adsabs/AstroCLIMB huggingface dataset:
Paper: Efficient and Accurate Force Replay in Cosmological-baryonic Simulations
Authors: Arpit Arora, Robyn Sanderson, Christopher Regan, Nicolás Garavito-Camargo, Emily Bregou, Nondh Panithanpaisal, Andrew Wetzel, Emily C. Cunningham, Sarah R. Loebman, Adriana Dropulic, Nora Shipp
Figure caption: Recovering tidal evolution in the potential model. Tidal disruption of a dwarf satellite with M ⋆ = 107  M ⊙ identified in N. Panithanpaisal et al. (2021) in the live simulation (first and third rows) and in the time-evolving potential model (second and fourth rows) over a period of 7.2 Gyr of evolution (arranged in columns from left to right), color-coded by a star’s stripping times. The top two rows show the stream’s distribution in the X–Z plane at different times. The bottom two rows present the phase-space distribution (radial velocity vs. distance from the center). Reconstructed streams demonstrate excellent recovery of the stream’s structure and kinematics.
Paper: Efficient and Accurate Force Replay in Cosmological-baryonic Simulations
Authors: Arpit Arora, Robyn Sanderson, Christopher Regan, Nicolás Garavito-Camargo, Emily Bregou, Nondh Panithanpaisal, Andrew Wetzel, Emily C. Cunningham, Sarah R. Loebman, Adriana Dropulic, Nora Shipp
Figure caption: Performance over multiple orbital periods. Relative position error at the final time step of integration (approximately 3.8 Gyr) vs. the total integration time in terms of the number of periods passed for each orbit. Orbits are color-coded by the average distance from the center for each star. About 70% of orbits have a relative error below 1 at the end of the integration time. Most orbits with ﹩\tfrac{{\rm{\Delta }}r}{r}\geqslant 1﹩ are integrated over ≥10 periods and are located close to the center of the host. The bound stars identified from Figure 5, which are expected to have larger error due to their unmodeled progenitor galaxy, are shown with gray markers.
Paper: Efficient and Accurate Force Replay in Cosmological-baryonic Simulations
Authors: Arpit Arora, Robyn Sanderson, Christopher Regan, Nicolás Garavito-Camargo, Emily Bregou, Nondh Panithanpaisal, Andrew Wetzel, Emily C. Cunningham, Sarah R. Loebman, Adriana Dropulic, Nora Shipp
Figure caption: Quality of orbits with lower temporal cadence. Fraction of orbits with error below the ranges marked with colors in recovered property: total angular momentum J tot (top row), total energy E tot (middle row), and positional error metric ﹩\tfrac{{\rm{\Delta }}r}{r}﹩ (bottom row) as a function of how frequently the potential is sampled for an orbit integration of 4 Gyr. J tot and E tot can be accurately recovered with higher sampling intervals (less frequent snapshots), with significant deterioration only observed at a 500 Myr sampling interval. ﹩\tfrac{{\rm{\Delta }}r}{r}﹩ is more sensitive, showing noticeable decrease at a 100 Myr sampling interval.
Paper: The Second Case of a Major Merger Triggering a Starburst in a Green Pea Galaxy
Authors: S. Purkayastha, N. Kanekar, S. Kumari, J. Rhoads, S. Malhotra, J. Pharo, T. Ghosh
Figure caption: (A) (left panel) VLA H I intensity image of the field of GP J1148+2546, at a resolution of 14″ × 12″. The locations of GP J1148+2546 and its two companions are indicated by the star, the “X,” and the “+” symbols, respectively. (B) (right panel) The VLA H I intensity image (in contours) overlaid on the DECaLS g-band image (in color). The contour levels are [−3.0, 3.0, 4.0, 5.0, 6.0, 7.0, 8.0] × σ, where σ = 0.045 Jy Beam−1 km s−1 is the rms noise on the image, corresponding to a H I column density of 3.1 × 1020 cm−2. The locations of GP J1148+2546 and its companions are indicated by the labels GP, G1, and G2 (and the possible third companion by G3). In both panels, the coordinates are relative to the J2000 coordinates of GP J1148+2546.
