adsabs/AstroCLIMB huggingface dataset:
Paper: Quantitative Exploration of the Similarity of Gamma-Ray Pulsar Light Curves
Authors: C. R. García, Diego F. Torres
Figure caption: Top panel: time series ts1 (green) and ts2 (yellow) used in the DTW example. The y-axis represents an arbitrary number of counts according to Equation (A1). The x-axis represents the phases for each value, from 0 to 1, defined by the number of values in each time series. Bottom panel: application of DTW. The orange lines represent πo, the connection between the pairs of the time series (i.e., the chosen (i, j) pairs from Equation (A4)).
Paper: Quantitative Exploration of the Similarity of Gamma-Ray Pulsar Light Curves
Authors: C. R. García, Diego F. Torres
Figure caption: Clusters with four or more pulsars and all members related to another by at least one similarity at a 3σ significance level. Each node represents a pulsar, and each colored edge connecting the nodes the similarity significance of the corresponding light curves (black for <1σ, red for cases between 1σ and 2σ, blue for cases between 2σ and 3σ, and green for >3σ). The light curves associated with each cluster are shown next. MSPs are denoted with a star-shaped node and on the pulsar name.
Paper: Quantitative Exploration of the Similarity of Gamma-Ray Pulsar Light Curves
Authors: C. R. García, Diego F. Torres
Figure caption: Each row shows the three most similar pairs of light curves according to ED for light curves with 25, 50, 100, and 200 bins. The plot in the first column of each row shows the 3PC data directly before processing. MSPs are denoted with a star on the pulsar name.
Paper: Quantitative Exploration of the Similarity of Gamma-Ray Pulsar Light Curves
Authors: C. R. García, Diego F. Torres
Figure caption: Distribution of the natural logarithm of DTW−1 values, ﹩\mathrm{ln}({{\rm{DTW}}}^{-1})﹩. The orange line shows the normal distribution identified as the best fit for the data. The dashed vertical lines denoted with 1σ (red), 2σ (blue), and 3σ (green) represent the intervals of the distribution according to the empirical rule.
Paper: Quantitative Exploration of the Similarity of Gamma-Ray Pulsar Light Curves
Authors: C. R. García, Diego F. Torres
Figure caption: The three most similar pairs of light curves according to DTW for light curves with 25, 50, 100, and 200 bins. The plot in the first column of each row shows the 3PC data directly before processing. MSPs are denoted with a star on the pulsar name.
Paper: Quantitative Exploration of the Similarity of Gamma-Ray Pulsar Light Curves
Authors: C. R. García, Diego F. Torres
Figure caption: Time series ts3 (green) and ts4 (yellow) seen in Equation (A5) connected via the Euclidean alignment (left) or DTW (right).
Paper: Inhomogeneous Dust Biases Photometric Redshifts and Stellar Masses for LSST
Authors: ChangHoon Hahn, Peter Melchior
Figure caption: The effect of dust on inferred photo-z (top) and M* (bottom). We present the difference between the MAP values of ﹩p(z,{M}_{* }\,| \,{{\boldsymbol{X}}}_{i,j}^{\mathrm{dust}})﹩ and ﹩p(z,{M}_{* }\,| \,{{\boldsymbol{X}}}_{i,j}^{\mathrm{no}\,\mathrm{dust}})﹩ as a function of AV. Each panel and color presents a different orientation from edge-on (top left; light) to face-on (bottom right; dark). The x-axis is scaled linearly above 0.1 and logarithmically below 0.1, for clarity. With AV ≲ 0.5 we infer overall unbiased z and M*. With AV > 0.5, there is a bias in photo-zs that depends on orientation: photo-zs are overestimated for more face-on orientations. For face-on, photo-zs are overestimated by  ∼0.02. There is also a bias in M* that depends on orientation: M* is underestimated for more edge-on orientations. For edge-on, M* are underestimated by  ∼0.4 dex. The current homogeneous dust screen assumption in SED modeling is insufficient at marginalizing the effect of dust and will impact LSST cosmological analyses.
