adsabs/AstroCLIMB huggingface dataset:
Paper: Emergence of cHz Quasiperiodic Oscillations from a Low-angular-momentum Flow onto a Supermassive Black Hole
Authors: Indu K. Dihingia, Yosuke Mizuno
Figure caption: Density distribution and PDS for two different resolution cases. We show the density distribution for the case with ﹩{ \mathcal F }=0.30﹩ and a = 0.94 at simulation time t = 5000 tg (panel (a) and (b)) and the corresponding PDS of mass accretion and normalized magnetic flux for these models in panel (c). The white contour in panels (a) and (b) corresponds to ur = 0.
Paper: Emergence of cHz Quasiperiodic Oscillations from a Low-angular-momentum Flow onto a Supermassive Black Hole
Authors: Indu K. Dihingia, Yosuke Mizuno
Figure caption: Density distribution and PDS of the accretion rate for different values of α. The density distribution is presented at simulation time t = 5000 tg. In the simulations we used ﹩{ \mathcal F }=0.5﹩, but the α value was changed to 0, 5, and 10. The white contour corresponds to ur = 0. In the inset, the same is shown on the equatorial plan.
Paper: Emergence of cHz Quasiperiodic Oscillations from a Low-angular-momentum Flow onto a Supermassive Black Hole
Authors: Indu K. Dihingia, Yosuke Mizuno
Figure caption: Evolution of the mass accretion rate and normalized magnetic flux. The mass accretion rate (﹩\dot{M}﹩, panel (a)) and normalized magnetic flux (﹩{\phi }_{{\rm{BH}}}/\sqrt{\dot{M}}﹩, panel (b)) were calculated at the horizon for different models with different ﹩{ \mathcal F }﹩.
Paper: The Miscibility of Hydrogen and Water in Planetary Atmospheres and Interiors
Authors: Akash Gupta, Lars Stixrude, Hilke E. Schlichting
Figure caption: The pressure–temperature conditions of our simulations that result in two coexisting phases (blue circles) or a single homogeneous phase (gray circles), the critical curve derived from our results (bold black line) and as constrained by experiments at low pressure (bold dashed black line; T. M. Seward & E. U. Franck 1981), other experimental results (blue squares: two phases, gray squares: one phase; E. Bali et al. 2013; K. Vlasov et al. 2023), the phase boundary computed from our results at x = 0.6 (black dotted line), model temperature profiles for Uranus (green) and Neptune (blue; L. Scheibe et al. 2019), and a hot Uranus temperature profile with T1 = 85 K (dashed green). The blue-shaded hexagons and triangles represent conditions where we found pure H2O to be in crystalline (ice X) and superionic states, respectively, consistent with experimental results (e.g., M. Millot et al. 2019). The red lines represent possible loci of the boundary between the hydrogen-rich and the water-rich layer in models of the K2-18b according to N. Madhusudhan et al. (2020) for internal temperatures of 50 K (light red curve) and 25 K (dark red curve). The numbered points (red stars) refer to the boundary between the hydrogen-rich and the water-rich layers in three possible internal structure models that are examined in more depth by N. Madhusudhan et al. (2020).
Paper: The Miscibility of Hydrogen and Water in Planetary Atmospheres and Interiors
Authors: Akash Gupta, Lars Stixrude, Hilke E. Schlichting
Figure caption: Coexistence curves along several isotherms indicated, showing the compositions of the two coexisting phases as determined from our simulations (gray symbols with error bars) and the best-fit coexistence curves to these results (black dashed curves with pink uncertainty envelopes). No coexistence curve is shown for 6000 K because at that temperature we find a single homogeneous phase across the entire pressure range we have explored.
