adsabs/AstroCLIMB huggingface dataset:
Paper: Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed
Authors: Tim Cunningham, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, Paul Duffell, Chris Martin, Odette Toloza, David Charbonneau, Scott J. Kenyon, Zeren Lin, Mateusz Matuszewski, Rosalie McGurk, Abigail Polin, Philippe Z. Yao
Figure caption: Examples of the Gaussian-fitting to the blue- and redshifted [S II] doublets. Each panel shows the mean-averaged spectrum over a 3 × 3 sky pixel region. The horizontal blue line indicates a 3σ noise threshold relative to the local continuum. The two vertical lines indicate the rest wavelengths of the [S II] 6717 Å/6731 Å doublet.
Paper: Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed
Authors: Tim Cunningham, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, Paul Duffell, Chris Martin, Odette Toloza, David Charbonneau, Scott J. Kenyon, Zeren Lin, Mateusz Matuszewski, Rosalie McGurk, Abigail Polin, Philippe Z. Yao
Figure caption: Deprojected radial structure of the observed fraction of the nebula assuming that all material was ejected in the year 1181 and that the velocities have remained constant in time. The x-axis shows the radial distance between the central star and a given filament projected on the plane of the sky assuming the Gaia distance to the central star of D = 2.3 kpc. The y-axis shows the reconstructed line-of-sight distance from the central star, using Equation (1) and an age of τ = 842 yr.
Paper: Expansion Properties of the Young Supernova Type Iax Remnant Pa 30 Revealed
Authors: Tim Cunningham, Ilaria Caiazzo, Nikolaus Z. Prusinski, James Fuller, John C. Raymond, S. R. Kulkarni, James D. Neill, Paul Duffell, Chris Martin, Odette Toloza, David Charbonneau, Scott J. Kenyon, Zeren Lin, Mateusz Matuszewski, Rosalie McGurk, Abigail Polin, Philippe Z. Yao
Figure caption: Upper panel: velocity map for all sky positions with detectable redshifted emission in the [S II] 6717/6731 Å doublet. We find a line-of-sight velocity gradient as a function of projected sky distance to the central star, which strongly implies a homologous velocity profile. Middle: similar to the top panel, but for all measured blueshifted components. Lower: combined velocity map for all filaments.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Initial parameters for evolved massive binaries at 15 (left) and 30 Myr (right). Each individual dot represents a simulated binary model, with its color reflecting its initial orbital period. The reddish brown, turquoise, and orange open symbols mark the binaries currently appearing as OB+helium-burning stars, OB+NSs (zero-kick), and OB+BH systems, respectively. The small dots not surrounded by open symbols represent systems not identified as such evolved massive binaries (e.g., merger products, post-MS stars, and preinteraction binaries) at these ages. The 1D projections of the data are depicted on the upper and right margins of the primary plot.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Comparison between the number of evolved massive binaries resulting from fiducial models and assumptions of idealized mass transfer stability, in which all Case B binaries undergo stable mass transfer and produce an OB+cc binary. The left panel shows results for OB+BH (solid lines) and OB+WD binaries (dotted lines), with gray lines indicating fiducial results and blue lines indicating results based on the idealized mass transfer stability assumption. This panel is bifurcated with the major lower section retaining the same y-axis range as in Figure 3 to facilitate a direct comparison. The right panel demonstrates the results for OB+NS binaries with (dotted lines) and without (solid lines) SN kicks, again with gray lines corresponding to fiducial results and blue lines corresponding to results based on idealized mass transfer stability.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Comparison between the number of evolved massive binaries resulting from fiducial models (gray lines) and the assumptions regarding SN explosions proposed by F. R. N. Schneider et al. (2021; blue lines). The solid lines show the results for OB+BH binaries. The dashed and dotted lines show the results for OB+NS binaries without and with SN kicks, respectively.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Predicted mass distribution for binaries comprising an OB star paired with an HeS, NS, or WD component, similar to Figure 4. Colors indicate the count of respective binaries in each pixel. For OB+HeS binaries, the mass distribution is depicted for both stellar components.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Same as Figure 4, but the results are obtained with the idealized mass transfer assumption.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Same as Figure 4, but the results are based on an alternative SN explosion assumption as proposed by F. R. N. Schneider et al. (2021).
