adsabs/AstroCLIMB huggingface dataset:
Paper: Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and H.E.S.S. Blazar Observations
Authors: F. Aharonian, J. Aschersleben, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, B. Bi, M. Bouyahiaoui, M. Breuhaus, R. Brose, F. Brun, B. Bruno, T. Bulik, C. Burger-Scheidlin, T. Bylund, S. Caroff, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, M. de Bony, K. Egberts, J.-P. Ernenwein, G. Fichet de Clairfontaine, M. Filipovic, G. Fontaine, M. Füssling, S. Funk, S. Gabici, S. Ghafourizadeh, G. Giavitto, D. Glawion, J. F. Glicenstein, P. Goswami, M.-H. Grondin, L. Haerer, T. L. Holch, M. Holler, D. Horns, M. Jamrozy, F. Jankowsky, V. Joshi, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, R. G. Lang, S. Le Stum, F. Leitl, A. Lemière, J.-P. Lenain, F. Leuschner, T. Lohse, A. Luashvili, I. Lypova, J. Mackey, D. Malyshev, D. Malyshev, V. Marandon, P. Marchegiani, A. Marcowith, G. Martí-Devesa, R. Marx, M. Meyer, A. Mitchell, R. Moderski, L. Mohrmann, A. Montanari, E. Moulin, J. Muller, T. Murach, K. Nakashima, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, S. Panny, M. Panter, R. D. Parsons, G. Peron, D. A. Prokhorov, H. Prokoph, G. Pühlhofer, M. Punch, A. Quirrenbach, P. Reichherzer, A. Reimer, O. Reimer, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, V. Sahakian, D. A. Sanchez, M. Sasaki, F. Schüssler, H. M. Schutte, U. Schwanke, J. N. S. Shapopi, H. Sol, S. Spencer, S. Steinmassl, H. Suzuki, T. Takahashi, T. Tanaka, A. M. Taylor, R. Terrier, C. Thorpe-Morgan, M. Tsirou, N. Tsuji, Y. Uchiyama, C. van Eldik, J. Veh, C. Venter, S. J. Wagner, R. White, A. Wierzcholska, Yu Wun Wong, M. Zacharias, D. Zargaryan, A. A. Zdziarski, S. Zouari, N. Żywucka, M. Meyer
Figure caption: A TS map for the LAT analysis of the ROI around 1ES 0229+200. Point sources within the ROI are marked with plus signs. The 68% containment radii at 1 GeV for the LAT point-spread function for the events with the worst and best angular reconstruction are shown as a dashed and solid circle, respectively. The thin white contour indicates a region where ﹩\sqrt{\mathrm{TS}}=3﹩.
Paper: Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and H.E.S.S. Blazar Observations
Authors: F. Aharonian, J. Aschersleben, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, B. Bi, M. Bouyahiaoui, M. Breuhaus, R. Brose, F. Brun, B. Bruno, T. Bulik, C. Burger-Scheidlin, T. Bylund, S. Caroff, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, M. de Bony, K. Egberts, J.-P. Ernenwein, G. Fichet de Clairfontaine, M. Filipovic, G. Fontaine, M. Füssling, S. Funk, S. Gabici, S. Ghafourizadeh, G. Giavitto, D. Glawion, J. F. Glicenstein, P. Goswami, M.-H. Grondin, L. Haerer, T. L. Holch, M. Holler, D. Horns, M. Jamrozy, F. Jankowsky, V. Joshi, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, R. G. Lang, S. Le Stum, F. Leitl, A. Lemière, J.