adsabs/AstroCLIMB huggingface dataset:
Paper: The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies
Authors: Juno Li, Elisabete Da Cunha, Jorge González-López, Manuel Aravena, Ilse De Looze, N. M. Förster Schreiber, Rodrigo Herrera-Camus, Justin Spilker, Ken-ichi Tadaki, Loreto Barcos-Munoz, Andrew J. Battisti, Jack E. Birkin, Rebecca A. A. Bowler, Rebecca Davies, Tanio Díaz-Santos, Andrea Ferrara, Deanne B. Fisher, Jacqueline Hodge, Ryota Ikeda, Meghana Killi, Lilian Lee, Daizhong Liu, Dieter Lutz, Ikki Mitsuhashi, Thorsten Naab, Ana Posses, Monica Relaño, Manuel Solimano, Hannah Übler, Stefan Anthony van der Giessen, Vicente Villanueva
Figure caption: Radial distributions of the median deviation in sSFR, A  V , and ﹩{{\rm{\Sigma }}}_{{M}_{* }}﹩ per radial bin measured from the center for all 14 sources, comparing the spatially resolved SED fits with and without ALMA (similar to the right-hand column of Figure 7). The shaded regions indicate the standard deviation for each radial bin.
Paper: The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies
Authors: Juno Li, Elisabete Da Cunha, Jorge González-López, Manuel Aravena, Ilse De Looze, N. M. Förster Schreiber, Rodrigo Herrera-Camus, Justin Spilker, Ken-ichi Tadaki, Loreto Barcos-Munoz, Andrew J. Battisti, Jack E. Birkin, Rebecca A. A. Bowler, Rebecca Davies, Tanio Díaz-Santos, Andrea Ferrara, Deanne B. Fisher, Jacqueline Hodge, Ryota Ikeda, Meghana Killi, Lilian Lee, Daizhong Liu, Dieter Lutz, Ikki Mitsuhashi, Thorsten Naab, Ana Posses, Monica Relaño, Manuel Solimano, Hannah Übler, Stefan Anthony van der Giessen, Vicente Villanueva
Figure caption: Radial distribution of the surface density of SFRUV (blue) and SFRIR (red) for all our CRISTAL galaxies. The error bars reflect the scatter within each radial bin. Straight lines show the best linear fits to the radial distributions. The best-fit values for the slopes are shown in the legend.
Paper: The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies
Authors: Juno Li, Elisabete Da Cunha, Jorge González-López, Manuel Aravena, Ilse De Looze, N. M. Förster Schreiber, Rodrigo Herrera-Camus, Justin Spilker, Ken-ichi Tadaki, Loreto Barcos-Munoz, Andrew J. Battisti, Jack E. Birkin, Rebecca A. A. Bowler, Rebecca Davies, Tanio Díaz-Santos, Andrea Ferrara, Deanne B. Fisher, Jacqueline Hodge, Ryota Ikeda, Meghana Killi, Lilian Lee, Daizhong Liu, Dieter Lutz, Ikki Mitsuhashi, Thorsten Naab, Ana Posses, Monica Relaño, Manuel Solimano, Hannah Übler, Stefan Anthony van der Giessen, Vicente Villanueva
Figure caption: Comparison between the resolved sum and integrated stellar mass (top panel) and SFR (bottom panel) of the CRISTAL galaxies. There are no offsets between the integrated and resolved properties.
Paper: The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies
Authors: Juno Li, Elisabete Da Cunha, Jorge González-López, Manuel Aravena, Ilse De Looze, N. M. Förster Schreiber, Rodrigo Herrera-Camus, Justin Spilker, Ken-ichi Tadaki, Loreto Barcos-Munoz, Andrew J. Battisti, Jack E. Birkin, Rebecca A. A. Bowler, Rebecca Davies, Tanio Díaz-Santos, Andrea Ferrara, Deanne B. Fisher, Jacqueline Hodge, Ryota Ikeda, Meghana Killi, Lilian Lee, Daizhong Liu, Dieter Lutz, Ikki Mitsuhashi, Thorsten Naab, Ana Posses, Monica Relaño, Manuel Solimano, Hannah Übler, Stefan Anthony van der Giessen, Vicente Villanueva
Figure caption: Resolved SED fitting results of CRISTAL-25 with all filters available included. Panels show the same properties as in Figure 2.
