adsabs/AstroCLIMB huggingface dataset:
Paper: AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star
Authors: Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome, Giacomo Terreran
Figure caption: Left: a comparison of the rest-frame g-band light curve of AT2023vto (black stars) to the classical TDE sample, consisting of TDE-H (red), TDE-H+He (green), and TDE-He (blue). AT2023vto is the brightest among this population of spectroscopically classified TDEs, outshining the second brightest event by ≈1.5 mag and the median by ≈4 mag. Right: a comparison of AT2023vto’s rest-frame g-band light curve to putative or possible TDEs, including featureless events, ambiguous events, and ANTs. AT2023vto is at the bright end of the featureless TDEs (yellow) and at the mean of the ANT population. Comparison data from S. Gezari et al. (2006), R. Chornock et al. (2014), S. van Velzen & G. R. Farrar (2014), I. Arcavi et al. (2014), T. W.-S. Holoien et al. (2014), T. W. S. Holoien et al. (2016b, 2016a), S. Dong et al. (2016), T. Hung et al. (2017), P. K. Blanchard et al. (2017), N. Blagorodnova et al. (2017), Ł. Wyrzykowski et al. (2017), S. van Velzen (2018), T. W. S. Holoien et al. (2019b), M. Nicholl et al. (2019), S. Gomez et al. (2020), P. Short et al. (2020), M. Nicholl et al. (2020), I. Arcavi et al. (2020), I. Perez-Fournon et al. (2020), J. Nordin et al. (2020), S. van Velzen et al. (2021a), T. Hung et al. (2021), G. Cannizzaro et al. (2021), Y. Yao et al. (2021a, 2021b), C. Fremling (2021), T. Wevers et al. (2022), X.-L. Liu et al. (2022), Y. Yao et al. (2022), P. Ramsden et al. (2022), M. Nicholl et al. (2022), E. Hammerstein et al. (2023), S. Gomez et al. (2023), Y. Yao et al. (2023), A. J. Goodwin et al. (2023), Y. Yao (2023), J. J. Somalwar et al. (2023), N. Sarin & B. D. Metzger (2024), P. Wiseman et al. (2024), J. T. Hinkle et al. (2024), and J. T. Hinkle (2024).
Paper: AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star
Authors: Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome, Giacomo Terreran
Figure caption: Top: the optical spectrum of AT2023vto compared to all TDE types (H, H+He, He, “featureless”), SLSN-II, ANT, and ASASSAN-15lh; the quoted phases are relative to the discovery date of each event. Bottom: a comparison to all other TDE-He events found to date. AT2023vto exhibits a bluer continuum compared to the other TDE-He (matched only by PS1-10jh but at a much earlier phase of its evolution). The width and blueshift of the He II λ4686 line of AT2023vto compared to the other TDE-He events are shown in the inset (colors match those of the spectra in the main panel). AT2023vto exhibits the largest velocity width and blueshift, although neither quantity is completely unprecedented in previous TDE-HE events. Comparison data from N. Smith et al. (2007), I. Arcavi et al. (2014), T. W. S. Holoien et al. (2016a, 2019a), S. Dong et al. (2016), G. Leloudas et al. (2019), S. van Velzen et al. (2021a), and P. Wiseman et al. (2024).
Paper: AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star
Authors: Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome, Giacomo Terreran
Figure caption: MMT/Binospec optical spectrum of AT2023vto obtained at a phase of +54 days, shown in rest-frame wavelength (the purple line is binned by a factor of 5). The narrow Mg II absorption doublet indicates a redshift of z = 0.48463 ± 0.00004 (left inset). We find a single broad emission feature centered at 4511 Å, with v FWHM ≈ 3.90 × 104 km s−1 and a blueshift of ≈1.11 × 104 km s−1 relative to the rest wavelength of He II λ4686 (right inset). This feature is inconsistent with Hβ (dotted vertical line), indicating a TDE-He classification.
Paper: AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star
Authors: Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome, Giacomo Terreran
Figure caption: Inferred disrupted star mass (M *) vs. black hole mass (M BH) from MOSFiT model fits of AT2023vto (black star) and optical TDEs, including the H (red), H+He (green), and He (purple) categories, as well as featureless (open yellow) and ambiguous events (open blue). AT2023vto stands out in this parameter space with an unusually high stellar mass and relatively large black hole mass. A few of the featureless TDEs seem to reside in the same region of parameter space as AT2023vto and indeed exhibit similar light curves (right panel of Figure 7).
