adsabs/AstroCLIMB huggingface dataset:
Paper: Star Formation under a Cosmic Microscope: Highly Magnified z = 11 Galaxy behind the Bullet Cluster
Authors: Maruša Bradač, Jon Judež, Chris Willott, Gregor Rihtaršic, Nicholas S. Martis, Anishya Harshan, Giordano Felicioni, Yoshihisa Asada, Guillaume Desprez, Douglas Clowe, Anthony H. Gonzalez, Christine Jones, Brian C. Lemaux, Maxim Markevitch, Vladan Markov, Lamiya Mowla, Gaël Noirot, Annika H. G. Peter, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki, Tim Schrabback, Roberta Tripodi
Figure caption: RGB (F277W, F357W, and F444W) image of the Bullet Cluster. Overlaid (in red) is the critical curve calculated at the redshift of BulletArc-z11 used in this Letter. In the inset (10″ × 10″), we use high-resolution RGB images (F115W, F150W, and F200W) to show BulletArc-z11 and the same red critical curve as well as in cyan the one with a cluster member added as described in Section 3.3.
Paper: Star Formation under a Cosmic Microscope: Highly Magnified z = 11 Galaxy behind the Bullet Cluster
Authors: Maruša Bradač, Jon Judež, Chris Willott, Gregor Rihtaršic, Nicholas S. Martis, Anishya Harshan, Giordano Felicioni, Yoshihisa Asada, Guillaume Desprez, Douglas Clowe, Anthony H. Gonzalez, Christine Jones, Brian C. Lemaux, Maxim Markevitch, Vladan Markov, Lamiya Mowla, Gaël Noirot, Annika H. G. Peter, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki, Tim Schrabback, Roberta Tripodi
Figure caption: MUV-versus-redshift plot for BulletArc-z11 (star) and the spectroscopically confirmed sources from the literature (circles, collated in G. Roberts-Borsani et al. 2025). Fill colors represent magnification μ given by the color bar. Open circles are blank-field sources with μ = 1. MUV values for different characteristic luminosities L* (at z ∼ 10, taken from C. J. Willott et al. 2024) are shown as dashed horizontal lines. The uncertainty on MUV for BulletArc-z11 is partly hidden behind the symbol and includes lensing uncertainties.
Paper: Star Formation under a Cosmic Microscope: Highly Magnified z = 11 Galaxy behind the Bullet Cluster
Authors: Maruša Bradač, Jon Judež, Chris Willott, Gregor Rihtaršic, Nicholas S. Martis, Anishya Harshan, Giordano Felicioni, Yoshihisa Asada, Guillaume Desprez, Douglas Clowe, Anthony H. Gonzalez, Christine Jones, Brian C. Lemaux, Maxim Markevitch, Vladan Markov, Lamiya Mowla, Gaël Noirot, Annika H. G. Peter, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki, Tim Schrabback, Roberta Tripodi
Figure caption: Results of the SED fitting using original full photometry using Photutils corrected by dividing by μ (labeled “All”; see also Table 1) and derived using Galfit for the smooth light component (G) and the three clumps (labeled C1–3). Shown are fluxes in red and SED-predicted fluxes in open circles in units of μJy. Derived stellar properties are given in the inset. While fluxes in F150W and shortward are shown, they were not included in the fit, as the redshift is only allowed to vary based on spectroscopic redshift measurement.
Paper: Star Formation under a Cosmic Microscope: Highly Magnified z = 11 Galaxy behind the Bullet Cluster
Authors: Maruša Bradač, Jon Judež, Chris Willott, Gregor Rihtaršic, Nicholas S. Martis, Anishya Harshan, Giordano Felicioni, Yoshihisa Asada, Guillaume Desprez, Douglas Clowe, Anthony H. Gonzalez, Christine Jones, Brian C. Lemaux, Maxim Markevitch, Vladan Markov, Lamiya Mowla, Gaël Noirot, Annika H. G. Peter, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki, Tim Schrabback, Roberta Tripodi
Figure caption: Source plane modeling using Lenstruction (L. Yang et al. 2020). From the top left, we plot the observed image (in F200W), the source model, the best-fit image model (after lensing and PSF convolution have been applied), and normalized residuals. The source was modeled using an underlying galaxy component G and three small clumps (#1–3) modeled using Gaussian profiles.