Paper: The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies
Authors: Juno Li, Elisabete Da Cunha, Jorge González-López, Manuel Aravena, Ilse De Looze, N. M. Förster Schreiber, Rodrigo Herrera-Camus, Justin Spilker, Ken-ichi Tadaki, Loreto Barcos-Munoz, Andrew J. Battisti, Jack E. Birkin, Rebecca A. A. Bowler, Rebecca Davies, Tanio Díaz-Santos, Andrea Ferrara, Deanne B. Fisher, Jacqueline Hodge, Ryota Ikeda, Meghana Killi, Lilian Lee, Daizhong Liu, Dieter Lutz, Ikki Mitsuhashi, Thorsten Naab, Ana Posses, Monica Relaño, Manuel Solimano, Hannah Übler, Stefan Anthony van der Giessen, Vicente Villanueva
Figure caption: Left: f obs vs. ﹩{{\rm{\Sigma }}}_{{M}_{* }}﹩ for CRISTAL-02 assuming the 2D T dust profile shown in the central panel. Center: 2D Sérsic T dust profile with n = 1 and R  e  = 0.″25 (R. K. Cochrane et al. 2019). The dust temperature profile peaks where the dust emission peaks, and is shifted up to achieve a maximum temperature ∼65 K and minimum temperature of 20 K. Right: f obs map of CRISTAL-02 with the T dust profile, generated using an optically thin modified blackbody dust emission model with emissivity index β = 2. The red contours show the observed ALMA Band 7 dust continuum.
Paper: The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies
Authors: Juno Li, Elisabete Da Cunha, Jorge González-López, Manuel Aravena, Ilse De Looze, N. M. Förster Schreiber, Rodrigo Herrera-Camus, Justin Spilker, Ken-ichi Tadaki, Loreto Barcos-Munoz, Andrew J. Battisti, Jack E. Birkin, Rebecca A. A. Bowler, Rebecca Davies, Tanio Díaz-Santos, Andrea Ferrara, Deanne B. Fisher, Jacqueline Hodge, Ryota Ikeda, Meghana Killi, Lilian Lee, Daizhong Liu, Dieter Lutz, Ikki Mitsuhashi, Thorsten Naab, Ana Posses, Monica Relaño, Manuel Solimano, Hannah Übler, Stefan Anthony van der Giessen, Vicente Villanueva
Figure caption: Resolved SED fitting results of CRISTAL-25 without the ALMA observation included. Panels show the same properties as in Figure 2.
Paper: Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Jonathan P. Williams, Caleb Painter, Alexa R. Anderson, Alvaro Ribas
Figure caption: The relation between disk and stellar masses for different surface density constraints. The blue points show the disk mass under the assumption that it is the dust mass multiplied by a gas-to-dust ratio of 100. The red and teal points show the masses where the minimum value of the Toomre parameter, ﹩{Q}_{\min }﹩ equals 1 or 2, respectively. The lines show linear fits in each case where the slope is 0.01 (M disk = 100 M dust), 0.11 (﹩{Q}_{\min }=2﹩), and 0.21 (﹩{Q}_{\min }=1﹩).
Paper: Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Jonathan P. Williams, Caleb Painter, Alexa R. Anderson, Alvaro Ribas
Figure caption: Surface density profiles for a ﹩{Q}_{\min }=1﹩ disk as a function of gas disk radius ranging from R CO,90% = 50 to 500 au. The filled circles along each curve show the dust disk size, R dust,90%, at λ = 1 mm for different values of the dust drift time, labeled in megayears. The profiles here all have γ = 1.
Paper: Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Jonathan P. Williams, Caleb Painter, Alexa R. Anderson, Alvaro Ribas
Figure caption: The radial variation of surface density and Toomre Q as in Figure 1 but for the full disk sample (Part II).