-P. Lenain, F. Leuschner, T. Lohse, A. Luashvili, I. Lypova, J. Mackey, D. Malyshev, D. Malyshev, V. Marandon, P. Marchegiani, A. Marcowith, G. Martí-Devesa, R. Marx, M. Meyer, A. Mitchell, R. Moderski, L. Mohrmann, A. Montanari, E. Moulin, J. Muller, T. Murach, K. Nakashima, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, S. Panny, M. Panter, R. D. Parsons, G. Peron, D. A. Prokhorov, H. Prokoph, G. Pühlhofer, M. Punch, A. Quirrenbach, P. Reichherzer, A. Reimer, O. Reimer, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, V. Sahakian, D. A. Sanchez, M. Sasaki, F. Schüssler, H. M. Schutte, U. Schwanke, J. N. S. Shapopi, H. Sol, S. Spencer, S. Steinmassl, H. Suzuki, T. Takahashi, T. Tanaka, A. M. Taylor, R. Terrier, C. Thorpe-Morgan, M. Tsirou, N. Tsuji, Y. Uchiyama, C. van Eldik, J. Veh, C. Venter, S. J. Wagner, R. White, A. Wierzcholska, Yu Wun Wong, M. Zacharias, D. Zargaryan, A. A. Zdziarski, S. Zouari, N. Żywucka, M. Meyer
Figure caption: Simulated halo photon flux per solid angle, ﹩{dN}/d{\rm{\Omega }}﹩, integrated above 1 GeV for the best-fit spectrum (see Section 3.2) for 1ES 0229+200. An activity time of ﹩{t}_{\max }={10}^{4}\,﹩ yr and a field strength of B = 3.2 × 10−16 G are assumed. The same 68% containment radius as in Figure 1 is shown for comparison, along with the On region for the H.E.S.S. observations (dotted−dashed circle). The hot spots correspond to individual simulated particles.
Paper: Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and H.E.S.S. Blazar Observations
Authors: F. Aharonian, J. Aschersleben, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, B. Bi, M. Bouyahiaoui, M. Breuhaus, R. Brose, F. Brun, B. Bruno, T. Bulik, C. Burger-Scheidlin, T. Bylund, S. Caroff, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, M. de Bony, K. Egberts, J.-P. Ernenwein, G. Fichet de Clairfontaine, M. Filipovic, G. Fontaine, M. Füssling, S. Funk, S. Gabici, S. Ghafourizadeh, G. Giavitto, D. Glawion, J. F. Glicenstein, P. Goswami, M.-H. Grondin, L. Haerer, T. L. Holch, M. Holler, D. Horns, M. Jamrozy, F. Jankowsky, V. Joshi, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, R. G. Lang, S. Le Stum, F. Leitl, A. Lemière, J.-P. Lenain, F. Leuschner, T. Lohse, A. Luashvili, I. Lypova, J. Mackey, D. Malyshev, D. Malyshev, V. Marandon, P. Marchegiani, A. Marcowith, G. Martí-Devesa, R. Marx, M. Meyer, A. Mitchell, R. Moderski, L. Mohrmann, A. Montanari, E. Moulin, J. Muller, T. Murach, K. Nakashima, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, S. Panny, M. Panter, R. D. Parsons, G. Peron, D. A. Prokhorov, H. Prokoph, G. Pühlhofer, M. Punch, A. Quirrenbach, P. Reichherzer, A. Reimer, O. Reimer, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, V. Sahakian, D. A. Sanchez, M. Sasaki, F. Schüssler, H. M. Schutte, U. Schwanke, J. N. S. Shapopi, H. Sol, S. Spencer, S. Steinmassl, H. Suzuki, T. Takahashi, T. Tanaka, A. M. Taylor, R. Terrier, C. Thorpe-Morgan, M. Tsirou, N. Tsuji, Y. Uchiyama, C. van Eldik, J. Veh, C. Venter, S. J. Wagner, R. White, A. Wierzcholska, Yu Wun Wong, M. Zacharias, D. Zargaryan, A. A. Zdziarski, S. Zouari, N. Żywucka, M. Meyer
Figure caption: TS maps as in Figure 1 for all other considered sources. Again, no significant excess is observed close to any considered source. The additional source in the ROI of 1ES 1101−232 is marked with a lowercase j and its coordinates.