Paper: AT2023vto: An Exceptionally Luminous Helium Tidal Disruption Event from a Massive Star
Authors: Harsh Kumar, Edo Berger, Daichi Hiramatsu, Sebastian Gomez, Peter K. Blanchard, Yvette Cendes, K. Azalee Bostroem, Joseph Farah, Estefania Padilla Gonzalez, D. Andrew Howell, Curtis McCully, Megan Newsome, Giacomo Terreran
Figure caption: Multiband MOSFiT TDE model light curves for AT2023vto. We note that the LCO U-band data (open symbols) were not used in the fit, but their inclusion does not change the resulting model parameters. The best-fit model parameters are listed in Table 2.
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: GJ 1214 b’s panchromatic transmission spectrum. We plot the combined results from HST WFC3 (L. Kreidberg et al. 2014), JWST NIRSpec (this work), and JWST MIRI (E. M. R. Kempton et al. 2023b), reanalyzed with our best-fit orbital parameters. The data are offset according to the best-fit chemically free model, as described in Appendix C.5. While our JWST NIRSpec spectrum is best fit with features of CO2 and (weakly) CH4, the models predict virtually featureless spectra in the HST and JWST MIRI wavelengths, consistent with previous studies (L. Kreidberg et al. 2014; P. Gao et al. 2023). Future high-precision characterization in the 2–5 μm wavelength range will lead to better characterization of the carbon, oxygen, and sulfur content of the atmosphere and allow for comparisons to planet formation models.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: Left: a free Gaussian fit to the spectrum as well as a Gaussian that has the same centroid and width as expected from CO2. Middle and right: posterior distributions of the free Gaussian centroid and width as compared to the best-fit value Gaussian for a CO2-rich model.
Paper: Possible Carbon Dioxide above the Thick Aerosols of GJ 1214 b
Authors: Everett Schlawin, Kazumasa Ohno, Taylor J. Bell, Matthew M. Murphy, Luis Welbanks, Thomas G. Beatty, Thomas P. Greene, Jonathan J. Fortney, Vivien Parmentier, Isaac R. Edelman, Samuel Gill, David R. Anderson, Peter J. Wheatley, Gregory W. Henry, Nishil Mehta, Laura Kreidberg, Marcia J. Rieke
Figure caption: Left: wavelength selections for CH4 and out-of-feature points. Right: differential light curve inside and outside of significant CH4 features. Colors and descriptions are the same as for Figure 3.
Paper: Lyman Continuum Leakers at z > 3 in the GOODS-S Field: Starburst or Not?
Authors: Shuairu Zhu, 帅儒 朱, Fang-Ting Yuan, Chunyan Jiang, Zhen-Ya Zheng, Ruqiu Lin
Figure caption: Star-forming properties of LyC leakers at z > 3. The filled and open circles indicate LyC leakers with and without JWST photometric data, respectively. Three LyC leakers at z > 3 in other fields (Ion3, J0121+0025, and J1316+2614) are also presented in this figure. The color indicates the f esc of each LyC leaker. LyC leakers with offset (see Table 1) are indicated by small circles. For comparison, we overplot a low-z (z ∼ 0.3) sample of LyC leakers from S. R. Flury et al. (2022) as squares. (a) UV-continuum slope β as a function of UV absolute magnitude M UV. The blue and orange lines show the β-M UV observed at z ∼ 4 and 7 from R. J. Bouwens et al. (2014), respectively. The shaded areas represent the 1σ dispersion of these relations. Most LyC leakers have bluer β than the star-forming galaxies at similar redshifts (z ∼ 4). Nine LyC leakers have extremely blue β, which are located even below the relation at z ∼ 7. The z ∼ 7 relation is also applicable for low-redshift (z ∼ 0.3) LyC leakers as reported by J. Chisholm et al. (2022). (b) SFR as a function of stellar mass. The blue, orange, and green dashed lines indicate the star formation main sequence (SFMS) at z ∼ 3.5 derived from J. S. Speagle et al. (2014), P. Santini et al. (2017), and P. Popesso et al. (2023), respectively. The gray dashed line indicates the SFMS at z ∼ 0.3 derived from P. Popesso et al. (2023). Shaded areas represent the 1σ dispersion of these relations.
