adsabs/AstroCLIMB huggingface dataset:
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: Upper panel: radial profile of the jet in 3C 273 with different models of power-law functions. Measurement data are the same as in Figure 8. The gray dashed line shows the best-fit single power-law function (r ∝ z  a ) with a = 0.80 obtained from all the data except for the gray shaded region. The red solid line shows the best-fit broken power-law function as presented in Figure 8. Lower panel: fractional deviations of the jet radii from the obtained models. The red and gray squares correspond to the deviations from the lines in the upper panel.
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: The core position along the large-scale jet axis as a function of the frequency based on the fitted power-law model. The core positions, denoted by the black dots, are relative to the 86 GHz core. The red line shows the best-fit power-law model, and the black line shows the best-fit location of the central black hole. The error bars of the best-fit core positions and the shaded area of the best-fit model indicate the 68% confidence interval estimated from the χ 2 surface of the fitted parameters (Section 5.4).
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: The jet radius and PA profiles of the 3C 273 jet, extended from Figure 8 to include measurements of the large-scale jet beyond the deprojected distance of ∼200 kpc traced with VLA 5 GHz and MERLIN 1.6 GHz.
Paper: Collimation of the Relativistic Jet in the Quasar 3C 273
Authors: Hiroki Okino, Kazunori Akiyama, Keiichi Asada, José L. Gómez, Kazuhiro Hada, Mareki Honma, Thomas P. Krichbaum, Motoki Kino, Hiroshi Nagai, Uwe Bach, Lindy Blackburn, Katherine L. Bouman, Andrew Chael, Geoffrey B. Crew, Sheperd S. Doeleman, Vincent L. Fish, Ciriaco Goddi, Sara Issaoun, Michael D. Johnson, Svetlana Jorstad, Shoko Koyama, Colin J. Lonsdale, Ru-Sen Lu, Ivan Martí-Vidal, Lynn D. Matthews, Yosuke Mizuno, Kotaro Moriyama, Masanori Nakamura, Hung-Yi Pu, Eduardo Ros, Tuomas Savolainen, Fumie Tazaki, Jan Wagner, Maciek Wielgus, Anton Zensus
Figure caption: The apparent velocity (top) and collimation profile (bottom) as functions of the projected distance from the black hole. The black dotted line represents the best-fit location of the collimation break.
Paper: Does the Gamma-Ray Binary LS I + 61°303 Harbor a Magnetar?
Authors: Arthur G. Suvorov, Kostas Glampedakis
Figure caption: “Weak-field” P(t) tracks for LSI, with assumed accretion rates of ﹩\dot{M}={10}^{-2}﹩ and ﹩{10}^{-3}{\dot{M}}_{{\rm{E}}{\rm{d}}{\rm{d}}}﹩ for t ≥ 5 kyr in the left and right panels, respectively, though with negligible propeller torques at earlier times. The blue (red) curve, whose width accounts for a fiducial uncertainty in the maximum period derivative, viz. ﹩3.2\leqslant \dot{P}/{10}^{-10}\leqslant 4.4﹩, has ξ = 0.09(0.04). We fix the (intrinsic) braking index at n = 3 and inclination angle at α = 0. The polar field strength, as shown in the panel legends, is chosen such that the torques produce the requisite ﹩\dot{P}﹩ when P = 0.269 s. The figure insets display the period derivative; the rapid rise occurs because strong propeller torques are turned on.
Paper: Proper Motions, Orbits, and Tidal Influences of Milky Way Dwarf Spheroidal Galaxies
Authors: Andrew B. Pace, Denis Erkal, Ting S. Li
Figure caption: Relative fractional error compared to the distance for the pericenter (﹩{\sigma }_{{r}_{\mathrm{peri}}};﹩ left panels) and apocenter (﹩{\sigma }_{{r}_{\mathrm{apo}}};﹩ right panels) due to fixing the error to zero for the systemic proper motion (blue points), distance (orange points), MW potential (green points), and LMC mass (red points). For each galaxy there are four entries, and in each entry three of the previously mentioned errors are set to the current value and one is set to zero to analyze its impact. Low factions correspond to the majority of current error being due to the fixed parameter, and high fractions indicate that current error in the fixed property does not significantly affect the total error. The current error in the pericenter is dominated by the distance and/or proper motion uncertainties, whereas the current error in the apocenter is dominated by the distance and/or potential uncertainties. To aid in interpreting the sources of error, we show a histogram of the fractional uncertainties next to each panel.