Paper: Constraints on the Intergalactic Magnetic Field Using Fermi-LAT and H.E.S.S. Blazar Observations
Authors: F. Aharonian, J. Aschersleben, M. Backes, V. Barbosa Martins, R. Batzofin, Y. Becherini, D. Berge, B. Bi, M. Bouyahiaoui, M. Breuhaus, R. Brose, F. Brun, B. Bruno, T. Bulik, C. Burger-Scheidlin, T. Bylund, S. Caroff, S. Casanova, J. Celic, M. Cerruti, T. Chand, S. Chandra, A. Chen, J. Chibueze, O. Chibueze, G. Cotter, M. de Bony, K. Egberts, J.-P. Ernenwein, G. Fichet de Clairfontaine, M. Filipovic, G. Fontaine, M. Füssling, S. Funk, S. Gabici, S. Ghafourizadeh, G. Giavitto, D. Glawion, J. F. Glicenstein, P. Goswami, M.-H. Grondin, L. Haerer, T. L. Holch, M. Holler, D. Horns, M. Jamrozy, F. Jankowsky, V. Joshi, I. Jung-Richardt, E. Kasai, K. Katarzyński, R. Khatoon, B. Khélifi, W. Kluźniak, Nu. Komin, K. Kosack, D. Kostunin, R. G. Lang, S. Le Stum, F. Leitl, A. Lemière, J.-P. Lenain, F. Leuschner, T. Lohse, A. Luashvili, I. Lypova, J. Mackey, D. Malyshev, D. Malyshev, V. Marandon, P. Marchegiani, A. Marcowith, G. Martí-Devesa, R. Marx, M. Meyer, A. Mitchell, R. Moderski, L. Mohrmann, A. Montanari, E. Moulin, J. Muller, T. Murach, K. Nakashima, J. Niemiec, S. Ohm, L. Olivera-Nieto, E. de Ona Wilhelmi, S. Panny, M. Panter, R. D. Parsons, G. Peron, D. A. Prokhorov, H. Prokoph, G. Pühlhofer, M. Punch, A. Quirrenbach, P. Reichherzer, A. Reimer, O. Reimer, B. Reville, F. Rieger, G. Rowell, B. Rudak, E. Ruiz-Velasco, V. Sahakian, D. A. Sanchez, M. Sasaki, F. Schüssler, H. M. Schutte, U. Schwanke, J. N. S. Shapopi, H. Sol, S. Spencer, S. Steinmassl, H. Suzuki, T. Takahashi, T. Tanaka, A. M. Taylor, R. Terrier, C. Thorpe-Morgan, M. Tsirou, N. Tsuji, Y. Uchiyama, C. van Eldik, J. Veh, C. Venter, S. J. Wagner, R. White, A. Wierzcholska, Yu Wun Wong, M. Zacharias, D. Zargaryan, A. A. Zdziarski, S. Zouari, N. Żywucka, M. Meyer
Figure caption: Likelihood profiles as a function of the IGMF strength for (a) ﹩{t}_{\max }=10\,\mathrm{yr}﹩, (b) ﹩{t}_{\max }={10}^{4}\,\mathrm{yr}﹩, and (c) ﹩{t}_{\max }={10}^{7}\,\mathrm{yr}﹩. Magnetic field values resulting in differences in the likelihood ﹩-2{\rm{\Delta }}\mathrm{ln}{ \mathcal L }\gt 2.71﹩ (indicated by the gray dotted line) are ruled out at the 95% confidence level, which is shown by the gray shaded region and arrow. The likelihood curves are smoothed using a quadratic spline interpolation.
Paper: PPDONet: Deep Operator Networks for Fast Prediction of Steady-state Solutions in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Lu Lu, Kwang Moo Yi, Sifan Wang, Paris Perdikaris
Figure caption: Empirical relationships for disk morphology. (a) presents the gap depth Σgap as a function of α, h 0, and q; (b) shows the gap width Δgap against α, h 0, and q; and (c) depicts the amplitudes of perturbed rotational velocity Δδ v  θ  against the dimensionless parameter K ≡ q 2 h 0 −5 α −1.