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Same as Figure 2 but for an age of 30 Myr.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Same as Figure 2 but for an age of 80 Myr.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Same as Figure 2 but for an age of 50 Myr.
Paper: Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models
Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer
Figure caption: Same as Figure 3, but the sample size is reduced to 60%, 40%, 20%, and 10% in each panel.
Paper: Effects of Dust Coagulation on Streaming Instability
Authors: Ka Wai Ho, Hui Li, Shengtai Li
Figure caption: Temporal evolution of the midplane maximum dust density (top) and the mass-averaged normalized stopping time (bottom) in simulations with the initial stopping time τ  s,0 = 10−2 (the first three runs in Table 1). We adopt c  s  = 0.4 km s−1 in all these runs. The result from a single dust size run with τ  s,0 = 10−2 without coagulation is also shown for reference (yellow line).
Paper: Effects of Dust Coagulation on Streaming Instability
Authors: Ka Wai Ho, Hui Li, Shengtai Li
Figure caption: Spatial distribution of dust density ratio ρ  d /ρ  g  (left) and the mass-averaged stopping time τ  s  (right) for varying fragmentation velocities v  f  = 1, 2, and 10 m s−1. (White region indicates local dust density falling below 10−8 ρ  g , and the mass-averaged statistics is not computed.) Each frame is chosen to be ∼100Ω−1 after the strong clumping phase has started for Runs 1–3 respectively (see Figure 1), which are t = 1300Ω−1 (Run 1), and 1350Ω−1(Runs 2 and 3).
Paper: Effects of Dust Coagulation on Streaming Instability
Authors: Ka Wai Ho, Hui Li, Shengtai Li
Figure caption: Temporal evolution of the midplane (∣z∣ < 0.05H) dust density ρ  d /ρ  g  and its mass-weighted size 〈τ  s 〉 for Runs 1–3 with three fragmentation velocities of 1 m s−1 (left column), 2 m s−1 (middle), and 10 m s−1 (right), respectively. The bottom row is the evolution of the probability density function of dust size distribution for Runs 1–3, respectively. All runs have an initial stopping time τ  s,0 = 10−2 and initial ρ  d /ρ  g  = 1.5 × 10−2.
Paper: Effects of Dust Coagulation on Streaming Instability
Authors: Ka Wai Ho, Hui Li, Shengtai Li
Figure caption: Temporal evolution for τ  s,0 = 10−3 case.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Confidence contours (1σ and 2σ) for the parameter space (Ω m , H 0, l, b, A, and B) from the joint data set in the dipole model. The left panel shows Ω m  = 0.32 ± 0.02, H 0 = ﹩{66.42}_{-1.19}^{+1.23}﹩ km s−1 Mpc−1, l = 319.°79﹩{}_{-21.20}^{+24.86}﹩, b = −9.°30﹩{}_{-18.51}^{+16.70}﹩, A = −5.2 ± 3.6 × 10−4, and B = −5.6 ± 1.0 × 10−3. The right panel shows Ω m  = 0.32 ± 0.02, H 0 = 66.39 ± 1.22 km s−1 Mpc−1, l = 140.°50﹩{}_{-21.14}^{+24.96}﹩, b = 10.°06﹩{}_{-15.09}^{+19.67}﹩, A = ﹩{5.2}_{-3.8}^{+3.4}﹩× 10−4, and B = −5.6 ± 1.1 × 10−3.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Confidence contours (1σ and 2σ) for the parameters space (Ω m , H 0, l, b, A, and B) from the joint data set in the dm model. The constraints of cosmological parameters are Ω m  = ﹩{0.32}_{-0.02}^{+0.02}﹩ and H 0 = ﹩{66.38}_{-1.22}^{+1.22}﹩ km s−1 Mpc−1. For correction parameters (l, b, and A), there are two constraints. The two constraints on parameter A are negative of each other, and the figure shows the superposition effect of two Gaussian distributions. The more accurate constraints of the correction parameters are given by Figure A1.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Confidence contours (1σ and 2σ) for the parameter space (H 0, q 0, j 0, l, b, A and B) from the low-redshift joint data set using the third-order expansion. The constraints of cosmological parameters are H 0 = 72.54 ± 0.27 km s−1 Mpc−1, q 0 = −0.33 ± 0.06, and j 0 = ﹩{0.03}_{-0.28}^{+0.29}﹩. For correction parameters (l, b, and A), there are two constraints. The two constraints on parameter A are negative of each other, and the figure shows the superposition effect of two Gaussian distributions. The more accurate constraints of the correction parameters are given by Figure A2.