma }_{\mathrm{in}}/{\sigma }_{\mathrm{hot}})﹩. The gray line shows the results for all galaxies, and error bars are obtained with bootstrap method. The vertical dashed lines show ﹩\mathrm{log}({\sigma }_{\mathrm{in}}/{\sigma }_{\mathrm{hot}})=-0.3﹩. We do not show the results in bins with galaxy number less than 20.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: Similar to Figure 14 but here we show sSFR and f AGN for galaxies along the vertical sequence (﹩\mathrm{log}({\sigma }_{\mathrm{in}}/{\sigma }_{\mathrm{hot}})\gt -0.3﹩) as functions of ﹩\mathrm{log}({\sigma }_{\mathrm{out}}/{\sigma }_{\mathrm{hot}})﹩. The vertical dashed lines show ﹩\mathrm{log}({\sigma }_{\mathrm{out}}/{\sigma }_{\mathrm{hot}})=-0.3﹩.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: Stellar velocity dispersion (σ(R)) profiles for FQGs (red), PQGs (green), FSGs (blue), and QCCs (purple). The solid and dashed lines show the median profiles of σ(R) while the shaded areas are the 16th and 84th percentiles. For galaxies, we show profiles up to the median of 1.5R e. For QCCs, we show the profiles to the median of R q. The results for galaxies and objects with different mass are presented in different panels. We ignore the results if the number of galaxies or objects is less than 10.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: Top-left panel: Σ1 vs. stellar mass; top-right panel: Sérsic index n (r band) vs. stellar mass; bottom-left panel: Σ1 vs. σ in; bottom-right panel: Sérsic index n vs. σ in/σ hot(M *). FSGs, PQGs, and FQGs are shown in blue squares, green triangles, and red circles, respectively.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: Similar to Figure 13 but here we show the structural parameters for galaxies along the vertical sequence (﹩\mathrm{log}({\sigma }_{\mathrm{in}}/{\sigma }_{\mathrm{hot}})\gt -0.3﹩) as functions of ﹩\mathrm{log}({\sigma }_{\mathrm{out}}/{\sigma }_{\mathrm{hot}})﹩. The vertical dashed lines show ﹩\mathrm{log}{\sigma }_{\mathrm{out}}/{\sigma }_{\mathrm{hot}}=-0.3﹩.
Paper: Dynamical Hotness, Star Formation Quenching, and Growth of Supermassive Black Holes
Authors: Hui Hong, Huiyuan Wang, H. J. Mo, Ziwen Zhang, Guangwen Chen, Wentao Luo, Tinggui Wang, Pengfei Li, Renjie Li, Yao Yao, Aoxiang Jiang
Figure caption: The left panel shows results for galaxies with b/a < 0.4. In the right panel, R e is required to be greater than 5″. Contour levels correspond to 40% and 80%. FQGs, PQGs, and FSGs are in red, green, and blue, respectively.
Paper: High-energy Neutrino Constraints on Cosmic-Ray Reacceleration in Radio Halos of Massive Galaxy Clusters
Authors: Kosuke Nishiwaki, Katsuaki Asano, Kohta Murase
Figure caption: Constraints on f ep and the central magnetic field B 0. The shaded region is excluded from the neutrino upper limit for the E −2.5 spectrum shown in Figure 4. We have assumed that the neutrino background is dominated by the massive clusters with M 500 ≈ 1015 M ⊙. The contour shows the fractional contribution to the all-sky neutrino intensity calculated with Equation (7) with q = 3.45 and z = 0.2. We fix η  B  = 0.5 for the magnetic field profile, and the ICM density profile of the Coma cluster is adopted. The dashed line with arrows shows the minimum value of B 0 for the Coma cluster constrained by the Fermi-LAT upper limit in the reacceleration model (Brunetti et al. 2017). Note that the parameters in Brunetti et al. (2017) are similar to our model: η  B  = 0.5, f ep = 0, t acc = 260 Myr, and ΔT/t acc ≈ 2.8. The limit is scaled with f ep as shown in Equation (6).
