adsabs/AstroCLIMB huggingface dataset:
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Residual PSF size after subtracting the size of the PSF models from that of the stars. The PSF models match the size of the stars to ≲0.3%. This residual in size is below the dominant systematic effects of undersampling and the BFE and thus is acceptable for our future weak-lensing analysis.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Observed subpixel centroid dependence of e 1 (top row), e 2 (middle row), and R (bottom row) of stars in the FLT frames of NGC 104. Black circles represent the quadrupole measurements of individual stars. Blue circles are median values with a bin width of 0.1 pixels. The standard error (﹩\sigma /\sqrt{n}﹩) for each of the blue circles is <0.01%. In the top row, the images of stars (PSF) centered in a pixel have ellipticities in the y direction. Subpixel x shifts cause a systematic elongation of the PSF in the x direction, which leads to a rounder PSF, while subpixel y shifts cause an elongation of the PSF in the y direction. In the middle row, subpixel shifts do not cause a discernible variation in the e 2 component. In the bottom row, the size of the PSF increases for both x and y shifts away from the center of the pixel. Thus, there is a subpixel location dependency for the ellipticity and size of the PSF.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Magnitude and direction of the ellipticity of stars from a single NGC 104 frame observed with the F160W filter. The red line represents an ellipticity of e 1 = 0.05, e 2 = 0. Left: stars from an FLT frame that has not been corrected for geometric distortion. Geometric distortion causes the y-axis elongation of the PSF. The plate scale is approximated as 0.13 arcsec pixel−1 for display purposes. Middle:  stars from the same frame after the geometric distortion is corrected by Astrodrizzle. The drizzled PSF elongates in the x direction, and the ellipticity is smaller than in the FLT frame. In the right panel, an improper weight function applied when measuring the shapes of stars in the drizzled frame emphasizes aliasing, which causes the ellipticity of the stars to systematically align with the x and y detector axes.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Effect of undersampling on galaxy shape measurement. The simulated galaxy has x-direction elongation (e 1 = 0.02, e 2 = 0.0) and Sérsic parameters of half-light radius = 0.″18 and n = 0.5. The galaxy has been convolved with a circular Gaussian PSF with FWHM = 0.″2. The solid black curve traces the multiplicative galaxy shape bias caused by undersampling when the source is perfectly centered in a pixel. The shaded regions represent subpixel shifts of the galaxy centroid in the x (blue) and y (green) directions. The solid (dotted) gray lines mark subpixel shifts of 0.5 (0.25) pixels. Vertical lines indicate the sampling rate of notable filters, as labeled. The Roman F213 suffers the least from undersampling bias because of its larger PSF. The subpixel dependence of the galaxy shape is small for Roman F184 and Euclid VIS. For HST F160W and Roman F158, the dependence leads to a multiplicative bias variation of ∼0.012. The Euclid NISP filter has a sampling rate of ∼0.43 and will have severe bias from undersampling.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Simulated undersampling of an elliptical Gaussian distribution with e 1 = −0.03, e 2 = 0, and a sampling rate S = 0.6. In the first row, the color scheme showing the subpixel dithers along the off axis, where black represents no subpixel shift, and yellow is the maximum subpixel shift of 0.5 pixels. In the second row, shifts in the x direction elongate the PSF in the x direction, which circularizes the PSF. Shifts in the y direction elongate the PSF in the y direction, making it more elliptical. The simulation highlights that the scatter in Figure 3 is partly caused by shifts along the opposite axis. In the third row, as in the observed PSF, the e 2 component is not significantly affected by shifts. In the fourth row, the size of the PSF with both x or y shifts enlarges the PSF.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Astrometric offset of the CANDELS Treasury mosaics v1.0 (gray) and the mosaics produced in this work (blue) from the positions of stars in the proper motion–corrected Gaia catalog DR3. Vertical dashed (this work) and dotted (Treasury) lines mark the median astrometric offset. On average, our updated mosaics have an astrometric offset from the Gaia catalog of 0.″02, a factor of several improvement compared to the Treasury mosaics.