adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining Baryon Loading Efficiency of Active Galactic Nuclei with Diffuse Neutrino Flux from Galaxy Clusters
Authors: Xin-Yue Shi, Ruo-Yu Liu, Chong Ge, Xiang-Yu Wang
Figure caption: Left: the normalized radial density distribution of neutrino emissivity with energy E  ν  = 1 TeV for a cluster with virial mass M vir = 1014 M ⊙ (red), 1015 M ⊙ (green), and redshift z = 0. The flux is normalized by fixing it to unity at the center of the cluster with M vir = 1014 M ⊙. The total neutrino emissivity derived from l c = 0.1r vir,200 under different CR injection rates, regarding either the same total CR injection ﹩{W}_{p}=\mathrm{const}﹩ (dashed line) or a constant baryon loading factor ﹩{\eta }_{p,\mathrm{grav}}=\mathrm{const}﹩ (solid line). The latter is the model employed in our study. Right: the relation between the virial mass of a galaxy cluster and the total neutrino emissivity at redshift z = 0. The emissivity is normalized by fixing the value to be unity for the cluster of M vir = 1014 M ⊙. The line types correspond to the same assumptions as in the left panel.
Paper: Constraining Baryon Loading Efficiency of Active Galactic Nuclei with Diffuse Neutrino Flux from Galaxy Clusters
Authors: Xin-Yue Shi, Ruo-Yu Liu, Chong Ge, Xiang-Yu Wang
Figure caption: Cumulative γ-ray flux from the galaxy clusters for different proton injection spectral index α = 2.0 (dashed), 2.2 (solid), 2.5 (dotted). The flux is compared with the IGRB observations from Fermi-LAT. The differential upper limits for the distance weighting (1/d 2) scheme from IceCube analysis are also shown in the figure for comparison.
Paper: Constraining Baryon Loading Efficiency of Active Galactic Nuclei with Diffuse Neutrino Flux from Galaxy Clusters
Authors: Xin-Yue Shi, Ruo-Yu Liu, Chong Ge, Xiang-Yu Wang
Figure caption: Integrated muon-neutrino flux (red lines) from galaxy clusters in this work. Different injection spectral index α = 2 (dashed), 2.2 (solid), and 2.5 (dotted) are illustrated separately. It is compared with the differential upper limits in one-decade energy bins for the distance weighting (1/d 2) scheme from IceCube analysis (Abbasi et al. 2022). The IGRB observed by Fermi-LAT (Ackermann et al. 2015) is also shown for comparison.
Paper: Energy Conversion through a Fluctuation–Dissipation Relation at Kinetic Scales in the Earth’s Magnetosheath
Authors: Federica Chiappetta, Emiliya Yordanova, Zoltán Vörös, Fabio Lepreti, Vincenzo Carbone
Figure caption: The values of γ and ﹩{\lambda }_{\max }﹩ as a function of the electron plasma-β parameter of the seven samples we used. The full lines correspond to the scaling reported in the text.
Paper: Energy Conversion through a Fluctuation–Dissipation Relation at Kinetic Scales in the Earth’s Magnetosheath
Authors: Federica Chiappetta, Emiliya Yordanova, Zoltán Vörös, Fabio Lepreti, Vincenzo Carbone
Figure caption:  E(f) vs. f as obtained from data (dots) and from Equation (5) (red line) for the seven different samples. The positions of γ, ﹩{\lambda }_{\min }﹩, ﹩{\lambda }_{\max }﹩, and of the two characteristic electron plasma frequencies of each sample are indicated on the plots. The values of the electron plasma-β and the scaling exponent μ obtained from the fit are reported in each figure.
Paper: Constraining Baryon Loading Efficiency of Active Galactic Nuclei with Diffuse Neutrino Flux from Galaxy Clusters
Authors: Xin-Yue Shi, Ruo-Yu Liu, Chong Ge, Xiang-Yu Wang
Figure caption: The upper limits of baryon loading factor η  p,grav constrained by diffuse muon-neutrino and γ-ray flux with different indices α of the injected protons from 2.0 to 2.5.