Paper: The Miscibility of Hydrogen and Water in Planetary Atmospheres and Interiors
Authors: Akash Gupta, Lars Stixrude, Hilke E. Schlichting
Figure caption: Variation of the critical composition of the hydrogen–water system with pressure (top), speciation (middle), and electronic entropy (bottom) of the homogeneous fluid along the critical curve. In the top panel, the green dots show the experimentally determined values of the critical composition and its comparison with those from this study. The middle panel shows the fraction of the species indicated in the homogeneous fluid along the critical line. The blue dashed curve is based on a Fermi–Dirac-like function tracing the change in the H-fraction and showcases the molecular-to-atomic transition in the fluid at ∼30–100 GPa and 3000–4000 K. The bottom panel shows the change in the electronic entropy along the critical curve and indicates the metallization of the homogeneous fluid as it transitions from molecular to atomic.
Paper: Meridional Circulation. I. A Formation Channel for Lithium-rich and Super-lithium-rich Red Clump Stars
Authors: Xue-Feng Li, Jian-Rong Shi, Yan Li, Hong-Liang Yan, Jing-Hua Zhang
Figure caption: Angular velocity distribution and mass fraction of H in the He flashes and core He-burning phases. Stellar parameters are 1.2 M⊙, Z = 0.017, vin,ZAMS = 10 km s−1, and A(Li)in,ZAMS = 3.3 dex. Here, there is no input velocity vin, RC. The two ends of the horizontal axis are X = 0.70 and the bottom of the convective envelope. The vertical lines represent ﹩{{\rm{\Omega }}}_{r}=(1+| 0.1| )\,{{\rm{\Omega }}}_{{r}_{1}}﹩, the right side of which is regarded as the rigid body. Yc is the mass fraction of central He. Note that the figure does not include the effect of meridional circulation.
Paper: Meridional Circulation. I. A Formation Channel for Lithium-rich and Super-lithium-rich Red Clump Stars
Authors: Xue-Feng Li, Jian-Rong Shi, Yan Li, Hong-Liang Yan, Jing-Hua Zhang
Figure caption: Similar to Figure A1, but only showing the distributions of Ωr and X in the core He-burning stage. The input velocity of the three panels vin,RC is 1, 10, and 100 km s−1, respectively.
Paper: Meridional Circulation. I. A Formation Channel for Lithium-rich and Super-lithium-rich Red Clump Stars
Authors: Xue-Feng Li, Jian-Rong Shi, Yan Li, Hong-Liang Yan, Jing-Hua Zhang
Figure caption: Evolution for stellar radius with age in the He-burning phase. We take the time of the He flash stage corresponding to the intersection S as the input moment of vin, HeF. The radius of the star at time S is the minimum value for the entire core He-burning phase.
Paper: Meridional Circulation. I. A Formation Channel for Lithium-rich and Super-lithium-rich Red Clump Stars
Authors: Xue-Feng Li, Jian-Rong Shi, Yan Li, Hong-Liang Yan, Jing-Hua Zhang
Figure caption: Similar to Figure A1, but only showing the distributions of Ωr and X in the late stage of He flash (after the time S in Figure A5). The input velocity vin,HeF is 1, 10, 30, 50, and 100 km s−1, respectively.
Paper: Meridional Circulation. I. A Formation Channel for Lithium-rich and Super-lithium-rich Red Clump Stars
Authors: Xue-Feng Li, Jian-Rong Shi, Yan Li, Hong-Liang Yan, Jing-Hua Zhang
Figure caption: Similar to Figure 1, but the transport process of material of meridional circulation is excluded.
Paper: Meridional Circulation. I. A Formation Channel for Lithium-rich and Super-lithium-rich Red Clump Stars
Authors: Xue-Feng Li, Jian-Rong Shi, Yan Li, Hong-Liang Yan, Jing-Hua Zhang
Figure caption: Evolution of diffusion coefficient with the age of the RC stars. The input equatorial velocities corresponding to the three evolutionary trajectories are 30, 50, and 100 km s−1, respectively.