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Half-light radius (pixel) vs. F160W magnitude diagram of sources in the CANDELS/UDS field. Darker gray represents a denser region of sources in this figure. There is a tight sequence of stars that is mostly below the red line defined as half-light radius <−0.115 × F160W + 5.15. The additional magnitude cuts are shown by vertical dashed black lines, F160W = 19 (saturation limit) and 25 AB magnitudes, respectively. Blue points indicate stars classified from our star selection criteria.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Astrometric offset of stars in the Gaia catalog to stars in the mosaics from CANDELS Treasury (left panel) and our work (right panel). The Treasury mosaic is well aligned but shows a slight systematic variation at the edge of the mosaic. Our mosaic has removed the systematic variation, and, on average, the astrometry of the GOODS-N field is improved from 0.″05 to 0.″02.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: The PSF properties of drizzled frames from observations of NGC 104. The intrinsic ellipticity of the PSF is in the detector x direction. Top:  subpixel shifts in x lead to increased ellipticity of the PSF, and subpixel shifts in y decrease the ellipticity. Middle: subpixel shifts have a minimal effect on the e 2 component. Bottom:  shifts in either direction lead to an increase in the size of the PSF.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Astrometric offset of stars in the Gaia catalog to stars in the mosaics from CANDELS Treasury (left panel) and our work (right panel). The Treasury mosaic of COSMOS has an ∼0.″11 shift from the Gaia positions. Our mosaic has removed the shift. The average astrometry of the COSMOS field is improved from 0.″11 to 0.″02.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: The PSF properties of the FLT frames from observations of NGC 104. Bluer filters are more subject to the undersampling effect because their PSF is smaller. Clearly, the F160W filter is the best choice for mitigating the undersampling effect in WFC3-IR imaging. Future missions should consider the impact that undersampling could have on the science when selecting filter and plate scales.
Paper: Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. I. Point-spread Function Modeling and Systematics
Authors: Kyle Finner, Bomee Lee, Ranga-Ram Chary, M. James Jee, Christopher Hirata, Giuseppe Congedo, Peter Taylor, Kim HyeongHan
Figure caption: Astrometric offset of stars in the Gaia catalog to stars in the mosaics from CANDELS Treasury (left panel) and our work (right panel). The Treasury mosaic for the EGS is well aligned, but stars near the center of the image have larger offsets than stars near the boundary. Our new alignment to Gaia has corrected this variation. On average, the astrometry of the EGS field is improved from 0.″07 to 0.″03.
Paper: Understanding the Kinetic Energy Deposition within Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Shaobo Zhang, Qing-Zeng Yan, Yan Sun, Xin Zhou, Xuepeng Chen, Hongchi Wang, Zhiwei Chen
Figure caption: Distributions of the differences between the centroid velocities from 12CO emission (﹩{V}_{\mathrm{cen}{,}^{12}\mathrm{CO}}﹩) and 13CO emission (﹩{V}_{\mathrm{cen}{,}^{13}\mathrm{CO}}﹩) in MCs. “All” represents the whole 2851 MCs, and “Single” and “Multiple” correspond to MCs with single and multiple (more than one) 13CO structures, respectively. In the middle and right panels, each dot represents a 12CO MC. The colors on these dots represent the distribution of the probability density function (2D-PDF) of their 12CO MCs, which are calculated utilizing the kernel-density estimation through Gaussian kernels in the PYTHON package (scipy.stats.Gaussian_kde). The cyan dashed lines indicate the lines with ﹩{V}_{\mathrm{cen}{,}^{12}\mathrm{CO}}﹩ = ﹩{V}_{\mathrm{cen}{,}^{13}\mathrm{CO}}﹩.
Paper: Understanding the Kinetic Energy Deposition within Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Shaobo Zhang, Qing-Zeng Yan, Yan Sun, Xin Zhou, Xuepeng Chen, Hongchi Wang, Zhiwei Chen
Figure caption: Distributions of the optical depths of 12CO emission (﹩{\tau }_{{}^{12}\mathrm{CO}}﹩) and β  τ  in the whole regions, 13CO-bright regions, and 13CO-dark regions of our 2851 MC samples. The green histograms represent the distributions of the minimal values of ﹩{\tau }_{{}^{12}\mathrm{CO}}﹩ and β  τ  in the whole regions, 13CO-bright regions, and 13CO-dark regions of MCs. The gray histograms are for their mean values and the magenta histograms are for their maximum values. The median values for the distributions of these minimal, mean, and maximum ﹩{\tau }_{{}^{12}\mathrm{CO}}﹩ and β  τ  in the MC samples are noted in each panel.