Paper: Inhomogeneous Dust Biases Photometric Redshifts and Stellar Masses for LSST
Authors: ChangHoon Hahn, Peter Melchior
Figure caption: Posteriors, p(z, M* ∣ Xi,j), for a single simulated NIHAO-SKIRT galaxy (i = 64) observed from different orientations, j. We present 5 of the 10 orientations ranging from edge-on to face-on (light to dark). We also include the posterior inferred from ﹩{{\boldsymbol{X}}}_{i,j}^{\mathrm{no}\,\mathrm{dust}}﹩, LSST photometry constructed from SEDs with no dust (black), as well as the true z and M* (red star). Dust introduces orientation-dependent biases in the inferred z and M*.
Paper: Formation of the Dark Matter–Deficient S0 Galaxy NGC 4111 under the Tidal Interactions
Authors: Mei Ai, Ming Zhu, Nai-ping Yu, Jin-long Xu, Xiao-lan Liu, Yingjie Jing, Qian Jiao, Yao Liu, Chuan-peng Zhang, Jie Wang, Peng Jiang
Figure caption: The NGC 4111 galaxy group system. White contours show the H I column-density map for this system derived from FAST data, overlaid on the DECaLS optical image. Nine galaxies are on this map, and their names are labeled. The velocity range for the integration is from 600 to 1200 km s−1. The FAST beam size is labeled as a green circle at the bottom right corner. The H I contour levels are 1.9 × 1018 cm−2, 3.4 × 1018 cm−2, 5.5 × 1018 cm−2, 7.0 × 1018 cm−2, 9.6 × 1018 cm−2, 1.4 × 1019 cm−2, 1.8 × 1019 cm−2, 2.8 × 1019 cm−2, 4.4 × 1019 cm−2, 6.3 × 1020 cm−2, and 7.3 × 1019 cm−2. The red contours are derived from the WSRT ATLAS3D public data, and the column-density levels are 2.7 × 1019 cm−2, 1.4 × 1020 cm−2, 5.4 × 1020 cm−2, and 1.4 × 1021 cm−2.
Paper: Formation of the Dark Matter–Deficient S0 Galaxy NGC 4111 under the Tidal Interactions
Authors: Mei Ai, Ming Zhu, Nai-ping Yu, Jin-long Xu, Xiao-lan Liu, Yingjie Jing, Qian Jiao, Yao Liu, Chuan-peng Zhang, Jie Wang, Peng Jiang
Figure caption: The method for extracting the H I integral spectrum for NGC 4111 from the entire H I complex. Left: the H I column-density map around the NGC 4111 region integrated from 600 to 900 km s−1. The blue ellipse shape marks the optical disk of NGC 4111, and the dashed blue line indicates the direction of the simulated major H I disk, see Section 4. The contour levels are 2.5 × 1019 cm−2, 3.3 × 1019 cm−2, 4.1 × 1019 cm−2, 4.9 × 1019 cm−2, 5.8 × 1019 cm−2, 6.8 × 1019 cm−2, and 7.4 × 1019 cm−2. The right panel is the integral H I spectra of NGC 4111, which is the sum of all the spectra inside of the lowest contour level (the red dashed contour line) in the left panel.
Paper: Formation of the Dark Matter–Deficient S0 Galaxy NGC 4111 under the Tidal Interactions
Authors: Mei Ai, Ming Zhu, Nai-ping Yu, Jin-long Xu, Xiao-lan Liu, Yingjie Jing, Qian Jiao, Yao Liu, Chuan-peng Zhang, Jie Wang, Peng Jiang
Figure caption: Three position–velocity (P–V) plots in three directions that centered on NGC 4111, illustrating its interactions with UGC 7094, NGC 4117, and Cloud A in the radial direction. The upper left panel shows the H I moment 0 map for the NGC 4111 system. Three directions (a), (b), and (c) are overlaid around NGC 4111. The contour levels are the same as in Figure 1. The remaining three panels exhibit the P–V diagrams along the directions (a), (b), and (c). The contour levels for the three P–V diagrams are 1.1, 2.2, 4.9, 6.9, 8.8, 10.4, 11.5, 16.4, 20.5, 23.29, and 25.2 mJy beam−1.