Paper: The Second Case of a Major Merger Triggering a Starburst in a Green Pea Galaxy
Authors: S. Purkayastha, N. Kanekar, S. Kumari, J. Rhoads, S. Malhotra, J. Pharo, T. Ghosh
Figure caption: (A) The VLA H I 21 cm spectrum of GP J1148+2546 (blue), overlaid on the Arecibo single-dish spectrum (red); the two are seen to be in excellent agreement. Note that the VLA spectrum includes H I 21 cm emission from the entire region surrounding the Green Pea, including the two companions and the extended H I 21 cm emission seen in Figure 1(A). (B) The VLA H I 21 cm spectrum from the region immediately around GP J1148+2546, indicated by the circle in Figure 1(A).
Paper: The Second Case of a Major Merger Triggering a Starburst in a Green Pea Galaxy
Authors: S. Purkayastha, N. Kanekar, S. Kumari, J. Rhoads, S. Malhotra, J. Pharo, T. Ghosh
Figure caption: (A) The H I velocity field (i.e., the moment-1 image) of GP J1148+2546 and the surrounding region, at a resolution of 14″ × 12″. (B) The H I velocity dispersion (i.e., the moment-2 image) . The highest velocity dispersion is seen to arise in the region between galaxies G1 and G2. In both panels, the coordinates are relative to the J2000 coordinates of GP J1148+2546, and the locations of GP J1148+2546 and its two companions are indicated by the star, the “X,” and the “+” symbols, respectively.
Paper: The Second Case of a Major Merger Triggering a Starburst in a Green Pea Galaxy
Authors: S. Purkayastha, N. Kanekar, S. Kumari, J. Rhoads, S. Malhotra, J. Pharo, T. Ghosh
Figure caption: The VLA 1.36 GHz continuum image of the field of GP J1148+2546 (in contours), overlaid on the DECaLS g-band image (in color). The contour levels are [−3.0, 3.0, 4.2, 6.0, 8.4, 12.0, 16.8, 24.0, 33.6, 48.0, 67.2] × σ, where σ = 36 μJy Beam−1 is the rms noise on the VLA 1.36 GHz continuum image. The locations of GP J1148+2546 and its companions are indicated by the labels GP, G1, and G2 (and the possible third companion by G3). The coordinates are relative to the J2000 coordinates of GP J1148+2546.
Paper: The Second Case of a Major Merger Triggering a Starburst in a Green Pea Galaxy
Authors: S. Purkayastha, N. Kanekar, S. Kumari, J. Rhoads, S. Malhotra, J. Pharo, T. Ghosh
Figure caption: The contours show the channel maps at a velocity resolution of 10 km s−1 of the uniformly weighted cube, at an angular resolution of 14.″0 × 12.″0. The velocity-integrated H I 21 cm line flux density image is shown in color scale in all panels for comparison. The channel velocities are marked at the top left of each panel. The contours are at (−3.0, 3.0, 4.0, 5.0, 6.0) × σ significance, where σ = 0.76 mJy Beam−1 is the per-channel rms noise.
Paper: The Second Case of a Major Merger Triggering a Starburst in a Green Pea Galaxy
Authors: S. Purkayastha, N. Kanekar, S. Kumari, J. Rhoads, S. Malhotra, J. Pharo, T. Ghosh
Figure caption: A position–velocity (P–V) slice across galaxies G1 and G2, and the region in between. The location of the slice is indicated by the two dashed black lines in the left panel (A), overlaid on the velocity-integrated H I 21 cm flux density image. The offset increases from southeast to northwest, i.e., from G2 to G1. The right panel (B) shows the resulting P–V diagram: it is clear that the central region, between galaxies G1 and G2 (at an offset of ≈0″) contains emission at two velocities, ≈−150 km s−1, and ≈+90 km s−1.
