adsabs/AstroCLIMB huggingface dataset:
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Posterior predictive distribution and best-fit model of the bolometric pulse on the left panel and of the phase-averaged spectrum on the right panel. The posterior predictive distribution represents the posterior probability distribution of the observables. The contribution of the individual model components are shown in orange for ST, blue for PDT (left panel only) and purple for the background (BKG). The combined model components are in green for ST+PDT, and in light blue for the total (expected, i.e., ST+PDT+BKG). The shaded regions, from darker to lighter, represent, respectively, the 68% and 95% (and 99% for the right panel only) credible interval computed over 5000 samples. The solid lines represent the maximum likelihood model and the black dashed line the data. The left panel has a discontinuous y-axis and the horizontal line at ∼13,000 counts represent the phase-independent maximum likelihood background. On the right panel, the expected distribution, maximum likelihood and data all overlap. Note that the sampling procedure does not fit individually the ST, PDT, or BKG components but their sum (see Section 4.4 for details).
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Representation of the best-fit geometries, as seen from Earth, for the two main modes uncovered by the Headline ST+PDT run. The pulsar is represented without gravitational or relativistic effects at phase zero of the data. The hotspots located behind the star are plotted with dimmed colors. The hotspot color changes from blue to red, from the hottest to the coldest temperatures. The equatorial ST hotspot can be seen at phase ϕ ∼ 0.4 (behind the star) for both modes. The polar PDT hotspot has two possible configurations, where the smaller and hotter components can be either ceding or superseding components (see Section 4.2). The right geometry is the overall best-fit geometry. These representations do not capture the full posterior distributions of the geometric parameters and should be considered with care.
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Mass–radius posterior distributions in golden obtained from the EOS inference using the N3LO χEFT band up to 1.5n0 and the PP (left panel) or CS extensions (right panel). The EOS inference includes the mass–radius likelihood from PSR J0614−3329 obtained in this work in blue, PSR J0740+6620 in purple, PSR J0437−4715 in red, the ST+PDT model of PSR J0030+0451 in cyan, and the GW170817 constraints from the tidal deformability (for details without PSR J0614−3329 see the “New” scenario in N. Rutherford et al. 2024). The dark (light) regions give the 68% (95%) credible regions. The insets show the radius distribution for a 1.4 M⊙ star, indicated by the black horizontal lines.
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Prior (gray) and posterior distributions of the pressure at 2, 3, and 4n0 using the EOS inference based on the N3LO χEFT band up to 1.5n0 and the PP (left violins) and CS extensions (right violins). We compare the posterior distributions without the new NICER results given by N. Rutherford et al. (2024, blue) and including the mass–radius constraint from PSR J0614−3329 obtained in this work (golden). The vertical thick (thin) lines mark the equal-tailed 68% (95%) credible intervals (see Table 2 for associated values).
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Histogram of ﹩{\rm{\Delta }}{\mathrm{ln}}\,\rm{L}\,﹩ for the three exploratory ST-U, ST+PDT, and PDT-U runs and for the Headline ST+PDT run. The short colored vertical lines represent the median of each distribution. The thick (thin) horizontal lines at the base of the distributions represent the 68% (95%) equal-tailed credible intervals. For visualization purpose, a dashed vertical line centered on ﹩{\rm{\Delta }}{\mathrm{ln}}\,\rm{L}\,=0﹩ is plotted.
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Extracted source (blue) and background (green) spectra from all EPIC instruments used for inference. The green shaded area represents the uniform prior range for the background (±3σ, see Section 3.3). Backgrounds are rescaled using the source and background BACKSCAL values. For visualization purpose only, the rescaled source and background spectra grouped in 13 uniformly sized bins are shown, respectively, in purple and orange.
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: One dimensional marginal distributions of all the parameters for the ST+PDT exploratory runs with different phase shifts applied to the input data. The top of the “violin” distributions (green and blue) show the results from the inference on shifted data and the bottom (yellow) is for the reference ST+PDT run with no shift. Beside the spot phases ϕp and ϕs, all runs have highly similar posteriors. For visualization purposes, the units along the x-axis are arbitrary. The parameter nomenclature and descriptions can be found in Appendix B.
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Posterior distributions of the mass, radius, and compactness for the runs presented in Section 4. Dashed–dotted black lines on the diagonal plots show the marginalized prior distributions, shared across all runs. The shaded vertical bands show the 68.3% credible intervals. The contours in the 2D posteriors show the 68.3%, 95.4%, and 99.7% credible regions, which are filled for the Headline result.