Paper: Heavy-ion Acceleration in 3He-rich Solar Energetic Particle Events: New Insights from Solar Orbiter
Authors: G. M. Mason, I. Roth, N. V. Nitta, R. Bučík, D. Lario, G. C. Ho, R. C. Allen, A. Kouloumvakos, R. F. Wimmer-Schweingruber, J. Rodriguez-Pacheco
Figure caption:  3He-rich SEP event starting 2022 November 9. Top panel: time profiles of H, 3He, 4He, O, and Fe ions of 0.23–0.32 MeV nucleon−1. Middle panel: mass spectrogram for elements from He to Fe for ions with energies 0.3–10 MeV nucleon−1. Bottom panel: plot of 1/ion speed vs. time of arrival for ions of mass 10–70 amu. The oblique line indicates the arrival times assuming an Archimedes spiral magnetic path length of 0.61 au.
Paper: Multi-spacecraft Observations of the 2022 March 25 CME and EUV Wave: An Analysis of Their Propagation and Interrelation
Authors: Alessandro Liberatore, Paulett C. Liewer, Angelos Vourlidas, Carlos R. Braga, Marco Velli, Olga Panasenco, Daniele Telloni, Salvatore Mancuso
Figure caption: EUV wavefront evolution observed on a Carrington map showing the contour of magnetic field strength calculated from a PFSS model for 2022 March 25 12:04 UTC, 1.2 R ⊙; R  ss  = 2.5. Notice how the wave seems to avoid strong magnetic field regions (top and top left regions) while being free to propagate through the low field regions (right-side regions). This behavior is consistent with a fast-mode wave. The high-density region close to the ARs does not affect/stop the initial propagation of the wave because, at that time, the wave is a driven wave led by the expansion of the CME. The thick black line on the map shows the predicted heliospheric current sheet, and the blue and green areas are the polar coronal holes with opposite polarity. The dark green dot (“E”) shows the position of the Earth (the cross and circle symbols show the regions magnetically connected with the Sun).
Paper: Multi-spacecraft Observations of the 2022 March 25 CME and EUV Wave: An Analysis of Their Propagation and Interrelation
Authors: Alessandro Liberatore, Paulett C. Liewer, Angelos Vourlidas, Carlos R. Braga, Marco Velli, Olga Panasenco, Daniele Telloni, Salvatore Mancuso
Figure caption: EUV wavefront evolution observed on a map of the Alfvén velocity v  A  at different Carrington latitudes and longitudes (from MAS model). The wave propagates with a speed of v ≈ 200 km s−1 in regions with Alfvén velocity v  A  < 200 km s−1 and stops in regions with much higher v  A  (i.e., ﹩\mathrm{LN}\lt 60﹩°, ﹩\mathrm{LN}\gt 130^\circ {-}140^\circ ﹩ and LT < −60°, LT > 0°). This is consistent with the behavior of a fast-mode MHD wave. The initial phases (blue fronts) are associated with the driven phase (see Figure 7).
Paper: Multi-spacecraft Observations of the 2022 March 25 CME and EUV Wave: An Analysis of Their Propagation and Interrelation
Authors: Alessandro Liberatore, Paulett C. Liewer, Angelos Vourlidas, Carlos R. Braga, Marco Velli, Olga Panasenco, Daniele Telloni, Salvatore Mancuso
Figure caption: Composite dynamic radio spectrum of the type II radio burst observed on 2022 March 25 obtained by combining ground-based Learmonth e-Callisto ASSA (>16 MHz) and space-based STEREO-A/WAVES (<16 MHz) data. The dashed lines in the figure show the fundamental (F) and harmonic (H) bands as obtained from the density model profiles.
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: Top panel: the blue dots show the α fitted by comparing the galaxy number density profile model of halos (Equation (2)) to the measurements of DARK SAGE in each halo mass bin. The yellow curve is the model (Equation (5)) fit to the blue dots. Similarly, in the bottom panel, the blue dots show the fitted β of the measurements of DARK SAGE satellites in each halo mass bin, and the yellow curve is the (Equation (6)) fit to the blue dots. In both cases, the red pentagrams are the results from the SDSS data (see Section 5).
