adsabs/AstroCLIMB huggingface dataset:
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Fractional change in the transit depth as a function of wavelength after subtracting the flare contamination model for TRAPPIST-1f (top left) and b (top right). The spectrum of the star is shown in gray for reference. The larger F3 flare induces contamination at the 2100 ppm level at 2 μm, while the smaller F4 flare causes contamination of ∼500 ppm at 2 μm. TRAPPIST-1's flare rate predicts that flares of these sizes occur multiple times per day. The improvement in the rms of the transit spectrum before and after applying the transit correction is shown for TRAPPIST-1f (bottom left) and b (bottom right).
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Left: the best-fit model for the observed strengths of the Hα and He I IRT lines in our F3 flare, with and without continuum from the F13 kernel. Continuum from the 5F11 ribbon is included in both cases. Middle and right: the F13 kernel flux is pressure broadened to a greater degree than the 5F11 ribbon flux, especially for Hα. As a result, the 5F11 flux dominates the fit to the line centers and the F13 flux dominates the wings.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Correction of flare contamination across a range of wavelengths for the transit spectra of TRAPPIST-1f. The F3 flare peaks just prior to ingress. The original NIRISS order 1 and 2 spectra of the uncorrected transit are shown for reference in gray, while the corrected spectra are color-coded by wavelength. While the F3 flare is clearly seen in the uncorrected spectra, it is much weaker in the corrected spectra after the best-fit blackbody model from Figure 7 is subtracted and the activity lines are masked.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Correction of flare contamination across a range of wavelengths for the transit spectra during the second visit on TRAPPIST-1b. The F4 flare peaks during the flat bottom and continues through egress. The original NIRISS order 1 and 2 spectra of the uncorrected transit are shown for reference in gray, while the corrected spectra are color-coded by wavelength. The F4 flare is much smaller than the F3 event, leading to a less pronounced difference between the uncorrected and corrected spectra during the flare.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: Same as Figure 9 but for Cases 11–13.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: The emission contribution from the hot and cold materials (above or below 0.158 MK) in the corona for all cases.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: Same as Figure 9 but for Cases 4–6.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: Same as Figure 9 but for Cases 7–10.
Paper: Temporal and Spectral Properties of the Persistent Radio Source Associated with FRB 20190520B with the VLA
Authors: Xian Zhang, Wenfei Yu, Casey Law, Di Li, Shami Chatterjee, Paul Demorest, Zhen Yan, Chenhui Niu, Kshitij Aggarwal, Reshma Anna-Thomas, Sarah Burke-Spolaor, Liam Connor, Chao-Wei Tsai, Weiwei Zhu, Gan Luo
Figure caption: Light curves of the PRS associated with FRB 20190520B at all observing bands in the 2020 and 2021 VLA campaign. No significant variability is seen for either observing band, though the PRS at 3 GHz has varied with η ∼ 2.14 in the observing campaign from 2020 to 2021. The flux of the PRS at 3 GHz rose from 160±21 μJy on MJD 59104 to 233 ± 29 μJy on MJD 59167 (a span of 63 days, shown by the black solid line) and decreased by a significance of ∼3.2σ from 193.5 ± 10.1 μJy to 111.5 ± 23.7 μJy between 2020 and 2021. The errors in the plot represent the sum of the statistical errors and 5% additional systematic flux scale errors. We also show in the plot the number of bursts detected at 1.5, 3, and 5.5 GHz by VLA/realfast in the 2020 observations, marked with triangles at the bottom left with the same color code as that of the continuum emission. Note that the realfast system was not run on the last observation of 2020 due to a system error and was not equipped during the 2021 observations.
Paper: Temporal and Spectral Properties of the Persistent Radio Source Associated with FRB 20190520B with the VLA
Authors: Xian Zhang, Wenfei Yu, Casey Law, Di Li, Shami Chatterjee, Paul Demorest, Zhen Yan, Chenhui Niu, Kshitij Aggarwal, Reshma Anna-Thomas, Sarah Burke-Spolaor, Liam Connor, Chao-Wei Tsai, Weiwei Zhu, Gan Luo
Figure caption: Radio spectrum of the PRS across the 1–12 GHz frequency range in the 2020 and 2021 VLA observations. The time-averaged spectrum is well fitted by a power law with an index of −0.40 ± 0.06 in the 2020 observations when including 5% VLA flux scale systematics on the measured flux densities. In the 2021 observations, the power-law index was −0.33 ± 0.14. We observe a flux decrease between the 2020 and 2021 observations. The normalizations of the two power-law spectra (indices fixed to −0.4) differ by 2.8σ, from 291 ± 8 to 228 ± 21 μJy at 1 GHz, suggestive of an overall ∼20% yearly flux decrease in the broad band.