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Graphic model comparison between ST-U, ST+PDT, and PDT-U for 104 posterior samples. The black circles and bars represent ELPD and its uncertainty. The gray triangles for ST-U and ST+PDT represent the same ELPD values, but their error bars display the uncertainty on the ELPD differences with respect to the PDT-U one.
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Comparison of likelihood accuracies and computation times for different settings configurations. The first two rows show variation of individual settings, all other settings being fixed to their LR values, while the last row shows the variation of different settings relative to an HR configuration. Along with the computation time totaled across all samples, the abscissae axes represent the used X-PSI setting value for the first two rows and is arbitrary for the final one. The ordinate axes give the likelihood accuracy ﹩| {\rm{\Delta }}{\mathrm{ln}}\,\rm{L}\,| ﹩ with respect to a reference with the highest setting value tested, whose configuration is in the title of each panel. The colorbars represent the ratio of computation time of each sample to the reference setting, with a single colorbar shared for the first two rows and a different one for the last row. Gray lines link together points obtained with the same posterior sample.
Paper: A NICER View of the 1.4 M⊙ Edge-on Pulsar PSR J0614-3329
Authors: Lucien Mauviard, Sebastien Guillot, Tuomo Salmi, Devarshi Choudhury, Bas Dorsman, Denis González-Caniulef, Mariska Hoogkamer, Daniela Huppenkothen, Christine Kazantsev, Yves Kini, Jean-Francois Olive, Pierre Stammler, Anna L. Watts, Melissa Mendes, Nathan Rutherford, Achim Schwenk, Isak Svensson, Slavko Bogdanov, Matthew Kerr, Paul S. Ray, Lucas Guillemot, Ismaël Cognard, Gilles Theureau
Figure caption: Posterior distribution of the radius, hotspot geometric parameters, and hydrogen column density for the Headline ST+PDT run. Individual mode distributions (red, blue, purple, orange) are plotted along with the full distribution (green). The left plot from Figure 4 corresponds to Mode 1 and the right plot to Mode 2. The dashed–dotted black lines on the diagonal plots show the marginalized prior distributions, shared across all runs. The shaded vertical bands show the 68.3% credible intervals. The contours in the 2D posteriors show the 68.3%, 95.4%, and 99.7% credible regions, which are filled for the mode-averaged distribution only. The full posterior distribution, including all 21 parameters, can be found in the Zenodo repository (L. Mauviard et al. 2025).
Paper: Quasiperiodic Polarized Emissions from Kink Structure in Magnetized Relativistic Jets
Authors: Xu-Fan Hu, Hong-Xuan Jiang, Yosuke Mizuno, Christian M. Fromm, Bhargav Vaidya
Figure caption: Panel (a) shows the light curves of normalized intensity at four representative frequencies: 1.5 GHz (pink), 219 GHz (orange), 521 nm (green), and 1.2 keV (blue). Panel (b) presents PSDs of light curves, where a Hanning window of 228 segments is applied to smooth the signals. The vertical dashed red lines indicate the peak frequencies, which are 20, 29, and 44 mHz, respectively. Panel (c) plots the time evolution of the total polarization degree of the kink region at four frequencies. Panel (d) shows the corresponding PSDs of degrees of polarization with a Hanning window of 178 segments. The vertical dashed red line marks 44 mHz. All of the PSDs are normalized at the lowest frequency. Panel (e) shows the intensity and degree of polarization at 521 nm during a time interval with ts = 428–456. The gray shaded interval (ts = 430–454) is used for plotting panel (f). Panel (f) plots the Q–U plane for 521 nm. The colors of scattered points change over time.
Paper: Quasiperiodic Polarized Emissions from Kink Structure in Magnetized Relativistic Jets
Authors: Xu-Fan Hu, Hong-Xuan Jiang, Yosuke Mizuno, Christian M. Fromm, Bhargav Vaidya
Figure caption: Ray-traced intensity images of an overpressured magnetized jet at ts = 400 with an inclination angle i = 10° at the frequencies of (a) 1.5 GHz, (b) 521 nm, (c) 1.2 keV, and (d) 86 GHz with a tracer to exclude the environment. Here, we use the κ distribution.
Paper: Quasiperiodic Polarized Emissions from Kink Structure in Magnetized Relativistic Jets
Authors: Xu-Fan Hu, Hong-Xuan Jiang, Yosuke Mizuno, Christian M. Fromm, Bhargav Vaidya
Figure caption: Normalized ray-traced snapshot images of overpressured magnetized jet of 86 GHz frequency at ts = 400 with inclination angles i = 1° (left upper) , 10° (left lower) and 90° (right) for thermal (left), κ (middle), and broken power-law distribution (right). In each panel, we normalize with the maximum intensity. White lines mark EVPA patterns (shown only degrees of polarization exceeding 10%).