Paper: Understanding the Kinetic Energy Deposition within Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Shaobo Zhang, Qing-Zeng Yan, Yan Sun, Xin Zhou, Xuepeng Chen, Hongchi Wang, Zhiwei Chen
Figure caption: Left panel: Relation between the ratio of ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{re}}^{2}﹩ over ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}^{2}﹩ with ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}^{2}﹩. Right panel: Relation between the ratio of ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}^{2}﹩ over ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}^{2}﹩ with ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}^{2}﹩. Each dot in both panels represents an MC in the “Multiple” regime. The colors on the dots represent the distribution of the probability density function (2D-PDF) of their 12CO MCs. The black-dashed lines show the values of ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{re}}^{2}﹩/﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}^{2}﹩= 0.8 in the left panel and ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}^{2}﹩/﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}^{2}﹩= 0.2 in the right panel.
Paper: Understanding the Kinetic Energy Deposition within Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Shaobo Zhang, Qing-Zeng Yan, Yan Sun, Xin Zhou, Xuepeng Chen, Hongchi Wang, Zhiwei Chen
Figure caption: Correlations between the ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}^{2}﹩ with the ﹩{\sigma }_{{}^{12}\mathrm{CO},\mathrm{tot}}^{2}﹩ for the MC samples in the “All,” “Multiple,” and “Single” regimes. The V sys used in Equation (5) is the ﹩{V}_{\mathrm{cen},{}^{13}\mathrm{CO}}﹩ of each MC. Each dot in the panels represents a 12CO MC. The colors on these dots represent the distribution of the probability density function (2D-PDF) of their 12CO MCs. The corresponding Spearman’s rank correlation coefficient (R-value) is noted in each panel.
Paper: Understanding the Kinetic Energy Deposition within Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Shaobo Zhang, Qing-Zeng Yan, Yan Sun, Xin Zhou, Xuepeng Chen, Hongchi Wang, Zhiwei Chen
Figure caption: Correlations between ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}^{2}﹩, ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{re}}^{2}﹩, and ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}^{2}﹩ with ﹩{\sigma }_{{}^{12}\mathrm{CO},\mathrm{tot}}^{2}﹩ for the MC samples in the “All,” “Multiple,” and “Single” regimes, respectively. Each dot in the panels represents a 12CO MC. The colors on these dots represent the distribution of the probability density function (2D-PDF) of their 12CO MCs. The corresponding Spearman’s rank correlation coefficient (R-value) is noted in each panel.
Paper: Understanding the Kinetic Energy Deposition within Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Shaobo Zhang, Qing-Zeng Yan, Yan Sun, Xin Zhou, Xuepeng Chen, Hongchi Wang, Zhiwei Chen
Figure caption: Correlations between the ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}^{2}﹩, ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{re}}^{2}﹩, and ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}^{2}﹩ with ﹩{\sigma }_{{}^{12}\mathrm{CO},\mathrm{tot}}^{2}﹩ for all the samples. The V sys used in Equation (5) is the ﹩{V}_{\mathrm{cen},{}^{13}\mathrm{CO}}﹩ of each MC. Each dot in the panels represents a 12CO MC. The colors on these dots represent the distribution of the probability density function (2D-PDF) of their 12CO MCs. The corresponding Spearman’s rank correlation coefficient (R-value) is noted in each panel.
Paper: Understanding the Kinetic Energy Deposition within Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Shaobo Zhang, Qing-Zeng Yan, Yan Sun, Xin Zhou, Xuepeng Chen, Hongchi Wang, Zhiwei Chen
Figure caption: Correlations between ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{re}}^{2}﹩ with ﹩{\sigma }_{{}^{12}\mathrm{CO},\mathrm{tot}}^{2}﹩ (left panel) and ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}^{2}﹩ with ﹩{\sigma }_{{}^{12}\mathrm{CO},\mathrm{tot}}^{2}﹩ (right panel) for the MC samples. The green dots in the panels represent 12CO MCs harboring at least ten 13CO structures; the corresponding Spearman’s rank correlation coefficient (R-value) is noted in each panel. The gray crosses are for the left 12CO MCs, whose number of 13CO structures is less than 10.