Paper: PPDONet: Deep Operator Networks for Fast Prediction of Steady-state Solutions in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Lu Lu, Kwang Moo Yi, Sifan Wang, Paris Perdikaris
Figure caption: PPDONet architecture used in this work. A fully connected subnetwork, called “branch network,” encodes scalar parameters, the disk and planet properties, while another fully connected subnetwork, called “trunk network,” encodes the coordinates. We produce the inputs x  i , i = 1,…,d, d = 50, for the third network (“Z network”) by element-wise multiplication of the outputs from the branch and trunk networks. The Z network is a fully connected single-hidden-layer network whose output represents surface density or velocity. The σ in blue nodes are neurons in layers.
Paper: PPDONet: Deep Operator Networks for Fast Prediction of Steady-state Solutions in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Lu Lu, Kwang Moo Yi, Sifan Wang, Paris Perdikaris
Figure caption: Two-dimensional comparisons of predicted surface density and velocity distribution. Case 1: ﹩\left(\alpha ,{h}_{0},q\right)=\left(0.013,0.092,6.0\times {10}^{-4}\right)﹩. Case 2: ﹩\left(\alpha ,{h}_{0},q\right)=\left(5.2\times {10}^{-4},0.053,1.6\times {10}^{-3}\right)﹩. Left (a), (c), and (e): ground truth generated from FARGO3D simulations. Middle (b), (d), and (f): Neural network predictions. For the two left columns, we subtract the initial value from the two velocities to highlight the perturbations. Two right columns: Differences or ratios. Surface density differences are measured by the ratio Σpred/Σtruth, so that the gap region is highlighted. Velocity differences are shown in absolute errors.
Paper: Is the Large-scale Structure Traced by the BOSS LOWZ Galaxies Consistent with Planck?
Authors: Zhiwei Shao, Ying Zu, Huanyuan Shan
Figure caption: Cross-correlation matrix ﹩{ \mathcal Q }﹩. The size of each circle corresponds to the value of the cross-correlation coefficient r gg between two stellar mass bins, indicated by the four circles on the right. Filled circles represent near-perfect correlations with r gg ≥ 0.95. The black solid curve on top shows the stellar mass distribution of the LOWZ galaxies, with the black dashed line indicating the stellar mass limit (﹩\mathrm{log}{M}_{* }=11.3﹩) of our C-LOWZ sample selection.
Paper: PPDONet: Deep Operator Networks for Fast Prediction of Steady-state Solutions in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Lu Lu, Kwang Moo Yi, Sifan Wang, Paris Perdikaris
Figure caption: Comparison of prediction errors for neural networks trained with different data set sizes. The four columns represent networks trained on data set sizes of 64 (leftmost column), 128, 256, and 488 (rightmost column) samples, respectively. The representative cases and difference calculation methodology correspond to those utilized in Figure 2.
Paper: PPDONet: Deep Operator Networks for Fast Prediction of Steady-state Solutions in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Lu Lu, Kwang Moo Yi, Sifan Wang, Paris Perdikaris
Figure caption: Gap profile comparison for one example case with α = 5.2 × 10−4, h 0 = 0.053, and q = 1.6 × 10−3. Blue: ground truth from FARGO3D. Red: PPDONet prediction. Bottom panel: the ratio between the two.
Paper: PPDONet: Deep Operator Networks for Fast Prediction of Steady-state Solutions in Disk–Planet Systems
Authors: Shunyuan Mao, 顺元 毛, Ruobing Dong, 若冰 董, Lu Lu, Kwang Moo Yi, Sifan Wang, Paris Perdikaris
Figure caption: Comparison of test errors for neural networks trained using training data set with different sizes. The three columns represent networks trained for surface density (left), radial velocity (middle), and azimuthal velocity (right), respectively. We calculate the losses using the method described in Section 3.2.