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: The PDF (the radial distribution) of satellite galaxies f cs for two example halo mass bins. The pink and blue filled circles are the measurements from DARK SAGE for halo mass bins centered on M = 11.73, 14.86, respectively. The solid curves are the models fit to the measurements. The dashed curves compare an NFW profile for these masses. All of them are normalized to integrate to one in the interval x ∈ [0, 1].
Paper: The Galaxy Number Density Profile of Halos
Authors: Fei Qin, David Parkinson, Adam R. H. Stevens, Cullan Howlett
Figure caption: The halo mass function of SDSS (blue dots) and DARK SAGE (yellow dots). Here we only intend to show the turning point of the halo mass function of SDSS.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: Mass–metallicity relation at z ≈ 8 compared with local-analog candidates: blueberry and green pea galaxies. The large colored data points show the measured masses and metallicities of the galaxies in our z ≈ 8 sample; the solid orange (solid red) line shows the best-fit mass–metallicity relation with a fixed (free) slope and the shaded orange (shaded pink) region show its 1σ uncertainty region. Blueberry galaxies and green peas are shown with the small purple and light-green data points, respectively. Only green peas which lie within the 2σ confidence interval of the z ≈ 8 galaxies in the [O III] 5007 Å/Hβ vs. [O II] 3727, 3729 Å/Hβ and O32 vs. R23 − 0.08 × O32 metallicity diagnostic plots (Figures 6 and 7, respectively) are shown. We plot all the blueberry galaxies, because Figures 6 and 7 indicate that they have similar metallicities to the z ≈ 8 emission line galaxies. This figure shows that although blueberry galaxies and green peas have similar metallicities to the z ≈ 8 galaxies, this degeneracy is broken down by considering the mass–metallicity relation; at a fixed stellar mass, green peas and blueberries have systematically higher metallicities compared to z ≈ 8 galaxies.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: Strong line metallicity measurements plotted against direct T  e  metallicity measurements (from Curti et al. 2022) for the SMACS0723 galaxies. Although the metallicities for individual galaxies differ slightly depending on the adopted metallicity measurement method, we confirm that the overall effect on the best-fit mass–metallicity relation is negligible.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the RX2129–ID11027 galaxy.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the SMACS0723–ID10612 galaxy.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the SMACS0723–ID4590 galaxy.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the SMACS0723–ID6355 galaxy.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the MACS1149–JD1 galaxy.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the MACS0416–Y1 galaxy.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the A2744–YD4 galaxy.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the B14–65666 galaxy.
Paper: Evolution of the Mass–Metallicity Relation from Redshift z ≈ 8 to the Local Universe
Authors: Danial Langeroodi, Jens Hjorth, Wenlei Chen, Patrick L. Kelly, Hayley Williams, Yu-Heng Lin, Claudia Scarlata, Adi Zitrin, Tom Broadhurst, Jose M. Diego, Xiaosheng Huang, Alexei V. Filippenko, Ryan J. Foley, Saurabh Jha, Anton M. Koekemoer, Masamune Oguri, Ismael Perez-Fournon, Justin Pierel, Frederick Poidevin, Lou Strolger
Figure caption: SED fitting results for the SXDF–NB1006–2 galaxy.
Paper: Deflection of Coronal Mass Ejections in Unipolar Ambient Magnetic Fields
Authors: Michal Ben-Nun, Tibor Török, Erika Palmerio, Cooper Downs, Viacheslav S. Titov, Mark G. Linton, Ronald M. Caplan, Roberto Lionello
Figure caption: Initial configuration for Runs 1, 3, 5, and 7. The sphere shows B  r  at the solar surface; north (south) is at the top (bottom). In Runs 1 and 3, the AR is placed below the streamer belt and HCS (see Figure 2(b)), and in Runs 5 and 7 within an area of unipolar open field at 45° north. Green (closed) and magenta (open) field lines are shown, together with electric currents visualized by ∣ j ∣/∣ B ∣ in the plane ϕ = π that cuts through the AR center. The insets show the AR magnetogram and the MFR (orange field lines) in a top-down view, where east (west) is on the left (right). The MFR axial current (black arrows) is oppositely directed in the configurations on the left and right, respectively, because of the opposite orientations of the AR main polarities. All MFRs shown are right-handed (positive helicity).
