adsabs/AstroCLIMB huggingface dataset:
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: NIRSpec 2D (top panel) and 1D spectra (bottom panel) of the RX2129–ID11022 galaxy at z spec = 8.15. The red dashed lines show the identified emission lines, and the thin gray lines show the 1σ uncertainties. The fits to the emission lines and continuum are shown in Figure 5, and the emission line flux measurements are presented in Table 2. The spectrum is not corrected for lensing magnification. The blue part of the spectrum is missing for this galaxy because the NIRSpec MSA configuration caused the spectrum to fall only partially on the detector.
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: NIRSpec 2D (top panel) and 1D (bottom panel) spectra of the RX2129–ID11002 galaxy at z spec = 8.16. The red dashed lines show the identified emission lines, and the thin gray lines show the 1σ uncertainties. The fits to the emission lines and continuum are shown in Figure 4, and the emission line flux measurements are presented in Table 2. The spectrum is not corrected for lensing magnification.
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: Same as Figure 4, but for the RX2129–ID11022 galaxy at z spec = 8.15. The 1D spectrum is shown in Figure 3.
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: Same as Figure 8, but showing the SED fitting results for the RX2129–ID11022 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: Sketch illustrating the effective  I  ×  B  force introduced in Section 1. (a) Unipolar background field. (b) The intrusion of a perfectly conducting MFR i.e., I = 0, with a fully balancing “direct” and “return” axial current (not shown) leads to the formation of surface SCs (shown in red and blue, where red depicts currents directed into the plane and blue depicts currents directed toward the viewer) and a deformation of the background field. (c) An MFR with a DC (I > 0) additionally produces a magnetic-pressure difference in the ambient field, yielding a sideways deflection force. (d) Most general case with an RC (light blue) and a DC, where the RC partially balances the DC. See text for further details.
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: Top: heliocentric latitude at the position of the CME’s leading-edge height (as determined from the GCS model apex) for Run 5 (blue) and Run 7 (orange). The circles and squares denote the latitudes estimated from the GCS-fitting method and the tracer-particles method, respectively, at corresponding times. The green cross marks the location of the source AR at 45° north. For the GCS-fitting method, the error bars indicate the estimates for the average deviations in latitude (±1.°8) and height (±0.48 R ⊙), found by Thernisien et al. (2009). Bottom: heliocentric latitude but as a function of time from the tracer-particles method. The blue and orange lines use all the tracer-particles data (up to 14 hr), while the squares correspond to the data points shown in the top panel. The green vertical line marks the arrival time of the CME’s leading edge at the outer boundary of the simulation domain.
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: CMEs for Runs 1, 3, 5, and 7 after 25 Alfvén times (≈10 hr), visualized by ∣ j ∣/∣ B ∣ (in code units) in the ϕ = π plane. The dashed black line marks the radial direction above the AR. The radial extension of the simulation domain is (1–30) R ⊙. Runs 1 and 3 propagate along the HCS, while Runs 5 and 7 propagate in a unipolar radial ambient field (see Figure 3).
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: Example of graduated cylindrical shell (GCS) fitting results for (a–f) Run 5 and (g–l) Run 7. Panels (a–c) and (g–h) show base-difference synthetic coronagraph images (where the frame at t = 0 hr is subtracted from the frame at t = 8.8 hr) from the simulated L5, L1, and L4 points, while panels (d–f) and (j–l) show the same images with the GCS wire-frame projection (in red) overlaid.
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: Trajectories of tracer particles in the (θ, ϕ) plane (with respect to their initial positions in that plane) along the north–south (−Δθ) and east–west (Δϕ) directions for Run 5 (top) and Run 7 (bottom). The mean trajectories, obtained from a center-of-mass calculation (see text for details) are shown in red. The first three panels show, respectively, tracers starting from the initial MFR axis, the arc above this axis, and five MFR cross sections around the initial axis apex; the rightmost panel shows all tracers combined. The annotated values are the mean angular deviations at the time when the first tracer of the respective group reaches the outer boundary of the simulation domain.
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 electric currents in the ϕ = π plane for Runs 1, 3, 5, and 7 after five Alfvén times (≈2 hr), visualized by j  p  r 2 (in code units), where j  p  is the current density along the ϕ direction (which points into the plane) and r is the (Sun-centered) radial coordinate. Hence, red colors show currents directed into the plane, while blue colors show colors directed toward the viewer.
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: Contours of B 2 (in code units) for Runs 5 (top) and 7 (bottom) at 2 (left) and 5 (right) R ⊙ for the total magnetic field (including the AR) at the beginning of the simulation. The inner sphere shows the radial magnetic field (in gray scale) at the solar surface. The view is centered on the AR at 45° north. The small magenta (green) ball marks the position of the solar north pole (its radial projection onto the respective outer sphere).
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: Representative example of a 100 s long light curve of LE in the energy range of 1–10 keV and its corresponding IMFs. In this example, we set K = 5 and α = 4000 for the VMD algorithm, hence obtaining five IMFs. The IMF C2 corresponds to the QPO signal at ∼0.3 Hz, and the IMF C3 corresponds to the second harmonic of the QPO. In this plot, the characteristic frequency (f) and the approximate bandwidth (BW) for each mode are also presented.