Paper: Meridional Circulation. I. A Formation Channel for Lithium-rich and Super-lithium-rich Red Clump Stars
Authors: Xue-Feng Li, Jian-Rong Shi, Yan Li, Hong-Liang Yan, Jing-Hua Zhang
Figure caption: Similar to Figure 1, but the input velocity is vin,HeF.
Paper: The Critical Role of Dark Matter Halos in Driving Star Formation 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Luis C. Ho, Alvio Renzini, Yong Shi, Emanuele Daddi, Dingyi Zhao, Chengpeng Zhang, Zeyu Gao, Di Li, Cheqiu Lyu, Filippo Mannucci, Roberto Maiolino, Tao Wang, Feng Yuan
Figure caption: The average halo mass Mhalo (upper panels) and disk radius Rdisk (lower panels) on the SFEH I–sSFR plane for central spirals in the ALFALFA-SDSS matched sample, obtained by using a moving box of size 0.5 dex in sSFR and 0.5 dex in SFEH I. The galaxies are divided into low-mass bin 9.5  <  log M*(M⊙) <  10 (left panels), intermediate-mass bin 10  <  log M*(M⊙) <  10.6 (middle panels), and high-mass bin 10.6  <  log M*(M⊙) <  11 (right panels). In all panels, the blue vertical line indicates the approximate position between star-forming galaxies and passive galaxies. The purple diagonal lines indicate four different values of constant μH I of 1%, 10%, 100%, and 10. The gray thick line indicates the molecular gas FFR found in J. Dou et al. (2021a).
Paper: The Critical Role of Dark Matter Halos in Driving Star Formation 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Luis C. Ho, Alvio Renzini, Yong Shi, Emanuele Daddi, Dingyi Zhao, Chengpeng Zhang, Zeyu Gao, Di Li, Cheqiu Lyu, Filippo Mannucci, Roberto Maiolino, Tao Wang, Feng Yuan
Figure caption: Proposed evolutionary scenario illustrating how halo mass growth regulates the conversion of H I to H2, star formation, and the eventual quenching of galaxies. Based on the lower right panel of Figure 1, this diagram includes possible evolutionary paths (labeled as ①, ② and ③) that galaxies may follow as they transition through different states. In lower mass halos, galaxies are supported primarily in a cold accretion mode, which promotes efficient star formation. As halo mass increases, galaxies progress along paths ① (quenching at higher redshift) and ② (quenching at low redshift), with gas transitioning to a hot accretion mode that inhibits the conversion of H I to H2, suppressing star formation and eventually leading to a quenched state.
Paper: The Critical Role of Dark Matter Halos in Driving Star Formation 
Authors: Jing Dou, Yingjie Peng, Qiusheng Gu, Luis C. Ho, Alvio Renzini, Yong Shi, Emanuele Daddi, Dingyi Zhao, Chengpeng Zhang, Zeyu Gao, Di Li, Cheqiu Lyu, Filippo Mannucci, Roberto Maiolino, Tao Wang, Feng Yuan
Figure caption: Distribution of central spiral galaxies in the ALFALFA-SDSS matched sample on the SFR–stellar mass (M*) plane (left panel) and the disk size (Rdisk)–M* plane (right panel). Contours represent galaxy populations separated by sSFR: blue contours show galaxies with log sSFR  >  −2 Gyr−1, and red contours show galaxies with log sSFR  <  −2 Gyr−1. Both populations have been normalized.
Paper: Emergence of cHz Quasiperiodic Oscillations from a Low-angular-momentum Flow onto a Supermassive Black Hole
Authors: Indu K. Dihingia, Yosuke Mizuno
Figure caption: Distribution of logarithmic density on the poloidal plane at time t = 5000 tg. From left to right panels, different values of angular momentum (﹩{ \mathcal F }﹩) are used. The white contour corresponds to ur = 0, which is a boundary between the inflow and outflow regions. The inserted panels show the distribution of logarithmic density on the equatorial plane.
