adsabs/AstroCLIMB huggingface dataset:
Paper: Determining the State of Jupiter’s Magnetosphere Using In Situ and Remote Sensing Observations
Authors: J. W. Sun, L. Xie, Z. H. Yao, S. Y. Fu, B. Zhang, Y. Xu, F. Leppard, Y. N. Chen, D. Grodent, L. C. Ray, B. Bonfond, W. R. Dunn
Figure caption: Identification of magnetospheric states based on ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩ measurements. (a-c) illustrate the lobelike region selection process with data from 2017 May 10. (a) R-Theta-Phi magnetic field components in Jupiter-De-Spun-Sun (JSS) coordinates. (b) 100 eV–100 keV electron energy spectra measured by Jovian Auroral Distributions Experiment (JADE). (c) Total magnetic field strength. Orange stars denote points algorithmically selected as lobelike using the criterion described in the main text. The orange shading indicates regions manually identified as lobelike based on a quasi-constant magnetic field and low plasma density. These points all lie within the orange-shaded regions, which demonstrates the reliability and effectiveness of our lobelike region selection method. (d) Radial distribution of measured ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩. Red and blue curves indicate fitted upper and lower envelopes, respectively. Events are classified as compressed (light red; higher ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩) or quiet (light blue; lower ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩) based on these envelopes.
Paper: Determining the State of Jupiter’s Magnetosphere Using In Situ and Remote Sensing Observations
Authors: J. W. Sun, L. Xie, Z. H. Yao, S. Y. Fu, B. Zhang, Y. Xu, F. Leppard, Y. N. Chen, D. Grodent, L. C. Ray, B. Bonfond, W. R. Dunn
Figure caption: Distribution of ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩ values across radial distances with trend-describing curves. (a) Gray points represent ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩ values versus radial distance measured by Juno from 2016 July to 2023 July, identical to the gray points in (b). The two lines are curves provided by Y. Xu et al. (2023) describing ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩ variations under different states. During quiet auroras, ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩ values at different radial distances follow the Q line, distinct from those observed during X-family auroras (following the X line). (b) Red diamonds mark the upper boundary points of ﹩{B}_{\mathrm{lobe}-\mathrm{like}}﹩ distribution, while blue diamonds indicate the lower boundary points. The red line represents the upper envelope curve fitted using upper boundary points, and the blue line shows the lower envelope derived from lower boundary points.
Paper: Determining the State of Jupiter’s Magnetosphere Using In Situ and Remote Sensing Observations
Authors: J. W. Sun, L. Xie, Z. H. Yao, S. Y. Fu, B. Zhang, Y. Xu, F. Leppard, Y. N. Chen, D. Grodent, L. C. Ray, B. Bonfond, W. R. Dunn
Figure caption: Juno’s trajectory in the (a) XY and (b) YZ planes of the JSO coordinate system, where X points from Jupiter toward the Sun and Z is northward normal to Jupiter’s orbital plane. White dots mark Juno’s positions of events with consistent magnetospheric state identifications between auroral and bKOM methods, purple dots indicate inconsistent cases, and event #18 in Table 1 (light green) is excluded from discussion.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The magnetospheric radius Rm as a function of the dipole strength. The red circles are the computed radii in each magnetic field simulation. The gray circles mark the corresponding radii ﹩{R}_{{\rm{m}}}^{{\rm{scl}}}﹩ of each magnetic field simulation scaled by ﹩{\dot{M}}^{2/7}﹩ due to the different accretion rate in each simulation. The red and gray dashed lines show the fitted function on the computed data, and the black solid curve corresponds to the shape of the analytical solution of R. F. Elsner & F. K. Lamb (1977).
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The radiation energy density ﹩\hat{E}﹩ (left-half panel) and the rest-mass density ρ (right-half panel) are shown in each panel. Magnetic field lines are plotted as iso contours of the vector potential, Aϕ. The magnetic dipole strength is as labeled on each frame. The plot is produced from the time-averaged data.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The efficiency ﹩L/(\dot{M}{c}^{2})﹩ of total luminosity Ltot and its components for two simulations with dipole 1010 G (top panel) and 1011 G (bottom panel). Efficiency in each energy is denoted by a different color and line style.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The accretion ﹩\dot{M}﹩, inflow ﹩{\dot{M}}_{{\rm{in}}}﹩, and outflow ﹩{\dot{M}}_{{\rm{out}}}﹩ rates in the unit of LEdd/c2 are shown in the top, middle, and bottom panels, respectively. Simulations with different strengths of magnetic dipoles are shown in different colors and line styles.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The radiation energy density ﹩\hat{E}﹩ (left-half panel) and the rest-mass density ρ (right-half panel) are shown in each panel. Magnetic field lines are plotted as contours of the vector potential, Aϕ. The left column shows the simulation with 3 × 1010 G and the right column with 1 × 1010 G, with the accretion rate labeled on each frame.