Paper: Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Jonathan P. Williams, Caleb Painter, Alexa R. Anderson, Alvaro Ribas
Figure caption: The radial variation of surface density and Toomre Q as in Figure 1 but for the full disk sample (Part I).
Paper: Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Jonathan P. Williams, Caleb Painter, Alexa R. Anderson, Alvaro Ribas
Figure caption: The ratio of drift time to stellar age for different values of the stability threshold, ﹩{Q}_{\min }﹩.
Paper: NGC 7314: X-Ray Study of the Evolving Accretion Properties
Authors: Debjit Chatterjee, Arghajit Jana, A. Mangalam, Hsiang-Kuang Chang
Figure caption: Variation of χ ((data-model)/error) for (a) Model 1 (TBABS*ZTBABS*ZCUTOFFPL), (b) Model 2 (TBABS*ZTBABS*(BBODY+ZGAUSSIAN+ZCUTOFFPL)), (c) Model 3 (TBABS*ZTBABS*(RELXILL+BBODY)), and (d) Model 4 (TBABS*ZTBABS*GABS*(RELXILL+BBODY+XILLVER)). The black, red, and green represent the 0.5–10 keV XMM-Newton, 3–78 keV NuSTAR FPMA and FPMB spectra, respectively.
Paper: NGC 7314: X-Ray Study of the Evolving Accretion Properties
Authors: Debjit Chatterjee, Arghajit Jana, A. Mangalam, Hsiang-Kuang Chang
Figure caption: (a) Unfolded spectrum of RELXILL+BBODY+XILLVER. (b) χ 2 variation of the upper panel spectrum. The black, red, and green represent the 0.5–10 keV XMM-Newton and the 3–78 keV NuSTAR FPMA and FPMB spectra, respectively. The dashed orange, cyan, and magenta lines indicate the BBODY, relxill, and XILLVER component, respectively. The blue line represents the combined model fitted spectrum.
Paper: NGC 7314: X-Ray Study of the Evolving Accretion Properties
Authors: Debjit Chatterjee, Arghajit Jana, A. Mangalam, Hsiang-Kuang Chang
Figure caption: Variation of photon indices (Γ) with log λ for RXTE/PCA data. λ is the ratio between L bol and L Edd. L bol is considered to be 20 × L 2−10 keV (R. V. Vasudevan et al. 2009; F. Duras et al. 2020).
Paper: NGC 7314: X-Ray Study of the Evolving Accretion Properties
Authors: Debjit Chatterjee, Arghajit Jana, A. Mangalam, Hsiang-Kuang Chang
Figure caption: Variation of photon indices (Γ) and power-law flux (in 10−11 erg s−1 cm−2) with MJD (for RXTE/PCA data).
Paper: NGC 7314: X-Ray Study of the Evolving Accretion Properties
Authors: Debjit Chatterjee, Arghajit Jana, A. Mangalam, Hsiang-Kuang Chang
Figure caption: 300 s time binned light curves of four XMM-Newton data. The dates are mentioned at the bottom of each column. The three rows represent 0.2–3 keV (soft; red), 3–10 keV (hard; green), and 0.2–10 keV (total; blue) light curves, respectively.