Paper: Temporal and Spectral Properties of the Persistent Radio Source Associated with FRB 20190520B with the VLA
Authors: Xian Zhang, Wenfei Yu, Casey Law, Di Li, Shami Chatterjee, Paul Demorest, Zhen Yan, Chenhui Niu, Kshitij Aggarwal, Reshma Anna-Thomas, Sarah Burke-Spolaor, Liam Connor, Chao-Wei Tsai, Weiwei Zhu, Gan Luo
Figure caption: Deep image of the PRS associated with FRB 20190520B at 1.5 GHz in the 2020 VLA observations. The inset shows the image of the PRS, the averaged position of the bursts detected by VLA overplotted as the white ellipse, and the synthesized beam manually overplotted to the left of the PRS as an ellipse (the size is 4.″7 × 2.″9 and the position angle is −19.°2). The PRS is spatially and physically associated with FRB 20190520B given the chance of coincident association is negligible.
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: Spectral decomposition using physically motivated SEDs. The SEDs, F  ν,i , are shown in the left column. Wide filter bands are indicated with filled circles, narrow ones with open circles. The ejecta spectrum SEDs does not have significant emission in all eight bands. The figures in the right column show the derived spatial distribution of the emission, A  i (α, δ), from each of the SEDs. All are displayed on the same linear scale [−5, 20] to illustrate the relative importance of the different components.
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: Spectral decomposition using observed SEDs. The SEDs, F  ν,i , (from locations shown in Figure 10) are shown in the left column. Wide filter bands are indicated with filled circles, narrow ones with open circles. The figures in the right column show the derived spatial distribution of the emission, A  i (α, δ), from each of the SEDs. All are displayed on the same linear scale [−5, 20] to illustrate the relative importance of the different components.
Paper: JWST NIRCam Observations of SN 1987A: Spitzer Comparison and Spectral Decomposition
Authors: Richard G. Arendt, Martha L. Boyer, Eli Dwek, Mikako Matsuura, Aravind P. Ravi, Armin Rest, Roger Chevalier, Phil Cigan, Ilse De Looze, Guido De Marchi, Claes Fransson, Christa Gall, R. D. Gehrz, Haley L. Gomez, Tuomas Kangas, Florian Kirchschlager, Robert P. Kirshner, Josefin Larsson, Peter Lundqvist, Dan Milisavljevic, Sangwook Park, Nathan Smith, Jason Spyromilio, Tea Temim, Lifan Wang, J. Craig Wheeler, Charles E. Woodward
Figure caption: Locations chosen for the empirical SEDs used for spectral decomposition, indicated on the F150W image after convolution to F444W resolution. See Section 5.1. The crop and display range are the same as Figure 1.
Paper: Mock Observations: Formation and Evolution of Diffuse Light in Galaxy Groups and Clusters in the IllustrisTNG Simulations
Authors: Lin Tang, Weipeng Lin, Yang Wang, Jing Li, Yanyao Lan
Figure caption: Left: relationship between the stellar mass of the diffuse light and the total stellar mass of satellites that are more massive than 108 M ⊙. Right: relationship between the stellar mass of the diffuse light and the number of satellites that are more massive than 108 M ⊙. These relationships are analyzed at different redshifts—z = 0.1, 0.3, 0.5, and 1.0—represented by the colors black, red, green, and blue, respectively. Our results are depicted by the open circles with error bars, where the error bars represent the standard deviation within each mass bin. The solid lines represent fitting lines using different functions. The fitting functions and parameters can be found in Table 2. Note that the inset in the right panel provides the same results but with a linear axis for the satellite number, instead of a logarithmic scale.