Paper: Does the Gamma-Ray Binary LS I + 61°303 Harbor a Magnetar?
Authors: Arthur G. Suvorov, Kostas Glampedakis
Figure caption: Propeller spin-down rate for LSI, ﹩\dot{\nu }﹩, calculated with the torque (Equation (10)), as a function of the polar field, B  p /1012 G. Each of the two shaded bands corresponds to an ﹩\dot{M}﹩ range varying from ﹩\dot{M}={10}^{-2}﹩ (leftmost dashed curves) to ﹩{10}^{-4}{\dot{M}}_{{\rm{E}}{\rm{d}}{\rm{d}}}﹩ (rightmost solid curves). The former (latter) value corresponds to the estimated quiescent L X luminosity of LSI at periastron (apastron). The left (right) band corresponds to ξ = 0.1 (ξ = 1). The horizontal band marks the maximum spin-down rate of LSI, viz. ﹩-6.04\lt \dot{\nu }/{10}^{-9}{{\rm{s}}}^{-2}\,\lt -4.39﹩ (Weng et al. 2022).
Paper: No Peaks without Valleys: The Stable Mass Transfer Channel for Gravitational-wave Sources in Light of the Neutron Star–Black Hole Mass Gap
Authors: L. A. C. van Son, S. E. de Mink, M. Renzo, S. Justham, E. Zapartas, K. Breivik, T. Callister, W. M. Farr, C. Conroy
Figure caption: Model predictions for the masses of BBH and BHNS systems formed through the stable channel. Left: ﹩\min ({M}_{\mathrm{primary}})﹩ as a function of the ZAMS mass ratio q ZAMS. Lines show our analytical prediction from Equation (10). Solid (dashed) lines indicate that M primary comes from M BH,a (M BH,b), described by Equations (8) and (9). Triangles show results from numerical simulations; 99% of the simulation has a mass M primary larger than that value for bins in q ZAMS of 0.02. Right: Histogram of M primary for BBH and BHNS from the stable channel for bins in M primary of 1  M ⊙. The rate is calculated at redshift 0.2; the total rate is annotated in the legend. Star markers indicate the reference model (see Table 1). The light-shaded area shows the 90% sampling uncertainty, obtained by bootstrapping. We show variations in the stability criteria (ζ eff and q crit,2, top), the mass transfer efficiency (β acc, middle), and the core mass fraction (﹩{f}_{\mathrm{core}}﹩, bottom). This shows that the analytically derived minimum can explain the numerical results well. It furthermore displays how the cutoff mass in the stable channel leads to a dearth of BBH and BHNS systems with low primary masses for most variations.
Paper: No Peaks without Valleys: The Stable Mass Transfer Channel for Gravitational-wave Sources in Light of the Neutron Star–Black Hole Mass Gap
Authors: L. A. C. van Son, S. E. de Mink, M. Renzo, S. Justham, E. Zapartas, K. Breivik, T. Callister, W. M. Farr, C. Conroy
Figure caption: Intrinsic distribution of primary masses from binary black hole (BBH) merging at redshift 0.2. We show the fiducial predictions for the stable channel in the pink kernel density distributions. The light-shaded area shows the 90% sampling uncertainty as obtained from bootstrapping. The total merger rate of BBHs at z = 0.2 is annotated in the legend. The power law+peak model from Abbott et al. (2021b) is shown in gray; light gray bands show the 90% credible intervals. We indicate a tentative rise observed in the GW data with the filled blue area (see text). We see that the local rate and the location of the peak at the low-mass end of the primary black hole mass distribution can be explained remarkably well by the stable channel under our fiducial assumptions.