Paper: Formation of the Dark Matter–Deficient S0 Galaxy NGC 4111 under the Tidal Interactions
Authors: Mei Ai, Ming Zhu, Nai-ping Yu, Jin-long Xu, Xiao-lan Liu, Yingjie Jing, Qian Jiao, Yao Liu, Chuan-peng Zhang, Jie Wang, Peng Jiang
Figure caption: The scaling relations for the member galaxies in the NGC 4111 group system. Left: the correlation between H I mass fraction and stellar mass. The black dotted line marks the place where the galaxy stellar mass equals the H I gas mass (F. Lelli 2022). The green dashed line indicates the typical correlation between H I mass fraction and stellar mass. Right: the correlation between stellar masses and g − r colors for the member galaxies. The green dashed line is the constant g − r value of 0.65, which we take to differentiate between blue and red galaxies (D. Nelson et al. 2018).
Paper: A Massive H I-absorption-selected Galaxy at z ≈ 2.356
Authors: B. Kaur, N. Kanekar, M. Neeleman, Y. Zhu, J. X. Prochaska, M. Rafelski, G. Becker
Figure caption: The SDSS spectrum of QSO J1020+2733 centered on the Lyα absorption feature at z = 2.3553. The green line is the continuum fit to the quasar spectrum obtained with the python package linetools. The orange line is a fit to the Lyα absorption profile at z = 2.3553, while the orange-shaded region shows the 1σ uncertainty on the fit. The 1σ uncertainty on the spectrum is shown in red. The spectrum also shows saturated Lyα absorption at z = 2.2876 (≈4000 Å).
Paper: Decay of Turbulent Upper-hybrid Waves in Weakly Magnetized Solar Wind Plasmas
Authors: F. J. Polanco-Rodríguez, C. Krafft, P. Savoini
Figure caption: (a)–(h): Spectral electric field energy ﹩{|{{\boldsymbol{E}}}_{{\boldsymbol{k}}}|}^{2}﹩ in the map (kxλD, kyλD), filtered around ωp, at times ωpt = 3100,  4400, 7200, and 14,800, for an unmagnetized plasma (upper row (a)–(d)) and a magnetized plasma with ωc/ωp = 0.07 (middle row (e)–(h)); superimposed black dashed lines represent the circles k = k0/2 and k = k0 (upper row) and the curves k*(θ) and k0 + k*(θ) (middle row); note that ﹩|{k}_{\ast }(\theta )|\lesssim 0.01{\lambda }_{D}^{-1}﹩. Black dots in panels (a), (b), (e), and (f) indicate the central wavenumbers of ﹩{ \mathcal L }{{ \mathcal Z }}^{(3)}﹩ and ﹩{ \mathcal L }{{ \mathcal Z }}^{(4)}﹩ broad spectral domains, estimated in 1D geometry; black and white arrows (in (b), (c), (f), and (g)) indicate forward or backward scatter and energy transport, respectively. Spectral domains of ﹩{{ \mathcal L }}^{(3)}﹩ and ﹩{{ \mathcal L }}^{(4)}﹩ (﹩{ \mathcal L }{{ \mathcal Z }}^{(3)}﹩ and ﹩{ \mathcal L }{{ \mathcal Z }}^{(4)}﹩) waves are delimited by black solid lines (in (a), (b), and (e)–(f)). (f): The region of ﹩{ \mathcal O }﹩-mode wave excitation is indicated by an arrow. Colorbars are the same for panels (a)–(h). (i) Dispersion relation of ﹩{\left|{{\boldsymbol{E}}}_{{\boldsymbol{k}}}\right|}^{2}﹩ integrated over propagation angles θ, in the plane (sign(kx)kλD, ω/ωp), for the magnetized plasma case, at late time ωpt = 13,500; superimposed white lines represent the dispersion curves of ﹩{ \mathcal L }{ \mathcal Z }﹩ waves as well as of electromagnetic ﹩{ \mathcal O }﹩-, ﹩{ \mathcal X }﹩- and ﹩{ \mathcal Z }﹩-mode waves, calculated via the magnetoionic theory at θ = 0 (solid lines) and θ = π/2 (dashed lines). The inset presents the theoretical dispersion curves (k, ω) of these modes calculated in a thermal plasma without beam and for monochromatic waves; the wavenumbers k*∥ and k*⊥ mentioned in the text are indicated by red dots. In panels (a)–(i), spectral energies are shown in arbitrary units and logarithmic scales. The lengths of simulation boxes are ﹩{L}_{x}\times {L}_{y}=5792\times 2896{\lambda }_{D}^{2},﹩ with grid numbers Nx = 4096 and Ny = 2048. All variables are normalized. The first set of physical parameters is used (see above).