Paper: Deflection of Coronal Mass Ejections in Unipolar Ambient Magnetic Fields
Authors: Michal Ben-Nun, Tibor Török, Erika Palmerio, Cooper Downs, Viacheslav S. Titov, Mark G. Linton, Ronald M. Caplan, Roberto Lionello
Figure caption: Global background magnetic configuration for our CME runs. (a) Initial configuration (global dipole). The sphere shows the solar surface, colored by the radial magnetic field, B  r . Only half of the simulation domain (out to about 15 R ⊙) is shown here. Field lines are colored by B  r /∣ B ∣. (b) Configuration after MHD relaxation, during which the solar wind opens up flux and the HCS (shown here in the plane ϕ = π by the quantity ∣ j ∣/∣ B ∣) is formed. (c) Zoom into the streamer base, with the (r, θ) numerical mesh depicted in the plane ϕ = π (only every third grid point is shown in each direction). The mesh is finer at the equator and at 45° north, where an AR will be inserted.
Paper: Deflection of Coronal Mass Ejections in Unipolar Ambient Magnetic Fields
Authors: Michal Ben-Nun, Tibor Török, Erika Palmerio, Cooper Downs, Viacheslav S. Titov, Mark G. Linton, Ronald M. Caplan, Roberto Lionello
Figure caption: Simplified proof-of-concept numerical experiment. (a) Freely expanding toroidal MFR in a Cartesian box (side view, perpendicular to the torus axis). Shown are the initial state (left) and the MFR during its expansion (right). Rainbow-colored (purple) field lines show the MFR core (the field produced by the MFR current). The symbols denote the direction of the axial current. Red and blue colors show the horizontal component of the Lorentz force density, j × B, in two MFR cross sections. (b) Same initial MFR as in (a), now with a uniform vertical magnetic field, B  z  > 0, superimposed. This leads to a rotation of the MFR during its expansion.
Paper: Deflection of Coronal Mass Ejections in Unipolar Ambient Magnetic Fields
Authors: Michal Ben-Nun, Tibor Török, Erika Palmerio, Cooper Downs, Viacheslav S. Titov, Mark G. Linton, Ronald M. Caplan, Roberto Lionello
Figure caption: Erupting MFR after three Alfvén times (72 minutes) in Run 7. Field lines are colored by the normalized transverse magnetic field ﹩{({B}_{\theta }^{2}+{B}_{\phi }^{2})}^{1/2}/| {\boldsymbol{B}}| ﹩ (denoted here as Btang/B). Electric currents are shown by ∣ j ∣/∣ B ∣ in the ϕ = π plane, outlining the HCS and the shock wave produced by the CME.
Paper: Deflection of Coronal Mass Ejections in Unipolar Ambient Magnetic Fields
Authors: Michal Ben-Nun, Tibor Török, Erika Palmerio, Cooper Downs, Viacheslav S. Titov, Mark G. Linton, Ronald M. Caplan, Roberto Lionello
Figure caption: Distribution of tracer particles in and above the initial MFR (here for Run 7; see the corresponding inset in Figure 3). For clarity, only selected tracers are displayed (as small spheres). Shown are 19 of the 1000 arc (yellow) and axis (magenta) tracers, and three of the 49 cross sections (nos. 8, 25, and 42; in cyan) with 129 tracers each. Field lines originating at the tracers are shown for the arc and the axis. The transparent gray isosurface shows ﹩j=0.025\,{j}_{\max }﹩, outlining the edge of the MFR.