Paper: Lyman Continuum Leakers at z > 3 in the GOODS-S Field: Starburst or Not?
Authors: Shuairu Zhu, 帅儒 朱, Fang-Ting Yuan, Chunyan Jiang, Zhen-Ya Zheng, Ruqiu Lin
Figure caption: Probability density distributions for physical parameters (age, E(B − V), SFR, M *, and β) derived from SED fitting for five of the high-confidence LyC leakers. The blue dashed lines are the probability distributions using 3D-HST photometric observations. The red solid lines are the probability distributions using 3D-HST photometric observations plus the observations of JWST. The use of the JWST photometric data provides better constraints on these star-forming parameters. In the last column, we also present the probability density distributions for f esc. For reference, the f esc values with their 1σ errors reported in the literature are represented by the black lines and the gray areas.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Geological context and crater statistics for the Chang’E-6 landing mare. Red stars mark the landing site. The landing mare contains the western and eastern mare, which have different compositions and model ages, roughly separated by a wrinkle ridge (red curve; Y. Qian et al. 2024). (a) Blue and yellow polygons are areas used to map potential production populations with  D ≥ 1 km and  D ≥ 75 m, respectively. The base map is the Chang’E-2 DOM mosaic. (b) Nonuniform distribution of craters with  D ≥ 400 m in the western and eastern mare. The areas of spatial analyses are outlined by the blue polygons shown in panel (a). Cells are colored based on the confidence level for the significance of spatial clustering, as cool, warm, and white colors represent significant (90% confidence level) clustering, sparse, and nearly random distributions, respectively. The western mare is divided into two subareas to investigate the effect of clustered craters on crater statistics (e.g., black polygon). Subareas with random distributions (blue polygons) are extracted to investigate the potential production population. The base map is the Kaguya TC morning map. Detailed IDs and available addresses of data used in panels (a) and (b) are summarized in Table A1.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: SFDs of crater populations collected in the Chang’E-6 landing mare. The upper row shows the relative SFD, and the middle row shows the cumulative SFD constructed using the method introduced in Section 2. The lower row shows the cumulative SFD based on the traditional method (Crater Analysis Techniques Working Group 1979). (a), (b), (c) Status of equilibrium of crater populations collected in the yellow polygons shown in Figure 1(a). (d), (e), (f) Crater SFD at  D ≥ 400 m in the blue polygons shown in Figure 1(a). (g), (h), (i) Crater SFD at  D ≥ 400 m in the blue polygons shown in Figure 1(b) (i.e., random distribution). (j), (k), (l) Crater SFD at  D ≥ 1 km in the blue polygons shown in Figure 1(a).
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Implications for the derived N(1) values for lunar crater chronology. The  N (1) values (dashed lines) and their uncertainties (shades) are derived from direct observations of craters with  D ≥ 1 km in the specific areas (Section 3), and the red and blue colors are for the western and eastern mare, respectively. The different crater chronology models of the Moon are shown as solid lines with different colors. (a) Positions of the N(1) values of the western and eastern mare in available crater chronology models. Gray dots denote calibration points established by the Apollo, Luna, and Chang’E-5 samples (e.g., Z. Xiao et al. 2024). (b), (c) Earlier-reported model ages (orange dots) and their employed chronology models for the western and eastern mare at the Chang’E-6 landing site, respectively.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Pronounced impact rays and secondaries formed by the Chaffee S crater in the northwestern sector of the Chang’E-6 landing mare. The landing site is marked as a red star. (a) The northwestern sector of the landing mare has higher reflectance due to coverage by rays of the Chaffee S crater. The base map is from the Chang’E-2 orthophoto mosaic. (b) and (c) Widespread secondaries formed by the Chaffee S crater. Their locations are marked in panel (a), and they are part of areas that are clustered with craters at D ≥ 400 m (Figure 1(b)). The base image is from the Kaguya TC morning map. IDs and available addresses of data used in this figure are summarized in Table A1.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Comparisons of potential production populations at different diameter ranges in the Chang’E-6 landing mare. The first column shows the relative SFD, and the middle column shows the cumulative SFD constructed using the method introduced in Section 2. The last column shows the cumulative SFD based on the traditional method (Crater Analysis Techniques Working Group 1979). (a), (b), (c) and (d), (e), (f) are the three potential production populations on the western and eastern mare, respectively. Using the G. Neukum et al. (2001) chronology model, crater density isochrons of 2.4–3.3 Ga and 3.2–3.5 Ga are plotted for reference in panels (c) and (f), respectively.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Widespread secondaries in the Chang’E-6 landing mare (a) and their various sizes and preservation states (b)–(e). The landing site is marked as a red star. Panel (a) is from the Chang’E-2 orthophoto mosaic, and it shows the locations of panels (b)–(e), which are based on the Kaguya TC morning map. IDs and available addresses of data used in this figure are summarized in Table A1.