Paper: The Second Case of a Major Merger Triggering a Starburst in a Green Pea Galaxy
Authors: S. Purkayastha, N. Kanekar, S. Kumari, J. Rhoads, S. Malhotra, J. Pharo, T. Ghosh
Figure caption: The HST COS spectrum of GP1148+2546 (HST prog. 15840; D. A. Berg et al. 2022), zooming in on the redshifted Lyα line. The narrow Lyα emission (also shown in the inset figure) and the wide damping wings are clearly visible. The blue/cyan dashed curve shows the Voigt profile fit to the damped Lyα absorption.
Paper: The Second Case of a Major Merger Triggering a Starburst in a Green Pea Galaxy
Authors: S. Purkayastha, N. Kanekar, S. Kumari, J. Rhoads, S. Malhotra, J. Pharo, T. Ghosh
Figure caption: (A) The SDSS spectrum of GP J1148+2546, showing extreme emission lines, especially [O III]λ5007. (B) The SDSS spectrum of galaxy G1, showing strong Hα, Hβ, and [O II]λ3727 emission lines, indicative of a normal star-forming galaxy.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: The network structure of the SynNN. The SmallNet component in the model structure consists of three linear layers with inputs of 200, 1000, and 400 units, respectively, and concludes with a layer that uses a convolutional kernel size of 5. The activation function for each layer is the ReLU. SynNN takes eight parameters as input and outputs four separate 56-dimensional signals for the Stokes I, Q, U, and V profiles, resulting in a total output of 224 dimensions.
Paper: Mining for Protoclusters at z ∼ 4 from Photometric Data Sets with Deep Learning
Authors: Yoshihiro Takeda, Nobunari Kashikawa, Kei Ito, Jun Toshikawa, Rieko Momose, Kent Fujiwara, Yongming Liang, Rikako Ishimoto, Takehiro Yoshioka, Junya Arita, Mariko Kubo, Hisakazu Uchiyama
Figure caption: (Left) Distribution of i-band magnitude of protocluster member galaxies that were detected by PCFNet (green; Detected), nonmember field galaxies (blue; Field), and actual protocluster member galaxies (pink; Actual) at z ∼ 4 in PCcone. (Right) Similar to the left but in observational data. The blue line represents the distribution of field galaxies not detected as protocluster member galaxies (Field), and the green line represents the distribution of protocluster member galaxies detected by PCFNet (Detected). The pink line shows the distribution corrected for model bias using Equation (15) (Corrected) and the distribution of field galaxies (Field ×4) multiplied by 4.0 to match the scale on the faint side. The error bars of each line indicate Poisson errors. The curves in both upper figures are pdfs for each normalized distribution.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: The MAE between the SynNN-predicted and true synthetic Stokes profiles in the 100,000 test set. The three orange dashed lines represent statistical values corresponding to the 16th, 50th, and 84th percentiles of the residual distribution. These lines indicate the lower error bound, median, and upper error bound of the residuals, as shown in the figure’s title. The unit of MAE is the continuum intensity.
Paper: Mining for Protoclusters at z ∼ 4 from Photometric Data Sets with Deep Learning
Authors: Yoshihiro Takeda, Nobunari Kashikawa, Kei Ito, Jun Toshikawa, Rieko Momose, Kent Fujiwara, Yongming Liang, Rikako Ishimoto, Takehiro Yoshioka, Junya Arita, Mariko Kubo, Hisakazu Uchiyama
Figure caption: Comparison of PR curves between different brightnesses (left: i ≤ 24.5; right: i > 24.5 ) in PCcone. The orange, blue, and yellow lines represent the PR curve of PCFNet, the 2DBM, and the 3DBM, respectively. The PR curves for all galaxies in Figure 6 are also shown as dotted lines. Note that the 2.5σ threshold indicated by the orange star with black lines is calculated from all galaxies.