Paper: Decay of Turbulent Upper-hybrid Waves in Weakly Magnetized Solar Wind Plasmas
Authors: F. J. Polanco-Rodríguez, C. Krafft, P. Savoini
Figure caption: (a) Variations with time of the energy densities W carried by the beam-driven ﹩{ \mathcal L }﹩ and ﹩{ \mathcal L }{ \mathcal Z }﹩ waves and their decay products ﹩{{ \mathcal L }}^{(n)}\,﹩and ﹩{ \mathcal L }{{ \mathcal Z }}^{(n)}﹩, respectively, with n ≤ 4,  for an unmagnetized plasma and weakly magnetized plasmas with ωc/ωp = 0.07 and ωc/ωp = 0.14. ﹩{ \mathcal L }{ \mathcal Z }﹩ and ﹩{ \mathcal L }﹩ are indicated by solid lines, ﹩{ \mathcal L }{ \mathcal Z }^{\prime} ﹩ and ﹩{ \mathcal L }^{\prime} ﹩ by dashed lines, ﹩{ \mathcal L }{ \mathcal Z }^{\prime\prime} ﹩ and ﹩{ \mathcal L }^{\prime\prime} ﹩ by dashed-dotted lines, ﹩{ \mathcal L }{{ \mathcal Z }}^{(3)}﹩ and ﹩{{ \mathcal L }}^{(3)}﹩ by dotted lines, and ﹩{ \mathcal L }{{ \mathcal Z }}^{(4)}﹩ and ﹩{{ \mathcal L }}^{(4)}﹩ by solid lines (see also legend). (b) Variations with time of wave energy densities W> (solid lines) and W< (dashed lines) within the spectral domains k > 2k0 and k < 2k0,  respectively, for ωc/ωp = 0, 0.02, 0.07,  and 0.14 (see also legend). Panels (a) and (b): Energies are normalized by the initial beam energy and expressed in logarithmic scales. All energies are several orders of magnitude higher than numerical noise. Panels (c) and (d): Ion density profiles δni(x, t)/n0 = (ni(x, t) − n0)/n0 at fixed y = 33λD, filtered in wavelength ranges corresponding to ﹩{ \mathcal S }^{\prime} ﹩ and ﹩{{ \mathcal S }}^{{\prime\prime} }﹩ waves (c) and ﹩{{ \mathcal S }}^{(3)}﹩ and ﹩{{ \mathcal S }}^{(4)}﹩ waves (d), as a function of x/λD and ωpt. Energies of ﹩{{ \mathcal S }}^{(n)}﹩ waves propagate with group velocities cs/vT for n = 1 (c), n = 3 (d) and −cs/vT for n = 2 (c), n = 4 (d), as highlighted by the four orange-colored regions (see also the text). For comparison, green arrows with slopes ﹩\pm {c}_{s}/{v}_{T}=\pm 0.026﹩ are represented. All variables are normalized. Parameters are the same as in Figure 1.
Paper: Decay of Turbulent Upper-hybrid Waves in Weakly Magnetized Solar Wind Plasmas
Authors: F. J. Polanco-Rodríguez, C. Krafft, P. Savoini
Figure caption: Spectral electric field energy ﹩{\left|{{\boldsymbol{E}}}_{{\boldsymbol{k}}}\right|}^{2}﹩ around the frequency ωp (in logarithmic scales and arbitrary units) in the map (kxλD, kyλD), at different times ωpt = 5400,  9900, 14,800, and 25,000 corresponding to the four columns, respectively, for an unmagnetized plasma (upper row (a)–(d)) and a weakly magnetized plasma with ωc/ωp = 0.07 (bottom row (e)–(h)). Filtering in the frequency domain 0.9ωp ≤ ω ≤ 1.1ωp is performed. The circles k = k0 and k = 2k0 are represented by black dashed lines. The lengths of simulation boxes are Lx = Ly = 1448λD, with grid numbers Nx = Ny = 1024. All variables are normalized. The same colorbars are used for all panels, to enable relevant comparisons. The first set of physical parameters is used (see above).