Paper: High-energy Neutrino Constraints on Cosmic-Ray Reacceleration in Radio Halos of Massive Galaxy Clusters
Authors: Kosuke Nishiwaki, Katsuaki Asano, Kohta Murase
Figure caption: Spectra of the diffuse high-energy muon neutrino flux. The data points and green band show the all-sky muon neutrino intensity estimated with IceCube track events (Abbasi et al. 2022b). The red line shows the 90% CL upper limit derived from the stacking analysis of Planck-SZ clusters using the distance-weighting scheme (﹩{L}_{{E}_{\nu }}\propto {M}^{0}﹩; Abbasi et al. 2022a). The blue arrows show the upper limits in quasi-differential energy bins for the distance-weighting scheme (Abbasi et al. 2022a). The solid and dashed lines show the results of the fiducial and optimistic models, respectively.
Paper: High-energy Neutrino Constraints on Cosmic-Ray Reacceleration in Radio Halos of Massive Galaxy Clusters
Authors: Kosuke Nishiwaki, Katsuaki Asano, Kohta Murase
Figure caption: Fraction of RHs detectable with the ASKAP sensitivity at 1.4 GHz. The black and red points show the fraction predicted in the fiducial and optimistic models, respectively. The dashed line shows the mass range studied in previous observations (Cuciti et al. 2021b).
Paper: High-energy Neutrino Constraints on Cosmic-Ray Reacceleration in Radio Halos of Massive Galaxy Clusters
Authors: Kosuke Nishiwaki, Katsuaki Asano, Kohta Murase
Figure caption: Brightness temperature of the isotropic radio background expected from GCs. The solid and dashed lines show the results of the fiducial and optimistic models, respectively. The data points show the measured radio background after subtracting off the CMB temperature (Fixsen et al. 2011).
Paper: Effects of Coronal Magnetic Field Configuration on Particle Acceleration and Release during the Ground Level Enhancement Events in Solar Cycle 24
Authors: Wenlong Liu, Xiangliang Kong, Fan Guo, Lulu Zhao, Shiwei Feng, Feiyu Yu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: (a) Schematics of the locations of Earth (green), STEREO-A (STA; red), and STEREO-B (STB; blue) in the ecliptic plane as seen from the north of the Sun for the GLE 71 event on 2012 May 17. The arrow indicates the radial direction at the solar flare. The black curve plots the nominal Parker spiral magnetic field line connecting to the Earth. (b)–(d) EUV and white-light images of the CME eruption observed by SDO/AIA, STA/EUVI, and SOHO/LASCO C2 at different times. The CME feature at an early time is shown by EUV running-difference images of SDO/AIA in 193 Å at 01:28 UT, and STA/EUVI in 195 Å at 01:30 UT. Magnetic field lines obtained from the PFSS model are overplotted in panels (b) and (c). Closed field lines in magenta correspond to the face-on streamer in the FOV of LASCO C2 as indicated by the white arrow in panel (b), and open field lines are plotted in red (positive) and green (negative). The CME first appeared in the FOV of LASCO C2 at 01:48 UT.
Paper: Effects of Coronal Magnetic Field Configuration on Particle Acceleration and Release during the Ground Level Enhancement Events in Solar Cycle 24
Authors: Wenlong Liu, Xiangliang Kong, Fan Guo, Lulu Zhao, Shiwei Feng, Feiyu Yu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: (a)–(b) GOES 1–8 Å SXR light curves for the two GLE events, GLE 71 on 2012 May 17 and GLE 72 on 2017 September 10. The vertical solid lines indicate the flare start time. (c)–(d) Proton intensity profiles in different energy channels observed by EPEAD and HEPAD on board GOES 15. (e)–(f) Count rates recorded by NM stations from OULU for GLE 71 and FSMT for GLE 72. The red lines display the smoothed data and the vertical solid lines indicate the identified GLE onset time.