Paper: Is the Large-scale Structure Traced by the BOSS LOWZ Galaxies Consistent with Planck?
Authors: Zhiwei Shao, Ying Zu, Huanyuan Shan
Figure caption: Left: comparison of the projected clustering of C-LOWZ galaxies between the measurements (circles with error bars) and the best-fitting linear model prediction (solid curve) on scales 10 < R < 30 h −1Mpc (within the vertical dashed lines). The constraint on the product of b g A is shown by the horizontal band in the bottom panel. Middle: similar to the left panel but for the g–g lensing signal ϒgm. Right: joint posterior distribution of b g and A derived from combining the clustering and g–g lensing of C-LOWZ galaxies. Contours indicate the 68% and 95% 2D confidence regions, with the marginalized 1σ constraints listed in the bottom left.
Paper: Is the Large-scale Structure Traced by the BOSS LOWZ Galaxies Consistent with Planck?
Authors: Zhiwei Shao, Ying Zu, Huanyuan Shan
Figure caption: Constraints on the three parameters of the linear assessment model from our fiducial Bayesian analysis using the b g prior (dark, filled contours/histograms). Light, open contours/histograms show the constraints from the previous analysis without the b g prior. Contours in the off-diagonal panels indicate the 68% and 95% confidence regions on the 2D plane, while histograms in the diagonal panels show the 1D posterior distributions of individual parameters, with thin dashed curves in the b g and r gm panels representing the Gaussian priors. The two sets of 1σ posterior constraints are listed in the top right.
Paper: Is the Large-scale Structure Traced by the BOSS LOWZ Galaxies Consistent with Planck?
Authors: Zhiwei Shao, Ying Zu, Huanyuan Shan
Figure caption: Cluster-based bias measurement for the C-LOWZ galaxies (right panel) from the combination of cluster-galaxy cross correlation (left) and cluster weak lensing (middle). The formats of the left and middle panels are the same as in Figure 2. In the right panel, star symbols with error bars represent the ratio calculated using Equation (18), from which we derive ﹩{b}_{{\rm{g}}}^{\mathrm{clusters}}=1.76\pm 0.22﹩ (green horizontal band). Gray hexagon with error bar indicates the bias constraint (﹩{2.47}_{-0.30}^{+0.36}﹩) from the right panel of Figure 2.
Paper: Is the Large-scale Structure Traced by the BOSS LOWZ Galaxies Consistent with Planck?
Authors: Zhiwei Shao, Ying Zu, Huanyuan Shan
Figure caption: Comparison between galaxy biases measured from the cluster-based method (green vertical band), galaxy clustering (blue circles), and g–g lensing (red squares), under four different cosmologies, including Planck (A = 1.0), two low-σ 8 cosmologies with A = 0.9 and 0.8, and a representative low-S 8 cosmology that resolves the clustering–lensing mismatch. Filled (open) red squares are the ﹩{b}_{{\rm{g}}}^{\mathrm{lensing}}﹩ estimates when assuming r gm = 1 (0.95).