Paper: A Massive H I-absorption-selected Galaxy at z ≈ 2.356
Authors: B. Kaur, N. Kanekar, M. Neeleman, Y. Zhu, J. X. Prochaska, M. Rafelski, G. Becker
Figure caption: ALMA CO(3–2) emission from the H I-selected galaxy in the field of the z = 2.3553 DLA toward QSO J1020+2733. (a) The velocity-integrated ALMA CO(3–2) image of DLA1020+2733g. The contours are at (−3.0, 3.0, 4.2, 6, 8.5, 12, 17.0) × σ significance, with dashed negative contours. The axes are relative to the QSO position, indicated by the black star. (b) The ALMA CO(3–2) emission spectrum of DLA1020+2733g, obtained by taking a cut through the CO cube at the location of the peak in [A]. The dashed gray curves indicate the ±1σ error on the spectrum.
Paper: A Massive H I-absorption-selected Galaxy at z ≈ 2.356
Authors: B. Kaur, N. Kanekar, M. Neeleman, Y. Zhu, J. X. Prochaska, M. Rafelski, G. Becker
Figure caption: VLA CO(1–0) emission from the H I-selected galaxy in the field of the z = 2.3553 DLA toward QSO J1020+2733. (a) The velocity-integrated VLA CO(1–0) image of DLA1020+2733g. The contours are at (3.0, 4.0, 5.0, 6.0) × σ significance. We note that there are no negative contours at ≤−3σ significance in the image. The axes are relative to the QSO position, indicated by the black star. (b) The VLA CO(1–0) emission spectrum of DLA1020+2733g, obtained by taking a cut through the CO cube at the location of the peak in (a). The gray bands represent the edges of the digital subbands of the WIDAR correlator. The dashed gray curves indicate the ±1σ error on the spectrum.
Paper: A Massive H I-absorption-selected Galaxy at z ≈ 2.356
Authors: B. Kaur, N. Kanekar, M. Neeleman, Y. Zhu, J. X. Prochaska, M. Rafelski, G. Becker
Figure caption: A selection of low- and intermediate-ion metal lines associated with the DLA at z = 2.3553 toward QSO J1020+2733, detected in the ESI spectrum. The 1σ uncertainty on the ESI spectrum is shown in red. The metal column densities determined from the detected lines, over the velocity range (−350, +500) km s−1, are listed in Table 1. Absorption is seen over a velocity range of ≈700 km s−1, with Δv90 = 480 ± 50 km s−1, measured from the Zn IIλ2026 transition.
Paper: A Massive H I-absorption-selected Galaxy at z ≈ 2.356
Authors: B. Kaur, N. Kanekar, M. Neeleman, Y. Zhu, J. X. Prochaska, M. Rafelski, G. Becker
Figure caption: ALMA 104 GHz continuum image of the field of the z = 2.3553 DLA toward QSO J1020+2733. The location of the H I-selected galaxy DLA1020+2733g is indicated by the black plus, marked as “G.” The contours are at (3.0, 4.0) × σ significance, where σ = 27 μJy is the rms noise on the continuum image. We note that there are no negative contours at ≤−3σ significance in the image. The axes are relative to the QSO position, indicated by the black star.
Paper: A Massive H I-absorption-selected Galaxy at z ≈ 2.356
Authors: B. Kaur, N. Kanekar, M. Neeleman, Y. Zhu, J. X. Prochaska, M. Rafelski, G. Becker
Figure caption: A comparison between the velocity profiles of (a) the CO(3–2) emission and (b) the CO(1–0) emission detected from DLA1020+2733g, with that of [C] the low-ionization metal absorption line, Fe IIλ2600. The velocity scale is relative to the DLA redshift, z = 2.3553. The velocity extent of the absorption and emission are seen to be in remarkable agreement.