Paper: The Production Population of Impact Craters in the Chang’E-6 Landing Mare
Authors: Fanglu Luo, Zhiyong Xiao, Yichen Wang, Yizhen Ma, Rui Xu, Senmiao Wang, Minggang Xie, Yunhua Wu, Qingyun Deng, Pei Ma
Figure caption: Pre-mare craters in the Chang’E-6 landing mare that are observed based on their subdued morphology and embayment with the surrounding mare. The locations of these cases are marked in Figure A1(a). The base image is from the Kaguya TC morning map. IDs and available addresses of data used in this figure are summarized in Table A1.
Paper: Sun-as-a-star Analysis of the X1.6 Flare on 2023 August 5: Dynamics of Postflare Loops in Spatially Integrated Observational Data
Authors: Takato Otsu, Ayumi Asai, Kai Ikuta, Kazunari Shibata
Figure caption: (a-1)–(a-3) The results of the Sun-as-a-star analysis. (b-1) and (b-2) Integrated results with limb for the comparison. (a-1) The spatially integrated pre-event-subtracted Hα spectrum normalized by the full-disk integrated continuum is shown as a two-dimensional color map for the Sun-as-a-star spectra with the total region (A 1 + A 2 + A 3). Orange and purple indicate emission and absorption compared with the pre-event state, respectively. (a-2) The differenced Hα equivalent widths and the GOES light curve are plotted as red circles and sky blue histogram, respectively. (a-3) The light curves of AIA 94, 171 , and 304 Å are shown as the green dashed, orange solid, and dark red dotted lines, respectively. In panels (a-2) and (a-3), the vertical blue starred, green dashed, orange solid, dark red dotted, and purple dashed–dotted lines indicate the peak time of the light curves of GOES, AIA 94, 171, 304 Å, and Hα. The peak times are also indicated in the legends of panels (a-2) and (a-3). (b-1) and (b-2) The same as panels (a-1) and (a-2) but for results obtained over the integration involving the limb region (A limb) in addition to the total region. The gray regions in panels (a-1), (a-2), (b-1), and (b-2) mean that no data are available for the SDDI due to bad weather condition.
Paper: Sun-as-a-star Analysis of the X1.6 Flare on 2023 August 5: Dynamics of Postflare Loops in Spatially Integrated Observational Data
Authors: Takato Otsu, Ayumi Asai, Kai Ikuta, Kazunari Shibata
Figure caption: (a) The GOES soft X-ray light curve between 20:00 UT on 2023 August 5 and 04:00 UT on 2023 August 6 is shown as black solid line. The black arrow indicates the target X1.6 flare. The vertical gray dotted line indicates the time of the panels (b) and (c) (t = 95 minutes from 2023 August 5, 21:00 UT). The vertical gray dashed lines indicate the times in Figure 2 (t = 70, 120, and 210 minutes). (b) The Hα line center solar full-disk image taken by SMART/SDDI at 22:35 UT on 2023 August 5. Solar north and west are at the top and right. The white arrow indicates the target active region NOAA 13386. The white dashed and sky blue boxes correspond to the field of view in Figures 1(c) and 2, and the quiet region for calibration, respectively. (c) The integral and limb regions for Hα analyses. The Hα line center image taken by the SDDI at 22:35 UT on 2023 August 5 is shown with integral and limb regions. The black dashed, red solid, orange dashed–dotted, and white dotted regions correspond to the Regions 1, 2, 3, and limb, respectively (see the text).