Paper: NGC 7314: X-Ray Study of the Evolving Accretion Properties
Authors: Debjit Chatterjee, Arghajit Jana, A. Mangalam, Hsiang-Kuang Chang
Figure caption: 300 s time binned light curves of combined NuSTAR FPMA and FPMB. The three panels represent (a) 3–10 keV (soft; red), (b) 10–78 keV (hard; green), and (c) 3–78 keV (total; blue) light curves, respectively.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Subplot (a) displays a 3D view of the leading (crimson) and trailing (white) structures of the CMEs, overlaid on a 2D snapshot of the SW speed in the equatorial plane. The dashed white box indicates the regions shown in subplots (b) and (c). They depict the traced CME boundaries for cases (b) LSLDLF0 and (c) LSHDLF0, with color-filled contours illustrating the plasma speed regions: slow, fast, and >600 km s−1. The gray line contours indicate HD regions, with darker shades representing higher scaled densities. The blue, green, and orange dots mark the positions of virtual spacecraft at −10°, 0°, and +10°.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Reproduction of Figure 12 (satellite luminosity functions) of Paper II from DR2 with the DR3 SAGA data. Left: cumulative satellite r-band luminosity function for each of the 101 SAGA systems (colored solid lines), MW (black dashed line), and M31 (black dotted–dashed line). The colored solid lines show only the confirmed SAGA satellites, and the shaded region shows incompleteness correction as discussed in Appendix B.1. The SAGA Survey’s designed depth is about M  r,o  = −12, shown as the vertical gray line. Right: average cumulative satellite r-band luminosity function, with satellite luminosity normalized by the luminosities of their respective host galaxies (calculated as differences in magnitudes). The average luminosity function of SAGA systems is shown as the green-filled squares. The incompleteness correction is included in the filled squares, and uncorrected results are shown as green open squares. The yellow dotted–dashed line shows the average luminosity function of systems in the COSMOS field (Nierenberg et al. 2012), the purple band SDSS (Sales et al. 2013), and the blue-dashed line the incompleteness-corrected ELVES survey (Carlsten et al. 2022, the uncorrected version is shown as the faint blue-dashed line that is almost identical to the corrected line). See the text in Appendix A for the specific system selections. The error bars show Poisson noise on the luminosity functions.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The arrival of the trailing shock at the rear and at the front of CME1. Subplot (a) shows the result for the HSHDLF0 case along 0° and ±10°. Subplot (b) depicts the speed variation at the rear of CME1, along −10°, for all cases with 0° tilt. Similarly, subplot (c) shows the speed at the front of CME1.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The subplots demonstrate the evolution of the trailing shock in the inner heliosphere for cases LSLDLF0 (a1–a4) and LSHDLF0 (b1–b4). The displayed color map corresponds to the plasma temperature on the logarithmic scale.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Upper: the velocity difference between all pairs of confirmed satellites in the SAGA Survey, binned by the projected separation between the two satellites. In each bin, the distribution of the velocity difference is shown as the median value (red triangles) and the 16th and 84th percentiles (lower and higher caps). The light gray bands show the 1σ  distribution of the velocity difference when all satellites are assigned a position angle (relative to their hosts) uniformly at random. Lower: the number of pairs in bins of projected separation. The observed numbers are shown in red lines. The gray bands show the 1σ  distribution of the number of pairs when all satellites are assigned a position angle (relative to their hosts) uniformly at random.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: How SAGA satellite systems vary across host/system properties. The upper panels are the average number of satellites per system, and the lower panels are satellite stellar mass functions. The SAGA systems are split into quartiles using four different host/system properties: (from left to right) the stellar mass of the most massive satellite, the group (halo) mass, the sSFR of the host galaxy, and the H I mass of the host galaxy. Each panel in the upper row shows the average number of satellites per system as a function of the corresponding host/system property. The points connected by the gold line (lower line) show the average number of satellites in the Gold sample, and the higher points connected by the silver line (upper line) show that of the Gold+Silver sample. Each panel in the lower row shows how the average cumulative SMF changes with the corresponding host/system property. The colors of the points in the upper panel correspond to the colors of the lines in the lower panel, with darker colors indicating higher quartiles.
Paper: Study of Evolution and Geo-effectiveness of Coronal Mass Ejection–Coronal Mass Ejection Interactions Using Magnetohydrodynamic Simulations with SWASTi Framework
Authors: Prateek Mayank, Stefan Lotz, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: This figure showcases the propagation of reverse shocks inside CME2. The top subplots ((a1), (b1), and (c1)) show in situ measurements from virtual spacecraft as CME2 of the HSHDHF0 case passes through, highlighting forward shocks (FSs) and reverse shocks (RSs). The bottom subplots display 2D snapshots of (a2) radial velocity (km s−1), (b2) density (log scale, N cm–3), and (c2) magnetic field strength (log scale, nT). The white contour indicates the boundary of CME2.