Paper: Mining for Protoclusters at z ∼ 4 from Photometric Data Sets with Deep Learning
Authors: Yoshihiro Takeda, Nobunari Kashikawa, Kei Ito, Jun Toshikawa, Rieko Momose, Kent Fujiwara, Yongming Liang, Rikako Ishimoto, Takehiro Yoshioka, Junya Arita, Mariko Kubo, Hisakazu Uchiyama
Figure caption: Distribution of the stellar mass, SFR, and sSFR of protocluster members at z ∼ 4 in the simulation data. The legend of colors is the same as in the left panel of Figure 12.
Paper: Mining for Protoclusters at z ∼ 4 from Photometric Data Sets with Deep Learning
Authors: Yoshihiro Takeda, Nobunari Kashikawa, Kei Ito, Jun Toshikawa, Rieko Momose, Kent Fujiwara, Yongming Liang, Rikako Ishimoto, Takehiro Yoshioka, Junya Arita, Mariko Kubo, Hisakazu Uchiyama
Figure caption: CWQ fraction as a function of halo mass at z = 0 and 4 in the simulation data. The error bars indicate the Poisson error in each bin. Note that the fraction of core galaxies associated with QGs relative to the halo mass at z = 0 inclines more gradually with error than the others. For this reason, the number of bins is reduced to three in the figure.
Paper: Mining for Protoclusters at z ∼ 4 from Photometric Data Sets with Deep Learning
Authors: Yoshihiro Takeda, Nobunari Kashikawa, Kei Ito, Jun Toshikawa, Rieko Momose, Kent Fujiwara, Yongming Liang, Rikako Ishimoto, Takehiro Yoshioka, Junya Arita, Mariko Kubo, Hisakazu Uchiyama
Figure caption: 2D distribution of halo masses at z = 0 and z = 4 of CWQs in the simulation data. The color of the background represents the CWQ fraction. The white dots represent the CWQs.
Paper: Intergalactic Medium Rotation Measure of Primordial Magnetic Fields
Authors: Salome Mtchedlidze, Paola Domínguez-Fernández, Xiaolong Du, Ettore Carretti, Franco Vazza, Shane Patrick O'Sullivan, Axel Brandenburg, Tina Kahniashvili
Figure caption: Redshift evolution of the RMIGM of different PMF models (our main runs, 1 nG normalization). The black and gray lines show observed trends of RM rms from E. Carretti et al. (2023) when using 60 and 15 sources per redshift bin (the LoTSS data), respectively. The light green-dashed and dotted lines show theoretical estimations for Hubble- (∼4200 Mpc) and Jeans-scale (2.3 Mpc) magnetic fields from M. S. Pshirkov et al. (2016). In this latter work, magnetic fields were calculated from the density field, the redshift dependence of which was drawn from a lognormal distribution.
Paper: Intergalactic Medium Rotation Measure of Primordial Magnetic Fields
Authors: Salome Mtchedlidze, Paola Domínguez-Fernández, Xiaolong Du, Ettore Carretti, Franco Vazza, Shane Patrick O'Sullivan, Axel Brandenburg, Tina Kahniashvili
Figure caption: Redshift evolution of the RMIGM of the scale-invariant (km1) PMF model. In the bottom panel, we show the RM-rms trends (dashed–dotted lines) for the whole LOS; in the top panel, we show RM-rms trends for different initial normalizations of the magnetic field, 0.01 nG (pink solid) and 0.1 nG (pink dashed lines), and those using Equation (5) (densely dotted lines) for different ranges of magnetic field strength (<1 nG).
Paper: Intergalactic Medium Rotation Measure of Primordial Magnetic Fields
Authors: Salome Mtchedlidze, Paola Domínguez-Fernández, Xiaolong Du, Ettore Carretti, Franco Vazza, Shane Patrick O'Sullivan, Axel Brandenburg, Tina Kahniashvili
Figure caption: RM (first three rows from the top) and density (last row) maps for different redshift depths as are seen by an observer at z = 0 with a 2° FOV. The RM maps for the regions excluding galaxy clusters (referred to as RMIGM) are shown in the first and second rows for the k25 and scale-invariant models, respectively; the third row shows the RM for the whole LOS for the scale-invariant case.
