adsabs/AstroCLIMB huggingface dataset:
Paper: The Formation of Milky Way “Bones”: Ubiquitous HI Narrow Self-absorption Associated with CO Emission
Authors: Shenglan Sun, Ke Wang, Xunchuan Liu, Fengwei Xu
Figure caption: [HI]/[H2] abundance ratios observed in G28 and G47 (including ON-filament and OFF-filament regions), as compared to previously reported values in the literature (D. Li & P. F. Goldsmith 2003; P. Zuo et al. 2018; N.-Y. Tang et al. 2020; X. Liu et al. 2022; Y. Li et al. 2022, mostly for nearby low-mass clouds). The horizontal lines connect minimal to maximum values, and each data point is marked as a small open circle. The filled boxes encompass 25th percentile Q 1 to 75th percentile Q 3 of the corresponding [HI]/[H2] data set, and the red vertical lines in the boxes mark median values.
Paper: The Formation of Milky Way “Bones”: Ubiquitous HI Narrow Self-absorption Associated with CO Emission
Authors: Shenglan Sun, Ke Wang, Xunchuan Liu, Fengwei Xu
Figure caption: Time dependence of x HI for different total proton density (in cm−3). The values of total proton densities of the colorful curves are logarithmically spaced at intervals of 0.25, from 102.50 = 3.16 × 102 to 104. G28-ON, G28-OFF, G47-ON, and G47-OFF regions are plotted with pink dots, orange triangles, a green star, and blue diamonds, respectively. The fractional abundances of cold HI of G28-ON 3 and ON 4 are very close to the steady-state value, so their error bars of time are not plotted.
Paper: The Formation of Milky Way “Bones”: Ubiquitous HI Narrow Self-absorption Associated with CO Emission
Authors: Shenglan Sun, Ke Wang, Xunchuan Liu, Fengwei Xu
Figure caption: HINSA fitting and CO spectra toward G28. Descriptions are the same as Figure 1. For ON regions, the temperature of 13CO is magnified 3 times. For OFF regions, the temperatures of 12CO and 13CO are magnified 4 and 12 times, respectively.
Paper: The Formation of Milky Way “Bones”: Ubiquitous HI Narrow Self-absorption Associated with CO Emission
Authors: Shenglan Sun, Ke Wang, Xunchuan Liu, Fengwei Xu
Figure caption: HINSA fitting and CO spectra toward G47. Descriptions are the same as Figure 1.
Paper: Bulk and Atmospheric Metallicities as Direct Probes of Sequentially Varying Accretion Mechanisms of Gas and Solids Onto Planets
Authors: Yasuhiro Hasegawa, Mark R. Swain
Figure caption: Four stages of planet formation via core accretion and its schematic diagram. Top: sequential accretion of gas and solid divides the mass growth of planets into four stages. In Stage I, planetary cores form by solid accretion. As time goes on, solid accretion rates decrease, and gas accretion becomes dominated. One conservative estimate of a characteristic solid accretion rate is 10M ⊕/1 Myr ∼10−5 M ⊕ yr−1, as denoted by the black dashed–dotted line. Once the solid accretion rate becomes lower than the characteristic value, gas accretion comes into play. In Stage II, accretion of both gas and solids occurs. The gas accretion rate is regulated by cooling of accreted gas (i.e., ﹩{\dot{M}}_{{XY},\mathrm{KH}}﹩, denoted by the blue solid line). In Stage III, gas accretion is controlled by disk evolution. The corresponding rate becomes very high (i.e., ﹩{\dot{M}}_{{XY},\mathrm{hydro}}﹩, denoted by the green dotted line), and it is the main channel of forming subgiants. In Stage IV, gas accretion is reduced due to planet–disk interaction and the resulting gap formation in gas disks (i.e., ﹩{\dot{M}}_{{XY},\mathrm{gap}}﹩, denoted by the yellow dashed line). This is the final stage of giant plane formation. Mathematical expressions of accretion rates are summarized in Appendix A. Bottom: sequential accretion of gas and solid can be idealized by the onion-like model. As we show below, bulk and atmospheric metallicities can be used to trace when gap formation in both planetesimal and gas disks occurs, which corresponds to Stages III and IV, respectively. The purple and light salmon trapezoids represent gas and planetesimals disks, respectively. The brown circles denote solids, and the circular rings represent envelope gas.