Paper: The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way–mass Galaxies
Authors: Yao-Yuan Mao, Marla Geha, Risa H. Wechsler, Yasmeen Asali, Yunchong Wang, Erin Kado-Fong, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Benjamin Weiner, Mithi A. C. de los Reyes, John F. Wu
Figure caption: Same as Figure 16 but the y-axis here shows the host galaxy’s sSFR (inferred from NUV measurements; values shown are ﹩\mathrm{log}[{\dot{M}}_{\star }/{M}_{\star }\cdot \mathrm{yr}]﹩).
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Radiation spectra from simulations of a steady jet (left), a variable jet (center), and a precessing jet (right), at time t = 50 (in code units). In all three panels, the blue, orange, and green curves represent the inclination ﹩{\hat{{\boldsymbol{n}}}}_{\mathrm{los}}=90^\circ ﹩, 45°, and 10° respectively. Fluxes are integrated over the whole computational domain, similar to an unresolved core emission.
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Distribution of the peak frequency at which the electrons in a grid cell radiate. Shown for the steady jet Std90 (left), variable jet Var90 (center), and precessing jet Prc90 (right) at time t = 50 and for inclination to the LOS ﹩{\hat{{\boldsymbol{n}}}}_{\mathrm{los}}=90^\circ ﹩. The color bars shows the log of peak frequency (in GHz) of the grid cell. Different peak frequencies shown here correspond to different electron populations. This 2D distribution is derived from the intensity map, and thus the LOS-integrated 3D emissivity, projected into the plane of the sky.
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Mock radiant-intensity (ν I  ν ) distribution (in log scale) in the plane of the sky for the steady jet Std90 at time t = 50 and frequency ν = 1 GHz (left), 9 × 104 GHz (center), and 109 GHz (right), lying in the radio, optical, and X-ray regime, respectively. The color bars indicate the levels of radiant intensity in ﹩{10}^{9}\,\mathrm{erg}\,{{\rm{s}}}^{-1}{\mathrm{cm}}^{-2}{\mathrm{str}}^{-1}﹩ (in log scale).
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Distribution of the peak frequency at which the electrons in a grid cell radiate. Shown are the 2D slices of the 3D distribution at z = 220 (recollimation shock; left), z = 390 (strong, steady shock; center), and z = 685 (Mach shock; right) for the steady jet Std90 at time t = 50 and for inclination to the LOS ﹩{\hat{{\boldsymbol{n}}}}_{\mathrm{los}}=90^\circ ﹩. The color bars shows the log of peak frequency (in GHz) of the grid cell. Different peak frequencies shown here correspond to different electron populations. These 2D slices are derived from the 3D emissivity maps (ν J  ν ).
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Intensity distribution I  ν  at ν = 1 GHz in the 2D plane of the sky for the variable jet Var90 for t = 40–50, as mentioned in the panel titles. Indicated with different colors are the positions of various knots and their average pattern speed v av.
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Light curves of the integrated jet luminosity ν L  ν  showing variation of log of total luminosity with time t, representing an unresolved core luminosity. Shown are the values at frequency ν = 1, 9 × 104, and 109 GHz in blue, orange, and green color respectively, for the jet Std10 (left), Var10 (center), and Prc10 (right).
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Intensity distribution I  ν  at ν = 1 GHz in the 2D plane of the sky for the precessing-jet simulation Prc90 for times t = 40–50, as mentioned in the panel titles. Shown also, with the respective colors, are the relative distances ﹩{ \mathcal R }﹩ of various knots, from which we calculate their average pattern speed v av.
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Intensity I  ν  map for frequency ν = 1 GHz in the 2D plane of the sky for the steady jet Std90 for times t = 20, 30, 40, and 50 (from left to right). Indicated with different colors are the positions of various knots at different times (left) and their average pattern speed v av (right).
Paper: Particles in Relativistic Magnetohydrodynamic Jets. II. Bridging Jet Dynamics with Multi–wave band Nonthermal Emission Signatures
Authors: Ravi Pratap Dubey, Christian Fendt, Bhargav Vaidya
Figure caption: Histogram showing the number of (macro)particles (in log scale) with respect to their maximum electron energies ﹩{\gamma }_{\max }﹩ for simulation Std90 (blue), Var90 (orange), and Prc90 (green) at time t = 50, accounting for all the particles present in the domain.