Paper: Energy Flow and Radiation Efficiency in Radiative GRMHD Simulations of Neutron Star Ultraluminous X-Ray Sources
Authors: Fatemeh Kayanikhoo, Włodek Kluźniak, David Abarca, Miljenko Čemeljić
Figure caption: The initial rest-mass density ρ in the fluid frame. Solid gray lines indicate the vector potential Aϕ, which in our setup is parallel to the magnetic field lines. The strength of the magnetic field on the surface of the neutron star is 1011 G.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: The light curves of the beta-decay gamma-ray emission from the MR-SN are shown in Figure 1, over the whole energy range (left) and 550 ≤ Eγ ≤ 750 keV (right), assuming a distance of 10 kpc. The curve is color-coded according to the decaying nuclear species with the largest contribution at a given time. The gray lines represent the sensitivity limits of different MeV instruments. For times t less than 1 yr postexplosion, the sensitivity curve is scaled with focusing time = t. For t ≥ 1 yr, we adopt a sensitivity that corresponds to one year, which is a substantial fraction of the proposed operating time for all instruments we consider. The green line represents an estimate of the flux due to electron–positron annihilation within the SNR. Dotted lines indicate prompt (unabsorbed) emission, and solid lines indicate final emission (including absorption and Doppler broadening as in Section 2.4) from the SN.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Snapshot of the MR-SN model 35OC-RS from M. Reichert et al. (2021) at the end of the simulation time (1.306 s). Left panel: Tracers are drawn from the jet material in the multicolored region; the color map corresponds to the electron fraction (Ye). This material was unbound at the end of the simulation time; however, since the simulation ends before the explosion is complete, additional material (purple region, refer to the text for composition) is expected to be ejected by the end of the explosion. The light blue line represents the outline of the outgoing shock. Right panel: Red color indicates material with positive (outgoing) radial velocity, while blue corresponds to negative (inward-going) radial velocity. The purple line denotes the boundary of the material in the jet at 1.3 s, and everything else (labeled as additional material).
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Top panel: same as Figure 5 but for the observability of 60Co 1332 keV line using the 60Fe yield from the MN-SN model. Bottom panel: same as the top panel, but for CCSN. The 60Fe yield is taken from M. Limongi & A. Chieffi (2018) as 3.7 × 10−5 M⊙.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Observability of 126Sb 666 keV line with COSI (light and dark pink region) and next-generation telescopes (light pink region) if an SNR originated from an MR-SN described in Figure 1. The x-axis denotes the age, and the y-axis denotes the distance of the remnant. Labels for SNRs are as follows: a: Kes75, b: G350.1-0.3, c: G330.2+1.0, d: G320.4-1.2, e: RCW103, f: G11.2-0.3, g: W49B.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Gamma-ray spectra of four known SNRs, assuming they are remnants from the MR-SN event shown in Figure 1. The left panel shows the Doppler-broadened spectra due to the expansion of the remnant. The right panel shows the total number of prompt photons per area per time for a direct comparison with the line sensitivity limits. Detector sensitivities are colored gray with the same line style as in Figure 4 and have been scaled to 1 yr. These late-time remnants feature 126Sb as the dominant r-process signal. Gamma emission from 60Co (60Fe) is prominent between 1 MeV and 1.5 MeV.
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Final abundances for ejecta from the model shown in Figure 1 plotted against the mass number (left panel) and element number (right panel). The shaded region indicates the nuclear uncertainties introduced by different nuclear mass models and β decay rates in the r-process region. The abundances in the right panel are normalized to Zr (Z = 40). Several observed stellar abundance patterns are shown for comparison: HD 122563 (S. Honda et al. 2006), BD −18∘5550 (R. Cayrel et al. 2004) (P. François et al. 2007), HD 84937, HD 19445, HD 128279, and HD 140283 (I. U. Roederer et al. 2022).