Paper: Bulk and Atmospheric Metallicities as Direct Probes of Sequentially Varying Accretion Mechanisms of Gas and Solids Onto Planets
Authors: Yasuhiro Hasegawa, Mark R. Swain
Figure caption: Bulk and envelope metallicities of observed exoplanets and their trends. Bulk and envelope metallicities are denoted by the gray and salmon dots. For the latter, high and low values are separated by the gray and red edges. The gray shaded region covers the distribution of the bulk metallicities of observed exoplanets. The predicted profiles of the bulk and envelope metallicities are denoted by the black dashed and red solid lines, respectively. To obtain a better fit, the amplitudes of the profiles are adjusted. For the purpose of comparison , the solar system planets (i.e., Jupiter, Saturn, Uranus, and Neptune) are included (Y. Hasegawa et al. 2018, and references herein). Their bulk and atmospheric metallicities are denoted by the light and dark blue squares, respectively.
Paper: Bulk and Atmospheric Metallicities as Direct Probes of Sequentially Varying Accretion Mechanisms of Gas and Solids Onto Planets
Authors: Yasuhiro Hasegawa, Mark R. Swain
Figure caption: Exoplanet classification proposed by the onion-like model. Most observed planets are classified into two interior statues with some outliers: the globally mixed status and the locally (well-)mixed status. The shaded ellipses are added only for the purpose of visualization without quantitative estimates. Identification of the locally (well-)mixed status enables reliable verification of sequential accretion of gas and solids onto planets.
Paper: Bulk and Atmospheric Metallicities as Direct Probes of Sequentially Varying Accretion Mechanisms of Gas and Solids Onto Planets
Authors: Yasuhiro Hasegawa, Mark R. Swain
Figure caption: An example of primordial interior profiles of heavy elements for the locally well-mixed case. The profile changes from Z p = 1 to ﹩{Z}_{{\rm{p}}}\propto {R}_{{\rm{p}}}^{-7/3}﹩ and up to ﹩{Z}_{{\rm{p}}}\propto {R}_{{\rm{p}}}^{-2/3}﹩. The metallicity profile at planetary surfaces cannot be constrained by the current model due to the constant mass–radius relation there.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: Images of the NGC 315 jets at parsec and subparsec scales. Left: CLEAN image obtained with DIFMAP using VLBA data at 22 GHz on 2020 January 5, as published in P21. The restoring beam size is indicated in the bottom right corner. Intensity profiles along a transverse direction to the jet axis at two locations (along the white dashed lines) are presented. Middle: CLEAN image obtained with DIFMAP using GVA data at 22 GHz on 2022 November 9. The CLEAN model is restored with a circular Gaussian beam, with a size of the minor axis FWHM of the synthesized beam of approximately ∼0.17 mas. A limb-brightened jet morphology is observed at various locations, not visible in the lower-resolution VLBA-only image on the left. Right: representative RML image obtained with eht-imaging using the GVA data. The field of view corresponds to the yellow dotted box in the middle figure. The image was blurred using a circular Gaussian blurring kernel with an FWHM that is 30% of the diffraction limit (see Appendix B). The jet structure is clearly resolved transversely, revealing a limb-brightened jet morphology at sub-mas and mas scales.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: The figure displays the jet radius as a function of deprojected distance from the black hole in units of R g, with data from the RML image (magenta), the CLEAN image (from two Gaussian fittings, cyan; and from one Gaussian fitting, orange), and the previous study P21. The vertical black dashed line denotes the location of the jet collimation break. In the figure, the dark gray (light gray) segment denotes the outermost poloidal field line anchored to the equator of the event horizon, derived from the FFE solution for κ = 0.75 (κ = 1) over a black hole spin range of 0.5–0.99. This corresponds to z ∝ R 1.6 (z ∝ R 2) asymptotically, where R and z denote the jet radius and distance, respectively. Here, κ is a power-law index on the radius in the approximate formula of the magnetic stream function in polar coordinates in the Boyer–Lindquist frame (A. Tchekhovskoy et al. 2010; M. Nakamura et al. 2018).