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Confidence contours (1σ and 2σ) for the parameter space (H 0, q 0, j 0, l, b, A, and B) from the low-redshift joint data set using the third-order expansion. The constraints are (l = ﹩{326.85}_{-30.78}^{+30.24}﹩, b = ﹩{7.52}_{-26.65}^{+24.38}﹩, A = −3.2 ± 2.2 × 10−4, B = −6.3 ± 1.5×10−3) and (l = ﹩{140.50}_{-21.14}^{+24.96}﹩, b = ﹩{10.06}_{-15.09}^{+19.67}﹩, A = ﹩{5.2}_{-3.8}^{+3.4}﹩× 10−4, B = −5.6 ± 1.1 × 10−3), as shown in the left panel and the right panel, respectively.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Variation of H(z)/(1 + z) with redshift z. The orange solid line and shaded region represent the theoretical prediction and the corresponding 1σ range based on the constraints of the ΛCDM model. Green represents the result of the ΛCDM model considering the dipole correction. The purple points represent DESI BAO measurements, and the gray points represent other BAO measurements.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: A schematic diagram for the dm model. The blue dot represents the observer’s position. The shape is a segment of a three-dimensional sphere with radius r.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Confidence contours (1σ and 2σ) for the parameter space (H 0, q 0, j 0 and s 0) from the low-redshift joint data set utilizing the cosmography method.
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Comparison of our H 0 results with the Planck 2018 result (67.36 ± 0.50 km s−1 Mpc−1; Planck Collaboration et al. 2020b) and the SH0ES result (73.04 ± 1.04 km s−1 Mpc−1; A. G. Riess et al. 2022).
Paper: Hints of New Physics for the Hubble Tension: Violation of Cosmological Principle
Authors: J. P. Hu, X. D. Jia, J. Hu, F. Y. Wang
Figure caption: Confidence contours (1σ  and 2σ) for the parameters space (Ω m  and H 0) from the joint data set in the flat ΛCDM model. The fitting results are Ω m  = 0.33 ± 0.02 and H 0 = 73.15 ± 0.21 km s−1 Mpc−1.
Paper: First Detection of Molecular Gas in the Giant Low Surface Brightness Galaxy Malin 1
Authors: Gaspar Galaz, Jorge González-López, Viviana Guzmán, Hugo Messias, Junais, Samuel Boissier, Benoît Epinat, Peter M. Weilbacher, Thomas Puzia, Evelyn J. Johnston, Philippe Amram, David Frayer, Matìas Blaña, J. Christopher Howk, Michelle Berg, Roy Bustos-Espinoza, Juan Carlos Muñoz-Mateos, Paulo Cortés, Diego García-Appadoo, Katerine Joachimi
Figure caption: K-S diagram for the molecular gas in Malin 1 (R. C. Kennicutt 1998; M. R. Krumholz et al. 2009). This plot shows the range of stellar formation surface density as a function of the molecular gas surface density for different area coverage and detections. The star formation surface density ΣSFR in the very center (magenta star) is ∼2 × 10−3 M ⊙ yr−1 kpc−2 and has a molecular gas mass surface density ΣMol ∼ 5 M ⊙ pc−2, compared to the global ΣSFR (i.e., considering the total surveyed area; green star) of ∼6 × 10−5 M ⊙ yr−1 kpc−2 with a corresponding molecular gas surface density of ∼0.01 M ⊙ pc−2. The thin dotted lines represent linear relations with constant molecular gas depletion times of 0.1, 1, and 10 Gyr. The density contours (40%–80%–95% levels from inside to outside contours) represent the distributions of all 1.5 kpc scale regions with >3σ detections for both ΣMol and ΣSFR for galaxies studied in the PHANGS-ALMA sample (J. Sun et al. 2023). The colored-gradient trace represents the 5σ upper limit molecular gas surface density combined with the corresponding SFR surface density measured with MUSE (Junais et al. 2024). The different radii for the estimates are shown in the color bar on the right. We also show the position of the gLSBGs UGC 6614 and Malin 2 (M. Das et al. 2006, 2010; T. K. Wyder et al. 2009). See Section 4 for further details.