Paper: Star Formation under a Cosmic Microscope: Highly Magnified z = 11 Galaxy behind the Bullet Cluster
Authors: Maruša Bradač, Jon Judež, Chris Willott, Gregor Rihtaršic, Nicholas S. Martis, Anishya Harshan, Giordano Felicioni, Yoshihisa Asada, Guillaume Desprez, Douglas Clowe, Anthony H. Gonzalez, Christine Jones, Brian C. Lemaux, Maxim Markevitch, Vladan Markov, Lamiya Mowla, Gaël Noirot, Annika H. G. Peter, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki, Tim Schrabback, Roberta Tripodi
Figure caption: Mass fraction of stars formed as a function of lookback time (bottom axis) and redshift (top axis) for all components (All: blue, galaxy: orange, C1: green, C2: red, and C3: violet). All components seem to be forming 50% of their total mass by a redshift of ∼14 (t50 ∼ 150 Myr). Note, however, that the results indicate a large range of possible SFHs (as indicated by the errors given as the shaded regions).
Paper: GRB 240715A: Revealing a Novel Intrinsic Mechanism by Different Individual Pulses
Authors: Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Shi-Jie Zheng, Jiang He, Xiao-Yun Zhao, Yue Huang, Shu-Xu Yi, Bing Li, He Gao, Bo-bing Wu, Bing Zhang, Frédéric Daigne, Maria-Grazia Bernardini, Bin-Bin Zhang, Stéphane Basa, Bertrand Cordier, Jin-Song Deng, Yong-Wei Dong, Damien Dornic, Olivier GODET, Xu-Hui Han, Mao-Hai Huang, Cyril Lachaud, Hua-Li Li, Pierre Maggi, Frédéric Piron, Yu-Lei Qiu, Stéphane Schanne, Li-Ming Song, Damien Turpin, Susanna Vergani, Jing Wang, Ping Wang, Jian-Yan Wei, Chao Wu, Li-Ping Xin, Yang Xu, Li Zhang, Shuang-Nan Zhang
Figure caption: Spectrum fitting results. (a) Top panel: the light curve of GRM and the seven slices for the fine time-resolved spectrum were marked with different colors. The following three panels are, respectively, the photon index, Epeak, and flux of each slice fitted with GRM plus GBM data. (b) The Ep,z and Eiso correlation diagram. The best fit for type II (gray points) and type I (blue points) GRBs and MGFs (yellow points) are plotted (solid lines) with the 1σ boundary (dashed line) marked. The red dashed line represents the evolution of the Ep,z and Eiso of GRB 240715A as the redshift changes from 0.001 to 3. The GRB sample is from L. Lan et al. (2023), and the MGF sample is from H.-M. Zhang et al. (2020) and S. Mereghetti et al. (2024). (c) Epeak distribution of short GRBs observed by Fermi/GBM and GRB 240715A. The red bar represents Epeak and the error of GRB 240715A. The Epeak data reference is R.-J. Lu et al. (2017).
Paper: GRB 240715A: Revealing a Novel Intrinsic Mechanism by Different Individual Pulses
Authors: Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Shi-Jie Zheng, Jiang He, Xiao-Yun Zhao, Yue Huang, Shu-Xu Yi, Bing Li, He Gao, Bo-bing Wu, Bing Zhang, Frédéric Daigne, Maria-Grazia Bernardini, Bin-Bin Zhang, Stéphane Basa, Bertrand Cordier, Jin-Song Deng, Yong-Wei Dong, Damien Dornic, Olivier GODET, Xu-Hui Han, Mao-Hai Huang, Cyril Lachaud, Hua-Li Li, Pierre Maggi, Frédéric Piron, Yu-Lei Qiu, Stéphane Schanne, Li-Ming Song, Damien Turpin, Susanna Vergani, Jing Wang, Ping Wang, Jian-Yan Wei, Chao Wu, Li-Ping Xin, Yang Xu, Li Zhang, Shuang-Nan Zhang
Figure caption: (a) Spectral lag of each pulse of GRB 240715A. (b) Spectral lag of the whole light curve of GRB 240715A. (c) Spectral lags of each pulse for short GRBs from the GBM sample. The bars in different colors represent the lag of different pulses. The left panel shows the negative lags of pulses in GRBs, and the right panel shows the positive lags of pulses in GRBs. (d) The burst duration versus burst lag (in absolute value). The GRB sample is from N. Gehrels et al. (2006), M. G. Bernardini et al. (2015), A. Goldstein et al. (2017), and S. Xiao et al. (2022). (e) The histogram of the lags of the pulses in short GRBs, and the lag of the first pulse of GRB 240715A is labeled. (f) The pulse duration versus the ratio of the pulse lag and pulse duration (in absolute value). The type II GRB sample is from R.-J. Lu et al. (2018).