Paper: Emergence of cHz Quasiperiodic Oscillations from a Low-angular-momentum Flow onto a Supermassive Black Hole
Authors: Indu K. Dihingia, Yosuke Mizuno
Figure caption: Effect of tuning of angular momentum on the accretion rate profiles. Left: (a) evolution of accretion rate at the event horizon for two Kerr parameters a = 0.92 and a = 0.94 at different angular momentums around ﹩{ \mathcal F }=0.30﹩. Right: (b) evolution of the accretion rate at different radii (r = 1.5, 2.0, 3.0,  and 5.0 rg) for the cases of a = 0.92 and ﹩{ \mathcal F }=0.318﹩. Different colors indicate different cases that are marked on the top of the panel.
Paper: Emergence of cHz Quasiperiodic Oscillations from a Low-angular-momentum Flow onto a Supermassive Black Hole
Authors: Indu K. Dihingia, Yosuke Mizuno
Figure caption: PDS of the accretion rate at the horizon for different angular-momentum-accretion flows. Left: (a) PDS of the accretion rate at the event horizon for two different Kerr parameters a = 0.92 and a = 0.94 at different angular-momentum cases around ﹩{ \mathcal F }=0.30﹩. Right: (b) variation in the PDS of the accretion rate at the event horizon for the same Kerr parameter (a = 0.94) cases with different angular momentums. Each value of angular momentum and Kerr parameters is marked on the top of the figure.
Paper: Emergence of cHz Quasiperiodic Oscillations from a Low-angular-momentum Flow onto a Supermassive Black Hole
Authors: Indu K. Dihingia, Yosuke Mizuno
Figure caption: 3D volume rendering of logarithmic density distribution for Figure 3(d) to show the formation of PS close to the BH. Solid lines represent the magnetic field lines.
Paper: Discovery of a Low-mass Strong-lens System in SMACS J0723.3−7327
Authors: Limeng Deng, Yiping Shu, Lei Wang, Guoliang Li, Gabriel Bartosch Caminha, Jiang Dong, Zizhao He, Han Qu, Ruibiao Luo
Figure caption: Stellar mass vs. Einstein radius for a representative subset of known strong lenses. Blue circles represent SLACS lenses, green triangles represent SL2S lenses, orange squares represent S4TM lenses, the magenta pentagon represents iPTF16geu, and the cyan diamond represents MACS J1115-G1. SMACS J0723-SL is indicated by the red star. The blue, green, and orange bars indicate the typical stellar mass uncertainties (±1σ) for the SLACS, SL2S, and S4TM lenses.
Paper: Discovery of a Low-mass Strong-lens System in SMACS J0723.3−7327
Authors: Limeng Deng, Yiping Shu, Lei Wang, Guoliang Li, Gabriel Bartosch Caminha, Jiang Dong, Zizhao He, Han Qu, Ruibiao Luo
Figure caption: Left: pPXF velocity dispersion fitting result. The black line corresponds to the observed spectrum (smoothed for illustration purposes), and the red line corresponds to the best fit. Right: CIGALE SED fitting result. Open and filled circles correspond to the observed and model-predicted photometry.
Paper: Emergence of cHz Quasiperiodic Oscillations from a Low-angular-momentum Flow onto a Supermassive Black Hole
Authors: Indu K. Dihingia, Yosuke Mizuno
Figure caption: Light curve of polarized emission at 230 GHz. The case for ﹩{ \mathcal F }=0.318﹩ with a = 0.92 is presented. Panels (a)–(c) show the total intensity (I), linear polarization (﹩\sqrt{{Q}^{2}+{U}^{2}}﹩), and circular polarization (﹩\sqrt{{V}^{2}}﹩), respectively. Panel (d) presents the corresponding accretion rate (﹩\dot{M}﹩) at the horizon. Red rectangles show selected time periods of the oscillations.