Paper: Spectropolarimetry as a Means to Address Cloud Composition and Habitability for a Cloudy Exoplanetary Atmosphere in the Habitable Zone
Authors: Robert A. West, Philip Dumont, Renyu Hu, Vijay Natraj, James Breckinridge, Pin Chen
Figure caption: These four panels show contours of uncertainty σ for a single passband (0.1 μm, centered on 0.7 μm) for six cases (two example targets and three planet radii as indicated, as functions of star–planet distance in au and integration time (in the right panels the hour labels inside the borders apply to the case R = 2.5 R ⊕). Contours are shown for three cases (as per Table 1), σ = 1%, 0.5%, and 0.2% of the flux from the planet for a measurement consisting of two images in orthogonal polarizers. The integration time is the sum of integration times for two images in orthogonal polarizers obtained from two sequential exposures. These are for a phase angle of 90° with flux computed from the VLIDORT multiple scattering model. Other parameters are described in the text. The vertical dashed line shows the distance that corresponds to a 70 mas inner working angle, appropriate for phase angle 90°. The dashed–dotted line corresponds to the IWA limit for a phase angle of 30° (for sampling the rainbow).
Paper: Spectropolarimetry as a Means to Address Cloud Composition and Habitability for a Cloudy Exoplanetary Atmosphere in the Habitable Zone
Authors: Robert A. West, Philip Dumont, Renyu Hu, Vijay Natraj, James Breckinridge, Pin Chen
Figure caption: Left column: linear polarization (phase matrix elements −P21/P11) for single scattering for three compositions and five particle mean radii 〈r〉. All results are for wavelength 0.7 μm. Results are shown for steps of 1° in phase angle. Right column: corresponding net polarization, for single plus multiple scattering, and disk-averaged for the whole planet. Results are shown for 10° steps in phase angle. The solid curve is for water, the dashed–dotted curve is for 25% H2SO4, and the long-dashed curve is for 50% H2SO4.
Paper: No Peaks without Valleys: The Stable Mass Transfer Channel for Gravitational-wave Sources in Light of the Neutron Star–Black Hole Mass Gap
Authors: L. A. C. van Son, S. E. de Mink, M. Renzo, S. Justham, E. Zapartas, K. Breivik, T. Callister, W. M. Farr, C. Conroy
Figure caption: Same as Figure 3, but for variations in the fraction of the mass that is assumed to be lost from a circumbinary disk, f disk. Because Equation (10) does not capture variations in the orbital angular momentum loss, we only show the analytical solution for f disk = 0.0 in the left panel. Furthermore, we do not show f disk = 1.0 in the left panel because it contains too few samples to properly bin the distribution.
Paper: No Peaks without Valleys: The Stable Mass Transfer Channel for Gravitational-wave Sources in Light of the Neutron Star–Black Hole Mass Gap
Authors: L. A. C. van Son, S. E. de Mink, M. Renzo, S. Justham, E. Zapartas, K. Breivik, T. Callister, W. M. Farr, C. Conroy
Figure caption: Mass distributions in M primary for BBH and BHNS systems from the stable channel. We show variations in the supernova remnant mass function using the prescription from Fryer et al. (2022). Similar to the right column of Figure 3, but using a kernel density distribution. To prevent the kernel from smoothing over the cutoff mass in M primary, we only draw the distribution for M primary values where the corresponding histogram predicts a rate above ﹩{10}^{-5}\,{\mathrm{Gpc}}^{-3}\,{\mathrm{yr}}^{-1}\,{M}_{\odot }^{-1}﹩.
Paper: No Peaks without Valleys: The Stable Mass Transfer Channel for Gravitational-wave Sources in Light of the Neutron Star–Black Hole Mass Gap
Authors: L. A. C. van Son, S. E. de Mink, M. Renzo, S. Justham, E. Zapartas, K. Breivik, T. Callister, W. M. Farr, C. Conroy
Figure caption: Cartoon depiction of the stable mass transfer channel, including the most relevant parameters. See Section 2.1 and Table 1 for an explanation of the parameters.