Paper: Mock Observations: Formation and Evolution of Diffuse Light in Galaxy Groups and Clusters in the IllustrisTNG Simulations
Authors: Lin Tang, Weipeng Lin, Yang Wang, Jing Li, Yanyao Lan
Figure caption: Age–metallicity planes of satellites, compared to those of the diffuse light. Open diamonds and open squares represent the average values of the properties of satellites and diffuse light located in the same dark matter halo, respectively. The black, red, green, and blue symbols represent the results at redshifts z = 0.1, 0.3, 0.5, and 1.0, respectively. The error bars represent the standard deviations. We divide the stellar masses M ⋆ of the satellites or color [g − r]0.1 into four bins, ﹩8\lt {{\rm{log}}}_{10}({M}_{\star }/{M}_{\odot })\lt 9﹩, ﹩9\lt {{\rm{log}}}_{10}({M}_{\star }/{M}_{\odot })\lt 10﹩, ﹩10\lt {{\rm{log}}}_{10}({M}_{\star }/{M}_{\odot })\lt 11﹩, and ﹩11\lt {{\rm{log}}}_{10}({M}_{\star }/{M}_{\odot })﹩, from left to right, and −1 < [g − r]0.1 < 0, 0 < [g − r]0.1 < 0.4, 0.4 < [g − r]0.1 < 0.8, and 0.8 < [g − r]0.1, from top to bottom.
Paper: Mock Observations: Formation and Evolution of Diffuse Light in Galaxy Groups and Clusters in the IllustrisTNG Simulations
Authors: Lin Tang, Weipeng Lin, Yang Wang, Jing Li, Yanyao Lan
Figure caption: Radial profiles of intrinsic properties for the diffuse light, with the age, metallicity, and color shown from left to right. The lines in different colors (blue, green, and red) represent the profiles within halos of different mass ranges (﹩12\lt {{\rm{log}}}_{10}({M}_{200}/{M}_{\odot })\lt 13﹩, ﹩13\lt {{\rm{log}}}_{10}({M}_{200}/{M}_{\odot })\lt 14﹩, and﹩14\lt {{\rm{log}}}_{10}({M}_{200}/{M}_{\odot })\lt 15﹩). The error—indicated by sky blue, light cyan, and papaya—represents the standard deviations.
Paper: Mock Observations: Formation and Evolution of Diffuse Light in Galaxy Groups and Clusters in the IllustrisTNG Simulations
Authors: Lin Tang, Weipeng Lin, Yang Wang, Jing Li, Yanyao Lan
Figure caption: Dispersion of the best-fitting Equation (6) in left panel of Figure 6 as a function of γ. Specifically, we focus on dispersions in ﹩{\mathrm{log}}_{10}({M}_{\mathrm{star}}﹩ of diffuse light), as the dispersions in ﹩{\mathrm{log}}_{10}{M}_{\mathrm{star}}﹩ of satellites are nearly 0 for γ > 2.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Left panel: extinction E(B−V) map. Right panel: map of electron density calculated from the [S II]λ λ 6717,6731 line ratio. The red cross is the core (optical Gaia position).
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Left panel: the narrowband image from HST in the F502N filter that contains the emission from both the ionized [O III]λ5007 gas and the continuum. Middle panel: the continuum image from HST in the F547M filter. Right panel: difference image after subtraction of the scaled continuum F547M filter image from the narrowband F502N filter image. This difference image reveals an asymmetric biconical [O III]λ5007 outflow. The white cross in all the figures is the optical core (Gaia position).
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Gaussian fit to the observed Hβ (left) and [O III]λ5007 (right) emission lines along with the residuals (lower panel of each spectrum). Here, shaded blue is the Gaussian fit to the outflowing component, red and black are the Gaussian fits to the narrow and broad components, and the dotted black line is the best-fit spectrum. The observed spectra are shown as a solid blue line.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: The molecular H2 λ2.4085 image of NGC 4395. The core of NGC 4395 taken as the optical Gaia position is shown as a white cross.
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: Kinematics map of [O III]λ5007 line emission. Left panel: velocity map. Middle panel: map of the W90 parameter, which is equivalent to velocity dispersion. Right panel: map of asymmetry index. The red cross represents the core (optical Gaia position).