Paper: Sun-as-a-star Analysis of the X1.6 Flare on 2023 August 5: Dynamics of Postflare Loops in Spatially Integrated Observational Data
Authors: Takato Otsu, Ayumi Asai, Kai Ikuta, Kazunari Shibata
Figure caption: Hα dynamic spectra and their light curves. Panels (a-1), (b-1), and (c-1) are the same as Figure 4(a-1) but for the Region 1, 2, and 3 (Figure 1), respectively. In panels (a-2), (b-2), and (c-2), the differenced Hα equivalent widths are shown for the Region 1, 2, and 3, respectively. The GOES light curve is also plotted as sky blue histogram in the panels. In the gray regions in all panels, no data is available for the SDDI due to the bad weather condition.
Paper: Constraining the Properties of the Multicomponent Local Interstellar Medium: MHD-kinetic Modeling Validated by Voyager and New Horizons Data
Authors: Federico Fraternale, Nikolai V. Pogorelov, Ratan K. Bera
Figure caption: (a) Comparison of the electron density observed by V1/PWS in the OHS with several global simulations labeled from A to H as in Table 1. (b) Pressures along the radial trajectory corresponding to the mean direction of NH trajectory (ecliptic latitude of 2° and longitude of 285°) are compared with the NH data (D. J. McComas et al. 2022) for thermal protons (pth; gray points), PUIs (green), and the proton mixture (black). (c) Temperature distributions in simulation H; an arbitrary time instant is visualized, and the variability over the last three simulated solar cycles is shown with shaded areas.
Paper: Constraining the Properties of the Multicomponent Local Interstellar Medium: MHD-kinetic Modeling Validated by Voyager and New Horizons Data
Authors: Federico Fraternale, Nikolai V. Pogorelov, Ratan K. Bera
Figure caption: Plasma distributions in the B–V plane from simulation H. From top to bottom we show the number density, pressure, and temperature. From left to right the quantities are shown for protons (including the core and PUIs), He ions, and electrons. The black contours show the HP position (defined by the LS ψ = 0). Additionally, two gray contours of ψ = ± 0.98 offer qualitative insights about the extent of mixing and numerical diffusion of the SW and LISM at the HP.
Paper: Sun-as-a-star Analysis of the X1.6 Flare on 2023 August 5: Dynamics of Postflare Loops in Spatially Integrated Observational Data
Authors: Takato Otsu, Ayumi Asai, Kai Ikuta, Kazunari Shibata
Figure caption: The time-slice diagram. From panels (a-1)–(d-1), time-slice diagrams along the slit in Figure 2 (t = 210 minutes) are shown for AIA 94 Å, 171 Å, 304 Å, and Hα line center, respectively. The GOES light curve is overplotted as the white dashed–dotted line. The inclined white dotted lines indicate a velocity of 4.5 km s−1. The horizontal white dashed lines indicate the solar limb, which are set as same for the three AIA channels but are different for the Hα line center. Panels (a-2)–(d-2) show the zoomed-in diagram corresponding to the white or black dashed regions in panels (a-1)–(d-1). The GOES peak time (t = 81 minutes) is indicated by the vertical white dotted line in panels (a-1)–(d-1) and (a-2). The vertical white or black dashed–dotted lines in panels (b-2)–(d-2) indicate the time of t = 90 minutes.
Paper: Sun-as-a-star Analysis of the X1.6 Flare on 2023 August 5: Dynamics of Postflare Loops in Spatially Integrated Observational Data
Authors: Takato Otsu, Ayumi Asai, Kai Ikuta, Kazunari Shibata
Figure caption: Time development of the target event in EUV images and Hα spectral images taken by SDO/AIA and SMART/SDDI, respectively. From left to right, images at 2023 August 5 22:10 UT (t = 70 minutes from 2023 August 5, 21:00 UT), 23:00 UT (t = 120 minutes), and 2023 August 6 00:30 UT (t = 210 minutes) are shown. In the top three rows, images of AIA 94 Å (a), 171 Å (b), and 304 Å (c) are shown. In the bottom three rows, Hα + 1.0 Å (d), Hα line center (e), and Hα − 1.0 Å are shown. The field of view of all the panels corresponds to the white dashed box in Figure 1(b). The white dashed line in each panel indicates the limb. Some notable points are indicated by the white arrows. The white dotted line connecting the white circle and cross is the artificial slit for the time-slice diagram in Figure 3.