Paper: GRB 240715A: Revealing a Novel Intrinsic Mechanism by Different Individual Pulses
Authors: Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Shi-Jie Zheng, Jiang He, Xiao-Yun Zhao, Yue Huang, Shu-Xu Yi, Bing Li, He Gao, Bo-bing Wu, Bing Zhang, Frédéric Daigne, Maria-Grazia Bernardini, Bin-Bin Zhang, Stéphane Basa, Bertrand Cordier, Jin-Song Deng, Yong-Wei Dong, Damien Dornic, Olivier GODET, Xu-Hui Han, Mao-Hai Huang, Cyril Lachaud, Hua-Li Li, Pierre Maggi, Frédéric Piron, Yu-Lei Qiu, Stéphane Schanne, Li-Ming Song, Damien Turpin, Susanna Vergani, Jing Wang, Ping Wang, Jian-Yan Wei, Chao Wu, Li-Ping Xin, Yang Xu, Li Zhang, Shuang-Nan Zhang
Figure caption: Spectral fitting results and “death line” of the photosphere of the third pulse. (a)–(d) The observed photon count spectrum and Fν energy spectrum of the BAND model, BAND-Cut model, mBB model, and synchrotron model, respectively. (e) The corner plot of the posterior probability distributions of the parameters of the mBB model. (f) The so-called “photosphere death line” constraints. The red line is for a strict blackbody, and the blue line is for a relativistic mBB outflow. The red dashed line represents the rest-frame peak energy Ep,z and the observed isotropic γ-ray luminosity Liso of the third pulse as the redshift varies.
Paper: GRB 240715A: Revealing a Novel Intrinsic Mechanism by Different Individual Pulses
Authors: Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Shi-Jie Zheng, Jiang He, Xiao-Yun Zhao, Yue Huang, Shu-Xu Yi, Bing Li, He Gao, Bo-bing Wu, Bing Zhang, Frédéric Daigne, Maria-Grazia Bernardini, Bin-Bin Zhang, Stéphane Basa, Bertrand Cordier, Jin-Song Deng, Yong-Wei Dong, Damien Dornic, Olivier GODET, Xu-Hui Han, Mao-Hai Huang, Cyril Lachaud, Hua-Li Li, Pierre Maggi, Frédéric Piron, Yu-Lei Qiu, Stéphane Schanne, Li-Ming Song, Damien Turpin, Susanna Vergani, Jing Wang, Ping Wang, Jian-Yan Wei, Chao Wu, Li-Ping Xin, Yang Xu, Li Zhang, Shuang-Nan Zhang
Figure caption: Light curves and pulse fitting. (a) Light curves of SVOM/GRM and Fermi/GBM with 5 ms bin width and the time–energy diagram of SVOM/GRM within the energy range from 10 to 1000 keV. (b) Multiwavelength light curves of SVOM/GRM with 10 ms bin width. (c) The triple-pulse fitting of the light curves in each energy band with the triple-Gaussian function. (d) The time delay of the peak of each pulse. (e) The width of each pulse in each energy band.
Paper: GRB 240715A: Revealing a Novel Intrinsic Mechanism by Different Individual Pulses
Authors: Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Shi-Jie Zheng, Jiang He, Xiao-Yun Zhao, Yue Huang, Shu-Xu Yi, Bing Li, He Gao, Bo-bing Wu, Bing Zhang, Frédéric Daigne, Maria-Grazia Bernardini, Bin-Bin Zhang, Stéphane Basa, Bertrand Cordier, Jin-Song Deng, Yong-Wei Dong, Damien Dornic, Olivier GODET, Xu-Hui Han, Mao-Hai Huang, Cyril Lachaud, Hua-Li Li, Pierre Maggi, Frédéric Piron, Yu-Lei Qiu, Stéphane Schanne, Li-Ming Song, Damien Turpin, Susanna Vergani, Jing Wang, Ping Wang, Jian-Yan Wei, Chao Wu, Li-Ping Xin, Yang Xu, Li Zhang, Shuang-Nan Zhang
Figure caption: Simulation of the lag generation. (a) Simulated Gaussian light curves in different energy bands along with α evolve from soft to hard. The parameters of A = 60, μ = 0.25, σ = 0.001, α0 = −1.5, kα = 7.3, and t0 = 0.19 s are adopted to be consistent with the observations. (b) The lag versus energy of the simulated Gaussian light curves. (c) Simulated FRED light curves in different energy bands along with α evolve from soft to hard. The parameters of A = 60, τr = 0.2, τd = 0.5, α0 = −1.5, kα = 0.2, and t0 = 0 are adopted. (d) The lag versus energy of the simulated Gaussian light curves.