Paper: First Detection of Molecular Gas in the Giant Low Surface Brightness Galaxy Malin 1
Authors: Gaspar Galaz, Jorge González-López, Viviana Guzmán, Hugo Messias, Junais, Samuel Boissier, Benoît Epinat, Peter M. Weilbacher, Thomas Puzia, Evelyn J. Johnston, Philippe Amram, David Frayer, Matìas Blaña, J. Christopher Howk, Michelle Berg, Roy Bustos-Espinoza, Juan Carlos Muñoz-Mateos, Paulo Cortés, Diego García-Appadoo, Katerine Joachimi
Figure caption:  12CO (1–0) line profiles of tentative detections. These correspond to the emissions shown in Figure 3. These detections have 3 ≤ S/N ≤ 4. Some features of the line fitting are shown in the upper right corner of each line profile.
Paper: Dynamics of Binary Planets within Star Clusters
Authors: Yukun Huang, 宇坤 黄, Wei Zhu, 伟 祝, Eiichiro Kokubo, 保英一郎 小久
Figure caption: Upper: orbital distributions and histograms of 1000 equal-mass binary planets after encountering a solar-mass star with v ∞ = 1 km s−1. Binaries are initialized with a 0 = 15 au, e 0 = 0, and m = 10 M J, while the chosen impact parameters correspond to a deep critical flyby (b cr/1.5, left panel), a critical flyby (b cr, middle panel), and a distant flyby (1.5b cr, right panel), respectively. The x-axis indicates the fractional energy change ﹩{\rm{\Delta }}{ \mathcal E }﹩. The left y-axis represents the binary eccentricity post-flyby, whereas the right y-axis denotes the number of binaries in each bin. The orange dashed line marks the energy change of 0, with a negative ﹩{\rm{\Delta }}{ \mathcal E }﹩ corresponding to a decrease in a, and vice versa (red arrows). The green shaded region denotes the observable JuMBOs with a > 25 au. Lower: histograms of semimajor axes of captured planets (a cap) from ionized JuMBO pairs.
Paper: Dynamics of Binary Planets within Star Clusters
Authors: Yukun Huang, 宇坤 黄, Wei Zhu, 伟 祝, Eiichiro Kokubo, 保英一郎 小久
Figure caption: Critical timescale t cr (Equation (7)) computed on the b–v ∞ space assuming a solar-mass star. Dashed lines denote the orbital periods of 10 M J JuMBOs with a wide range of semimajor axes a, of which critical flybys lie on the left-hand side. The solid line represents j  h  = 1 (﹩{e}_{h}=\sqrt{2}﹩), which divides the parameter space into the hyperbolic regime (j  h  > 1, above the line) and the near-parabolic regime (j  h  < 1, below the line).