Paper: Gamma Rays as a Signature of r-process Producing Supernovae: Remnants and Future Galactic Explosions
Authors: Zhenghai Liu, 正海 刘, Evan Grohs, Kelsey A. Lund, G. C. McLaughlin, M. Reichert, Ian U. Roederer, Rebecca Surman, Xilu Wang, 夕露 王
Figure caption: Ejecta yields from this work are compared with other r-process producing SNe studies (N. Nishimura et al. 2017; P. Mösta et al. 2018; J. M. Miller et al. 2020; M. Shibata et al. 2025). Models from N. Nishimura et al. (2017) are separated into two bands according to the applied neutrino luminosity scale factor ﹩{\hat{L}}_{\nu }﹩. The light green band denotes models B12.1.7l-H, B12.1.7l, B12.1.8h, B12.1.8l, B12.1.8l-H, and B12.1.9l from M. Shibata et al. (2025)
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Simulations at the magma ocean–atmosphere interface of K2-18b assuming real versus ideal gas behavior under various oxygen fugacity conditions. The oxygen fugacity (fO2) of the planet varies from ΔIW = −6 to 0, while other input parameters are fixed, with Tsurface = 3000 K, a total hydrogen mass fraction of 1% of the planet’s mass and C/H by mass of 100× solar (i.e., ∼0.3). The x-axis corresponds to fO2, expressed as log10 units relative to the IW buffer. The solid lines correspond to the cases assuming real gases, and the dashed lines assume ideal gas behavior. (a) Pressures of volatile species in the atmosphere (GPa) and the total atmospheric pressure (gray). (b) C/H (purple, left y-axis) and C/O (teal, right y-axis) in the atmosphere. (c) Solubility of each volatile species (wt%, i.e., fraction of the planet’s mantle mass). (d) Fugacity coefficient (ϕ) for each volatile species. The coefficient for ideal behavior (gray dashed line) is unity for all volatiles.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Atmospheric speciation of TRAPPIST-1e at 280 K above a planetary surface with stable condensates for atmospheres originally in equilibrium with a fully molten mantle. In all panels, the curve colors correspond to the gas species listed in the legend and condensate masses are relative to Earth oceans (EO). Upper panels show the percentage of models by dominant species (VMR > 50%) that satisfy the requirement of a minimum mass of (a) water, (b) graphite, (c) α-sulfur, and (d) ammonium chloride. Lower panels illustrate the composition and total pressure of the atmosphere for (e) CO2-rich above a water ocean, (f) CH4-rich above graphite, (g) CO2-rich above α-sulfur, and (h) CH4-rich above ammonium chloride. Median values are indicated by lines and shaded regions bracket the first and third quartiles. Compare to the atmospheric speciation derived from a partially molten mantle in Figure B5.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Cooled atmospheres at 280 K for TRAPPIST-1e, starting with the elemental abundances in the atmosphere for a partially molten mantle (10% melt fraction) and a surface temperature of 1800 K. Points are colored by oxygen fugacity of the initial, high-temperature atmosphere expressed relative to the IW buffer and sized in proportion to log10 C/H for the partially molten starting state. Condensed inventories of water, graphite, and α-sulfur are normalized by the Earth’s present-day ocean mass (EO). Other scatter plots show the VMR of major species in the atmosphere, total pressure, and molar mass. Density levels indicate areas with high likelihood in the scatter plots, while marginal distributions are shown on the diagonal. The 10th, 50th (median), and 90th percentiles of these distributions are also annotated above the marginal distributions as (p10, p50, and p90), respectively. Compare to the cool atmospheres derived from a fully molten mantle in Figure 5.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Atmospheric speciation of TRAPPIST-1e at 280 K above a planetary surface with stable condensates for atmospheres originally in equilibrium with a partially molten mantle (10% melt fraction). In all panels, the curve colors correspond to the gas species listed in the legend and condensate masses are relative to Earth oceans (EO). The upper panels show the percentage of models by dominant species (VMR > 50%) that satisfy the requirement of a minimum mass of (a) water, (b) graphite, (c) α-sulfur, and (d) ammonium chloride. Lower panels illustrate the composition and total pressure of the atmosphere for (e) CO2-rich above a water ocean, (f) CH4-rich above graphite, (g) CO2-rich above α-sulfur, and (h) CH4-rich above ammonium chloride. Median values are indicated by lines and shaded regions bracket the first and third quartiles. Compare to the atmospheric speciation derived from a fully molten mantle in Figure 9.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: For an early TRAPPIST-1e with a partially molten mantle (10% melt fraction, surface temperature of 1800 K), scatter plots of atmospheric molar abundance, total pressure, and molar mass, for N2 and minor species: ClH, S2, H2S, NH3, and Cl2. Points are colored by oxygen fugacity expressed relative to the IW buffer and sized in proportion to log10 C/H. Density levels indicate areas with high likelihood in the scatter plots, while marginal distributions are shown on the diagonal. The 10th, 50th (median), and 90th percentiles of these distributions are also annotated above the marginal distributions as (p10, p50, and p90), respectively. Compare to a fully molten mantle in Figure 2.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Atmospheric speciation of TRAPPIST-1e at 280 K in equilibrium with stable reservoirs of water, graphite, α-sulfur, and ammonium chloride. “True” indicates atmospheres above planetary surfaces where all four condensates coexist. Conversely, “False” means that at least one of the four condensates are not stable. From this classification, atmospheres that are more amiable to support surfaces primed for habitable environments can be distinguished. The width of each violin plot is proportional to the number of models, where interior dotted lines represent the first and third quartiles and dashed lines represent the second quartile (median).