Paper: Quasiperiodic Polarized Emissions from Kink Structure in Magnetized Relativistic Jets
Authors: Xu-Fan Hu, Hong-Xuan Jiang, Yosuke Mizuno, Christian M. Fromm, Bhargav Vaidya
Figure caption: Time-average SED at an inclination angle i = 10°. We make an average every five frequencies and mark the red horizontal lines. The whole jet region and the specified kink region are plotted in blue and green dashed lines, respectively. The light blue (green) shaded region indicates systematic uncertainty due to time variability and frequency bins.
Paper: Quasiperiodic Polarized Emissions from Kink Structure in Magnetized Relativistic Jets
Authors: Xu-Fan Hu, Hong-Xuan Jiang, Yosuke Mizuno, Christian M. Fromm, Bhargav Vaidya
Figure caption: 2D axial distribution of (a) logarithmic density and (b) magnetization of overpressured magnetized jet at ts = 400.
Paper: Quasiperiodic Polarized Emissions from Kink Structure in Magnetized Relativistic Jets
Authors: Xu-Fan Hu, Hong-Xuan Jiang, Yosuke Mizuno, Christian M. Fromm, Bhargav Vaidya
Figure caption: Dependency of w on Θe and κ at different efficiency ϵ = 0.3 (a), 0.5 (b), and 0.9 (c), which is the solution of Equation (B4). Contour lines at 102, 103, and 104 are plotted.
Paper: Investigation for Binary Characteristics of LS I + 61°303 with Optical Polarization
Authors: Jiaxin Liu, Haoyu Yuan, Xiangli Lei, Wenlong Xu, Jumpei Takata, Weihua Lei
Figure caption: Left: schematic picture of the colliding wind systems. The interaction between the pulsar wind from the pulsar (small filled circle) and outflow from the companion star (large filled circle) creates a shock (thick curved line) that wraps the pulsar. “I,” “II,” and “III” indicate the regions of the free expanding stellar wind, the shock surface, and the free expanding pulsar wind. “Z” indicates the direction of the orbital angular momentum. Right: coordinate system applied in this study. The direction of the observer is represented by no, where θo and νo are polar angle measured from Z-axis and azimuthal angle measured from X-axis, respectively. The X-axis directs toward the periastron. The ndisk represents the axis of the Be disk that is perpendicular to the disk plane. By measuring from a scattering point, P(r), the companion star covers the sky with a solid angle of ﹩\bigtriangleup {\rm{\Omega }}=2\pi (1-\cos {\theta }_{p})﹩, where θp is defined from ﹩\cos {\theta }_{p}=\sqrt{1-{R}_{* }^{2}/{r}^{2}}﹩.
Paper: Investigation for Binary Characteristics of LS I + 61°303 with Optical Polarization
Authors: Jiaxin Liu, Haoyu Yuan, Xiangli Lei, Wenlong Xu, Jumpei Takata, Weihua Lei
Figure caption: Comparison between the P.D.s calculated with the point-source approximation (dashed line) and the finite size of the companion star (solid line). The circular orbit is assumed and the phase zero corresponds to the direction of the observer measured from the companion star. The other model parameters are D = 0.1 au, ﹩\dot{M}/{v}_{{\rm{w}}}=6.7\times 1{0}^{11}\,{{\rm{g}}\,{\rm{cm}}}^{-1}﹩, θo = 45°, and η = 0.25.
Paper: Investigation for Binary Characteristics of LS I + 61°303 with Optical Polarization
Authors: Jiaxin Liu, Haoyu Yuan, Xiangli Lei, Wenlong Xu, Jumpei Takata, Weihua Lei
Figure caption: Schematic illustration of the geometry of the binary system. The parameter ν represents the true anomaly (angle measured from the periastron) of the pulsar.
Paper: Quasiperiodic Polarized Emissions from Kink Structure in Magnetized Relativistic Jets
Authors: Xu-Fan Hu, Hong-Xuan Jiang, Yosuke Mizuno, Christian M. Fromm, Bhargav Vaidya
Figure caption: Same as Figure 5 but at an inclination angle of 90°. In panel (b), a Hanning window of 182 segments are applied, and the vertical dashed red lines mark the peak frequencies, which are 19 and 46 mHz. In panel (d),a Hanning window of 202 segments is applied, and the vertical dashed red line indicates 46 mHz.