Paper: Multipoint Observations of Magnetic Reconnection in the Martian Magnetotail Triggered by an Interplanetary Magnetic Field Rotation
Authors: Yuanzheng Wen, Jasper S. Halekas, Han-Wen Shen, Abigail R. Azari, David A. Brain, Yaxue Dong, David L. Mitchell, Christian X. Mazelle, Jared R. Espley, James P. McFadden
Figure caption: Average magnetic field draping map in MSE coordinates from C. Zhang et al. (2022), shown in the XY (a) and YZ (b) planes. The color map represents the Bx component, with red indicating sunward and blue indicating tailward directions. MAVEN’s trajectory in MSE coordinates is shown with colored lines, and gray arrows indicate the magnetic field direction recorded by MAVEN. The dashed black arrow indicates the rapid transition of MAVEN’s trajectory in MSE coordinates after the IMF rotation.
Paper: Multipoint Observations of Magnetic Reconnection in the Martian Magnetotail Triggered by an Interplanetary Magnetic Field Rotation
Authors: Yuanzheng Wen, Jasper S. Halekas, Han-Wen Shen, Abigail R. Azari, David A. Brain, Yaxue Dong, David L. Mitchell, Christian X. Mazelle, Jared R. Espley, James P. McFadden
Figure caption: Zoom-in view of the event during 01:17:00–01:22:00 UT on 2021 December 5. (a) Three components of the magnetic field in LMN coordinates. (b)–(d) Velocity components of H+, O+, and ﹩{{\rm{O}}}_{2}^{+}﹩ ions in LMN coordinates. (e) Pitch angle distribution of electrons in the energy range of 111–140 eV. (f)–(h) Energy spectrograms of H+, O+, and ﹩{{\rm{O}}}_{2}^{+}﹩, respectively.
Paper: Multipoint Observations of Magnetic Reconnection in the Martian Magnetotail Triggered by an Interplanetary Magnetic Field Rotation
Authors: Yuanzheng Wen, Jasper S. Halekas, Han-Wen Shen, Abigail R. Azari, David A. Brain, Yaxue Dong, David L. Mitchell, Christian X. Mazelle, Jared R. Espley, James P. McFadden
Figure caption: Schematic representation of the reconfiguration of Mars’s induced magnetosphere in response to the IMF rotation. (a) The induced magnetosphere of Mars before the IMF rotation. (b) The IMF rotates and the reversed IMF starts to drape around Mars. (c) MAVEN observed a magnetic reconnection between the oppositely directed draped magnetic field lines, leading to the formation of Hall magnetic fields and ion jets. Panel (d) illustrates the final reconfiguration after the IMF rotation, with newly draped magnetic field lines surrounding Mars. Modified based on N. J. Edberg et al. (2011).
Paper: Multipoint Observations of Magnetic Reconnection in the Martian Magnetotail Triggered by an Interplanetary Magnetic Field Rotation
Authors: Yuanzheng Wen, Jasper S. Halekas, Han-Wen Shen, Abigail R. Azari, David A. Brain, Yaxue Dong, David L. Mitchell, Christian X. Mazelle, Jared R. Espley, James P. McFadden
Figure caption: Overview of the current sheet crossing event on 2021 December 5 during 01:10:00–01:25:00 UT. (a) Orbits of MAVEN and Tianwen-1 in the X–R plane, ﹩R=\sqrt{{Y}^{2}+{Z}^{2}}﹩. The black curve represents the bow shock and induced magnetosphere boundary models based on D. Vignes et al. (2000). (b) Tianwen-1 magnetic field data in MSO coordinates. (c) MAVEN magnetic field data in MSO coordinates. ((d), (e), (f)) Velocity components of O+, H+, and ﹩{{\rm{O}}}_{2}^{+}﹩, respectively, in MSO coordinates. (g) Electron spectrogram from MAVEN SWEA. ((h), (i), (j)) O+, H+, and ﹩{{\rm{O}}}_{2}^{+}﹩ energy spectrograms from MAVEN STATIC.