Paper: A Phase-resolved View of the Low-frequency Quasiperiodic Oscillations from the Black Hole Binary MAXI J1820+070
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Peng J. Wang, Jing Q. Peng, L. Ji, A. Santangelo, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, Y. Huang, L. Zhang, Hong H. Liu, P. Zhang, W. Yu, Z. Chang, J. Li, Wen T. Ye, Pan P. Li, Zhuo L. Yu, Z. Yan
Figure caption: HID of Insight-HXMT, where the hardness ratio is defined as the count ratio between the hard band (5–10 keV) and the soft band (1–5 keV), and the count rate is measured in the 1–10 keV energy range. The colored stars indicate the averaged results for each epoch.
Paper: A Phase-resolved View of the Low-frequency Quasiperiodic Oscillations from the Black Hole Binary MAXI J1820+070
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Peng J. Wang, Jing Q. Peng, L. Ji, A. Santangelo, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, Y. Huang, L. Zhang, Hong H. Liu, P. Zhang, W. Yu, Z. Chang, J. Li, Wen T. Ye, Pan P. Li, Zhuo L. Yu, Z. Yan
Figure caption: Phase dependence of the inclination across the four epochs. To obtain the modulations in the inclination (i), we set the reflection fraction to the best-fit values acquired from the phase-averaged spectral fittings. The uncertainties are reported at the 68% confidence level using the MCMC technique. Additionally, we include the QPO waveform in each panel as the gray dashed line.
Paper: A Phase-resolved View of the Low-frequency Quasiperiodic Oscillations from the Black Hole Binary MAXI J1820+070
Authors: Qing C. Shui, S. Zhang, Shuang N. Zhang, Yu P. Chen, Ling D. Kong, Peng J. Wang, Jing Q. Peng, L. Ji, A. Santangelo, Hong X. Yin, Jin L. Qu, L. Tao, Ming Y. Ge, Y. Huang, L. Zhang, Hong H. Liu, P. Zhang, W. Yu, Z. Chang, J. Li, Wen T. Ye, Pan P. Li, Zhuo L. Yu, Z. Yan
Figure caption: One- and two-dimensional projections of the posterior probability distributions, and the 0.16, 0.5, and 0.84 quantile contours derived from the MCMC analysis for each free spectral parameter. To test the convergence, we compare the one- and two-dimensional projections of the posterior distributions from the first (blue) and second (orange) halves of the chain, and we find no large differences. This illustration corresponds to the spectral fitting of the QPO trough phase in Epoch 4.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Emissivity j  I  (a), absorption α  I  (b), and emitted polarization fractions (c) as functions of the angle between propagation direction and magnetic field θ  B  at different anisotropy values: T ⊥ < T ∥ (η < 1, blue), isotropic (η = 1, black), and T ⊥ > T ∥ (η > 1, red). The free parameters are ν/ν  c  = 103 and ϵ ⊥ = 10 (near the peak of the optically thin synchrotron spectrum for an isotropic distribution function). In panel (c), the emitted linear ∣j  Q ∣/j  I  and circular ∣j  V ∣/j  I  polarization fractions are shown by solid and dashed lines, respectively. In panel (a), ﹩{\sin }^{2}{\theta }_{B}﹩ dependence is shown by a black dotted line.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Integrands ∣K  I  f(γ, ξ)∣ for j  I  (a) and ∣K  I  Df(γ, ξ)∣ for α  I  (b). Two parts of Df that include ∂ γ  f(γ, ξ) (c) and ∂ μ  f(γ, ξ) (d). The approximate location of the peak that corresponds to ﹩\cos {\theta }_{B}=\beta \mu ﹩ is shown by dotted lines. The free parameters are ν/ν  c  = 103, η = 10, ϵ ⊥ = 10. While the location of the peak is still the same as in the η = 1 case, a nonzero term with ∂ μ  f(γ, μ) appears, which, however, goes through zero at the peak of the integrand. Note the saturated color bar in panels (c) and (d).
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Comparison of numerical results for j  I  (a)–(b), α  I  (c)–(d), j  Q  (e)–(f), and j  V  (g)–(h) with the theoretical fits given by Equations (11) and (A14). Numerical results and theoretical fits are shown on the left by solid and dotted lines, respectively. On the right, the relative error is shown. Note that the dashed gray line on the right shows a relative error of 30%. The free parameters are ϵ ⊥ = 10 and ν/ν  c  = 103.