Paper: Multiple Shells in Supernova 2023ixf Support the Jittering Jets Explosion Mechanism
Authors: Noam Soker, Kobi Shiran
Figure caption: The time evolution of the photospheric radius from E. A. Zimmerman et al. (2024) based on photometry (not on spectroscopy). We fit two straight lines through two groups of points: the first four points, green stars, at t = 1.13–1.42 days that we mark as Shell 1, and the next 11 points, green pentagons, at t = 1.57–6.13 days that we mark as Shell 2. The red pentagons are excluded from the fitting; they belong to the phase when the photosphere is moving inward in the mass coordinate of the ejecta. We also indicate the velocity of each shell during the fitting period. The line for Shell 3 fits a later time period, as shown in Figure 2. We identify these shells as photospheric shells appearing one after the other. The straight lines for the three shells are Rph1 = 1.050t + 0.425, Rph2 = 0.808t + 0.477, and Rph3 = 0.445t + 0.723, where the time is in days and the radius in units of 1014 cm. All lines have a coefficient of determination (R-Squared) of R2 = 0.98. The velocities and their uncertainties are from fitting the ejecta photosphere radii without including the radii of the shells at t = 0. Including the radii at t = 0 changes the velocities little but substantially reduces the uncertainties, indicating that the three shells are distinct, by these photospheric radii (caveat: see the text on the possibility that Shells 1 and 2 are a single shell).
Paper: Multiple Shells in Supernova 2023ixf Support the Jittering Jets Explosion Mechanism
Authors: Noam Soker, Kobi Shiran
Figure caption: Similar to Figure 1, but including later times and different scales on the axes. As in Figure 1, red pentagons and pluses are excluded from fittings. We fit a third straight line to the points in the time period of t = 42.19–70.63 days (green pluses); this is Shell 3. The points from day 7 to day 41 (red pentagons) are the photospheric radius in the ejecta inward to Shell 2 and outside Shell 3. During that time, the photosphere moves inward in the mass coordinate of the ejecta. Therefore, each point corresponds to a deeper mass layer than the previous point; the points do not represent a single layer. For that, we cannot fit a straight line through these points. Around day 45, the front of Shell 3 becomes the photosphere. From there to about day 71, a straight line corresponds to the front of Shell 3. After day 71, Shell 3 became transparent, and the photosphere moved inward in the mass coordinate of the ejecta (red pluses).
Paper: A Precessing, Magnetically Dominated, Structured Jet Powering the Hour-scale Quasiperiodic GRB 250702B
Authors: Tao An
Figure caption: Qualitative placement of GRB 250702B (shaded rectangle) in (K, q) space, where K ≡ r/rISCO(a*) and q ≡ MT/MBH is the torus-to-BH mass ratio (M. H. P. M. van Putten et al. 2024). For the observed period P ≃ 2825 s and a fiducial MBH = 6 M⊙, GRB 250702B occupies K ≃ 59–130 for BH spins a* = 0.5–0.9 and q ∼ 10−4 (shaded band). The adopted q value places the event between canonical long GRBs (q ∼ 10−2) and SLSNe (q ∼ 10−7). The rectangular boxes show representative (K, q) regions for GW170817B (the post-merger BH spindown signal associated with GW170817 with estimated K ∼ 3–4 and q ∼ 10−3–10−2; M. H. P. M. van Putten et al. 2024) and M87 with minimal torus fraction q ∼ 10−7–10−8 (jet launching and collimation occur on scales of a few rISCO, inferred from VLBI constraints and jet kinematics—e.g., S. S. Doeleman et al. 2012; F. Mertens et al. 2016; J. Y. Kim et al. 2018; and further supported by the detection of jet precession—e.g., Y. Cui et al. 2023). Both GW170817B and M87 therefore anchor the “few–rISCO” end of the diagram, whereas GRB 250702B requires a much larger K, where the precession is set by the outer working annulus of a thick inner flow.