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: RML (left) and CLEAN (right) images of the NGC 315 jets observed with the GVA. Both images are rotated clockwise by 40°. Note that the field of view of the RML image is smaller than that in Figure 2, as we did not attempt to measure the jet width at distances greater than ∼2.5 mas from the core due to the faintness of the reconstructed jet structure. The green solid lines represent the location of jet ridge(s), and the green dashed lines indicate the location of the jet edge(s) (see the text for more details). The CLEAN image is obtained by restoring the CLEAN models with a circular beam, with a size of the major axis FWHM of the synthesized beam of approximately ∼0.25 mas.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: Closure phase as a function of time for six selected triangles: observed data (black), RML model (magenta), and CLEAN model (cyan). Both models generally align with the observed closure phases. However, the RML model is particularly effective in explaining the closure phases of triangles formed with very long baselines (e.g., AT-KY-MH), while the CLEAN model tends to better explain those formed with short baselines (e.g., LA-PT-YY). Refer to Table 1 for the stations corresponding to each station code.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: The u v-coverage for the GVA 22 GHz data is depicted, emphasizing baselines from LBA, Korean VLBI Network (KVN), VLBA+VLA, and EVN in magenta, blue, green, and red colors, respectively. The data have been averaged across the entire bandwidth.
Paper: Periodic Coronal Rain Driven by Self-consistent Heating Process in a Radiative Magnetohydrodynamic Simulation
Authors: Zekun Lu, Feng Chen, J. H. Guo, M. D. Ding, Can Wang, Haocheng Yu, Y. W. Ni, Chun Xia
Figure caption: (a) Distributions of the volumetric heating rate, Q  H , along the loop at all time steps (gray lines) during the evolution as in Figure 4(f), where the coronal loop is defined by its portion with densities below 10−12 g cm−3. The red and blue lines represent the time-averaged profile of Q  H  and Q  H /n  e , respectively. The black dashed lines denote the time-averaged position of footpoints of the coronal loop. Panels (b) and (c) display temporal evolution of the number density, ﹩{\bar{n}}_{e}﹩, and volumetric heating rate, ﹩{\bar{Q}}_{H}﹩, that are averaged along the coronal loop. The red and blue lines denote the values averaged within the half coronal loop close to positive and negative polarities, respectively. Panel (d) shows Q  H  at positive footpoint (in red), negative footpoint (in blue), and apex (in dark gray), as defined by the maxima around footpoints and the minimum over the loop. Panels (e) and (f) display the apex-to-footpoint heating ratio and footpoints heating asymmetry. The black dashed lines in panel (f) denote the asymmetry values of 3 and 1/3.
Paper: Periodic Coronal Rain Driven by Self-consistent Heating Process in a Radiative Magnetohydrodynamic Simulation
Authors: Zekun Lu, Feng Chen, J. H. Guo, M. D. Ding, Can Wang, Haocheng Yu, Y. W. Ni, Chun Xia
Figure caption: Distributions of the volumetric heating rate, Q  H , with respect to height, z, at all time steps (gray lines) during the evolution as in Figure 4(f). Panels (a) and (b) depict the heating rate of the half loop near positive and negative polarity, respectively. The red line represents the time-averaged profile of Q  H . The coronal loop is defined by its portion with densities below 10−12 g cm−3. The black dashed lines denote the time-averaged position of footpoints of the coronal loop.
Paper: Periodic Coronal Rain Driven by Self-consistent Heating Process in a Radiative Magnetohydrodynamic Simulation
Authors: Zekun Lu, Feng Chen, J. H. Guo, M. D. Ding, Can Wang, Haocheng Yu, Y. W. Ni, Chun Xia
Figure caption: The horizontally averaged height-dependent profiles of (a) mass density and (b) temperature at t = 0 minute and t = 44 minutes. The percentage differences of the quantities with respect to the initial state are shown in panels (c) and (d). The red and blue lines represent the profile of simulation snapshot with the refined mesh (96 × 96 × 32 km3) and coarse mesh (192 × 192 × 64 km3), respectively.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: Selected RML images from the output of the parameter survey are presented. The weights for each parameter set are indicated in each panel, along with the reduced χ 2 for closure phase (﹩{\chi }_{\mathrm{cph}}^{2}﹩) and log closure amplitude (﹩{\chi }_{\mathrm{lcamp}}^{2}﹩). Images with small reduced χ 2 values closely align with the representative image selected based on the smallest χ 2 values (Figure 2). Conversely, images with higher reduced χ 2 values show more pronounced artifacts surrounding the jet emission.