Paper: No Peaks without Valleys: The Stable Mass Transfer Channel for Gravitational-wave Sources in Light of the Neutron Star–Black Hole Mass Gap
Authors: L. A. C. van Son, S. E. de Mink, M. Renzo, S. Justham, E. Zapartas, K. Breivik, T. Callister, W. M. Farr, C. Conroy
Figure caption:  ζ RL as a function of the mass ratio between the donor and accretor star. Mass transfer is dynamically stable as long as ζ RL ≤ ζ eff. The intersections of ζ RL and ζ eff reveal different values of q crit,1 and q crit,2. Our default value of ζ eff = 6.0 for a star with a clear core-envelope structure is annotated. ζ MS = 2 shows the adopted stability criteria assumed for main-sequence stars (Ge et al. 2015).
Paper: No Peaks without Valleys: The Stable Mass Transfer Channel for Gravitational-wave Sources in Light of the Neutron Star–Black Hole Mass Gap
Authors: L. A. C. van Son, S. E. de Mink, M. Renzo, S. Justham, E. Zapartas, K. Breivik, T. Callister, W. M. Farr, C. Conroy
Figure caption: The distributions for the chirp mass, M Chirp, and the final mass ratio, q final = M secondary/M primary, for merging BBHs and BHNSs. Colors and symbols are the same as the right-hand panels of Figure 3. This shows that the less massive components can form NS masses, often closing any gap between the most massive NS and the least massive BH.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: H+ flux distribution maps at the altitude of ∼500 km in science cases (i) (Ganymede is above the center of the JPS; left column) and (iii) (Ganymede is below the center of the JPS; right column) for initial ion energies 10 (panels (A) and (B)), 30 (panels (C) and (D)), and 300 keV (panels (E) and (F)). Superimposed are the OCFBs (black lines). Smaller granular structures in regions where the flux is very low are caused by a finite number of test particles. The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 30 keV O++ flux precipitating at the surface (left panels (A), (C), and (E)) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 300 keV O++ flux precipitating at the surface (left panels (A), (C), and (E)) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 30 keV S+++ flux precipitating at the surface (left panels (A), (C), and (E)) at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: Ratio of the flux at the surface toward the flux at 500 km (with downward direction) for oxygen ions of initial energy equal to 30 keV, for the configuration when Ganymede is near the center of the JPS (linear scale).
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: Circulation maps of S+++ at initial energy equal to 30 keV in science case (i) (Ganymede above the center of the JPS; left panel) and (iii) (Ganymede below the center of the JPS; right panel), in the XZ plane. The GPhiO coordinates have been used: X is along the ambient flow direction (and Ganymede’s orbital motion), Z is along Jupiter’s spin axis, and Y points toward Jupiter (in units of Ganymede’s radii). The black arrow shows the direction of Ganymede’s orbital velocity.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: Left column: flux distribution of H+ of initial energy equal to 100 keV, downward and parallel to the field (upper panel), upward and parallel to the field (middle panel), and perpendicular to the field (lower panel). The science case (ii) has been considered (Ganymede is near the center of the JPS). Right column: flux distribution of O++ of initial energy equal to 100 keV, downward and parallel to the field (upper panel), upward and parallel to the field (middle panel), and perpendicular to the field (lower panel). The science case (ii) has been considered (Ganymede is near the center of the JPS). The scale is logarithmic.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 300 keV S+++ flux precipitating at the surface (left panels (A), (C), and (E)) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 1 keV H+ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 5 keV H+ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.
Paper: The Jovian Energetic Ion Environment of Ganymede: Planetary Space Weather Considerations in View of the JUICE Mission
Authors: Christina Plainaki, Stefano Massetti, Xianzhe Jia, Alessandro Mura, Elias Roussos, Anna Milillo, Davide Grassi
Figure caption: 10 keV H+ flux precipitating at the surface (left panels A, C, and E) and at the altitude of 500 km (right panels (B), (D), and (F)) for three different configurations of the moon’s magnetic field: panels (A) and (B) correspond to science case (i) (Ganymede above the center of the JPS), panels (C) and (D) to science case (ii) (Ganymede near the center of the JPS), and panels (E) and (F) to science case (iii) (Ganymede below the center of the JPS). Superimposed are the OCFBs (black lines). The W longitude system has been used meaning the leading hemisphere is at long = 90° and long = 0° is at the Jupiter-facing hemisphere apex.