Paper: Understanding the Kinetic Energy Deposition within Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Shaobo Zhang, Qing-Zeng Yan, Yan Sun, Xin Zhou, Xuepeng Chen, Hongchi Wang, Zhiwei Chen
Figure caption: Distributions of the calculated values of ﹩{\sigma }_{{}^{12}\mathrm{CO},\mathrm{tot}}﹩, ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{tot}}﹩, ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}﹩ and ﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{re}}﹩ for MCs. “All” represents the whole 2851 MCs, and “Single” and “Multiple” correspond to MCs with single and multiple (more than one) 13CO structures, respectively.
Paper: Understanding the Kinetic Energy Deposition within Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Fujun Du, Yang Su, Shaobo Zhang, Qing-Zeng Yan, Yan Sun, Xin Zhou, Xuepeng Chen, Hongchi Wang, Zhiwei Chen
Figure caption: Increasing trends of the velocity dispersion components following the quantiles at 0.05, 0.25, 0.5, 0.75, and 0.95 in their sequential data. “All” represents the whole 2851 MCs, and “Single” and “Multiple” correspond to MCs with single and multiple (more than one) 13CO structures, respectively.
Paper: Analyses of ∼0.05–2 MeV Ions Associated with the 2022 February 16 Energetic Storm Particle Event Observed by Parker Solar Probe
Authors: Joe Giacalone, C. M. S. Cohen, D. J. McComas, X. Chen, M. A. Dayeh, W. H. Matthaeus, K. G. Klein, S. D. Bale, E. R. Christian, M. I. Desai, M. E. Hill, L. Y. Khoo, D. Lario, R. A. Leske, R. L. McNutt, D. G. Mitchell, J. G. Mitchell, O. Malandraki, N. A. Schwadron
Figure caption: From the top panel, plasma number density, radial component of the solar-wind velocity, t- and n-components of the solar-wind velocity (red and green, respectively), magnetic field vector magnitude (black) and components (r, in blue, t in red, and n in green), and fluxes of 79.1 keV to 1.66 MeV energetic protons over a 9 hr period nearly centered at the shock crossing time, indicated with the vertical dashed line. The color code for the magnetic field and proton fluxes is the same as that shown in Figure 1.
Paper: Analyses of ∼0.05–2 MeV Ions Associated with the 2022 February 16 Energetic Storm Particle Event Observed by Parker Solar Probe
Authors: Joe Giacalone, C. M. S. Cohen, D. J. McComas, X. Chen, M. A. Dayeh, W. H. Matthaeus, K. G. Klein, S. D. Bale, E. R. Christian, M. I. Desai, M. E. Hill, L. Y. Khoo, D. Lario, R. A. Leske, R. L. McNutt, D. G. Mitchell, J. G. Mitchell, O. Malandraki, N. A. Schwadron
Figure caption: Overview of observations of the SEP event observed by PSP on 2022 February 16. The top panel shows the magnetic field vector, with components represented by colors as indicated at the right of the panel. The middle panel shows the differential intensity of energetic protons, with energies indicated at the right of the panel. The bottom panel shows the differential intensity, represented as a color spectrogram, of all protons in our study with energy along the vertical axis. The vertical dashed lines represent the time of significant events. The one on the left is the time in which STEREO-A/Cor2 first observed the CME, the middle one represents the arrival of the shock, and the far right one is the onset of the magnetic flux rope associated with the ICME.
Paper: Analyses of ∼0.05–2 MeV Ions Associated with the 2022 February 16 Energetic Storm Particle Event Observed by Parker Solar Probe
Authors: Joe Giacalone, C. M. S. Cohen, D. J. McComas, X. Chen, M. A. Dayeh, W. H. Matthaeus, K. G. Klein, S. D. Bale, E. R. Christian, M. I. Desai, M. E. Hill, L. Y. Khoo, D. Lario, R. A. Leske, R. L. McNutt, D. G. Mitchell, J. G. Mitchell, O. Malandraki, N. A. Schwadron
Figure caption: Results from the modeling of the solar wind in the inner heliosphere at about the time of the CME based on the ENLIL model (see the main text for details). Shown are two snapshots of the solar-wind density times r 2 in the ecliptic plane at two different times on 2022 February 16, as indicated above each image. The left image is for time = 00:00:26 UT, and the right image is for time = 00:06:24, when the CME was just about to cross over PSP, as indicated by the green square in each image. Also shown are the positions of five spacecraft, as indicated above each image. The dashed lines are magnetic field that connect from the spacecraft to the inner boundary of the model calculation, at about 0.1 au.