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: Jet width as a function of deprojected distance from the core is shown, derived from the RML image (green triangles) and the CLEAN image (yellow circles and squares), as well as from the previous studies P21 (22 and 43 GHz; blue squares) and B. Boccardi et al. (2021; 22, 43, and 86 GHz; pink circles). The length units are in pc for the bottom and left axes and in mas for the top and right axes. We used the same conversion factor of 1 mas to 0.331 pc and a jet viewing angle of 38° for deprojection as in B. Boccardi et al. (2021). The locations of the jet collimation breaks observed in those studies are indicated by the vertical dashed lines. Note that the distance from the core is specified at each frequency, as no core-shift effect was corrected.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: Top: u v-coverages of the original GVA data, the VLBA and phased VLA, the EVN, and the VLBA+EVN, from left to right. We overplot the u v-coverage of the GVA data in light gray for easier comparison. Bottom: reconstructed images from each array using eht-imaging. In the lower left corner of each image, we indicate the size of the blurring kernel for each image, determined by computing ρ NX(X, Y) for all possible combinations of the selected 10 images with the lowest overall χ 2 values for each blurring kernel size, as done in Appendix B. The limb brightening of the NGC 315 jet is successfully reconstructed only with the full GVA array.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: Dirty images of the residual visibilities, i.e., the final self-calibrated visibilities subtracted by the model visibilities, for RML (left) and CLEAN (right) models. A natural weighting scheme was used to produce the dirty images. The shape of the observed jet emission in each image (Figure 2) is indicated by the white contours. The rms values and the corresponding brightness temperature of the residual images are indicated in each panel.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: Amplitudes (top) and phases (bottom) of the self-calibrated visibilities (black) and RML model (red) are presented as a function of u v-distance in units of 109 wavelengths. The data have been averaged over the entire bandwidth and over time in 1 minute bins.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: Gain correction factors (1/∣G∣) from self-calibration for the representative RML image (blue) and the CLEAN image (green). The factors for the two images are in good agreement with each other. Refer to Table 1 for the stations corresponding to each station code.
Paper: Discovery of Limb Brightening in the Parsec-scale Jet of NGC 315 through Global Very Long Baseline Interferometry Observations and Its Implications for Jet Models
Authors: Jongho Park, Guang-Yao Zhao, Masanori Nakamura, Yosuke Mizuno, Hung-Yi Pu, Keiichi Asada, Kazuya Takahashi, Kenji Toma, Motoki Kino, Ilje Cho, Kazuhiro Hada, Phil G. Edwards, Hyunwook Ro, Minchul Kam, Kunwoo Yi, Yunjeong Lee, Shoko Koyama, Do-Young Byun, Chris Phillips, Cormac Reynolds, Jeffrey A. Hodgson, Sang-Sung Lee
Figure caption: Top: upper limit on I sp/I sh as a function of projected distance from the core, as derived in Section 3.3. Bottom: lower limit on Γsp required to explain the upper limit on I sp/I sh using the differential Doppler boosting effect.
Paper: Very Large and Long-lasting Anisotropies Caused by Sunward Streaming Energetic Ions: Solar Orbiter and STEREO A Observations
Authors: Wenwen Wei, Christina O. Lee, N. Dresing, L. Y. Khoo, L. K. Jian, J. G. Luhmann, C. M. S. Cohen, F. Fraschetti, B. Zhuang, J. Huang, C. J. Owen, G. Nicolaou, L. Rodríguez-García, E. Palmerio, I. C. Jebaraj, B. J. Lynch, F. Carcaboso
Figure caption: Overview of Solar Orbiter (left figure) and STEREO A (right figure) observations during 2022 February 16–19. For each of the figures, the top panel exhibits the energetic ion intensities of the widespread SEP event at several selected energies, whereas panels (a) to (f) show the magnetic field components in inertial RTN system, where the radial component R is oriented along the Sun–spacecraft line, the magnetic field azimuthal angle ϕ  B , the normalized e-PADs, the solar wind proton number density N  p , the bulk speed V  p , and the proton temperature T  p , respectively. In the left figure, panel (g) shows the omnidirectional ion intensities measured by EPD/EPT, whereas panels (h) to (j) display the ion intensities measured by the “Asun” and “Sun” telescopes of EPD/EPT along with their intensity ratios, respectively. The energy range in panels (h)–(i) is from 0.05 MeV to about 6 MeV, as indicated by the blue to red colors, and it is the same to the y-axis of panel (j), whereas the color bar in panel (j) shows the ratios. The unit of the differential intensities is cm−2 sr−1 s−1 MeV−1. Similarly, panels (g)–(j) in the right figure present the energetic ions observed by SEPT onboard STEREO A. The solid vertical lines in both figures mark the ion enhancements investigated in this work, and the shaded regions indicate an SFR observed by both spacecraft.