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: PDS of the original light curve (black dots), IMF C2 (red line), and IMF C3 (blue line) plotted in Figure 2.
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 seven free spectral parameters, including the temperature of the inner radius of the disk (T in), inner radius (R in), spectral index (Γ), electron temperature (kT e), reflection fraction (R f), and the normalization of relxillCp (Norm1) and xillverCp (Norm2), across the four epochs. 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: Top: the ratio between the spectra of QPO trough (0–0.1 cycles) and peak (0.4–0.5 cycles) phases across the four epochs. Bottom: the energy dependence of the jet speed (β) across the four epochs, where values of β are calculated by Equation (16). The gray scatters represent the calculation from the original spectra, while colored scatters represent rebinned values.
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: Constructed QPO waveforms of Epoch 1 by phase folding the light curve from LE, ME, and HE in the energy ranges of 1–10 keV (orange), 10–30 keV (blue), and 30–120 keV (pink), respectively. The black line represents the hardness defined as the ratio between constructed QPO waveforms of HE and LE.
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 optical depth across the four epochs. The colored scatters represent the calculated optical depth (τ) from Equation (10), using the best-fit parameters of Γ and kT e from the spectral fitting. The black dashed lines represent the calculated optical depth based on Equations (11) and (12).
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: Left: histogram of measured values of the phase difference between harmonics obtained using the HHT (black) and Fourier (red) methods. To show a clear peak, we repeat the data from 0 to π. Right: reconstructed QPO waveform derived from the HHT phase-folding (black) and Fourier (red) methods.
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: Constructed QPO waveforms of four epochs by phase folding the light curve from LE in the energy range of 1–10 keV.
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: Left: Hilbert spectrum of ∼0.3 Hz QPO IMF plotted in the third panel of Figure 2. The color on the z-axis represents the amplitude. Right: two-dimensional contour map of the WWZ power spectrum. Both of the two distinct methods present that the QPO frequency fluctuates between 0.2 and 0.4 Hz over time.
Paper: Influence of Crustal Magnetic Fields on Horizontal Plasma Transport and Ion Escape on Mars
Authors: Guokan Li, Haoyu Lu, Yun Li, Jinbin Cao, Xiaoxin Zhang, Shibang Li
Figure caption: Distributions of  V   r ,  V   θ , and  V   φ  at altitudes of 300, 400, 500, 600, and 700 km on the dayside. (a)  V   r  without crustal field; (b)  V   r  with crustal field; (c)  V   θ  without crustal field; (d)  V   θ  with crustal field; (e)  V   φ  without crustal field; (f)  V   φ  with crustal field. The three coordinate axes in the figure are longitude, latitude, and altitude, with ranges of 90° (dawn side) to 270° (dusk side), −90° (south) to 90° (north), and 300–700 km, respectively.
Paper: Influence of Crustal Magnetic Fields on Horizontal Plasma Transport and Ion Escape on Mars
Authors: Guokan Li, Haoyu Lu, Yun Li, Jinbin Cao, Xiaoxin Zhang, Shibang Li
Figure caption: Variations of  V   θ  (a, c, e, and g), and  V   φ  (b, d, f, and h) along the 30° S (a, b), 50° S (c, d), 30° N (e, f), and 50° N (g, h) latitude line at an altitude of 500 km. Solid/dashed lines represents the case with/without the crustal field.
Paper: Influence of Crustal Magnetic Fields on Horizontal Plasma Transport and Ion Escape on Mars
Authors: Guokan Li, Haoyu Lu, Yun Li, Jinbin Cao, Xiaoxin Zhang, Shibang Li
Figure caption: Variations in the distributions of  V   r  (red lines),  V   θ  (blue lines), and  V   φ  (green lines) (a) and crustal field strength (b) along the 180° W longitude line at an altitude of 500 km. The case with/without the crustal field is represented by the solid/dashed lines.
Paper: Influence of Crustal Magnetic Fields on Horizontal Plasma Transport and Ion Escape on Mars
Authors: Guokan Li, Haoyu Lu, Yun Li, Jinbin Cao, Xiaoxin Zhang, Shibang Li
Figure caption: Distributions of velocity in the (a) X–Z plane and (b) X–Y plane and the logarithmic magnetic field in the (c) X–Z plane and (d) X–Y plane. Black solid lines with arrows represent streamlines in (b) and magnetic field lines in (d). White and black solid quasi-parabolas represent the mean locations of MPB and BS from Vignes et al. (2000), respectively.
Paper: Influence of Crustal Magnetic Fields on Horizontal Plasma Transport and Ion Escape on Mars
Authors: Guokan Li, Haoyu Lu, Yun Li, Jinbin Cao, Xiaoxin Zhang, Shibang Li
Figure caption: The isosurfaces of total-ion number density = 1000 cm−3 in cases with (red surface) and without (gray surface) the crustal fields (a), and the same isosurfaces with the distribution of the crustal field strength on them (b). The two isosurfaces are created in the three-dimensional spherical-coordinate system and overlap with each other in both (a) and (b). The observing direction is from high to low altitude, along the altitude axis. (c) The isosurfaces of total-ion number density = 1000 cm−3 in cases with the crustal fields, colored by the distribution of altitude and superposed with the isolines.