Paper: Multipoint Observations of Magnetic Reconnection in the Martian Magnetotail Triggered by an Interplanetary Magnetic Field Rotation
Authors: Yuanzheng Wen, Jasper S. Halekas, Han-Wen Shen, Abigail R. Azari, David A. Brain, Yaxue Dong, David L. Mitchell, Christian X. Mazelle, Jared R. Espley, James P. McFadden
Figure caption: Panel (a) shows the magnetic field in LMN coordinates. Panel (b) shows densities of H+ (black), O+ (blue), and ﹩{{\rm{O}}}_{2}^{+}﹩ (red) in the time interval 01:15:00–01:25:00 UT.
Paper: Multipoint Observations of Magnetic Reconnection in the Martian Magnetotail Triggered by an Interplanetary Magnetic Field Rotation
Authors: Yuanzheng Wen, Jasper S. Halekas, Han-Wen Shen, Abigail R. Azari, David A. Brain, Yaxue Dong, David L. Mitchell, Christian X. Mazelle, Jared R. Espley, James P. McFadden
Figure caption: Scatter plot of averaged ion velocities in the Hoffmann–Teller (HT) frame vs. the Alfvén velocity before (left) and after (right) the current sheet crossing.
Paper: Multipoint Observations of Magnetic Reconnection in the Martian Magnetotail Triggered by an Interplanetary Magnetic Field Rotation
Authors: Yuanzheng Wen, Jasper S. Halekas, Han-Wen Shen, Abigail R. Azari, David A. Brain, Yaxue Dong, David L. Mitchell, Christian X. Mazelle, Jared R. Espley, James P. McFadden
Figure caption: Tianwen-1 and MAVEN trajectories along with observed magnetic field vectors (orange arrows) in (a) the XMSO–ZMSO plane and (b) the XMSO–YMSO plane.
Paper: Density Fluctuation–Mach Number Scaling in Compressible, High Plasma Beta Turbulence: In Situ Space Observations and High-Reynolds Number Simulations
Authors: Riddhi Bandyopadhyay, James R. Beattie, Amitava Bhattacharjee
Figure caption: The variation of relative density fluctuations, δρ/ρ0, with turbulent Mach number, ﹩{{ \mathcal M }}_{t}﹩, in Earth’s magnetosheath, measured by MMS (blue contours of the joint probability distribution function between, ﹩{{ \mathcal M }}_{t}﹩ and δρ/ρ0, ﹩p({{ \mathcal M }}_{t},\delta \rho /{\rho }_{0})﹩) and from a 10,0803, highly compressible MHD simulation (red dots; by combining Equations (14) and (16)). A best fit to the MMS data gives ﹩\delta \rho /{\rho }_{0}=(0.8{3}_{-0.58}^{+0.54}){{ \mathcal M }}_{t}^{0.9{2}_{-0.29}^{+0.30}}﹩ and the simulation data yields ﹩\delta \rho /{\rho }_{0}\,=(0.9{7}_{-0.23}^{+0.23}){{ \mathcal M }}_{t}^{0.9{4}_{-0.15}^{+0.15}}﹩. The two dashed lines of slope unity are shown for proportionality constants b = 1/3 and b = 1 (see Equation (5)).
Paper: Mass-dependent Radial Distribution of Single and Binary Stars in the Pleiades and Their Dynamical Implications
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption:  ﹩{R}_{50}-{{ \mathcal M }}_{{\rm{obj}}}﹩ relations for all objects (circles with error bars), single stars (green line), and binaries (orange line). Mass bins are separated by [0.38, 0.66, 1.14, 2.00]﹩{{ \mathcal M }}_{\odot }﹩, which are approximately equal logarithmic-mass intervals except for the most massive bin. The most massive bin for single stars is neglected due to insufficient numbers. R50,C is the half-number radius of the whole MS sample. The error bars are estimated from the interval of 16% to 84% of the corresponding R distribution of each subsample, but divided by the factor of ﹩{n}_{{\rm{sub}}}^{1/2}﹩. The gray degree of symbols represents the binary fraction in each mass bin. Horizontal green and orange dashed lines represent R50 values of singles and binaries for the entire mass range. The vertical black dotted line denotes the location of ﹩{{ \mathcal M }}_{{\rm{seg}}}﹩.