Paper: A Precessing, Magnetically Dominated, Structured Jet Powering the Hour-scale Quasiperiodic GRB 250702B
Authors: Tao An
Figure caption: LT “mass–meter” for the observed periodicity P = 2825 s. The curves show the BH mass M• implied by a precession radius ﹩\tilde{r}\equiv r/{r}_{{\rm{g}}}﹩ for spins a* = {0.3, 0.5, 0.9}. The horizontal dashed lines mark the IMBH band (104–106 M⊙); the dotted lines mark the stellar-mass band (3–30 M⊙); and the thin solid line highlights a GRB scale M• = 6 M⊙. For ﹩\tilde{r}\sim 10\,\unicode{x02013}\,50\,{r}_{{\rm{g}}}﹩, the period selects the IMBH regime; achieving the same period with a ∼6 M⊙ engine requires ﹩\tilde{r}\gtrsim 200\,\unicode{x02013}\,400\,{r}_{{\rm{g}}}﹩ or a different precession driver.
Paper: A Precessing, Magnetically Dominated, Structured Jet Powering the Hour-scale Quasiperiodic GRB 250702B
Authors: Tao An
Figure caption: Geometry of the precessing, magnetically dominated, structured-jet model proposed for GRB 250702B. A misaligned geometrically thick torus/wind collimates the jet and defines the precessing axis. The structured jet consists of a narrow spine (orange color) surrounded by a wider sheath (blue color), with a small kink at (2–4) × 102rg indicating where the jet is forced into precession by the disk wind. The observer’s LOS lies just outside the sheath at a small inclination to the jet axis, enabling lighthouse-like modulation and occasional “missing” pulses. An outer thin disk at r ≳ 250 rg is also indicated.
Paper: A Remote Brightening from Interactions between an Extreme-ultraviolet Jet and a Magnetic Null
Authors: Chao Zhang, Zhenghua Huang, Hengyuan Wei, Yuandeng Shen, Mijie Shi, Bo Li, Maria S. Madjarska, Xiuhui Zuo, Lidong Xia
Figure caption: (a)–(d) Evolution of the RS1 region seen in the 171 Å passband. The dashed line in panel (b) marks the inverted-Y structure. Arrows in panels (a) and (c) indicate the small loops. Red-boxed region in panel (a) is the region directly bombarded by the jet materials. Yellow-boxed region in panel (c) marks the inverted-Y center. (e)–(h) The RS1 region in AIA 304, 94, 193, and 211 Å passbands during the formation of the inverted-Y structure. The evolution of the event seen in AIA 171, 304, and 94 Å is shown on the right side of the animation associated with Figure 1.
Paper: A Remote Brightening from Interactions between an Extreme-ultraviolet Jet and a Magnetic Null
Authors: Chao Zhang, Zhenghua Huang, Hengyuan Wei, Yuandeng Shen, Mijie Shi, Bo Li, Maria S. Madjarska, Xiuhui Zuo, Lidong Xia
Figure caption: (a) The synthesized 171 Å image derived from the simulation at t = 120 s. Solid lines mark the position of the inverted-Y structure. The red solid box encloses the center of the inverted-Y structure. (b) The evolution of the current within the red box shown in panel (a) (black solid line) and the inflow speed around the current sheet (red solid line). (c) The lightcurves of the synthesized 171 Å passband within the red box shown in panel (a). The evolution of the simulated region in synthesized 171 Å is shown on the right side of the animation associated with Figure 6.
Paper: A Remote Brightening from Interactions between an Extreme-ultraviolet Jet and a Magnetic Null
Authors: Chao Zhang, Zhenghua Huang, Hengyuan Wei, Yuandeng Shen, Mijie Shi, Bo Li, Maria S. Madjarska, Xiuhui Zuo, Lidong Xia
Figure caption: The AIA 171 Å lightcurves of region “a” (green solid line) and region “b” (blue solid line) as shown in Figure 2 and relative variations of GOES 1.0–8.0 Å soft X-ray flux (purple solid line).