Paper: Influence of Crustal Magnetic Fields on Horizontal Plasma Transport and Ion Escape on Mars
Authors: Guokan Li, Haoyu Lu, Yun Li, Jinbin Cao, Xiaoxin Zhang, Shibang Li
Figure caption: Logarithmic number density (n  s ) distributions in the X–Z plane ((a)–(c)) and the radial flux Q  r  of O2 +, O+, and CO2 + ((d)–(f)) on the white line in (c), which represent the 0° W longitude line at 6 R M downstream. (a), (d) O2 +; (b), (e) O+; (c), (f) CO2 +. Red/blue lines represents the case with/without the crustal field.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Synchrotron emission of accreting plasma ray-traced from an MAD simulation for a BH with a = 0.98 at R high = 10 and inclination of θ = 163°. Each column represents different plasma anisotropy: mirror instability threshold (column 1), whistler instability threshold (column 2), isotropic plasma distribution (column 3), and firehose instability threshold (column 4). The first row represents the full image blurred with 20 μas FWHM Gaussian kernel on a linear scale (panels (a)–(d)), the second row shows a full unblurred image on a logarithmic scale, from which I  ν,0 (n = 0) and I  ν,1 (n = 1) are decoupled on the third (panels (i)–(l)) and forth (panels (m)–(p)) rows, respectively.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Asymmetry A (panel (a)) and diameter d (panel (b)) as functions of R high for a = 0.98 and M87* observing angle, θ = 163°, for images at 230 GHz blurred with 20 μas FWHM Gaussian kernel. Panel (c): asymmetry of unblurred images at θ = 163° and R high = 10 as a function of observing frequency, a = 0.98. Panel (d): asymmetry at R high = 10 as a function of observing angle θ for a = 0.98 (solid lines) and a = 0.5 (thin dotted lines) for Sgr A*. The green regions highlight EHT constraints for M87* (a,b) and Sgr A* (d). In each panel, the color of the lines represents four limiting cases: mirror instability, whistler instability, isotropic plasma distribution, and firehose instability.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Similar to Figure 3 but for a BH with spin parameter of a = 0.5. Inclination of θ = 163° and R high = 10 are identical to Figure 3. The first row represents the full image blurred with 20 μas FWHM Gaussian kernel on a linear scale (panels (a)–(d)), and the second row shows a full unblurred image on a logarithmic scale.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Plasma-β th (column 1, panels (a) and (g)), plasma temperature P/2ρ (column 2, panels (b) and (h)), anisotropy η (columns 3 and 4 for mirror and firehose, respectively), and normalized electron perpendicular temperature ϵ ⊥ (columns 5 and 6 for mirror and firehose, respectively) for a = 0.98 (at the time of 14,300r  g /c, top row) and a = 0.5 (at the time of 16,000r  g /c, bottom row).
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Average angle with the magnetic field along the ray, measured by emission-weighted sine of θ  B  for different spins and viewing angles. Lower spin decreases the average angle of the emitted photons relative to the magnetic field. This in turn enhances the effects of plasma anisotropy on the observed image (Figures 3–5).
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Angular profiles of n = 0 and n = 1 brightness (I 0 [solid] and I 1 [dotted] as functions of ﹩{\phi }_{\mathrm{im}}﹩ in the image plane, top row) and their ratio (bottom row) at an observing angle of θ = 163° at spins of 0.98 (thick lines) and 0.5 (thin lines). The first and second columns represent R high = 1 and 100, respectively. The color of the lines, as in Figure 7, represents four limiting cases: mirror, whistler, isotropic, and firehose.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Synchrotron emission of accreting plasma ray-traced from an MAD simulation with a = 0.98 at an inclination of θ = 163° and R high = 10 at frequencies of 345 GHz (panels (a)–(b)) and 86 GHz (panels (c)–(d)). The first and second columns represent two limiting cases (mirror and firehose, respectively).
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Synchrotron emission spectra for BHs with a = 0.98 (solid lines) and a = 0.5 (thin dotted lines) viewed at inclinations of θ = 135° (panels (a) and (b)) and 163° (panels (c) and (d)) at R high = 10 (panels (a) and (c)) and 100 (panels (b) and (d)). As in Figure 7, different models are represented by different colors.
Paper: Polarized Anisotropic Synchrotron Emission and Absorption and Its Application to Black Hole Imaging
Authors: Alisa Galishnikova, Alexander Philippov, Eliot Quataert
Figure caption: Synchrotron emission of accreting plasma ray-traced from an MAD simulation at an inclination of θ = 135° for a BH with a = 0.98. As in Figure 3, each column represents different plasma anisotropy. The first and second rows represent R high = 1 and 100 models, respectively.