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption: Same as Figure 9, but for the mixed jet model.
Paper: Intergalactic Medium Rotation Measure of Primordial Magnetic Fields
Authors: Salome Mtchedlidze, Paola Domínguez-Fernández, Xiaolong Du, Ettore Carretti, Franco Vazza, Shane Patrick O'Sullivan, Axel Brandenburg, Tina Kahniashvili
Figure caption: The initial (z = 50) magnetic power spectra for the stochastic setups (black lines) with respect to the initial conditions used in Paper I (low-opacity lines).
Paper: Intergalactic Medium Rotation Measure of Primordial Magnetic Fields
Authors: Salome Mtchedlidze, Paola Domínguez-Fernández, Xiaolong Du, Ettore Carretti, Franco Vazza, Shane Patrick O'Sullivan, Axel Brandenburg, Tina Kahniashvili
Figure caption: RM (two-dimensional) power spectra for different PMF models at z = 2 (solid) and z = 0.494 (dashed) redshift depths. For the k102 model, we also show the total (without excluding any regions) RM power spectra integrated up to z = 2.0 redshift depth (dotted lines).
Paper: Intergalactic Medium Rotation Measure of Primordial Magnetic Fields
Authors: Salome Mtchedlidze, Paola Domínguez-Fernández, Xiaolong Du, Ettore Carretti, Franco Vazza, Shane Patrick O'Sullivan, Axel Brandenburg, Tina Kahniashvili
Figure caption: RM rms growth factors (relative to RM rms obtained for 1 nG normalization) for the km1, k25, k50, and k102 cases. The inset panel shows the density PDFs with dashed lines PDFs from the 50 nG normalizations (km1 and k102 cases). The units of the x-axis in the inset are in grams per cubic centimeter.
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption: Same as Figure 9, but for the Gaussian jet model.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: Long-term light curves of 3C 454.3 at 4.8, 8.0, 14.5, 22, and 37 GHz during 1979–2013. The dashed blue line divides the light curves into Segments 1 and 2.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: Upper panel: Generalized Lomb–Scargle periodogram for the whole light curve (left) and Segment 1 (right) at 4.8 GHz. The blue dashed curves respectively denote 3σ significance using a broken power law as the underlying red-noise model. Lower panel: Wavelet analysis for the entire light curve (left) and Segment 1 (right). In each panel, the left plot is the color–color diagram showing the WWZ power, where red denotes the most concentrated power, and the power decreases toward violet and black. The right plot shows the time-averaged WWZ along with 3σ significance given by the dashed blue curve.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: As in Figure 3 for the 14.5 GHz light curve. The dashed–dotted brown line in the GLSP plot of Segment 1 marks the possible QPO period at around 600 days.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: As in Figure 3 for the 22 GHz light curve. The dashed–dotted brown line in the GLSP plot of Segment 1 marks the possible QPO period at around 600 days.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: As in Figure 3 for the 8 GHz light curve.
Paper: Revisiting Radio Variability of the Blazar 3C 454.3
Authors: Ashutosh Tripathi, Alok C. Gupta, Krista Lynne Smith, Paul J. Wiita, Margo F. Aller, Alexandr E. Volvach, Anne Lähteenmäki, Hugh D. Aller, Merja Tornikoski, Larisa N. Volvach
Figure caption: Flux distribution histograms for the light at radio frequencies at 4.8, 8.0, 14.5, 22.0, and 37.0 GHz and their best fits with log-normal and normal distribution.
Paper: Proton Acceleration in Low-β Magnetic Reconnection with Energetic Particle Feedback
Authors: Jeongbhin Seo, Fan Guo, Xiaocan Li, Hui Li
Figure caption: Left panels: The distribution of out-of-plane current density, j  z , at (a) t/τ  A  = 3.2, (b) 7.8, and (c) 10 for the CASE2 (R  i  = ρ NT,i /ρ 0 = 0.1), respectively. Middle panels: The distribution of plasma density, ρ  g , at (d) t/τ  A  = 3.2, (e) 7.8, and (f) 10 for the same case. Right panels: The distribution of nonthermal particle density, ρ NT, at (g) t/τ  A  = 3.2, (h) 7.8, and (i) 10 for the same case.