Paper: A Remote Brightening from Interactions between an Extreme-ultraviolet Jet and a Magnetic Null
Authors: Chao Zhang, Zhenghua Huang, Hengyuan Wei, Yuandeng Shen, Mijie Shi, Bo Li, Maria S. Madjarska, Xiuhui Zuo, Lidong Xia
Figure caption: Time–distance plots along paths 1–2 (panel (a)) and 1–3 (panel (b)) as marked in Figure 2(b). The solid lines trace the bidirectional flows.
Paper: A Remote Brightening from Interactions between an Extreme-ultraviolet Jet and a Magnetic Null
Authors: Chao Zhang, Zhenghua Huang, Hengyuan Wei, Yuandeng Shen, Mijie Shi, Bo Li, Maria S. Madjarska, Xiuhui Zuo, Lidong Xia
Figure caption: The initial state of temperature. White solid lines are the magnetic field lines. White arrows represent the initial velocity. The purple circle highlights the region where sound speed equals Alfvén velocity.
Paper: The Brown-dwarf Desert Persists as a Mass-ratio Desert around Low-mass Stars
Authors: Keming Zhang, 可名 张
Figure caption: Corner plot illustrating the posterior distribution of the power-law mass-ratio function fitted to the combined KMTNet and MOA-II samples (–3.4 ﹩\lt \mathrm{log}(q)\lt ﹩ –1.75), with the upper truncation value ﹩{q}_{{\rm{\max }}}\gt 0.017﹩ as a free parameter. Contours show the 1/2/3σ regions, with vertical lines in the 1D marginal plots showing the 16/50/84 percentiles. The parameter values differ from Equations (4)–(5), which adopted a fixed qmax = 0.017.
Paper: Multiple Shells in Supernova 2023ixf Support the Jittering Jets Explosion Mechanism
Authors: Noam Soker, Kobi Shiran
Figure caption: Two images of CCSN remnants with two full (or almost full) shells (but not spherical). Studies attributed their morphologies to the JJEM. In each image, we marked the two prominent shells that can form two photospheric shells one after the other during the photospheric phase of such CCSNe; the arrows point to only four points on the projection of each shell boundary onto the plane of the sky. Filled double-lined arrows point at the first shell, and the empty double-lined double-headed arrows point at the second shell. (a) A radio image of SNR G309.2-00.6 adapted from B. M. Gaensler et al. (1998), who already argued that jets shaped this CCSN. The rim-nozzle symmetry marks are from N. Soker (2024b). (b) A composite image of CCSNR W44 from a NASA site (www.nasa.gov/universe/nasas-fermi-proves-supernova-remnants-produce-cosmic-rays/). N. Soker (2024c) added the two double-headed arrows that depict the two axes of the two energetic pairs of jets that participated in the explosion of W44. Magenta: GeV gamma-ray from Fermi’s Large Area Telescope (LAT); yellow: radio from the Karl G. Jansky Very Large Array; red: infrared; blue: X-ray from ROSAT. Credit: NASA/Department of Energy/Fermi LAT Collaboration, NRAO/Associated Universities Inc., JPL-Caltech, and ROSAT.
Paper: Multiple Shells in Supernova 2023ixf Support the Jittering Jets Explosion Mechanism
Authors: Noam Soker, Kobi Shiran
Figure caption: Two images of CCSNRs where at least one shell is partial. (a) A MeerKat radio image at 1.28 GHz of SNR G0.9+0.1 adapted from I. Heywood et al. (2022). The inset on the upper left is a desaturated image of the pulsar wind nebula. N. Soker (2025a) added the pale-blue marks of structural features used to identify the point-symmetric morphology. For a line of sight along the large ear in the north, the three shells (their projection on the plane of the sky forms the rims) might form three photospheric shells. The first two (pointed at by the solid one-head yellow arrow and double-lined double-headed yellow arrow) are partial. The third shell (pointed at by the three-headed arrow) is the main shell of the supernova remnant. (b) A Chandra X-ray image of N63A (red, green, and blue for different X-ray energy bands); see also E. Karagöz et al. (2023). N. Soker (2024d) added the three red lines between the tips of opposite ears to mark the symmetry axis of three pairs of jets that participated in the explosion of this point-symmetric CCSNR. Each ear’s front can form the first photospheric shell, depending on the viewing angle. The main CCSNR forms the next photospheric radius. The light brown region to the upper right of the three red lines is optical light detected by Hubble. (Credit: enhanced Image by Judy Schmidt based on images provided courtesy of NASA/Chandra X-ray Observatory/Smithsonian Astrophysical Observatory and NASA/STScI.)