Paper: New Observations of Solar Wind 1/f Turbulence Spectrum from Parker Solar Probe
Authors: Zesen Huang, 泽森 黄, Nikos Sioulas, Chen Shi, 辰 时, Marco Velli, Trevor Bowen, Nooshin Davis, B. D. G. Chandran, Lorenzo Matteini, Ning Kang, 宁 康, Xiaofei Shi, 晓霏 石, Jia Huang, 佳 黄, Stuart D. Bale, J. C. Kasper, Davin E. Larson, Roberto Livi, P. L. Whittlesey, Ali Rahmati, Kristoff Paulson, M. Stevens, A. W. Case, Thierry Dudok de Wit, David M. Malaspina, J. W. Bonnell, Keith Goetz, Peter R. Harvey, Robert J. MacDowall
Figure caption: Example of a magnetically incompressible solar wind interval from PSP Encounter 10, close to the perihelion. The particle data of this interval are provided by SPAN (Livi et al. 2022). Right: Panels (a1)–(a5) show time series of magnetic field B rtn in radial, tangential, and normal coordinates; solar wind speed V SW and solar wind thermal speed V th; cross helicity σ  c  and plasma beta β; proton density n  p  and Carrington longitude; and heliocentric distance R in solar radii R ⊙ and advection time t adv = R/V SW, respectively. The selected interval is indicated with the red shaded area enclosed by two red dashed lines. Left: (b) Power-law fitting index α as a function of frequency f of trace PSD. (c) Fast Fourier transformation (FFT) is plotted in blue as background; smoothed FFT PSD is the green line; and Morlet wavelet transformation (WL) PSD is the orange line. The two pairs of red crosses accompanied by red and green shaded areas indicate the ranges of frequency over which the power-law fits are applied, and the two fitted lines are shown in dashed and dashed–dotted lines. The gray shaded area is the frequency range where more than 70% of points fall out of the cone of influence (CoI) of wavelet transformation. The red dashed line indicates the intersection of two fitted lines, interpreted as the low-frequency break point. (d) Power-law fitting index β as a function of frequency f of the normalized SF. (e) Normalized first-order SF 〈δ B/B〉 as a function of frequency f = 1/(2*Δt), where Δt is the temporal increment. Two fits are applied to the same frequency ranges from (c), which produce a similar low-frequency break point, indicated by the green dashed line.
Paper: New Observations of Solar Wind 1/f Turbulence Spectrum from Parker Solar Probe
Authors: Zesen Huang, 泽森 黄, Nikos Sioulas, Chen Shi, 辰 时, Marco Velli, Trevor Bowen, Nooshin Davis, B. D. G. Chandran, Lorenzo Matteini, Ning Kang, 宁 康, Xiaofei Shi, 晓霏 石, Jia Huang, 佳 黄, Stuart D. Bale, J. C. Kasper, Davin E. Larson, Roberto Livi, P. L. Whittlesey, Ali Rahmati, Kristoff Paulson, M. Stevens, A. W. Case, Thierry Dudok de Wit, David M. Malaspina, J. W. Bonnell, Keith Goetz, Peter R. Harvey, Robert J. MacDowall
Figure caption: (a) Histogram of power-law fit index β of the normalized first-order SF from both low- (blue) and MHD- (red) frequency ranges. The averages are indicated with corresponding dashed lines. (b) Scatters of power-law fit index pairs (α, β) of trace PSD and SF from both low- (blue) and MHD- (red) frequency ranges. The (α, β) pairs from artificial data are also shown with black crosses, and the theoretical relation α = 2β −1 is indicated with black dashed line. (c) Dependence of 〈δ B/B〉 from the saturated intervals (β Low > −0.07) on heliocentric distance R. The value ranges of 〈δ B/B〉 in the low-frequency range are indicated with error bars. The newly explored heliosphere radial range (R < 0.3 au) is indicated with red shaded area.
Paper: New Observations of Solar Wind 1/f Turbulence Spectrum from Parker Solar Probe
Authors: Zesen Huang, 泽森 黄, Nikos Sioulas, Chen Shi, 辰 时, Marco Velli, Trevor Bowen, Nooshin Davis, B. D. G. Chandran, Lorenzo Matteini, Ning Kang, 宁 康, Xiaofei Shi, 晓霏 石, Jia Huang, 佳 黄, Stuart D. Bale, J. C. Kasper, Davin E. Larson, Roberto Livi, P. L. Whittlesey, Ali Rahmati, Kristoff Paulson, M. Stevens, A. W. Case, Thierry Dudok de Wit, David M. Malaspina, J. W. Bonnell, Keith Goetz, Peter R. Harvey, Robert J. MacDowall
Figure caption: Example of C18 type of trace z + spectrum. The FFT spectrum is shown with blue line as background, the smoothed FFT is the green line, and the trace Morlet Wavelet (WL) PSD is the orange line. The gray shaded area indicates that more than 70% of points fall out of the Cone of Influence (CoI) of WL. The power-law fit is conducted on the smoothed FFT, and the moving window fit α(f) (window sized 1/3 decade) is shown in the overhead panel. The trace PSD is separated into three distinct frequency ranges (low, mid, MHD); each possesses a quasi-steady power-law range, indicated with red (low), blue (mid), and green (MHD) shaded areas. Power-law fits are applied to each of the ranges, and the fit indices α Low/Mid/MHD are shown in the legends. A “low-frequency break” is found as the intersection between the power-law fits from low-frequency and MHD-inertial ranges, indicated with orange dashed line.