Paper: Dynamics of Binary Planets within Star Clusters
Authors: Yukun Huang, 宇坤 黄, Wei Zhu, 伟 祝, Eiichiro Kokubo, 保英一郎 小久
Figure caption: Hyperbolic trajectory of the binary planet relative to the passing star. Two planets (blue circles) with a total mass m orbit their mutual barycenter (black cross) with the relative semimajor axis a. The periastron distance (closest approach) of the barycenter is denoted as q  h , which is related to the hyperbolic semimajor axis a  h  and eccentricity e  h . The geometry of the flyby trajectory is determined by the impact parameter b, the relative velocity between the binary barycenter and the star at infinity v ∞, and the stellar mass M ⋆.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Comparison between subimage definitions for a black hole with spin a * = 0.9375. Each panel considers the set of n  t  = 0 or n  t  = 1 geodesics and colors the y = 0 plane according to their n  z  (top) or n  θ  (bottom) classification. (Top left) At each point, we select the shortest geodesic connecting that point and an observer at inclination i = 17°. The selected geodesics at each point thus correspond to the n  t  = 0 definition. Regions where the same geodesics would be labeled n  z  = 0 are colored blue. Regions where the geodesics would be considered n  z  = 1 are red. In all panels, hashing indicates that the n  t  classification disagrees with the n  z  or n  θ  classification. (Top second) Similar to the top left panel, but here we select the second-shortest geodesics, i.e., the ones corresponding to the n  t  = 1 definition. Regions where the same geodesics would be considered n  z  = 0, 1, 2 are shown in blue, red, and green, respectively. Points in regions that are the same color in the n  t  = 0 and n  t  = 1 panels have multiple geodesics with the same n  z  classification that connect them to the observer. Emission produced in these regions therefore results in multiple features within the same n  z  subimage. (Bottom left, bottom second) Same as the two top left panels but for the n  θ  definition. (Four right panels) Same as the four left panels but for inclination i = 60°.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: (Left) Vertical (top) and horizontal (bottom) cross sections of the amplitude of the Fourier transform (visibility amplitude) shown in Figure 5 for the total image (dashed black curve), the direct subimage (n = 0; blue), as well as the n = 1 (red) and n = 2 (green) subimages. The curves show the incoherent average (i.e., the average of the visibility amplitude rather than the complex visibility) over about 20,000 snapshots spanning about 10,000 GM/c 3. The shaded bands show the ±2σ deviation across the time series. The variability in the n = 0 subimage is high, which washes out the ringing structure as the locations of the nulls change over time (see, e.g., L. Medeiros et al. 2018). (Right) Vertical and horizontal cross sections of the (self-)correlations (correlation between the flux at zero baseline and the flux at longer baselines with zero time delay) for the same simulation as the left panel. The higher-order subimages show considerably higher (self-)correlation than the direct image.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: Model of interpolation artifacts due to temporal sampling cadence. (Top) Diagram showing location of emitting sphere in snapshots A and B; the diagram shows the fluid state reconstructed by linear interpolation at t = 0.7. The distance between points A and B scales with the velocity of the sphere. (Bottom) Demonstration of how the light curve changes with the sphere velocity. The dip in the scaled flux density becomes more pronounced with increased sphere velocity, resulting in larger errors. The remaining parameters for this sphere model are observing frequency ν = 230 GHz, magnetic field strength B = 10 G, dimensionless electron temperature Θ e  = 10, and pitch angle between the magnetic field and photon wavevector θ = π/3. We assume the plasma density is low enough that the sphere is optically thin.
Paper: Measuring Black Hole Light Echoes with Very Long Baseline Interferometry
Authors: George N. Wong, Lia Medeiros, Alejandro Cárdenas-Avendaño, James M. Stone
Figure caption: (Left) Light curves computed for the same a * = 0.85 GRMHD simulation but sampled with different temporal resolutions (colors). At low temporal resolutions, linear interpolation artifacts due to nonlinearities in the absorption coefficients generate spurious variability and ringing features. At temporal resolutions ≲1 GM/c 3, the effect of the artifacts is subdominant, and the light curve converges. (Right) The PSD of the light curves is on the left. As expected, the low-resolution light curves see considerable excess power (i.e., excess variability) due to the interpolation artifacts and converge at temporal resolutions ≲1 GM/c 3.