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: For an early TRAPPIST-1e with a partially molten mantle (10% melt fraction, surface temperature of 1800 K), scatter plots of atmospheric molar abundance, total pressure, and molar mass for major species. Points are colored by oxygen fugacity expressed relative to the IW buffer and sized in proportion to log10 C/H. Density levels indicate areas with high likelihood in the scatter plots while marginal distributions are shown on the diagonal. The 10th, 50th (median), and 90th percentiles of these distributions are also annotated above the marginal distributions as (p10, p50, and p90), respectively. Compare to a fully molten mantle in Figure 1, noting that the extent of the axes for H2O and CH4 is different.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: For an early TRAPPIST-1e with a partially molten mantle (10% melt fraction, surface temperature of 1800 K), scatter plots of atmospheric and total C/H, C, H, and S dissolved in the interior relative to the total inventory of the element by mass, total pressure, and molar mass. Points are colored by oxygen fugacity and sized in proportion to log10 C/H. Density levels indicate areas with high likelihood in the scatter plots, while marginal distributions are shown on the diagonal. The 10th, 50th (median), and 90th percentiles of these distributions are also annotated above the marginal distributions as (p10, p50, and p90), respectively. Compare to a fully molten mantle in Figure 4.
Paper: Diversity of Low-mass Planet Atmospheres in the C–H–O–N–S–Cl System with Interior Dissolution, Nonideality, and Condensation: Application to TRAPPIST-1e and Sub-Neptunes
Authors: Dan J. Bower, Maggie A. Thompson, Kaustubh Hakim, Meng Tian, Paolo A. Sossi
Figure caption: Atmospheric speciation of TRAPPIST-1e at 280 K in equilibrium with stable reservoirs of water and graphite. “True” indicates atmospheres above planetary surfaces where both condensates coexist. Conversely, “False” means that at least one of the two condensates is not stable. From this classification, atmospheres that are more amiable to support surfaces primed for habitable environments can be distinguished. The width of each violin plot is proportional to the number of models, where interior dotted lines represent the first and third quartiles and dashed lines represent the second quartile (median). A scenario additionally including α-sulfur and ammonium chloride is presented in Figure 10.
Paper: Detection of CH﹩{}_{3}^{+}﹩ in the O-rich Planetary Nebula NGC 6302
Authors: Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
Figure caption: Left panel: the cartoon provides a schematic representation of the central region of NGC 6302. Blue and red colors indicate the blueshift and redshift caused by the expansion of the torus and inner bubble from the Earth’s perspective. The schematic is based on the results of M. Santander-García et al. (2017) and M. Matsuura et al. 2025, MNRAS, in press. The line-of-sight motion of the outer bubble is not constrained and thus is represented by arcs. Points A and B are two bright spots on CH﹩{}_{3}^{+}﹩ integrated surface brightness map. Right panel: integrated surface brightness map of CH﹩{}_{3}^{+}﹩, obtained by integrating the surface brightness over the 7.13–7.2 μm wavelength range at each pixel. The green boxes and ellipses represent the 25 apertures where we analyzed the CH﹩{}_{3}^{+}﹩ emission in more detail. Apertures 1–22 are 2 × 2 pixels, which is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩26 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩26. Apertures 23–25 are larger elliptical regions with areas of 3﹩\mathop{.}\limits^{^{\prime\prime} }﹩222, 6﹩\mathop{.}\limits^{^{\prime\prime} }﹩522, and 4﹩\mathop{.}\limits^{^{\prime\prime} }﹩362, respectively. The cyan line represents the cut used for studying spatial distribution in Sec 5.