Paper: New Observations of Solar Wind 1/f Turbulence Spectrum from Parker Solar Probe
Authors: Zesen Huang, 泽森 黄, Nikos Sioulas, Chen Shi, 辰 时, Marco Velli, Trevor Bowen, Nooshin Davis, B. D. G. Chandran, Lorenzo Matteini, Ning Kang, 宁 康, Xiaofei Shi, 晓霏 石, Jia Huang, 佳 黄, Stuart D. Bale, J. C. Kasper, Davin E. Larson, Roberto Livi, P. L. Whittlesey, Ali Rahmati, Kristoff Paulson, M. Stevens, A. W. Case, Thierry Dudok de Wit, David M. Malaspina, J. W. Bonnell, Keith Goetz, Peter R. Harvey, Robert J. MacDowall
Figure caption: (a) Histograms of power-law fit index α of low-frequency (blue) and magnetohydrodynamics (MHD) frequency (red) ranges. The averaged index values are indicated with corresponding dashed lines and are shown in the legends. The expected power spectral exponent value range from various phenomenologies is indicated with red shaded area. (b) Statistics of length and mean radial distance of the selected 109 intervals. (c) Histogram of interval lengths. The average length is 13.72 hr (shown as legend accompanied by dashed line), with minimum of 1.08 hr and maximum of 64.70 hr.
Paper: New Observations of Solar Wind 1/f Turbulence Spectrum from Parker Solar Probe
Authors: Zesen Huang, 泽森 黄, Nikos Sioulas, Chen Shi, 辰 时, Marco Velli, Trevor Bowen, Nooshin Davis, B. D. G. Chandran, Lorenzo Matteini, Ning Kang, 宁 康, Xiaofei Shi, 晓霏 石, Jia Huang, 佳 黄, Stuart D. Bale, J. C. Kasper, Davin E. Larson, Roberto Livi, P. L. Whittlesey, Ali Rahmati, Kristoff Paulson, M. Stevens, A. W. Case, Thierry Dudok de Wit, David M. Malaspina, J. W. Bonnell, Keith Goetz, Peter R. Harvey, Robert J. MacDowall
Figure caption: (a) Radial evolution of low-frequency power-law fit index α Low, sorted with advection time (t adv = R/V SW). The sizes of the circles indicate the interval length (weight), and the line plot is the binned weighted average of α Low. The error bars are 1 standard error of α Low from each bin. (b) Radial evolution of α Low sorted with heliocentric distance R. (c) Dependence of α Low on solar wind speed V SW.
Paper: Distance Duality Test: The Evolution of Radio Sources Mimics a Nonexpanding Universe
Authors: Pengfei Li
Figure caption: The median values of the calibrated angular size vs. redshift. Left: the total 613 data points are nearly equally populated into 34 bins. Right: 330 data points are distributed into 19 bins (18 sources within each bin for the first 17 redshift bins and 12 sources within each bin for the remaining 2 bins at high redshift). The uncertainties on the median angular size and redshift are estimated according to ﹩{\sigma }_{\mathrm{med}}=1.2533\tfrac{\sigma }{\sqrt{N}}﹩, where σ is the scatter around the mean value and N is the sample size within each bin. The predictions of the expanding and nonexpanding universes are presented as the solid and dashed lines, respectively.