Paper: Analyses of ∼0.05–2 MeV Ions Associated with the 2022 February 16 Energetic Storm Particle Event Observed by Parker Solar Probe
Authors: Joe Giacalone, C. M. S. Cohen, D. J. McComas, X. Chen, M. A. Dayeh, W. H. Matthaeus, K. G. Klein, S. D. Bale, E. R. Christian, M. I. Desai, M. E. Hill, L. Y. Khoo, D. Lario, R. A. Leske, R. L. McNutt, D. G. Mitchell, J. G. Mitchell, O. Malandraki, N. A. Schwadron
Figure caption: Top: (black plus symbols) flux of 165–184 keV protons (logarithmic middle energy of 174 keV) for a 3 day period including the ESP event of 2022 February 16. (Blue dashed line) an approximate estimate of the upper bound on the preexisting flux of particles within this energy range, for a ∼1 day period prior to the initial increase. A red dashed line shows the estimate of the increase of particles at the shock resulting from the acceleration of the preexisting particles at the shock based on diffusive shock acceleration theory for an injection energy of 2 keV. A black dashed line indicates the value of the flux at the shock arrival. Middle and Bottom: same format as the top panel, but for the cases of helium (middle) and oxygen (bottom) ions with approximately the same energy per nucleon as the protons. For helium, the range of total kinetic energy is 637–723 keV, and for oxygen, it is 2.38–2.73 MeV. See the main text for more details.
Paper: Analyses of ∼0.05–2 MeV Ions Associated with the 2022 February 16 Energetic Storm Particle Event Observed by Parker Solar Probe
Authors: Joe Giacalone, C. M. S. Cohen, D. J. McComas, X. Chen, M. A. Dayeh, W. H. Matthaeus, K. G. Klein, S. D. Bale, E. R. Christian, M. I. Desai, M. E. Hill, L. Y. Khoo, D. Lario, R. A. Leske, R. L. McNutt, D. G. Mitchell, J. G. Mitchell, O. Malandraki, N. A. Schwadron
Figure caption: Energy spectra of energetic protons for this SEP event taken over three separate time intervals, as indicated in the legend at the lower left of the figure. The dashed lines are representative power-law distributions, presented as a guide.
Paper: Analyses of ∼0.05–2 MeV Ions Associated with the 2022 February 16 Energetic Storm Particle Event Observed by Parker Solar Probe
Authors: Joe Giacalone, C. M. S. Cohen, D. J. McComas, X. Chen, M. A. Dayeh, W. H. Matthaeus, K. G. Klein, S. D. Bale, E. R. Christian, M. I. Desai, M. E. Hill, L. Y. Khoo, D. Lario, R. A. Leske, R. L. McNutt, D. G. Mitchell, J. G. Mitchell, O. Malandraki, N. A. Schwadron
Figure caption: Open-circle symbols are diffusion coefficients far upstream (black) and near the shock (red), as estimated from the rise-time analysis and tabulated in Table 1. The solid lines are least-squares fits to these data. The dashed lines are estimates based on quasi-linear theory using the measured power spectrum of magnetic field fluctuations for each of these time intervals. See the main text for more details.
Paper: Analyses of ∼0.05–2 MeV Ions Associated with the 2022 February 16 Energetic Storm Particle Event Observed by Parker Solar Probe
Authors: Joe Giacalone, C. M. S. Cohen, D. J. McComas, X. Chen, M. A. Dayeh, W. H. Matthaeus, K. G. Klein, S. D. Bale, E. R. Christian, M. I. Desai, M. E. Hill, L. Y. Khoo, D. Lario, R. A. Leske, R. L. McNutt, D. G. Mitchell, J. G. Mitchell, O. Malandraki, N. A. Schwadron
Figure caption: (Top panel) partial pressures of SEPs (violet symbols), dynamic pressure of solar wind (black symbols), and magnetic field pressure (red symbols). (Bottom panel) dynamic energy flux of the solar wind in the shock rest frame (black symbols), and the energetic-ion enthalpy flux (violet symbols). The dashed lines in the bottom panel show the values near the shock. See the main text for more details.