Paper: Evidence for Low-power Radio Jet–ISM Interaction at 10 pc in the Dwarf AGN Host NGC 4395
Authors: Payel Nandi, C. S. Stalin, D. J. Saikia, Rogemar A. Riffel, Arijit Manna, Sabyasachi Pal, O. L. Dors, Dominika Wylezalek, Vaidehi S. Paliya, Payaswini Saikia, Pratik Dabhade, Markus-Kissler Patig, Ram Sagar
Figure caption: X-ray Image of NGC 4395 in the 0.5–7 keV energy range from Chandra. The red cross is the optical Gaia the position.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Time evolution of a typical accelerated electron in the strongly cooled simulation. The right-hand panel shows the energy evolution of the particle with time. Panels (a)–(e) show the density slice and the magnetic field lines in the x–z plane at a particular time of the simulation (corresponding to the right-hand panel). The position and the velocity of the electron are shown with a colored circle and an arrow (color corresponds to its energy at that particular time). The magnetic field line passing through the position of the particle is shown as a blue line, with its thickness corresponding to the strength of the magnetic field. The electron starts cold upstream of the current layer (a) and is accelerated to the Lorentz factor up to ≈σ in the current sheet (b), after which it is picked up by the outflow from the X-point and gains further energy (c). Ultimately, the electron experiences an intensive slow-down when it collides with the magnetic field inside the plasmoid (d), where it remains throughout the rest of its lifetime (e).
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Archetypal trajectories (projected to the x–y and the x–z plane) and the energy evolution of two ions. The color of each dot corresponds to the Lorentz factor of the ion at that particular time, while the size of the dot indicates whether the ion is inside the current sheet (small dots) or upstream (large dots). The ion on the right-hand side accelerates to high energies (≫σ) by the large-scale electric field, E rec, in the region upstream of the layer, while the ion on the left-hand side gains only a marginal amount of energy (∼σ). The more energetic ion on the right primarily moves upstream of the current layer along the reconnection electric field (y-direction) and accelerates linearly in time. The slower particle is trapped inside the current sheet and experiences constant scatterings on local inhomogeneities.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Energy distributions of the pairs (solid lines) and the ions (dotted lines) at t = 2.25 L  x /c for different cooling regimes: purple lines correspond to strong cooling γ syn/σ = 0.2, and the red lines correspond to the uncooled runs, γ syn/σ = ∞ . Dynamically strong cooling effectively limits the maximum energy of pairs to ∼σ, but at the same time facilitates the formation of harder distribution for the ions. For reference, we also show the corresponding Larmor radii, ﹩{r}_{L}^{\mathrm{up}}﹩.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Time evolution of a sample of ions that reach energies, correspondingly, γ in = σ (odd columns), and γ in = 5σ (even columns). Results from two simulations are shown: with no cooling (first two columns) and with strong cooling current (last two columns). The upper row ((a1)–(a4)) shows the evolution of the Lorentz factor of the ions. The middle row ((b1)–(b4)) shows the evolution of the y component of their 3-velocities (along the reconnecting electric field E rec). The lower row ((c1)–(c4)) shows the value of the reconnection electric field E  y  experienced by these ions. In the strong cooling regime, most of the ions successfully accelerate in the reconnection electric field and experience little-to-no scatterings (evident from the narrow spread in their energy evolution, (a3)–(a4)). In the uncooled regime, the energy gain is more chaotic as ions constantly scatter inside the current sheet.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: A cross-section of typical plasmoids for uncooled ((a), (b)) and strongly cooled ((c), (d)) current sheets. The left-hand column ((a), (c)) shows density slices and the magnetic field lines. The region highlighted with a cyan-dotted boundary is shown in 1D cuts in ((b), (d)), where we plot the magnetic field, B 2/8π, and gas pressure, P, with the corresponding magnetic tension force, ( j  ×  B ) z , and the gradient of the pressure tensor, c∇ i  P  iz . On the one hand, in the uncooled case, the plasmoids are in equilibrium in terms of magnetic and thermal pressure, with the thermal pressure typically dominating inside the plasmoids. On the other hand, the equilibrium inside the cooled plasmoids is more dynamic, with the magnetic field pressure being larger than the upstream value, and dominating the plasmoid cores.
Paper: High-energy Radiation and Ion Acceleration in Three-dimensional Relativistic Magnetic Reconnection with Strong Synchrotron Cooling
Authors: Alexander Chernoglazov, Hayk Hakobyan, Alexander Philippov
Figure caption: Distribution of transverse sizes (along z) of the current layer for different cooling regimes. The scale is zoomed in for ﹩w\lt {r}_{L}^{\mathrm{up}}(\sigma )﹩. Stronger cooled current sheets form on average smaller structures due to significant compression. The peak of the distribution, i.e., most of the current sheet, has a thickness below the Larmor radius of particles accelerated up to σ: ﹩w\sim {r}_{L}^{\mathrm{up}}(\sigma )﹩.