Paper: Quasiperiodic Polarized Emissions from Kink Structure in Magnetized Relativistic Jets
Authors: Xu-Fan Hu, Hong-Xuan Jiang, Yosuke Mizuno, Christian M. Fromm, Bhargav Vaidya
Figure caption: Panel (a) shows the average displacement of x along the transverse cut of the jet (y = 0) at z = 40, 45, and 50. Panel (b) shows the corresponding PSDs of displacements with a Hanning window of 164 segments. The vertical dashed red lines mark the peak frequencies, which are 27 and 46 mHz.
Paper: Carbon Dioxide Ices—A Sexagennial Update of Infrared Intensities, Band Shapes, and the Formation and Destruction of Crystalline CO2
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Christopher K. Materese
Figure caption: Integrated intensities of the ν2 IR feature at 675–645 cm−1 of crystalline CO2 near 70 K. The red squares are from YP64. The black circular points are from this work. Panel (b) shows error bars and linear least-squares fits, with thickness uncertainties used for the calculation of each regression line.
Paper: Carbon Dioxide Ices—A Sexagennial Update of Infrared Intensities, Band Shapes, and the Formation and Destruction of Crystalline CO2
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Christopher K. Materese
Figure caption: Relative changes in IR band areas of the 13CO2 ν3 fundamental near 2280 cm−1 on irradiation at 50 and 20 K of two ices of the same column density. The initial thickness of each ice was about 0.24 μm, each ice being made at 70 K and then cooled to either 50 or 20 K for the irradiation. IR band areas after each dose are ratioed against the initial band area for the unirradiated sample.
Paper: Carbon Dioxide Ices—A Sexagennial Update of Infrared Intensities, Band Shapes, and the Formation and Destruction of Crystalline CO2
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Christopher K. Materese
Figure caption: IR spectrum of amorphous CO2 made at 10 K and then warmed to 20, 30, 50, and 70 K. The resolution was 0.25 cm−1.
Paper: Carbon Dioxide Ices—A Sexagennial Update of Infrared Intensities, Band Shapes, and the Formation and Destruction of Crystalline CO2
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Christopher K. Materese
Figure caption: IR spectra of the 660 cm−1 region of crystalline CO2 before (sharp peaks) and after (broad feature) irradiation at 50 K to a dose of about 45 eV per CO2 molecule.
Paper: Carbon Dioxide Ices—A Sexagennial Update of Infrared Intensities, Band Shapes, and the Formation and Destruction of Crystalline CO2
Authors: Reggie L. Hudson, Yukiko Y. Yarnall, Christopher K. Materese
Figure caption: Integrated intensities of the ν3 IR band near 2340 cm−1 of crystalline CO2 near 70 K. The three red squares are from YP64. The black circular points are from this work. Panel (b) shows error bars and linear least-squares fits, with thickness uncertainties used for the calculation of each regression line.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Plots of quiet time differential directional flux versus energy with spectral index and coefficient of determination (R2) values mentioned in each subplot for the PS (a), IM (b), EP (c), and NP (d) directions of AL1-ASPEX-STEPS. Spectral indices are calculated by fitting only the linear part in this log–log plots. The range of energy for the fitted linear part is mentioned in each subplot for PS, IM, EP ,and NP in red, blue, green, and magenta, respectively.
Paper: Multidirectional Investigations on Quiet Time Suprathermal Ions Measured by ASPEX-STEPS on Board Aditya L1
Authors: Aakash Gupta, Dibyendu Chakrabarty, Santosh Vadawale, Aveek Sarkar, Bijoy Dalal, Shiv Kumar Goyal, Jacob Sebastian, P. Janardhan, Nandita Srivastava, M. Shanmugam, Neeraj Kumar Tiwari, Aaditya Sarda, Piyush Sharma, Anil Bhardwaj, Prashant Kumar, Manan S. Shah, Bhas Bapat, Pranav R. Adhyaru, Arpit R. Patel, Hitesh Kumar Adalja, Abhishek Kumar, Tinkal Ladiya, Sushil Kumar, Nishant Singh, Deepak Kumar Painkra, Abhishek J. Verma, Swaroop Banerjee, K. P. Subramanian, M. B. Dadhania
Figure caption: Panels (a), (b), (c), and (d) present the temporal variations of differential directional fluxes of suprathermal ions measured by PS, EP, IM, and NP detectors of AL1-ASPEX-STEPS, respectively. Panels (e), (f), (g), and (h) present the corresponding quiet time directional differential flux of suprathermal ions in the PS, EP, IM and NP detectors, respectively. The energy channels for the panels are mentioned on the right side of the figure.