Paper: Proton Acceleration in Low-β Magnetic Reconnection with Energetic Particle Feedback
Authors: Jeongbhin Seo, Fan Guo, Xiaocan Li, Hui Li
Figure caption: (a) The time evolution of the energy spectrum of nonthermal protons across the entire domain for the CASE2. Colors indicate different time steps. Dashed lines indicate the slope of the saturated spectrum. (b) The energy spectra of three cases at t/τ  A  = 10 for CASE1 (red), CASE2 (green), and CASE3 (blue). Dashed lines indicate the slope of the power law.
Paper: Realistic Outcomes of Moon–Moon Collisions in Lunar Formation Theory
Authors: Uri Malamud, Hagai B. Perets
Figure caption: Resolution convergence tests for scenarios 20_2 (dark lines) and 20f_143 (light lines). The mass of the largest fragment M lr (a) and its rotation period P lr (b) are shown as a function of time. Different resolutions are marked by various line textures shown in the legend.
Paper: Proton Acceleration in Low-β Magnetic Reconnection with Energetic Particle Feedback
Authors: Jeongbhin Seo, Fan Guo, Xiaocan Li, Hui Li
Figure caption: Time evolution of the plasma density probability distributions function for the (a) CASE1, (b) CASE2, and (c) CASE3. The plasma density is normalized by the initial values in each simulation.
Paper: Proton Acceleration in Low-β Magnetic Reconnection with Energetic Particle Feedback
Authors: Jeongbhin Seo, Fan Guo, Xiaocan Li, Hui Li
Figure caption: (Left) Computational performance vs. the number of particles per cell, which is defined as the computational time divided by the total number of cells and the number of MHD cycles. Red, blue, and green colors indicate tests performed in 1D, 2D, and 3D, respectively. The dashed lines represent the performance with only solving MHD, with the dimension indicated by the respective color code. (Right) Weak scaling comparison between only MHD (red) and MHD with the SDE method (blue).
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: The X-ray light curves of the GRBs in our sample. GRB 060202 and GRB 180620A are the Gold samples, GRB 050730 is the Silver sample, and GRB 210610A is the Bronze sample. The black data points represent the XRT data of the afterglow, and the red solid curves are the smooth broken power-law model fitted to the XRT data.
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: Left panel: the sampled theoretical model points (red dots) prior to the break time obtained from the best-fitting model light curve in comparison with the XRT afterglow data (black dots) of GRB 180620A. Right panel: the PDS (red curve) of the theoretical sampled points before 2305 s, obtained from the LSP. The vertical red solid line represents the peak of the PDS, corresponding to P = 621 s. The vertical black solid line and dotted lines represent the period of 650 ± 50 s in the time interval (200, 2300)s taken from L. Zou & E.-W. Liang (2022). The horizontal blue dotted, dashed–dotted, and solid lines represent FAP levels of 1%, 0.1%, and 0.01%, respectively.
Paper: Signature of Triaxially Precessing Magnetars in Gamma-Ray Burst X-Ray Afterglows
Authors: Biao Zhang, Shu-Qing Zhong, Long Li, Zi-Gao Dai
Figure caption: The geometry of NS precession in the body frame. The unit angular momentum ﹩\hat{{\boldsymbol{L}}}﹩ precesses around ﹩{\hat{{\boldsymbol{e}}}}_{3}﹩, and the angle θ between them undergoes nutation during precession. The unit dipole moment ﹩\hat{{\boldsymbol{\mu }}}﹩ remains constant in the body frame, with its polar angle and azimuthal angle denoted as χ and η, respectively. The angle between the unit angular momentum ﹩\hat{{\boldsymbol{L}}}﹩ and the unit dipole moment ﹩\hat{{\boldsymbol{\mu }}}﹩ is represented by α.