Paper: Discovery of a Low-mass Strong-lens System in SMACS J0723.3−7327
Authors: Limeng Deng, Yiping Shu, Lei Wang, Guoliang Li, Gabriel Bartosch Caminha, Jiang Dong, Zizhao He, Han Qu, Ruibiao Luo
Figure caption: Best-fitting results. Within each of the first six rows, from left to right, we show the data, lens light model, lens light-subtracted data, lensed image model, normalized residual, and source light model. The first six rows correspond to the six filters and the last row is a color composite equivalent generated by combining the six filters.
Paper: The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center
Authors: Janik Karoly, Derek Ward-Thompson, Kate Pattle, Steven N. Longmore, James Di Francesco, Anthony Whitworth, Doug Johnstone, Sarah Sadavoy, Patrick M. Koch, Meng-Zhe Yang, Ray Furuya, Xing Lu, Motohide Tamura, Victor P. Debattista, David Eden, Jihye Hwang, Frédérick Poidevin, Bijas N., Szu-Ting Chen, Eun Jung Chung, Simon Coudé, Sheng-Jun Lin, Yasuo Doi, Takashi Onaka, Lapo Fanciullo, Tie Liu, Guangxing Li, Pierre Bastien, Tetsuo Hasegawa, Woojin Kwon, Shih-Ping Lai, Keping Qiu
Figure caption: Upper panel: the identified structures/clouds from astrodendro are plotted as closed colored lines over the 850 μm dust emission map and in the clouds that are identified as associated with a stream, the circularly averaged mean magnetic field of the cloud is represented by a white pseudovector. The three streams identified in Section 3 are plotted in brown, dark blue, and light blue. Lower panel: a plot of the difference between stream orientation (﹩{\theta }_{{\rm{grad}}}﹩) and the mean magnetic field of the associated cloud (﹩{\langle {\theta }_{{\rm{B}}}\rangle }_{{\rm{circ}}}﹩). The error bars are the standard error from the distribution of the magnetic field vectors within the clouds. Dashed lines are plotted at 30° and 60° to highlight the boundaries of “preferentially parallel” and “preferentially perpendicular,” respectively. Note the difference between the eastern and western sectors.
Paper: The JCMT BISTRO Survey: Magnetic Fields Align with Orbital Structure in the Galactic Center
Authors: Janik Karoly, Derek Ward-Thompson, Kate Pattle, Steven N. Longmore, James Di Francesco, Anthony Whitworth, Doug Johnstone, Sarah Sadavoy, Patrick M. Koch, Meng-Zhe Yang, Ray Furuya, Xing Lu, Motohide Tamura, Victor P. Debattista, David Eden, Jihye Hwang, Frédérick Poidevin, Bijas N., Szu-Ting Chen, Eun Jung Chung, Simon Coudé, Sheng-Jun Lin, Yasuo Doi, Takashi Onaka, Lapo Fanciullo, Tie Liu, Guangxing Li, Pierre Bastien, Tetsuo Hasegawa, Woojin Kwon, Shih-Ping Lai, Keping Qiu
Figure caption: The 850 μm Stokes I dust emission from SCUBA-2/POL-2. White line segments show the magnetic field direction (binned to 28″ and plotted with uniform length for clarity). The black contours show the integrated NH3 (3,3) emission at 20, 50, 100, and 200 K km s−1. The position of Sgr A* is shown as a filled yellow star and the more prominent molecular clouds of the CMZ are labeled. Clouds E/F through to Cloud B form the “Dust Ridge.” A scale bar and the beam sizes of the SCUBA-2/POL-2 and NH3 observations are shown in the bottom left. Galactic coordinates are plotted as a dotted grid and labeled on the upper and right axes.
Paper: Moving Plasma Structures and Possible Driving Mechanisms of Solar Microflares Observed with High-resolution Coronal Imaging
Authors: Qingmei Wang, Yi Bi, Hongfei Liang, JiaYan Yang, Liufan Gong
Figure caption: (a) Snapshots of 11 tiny ejections (E1–E11, as marked by red arrows) captured in EUI/HRIEUV 174 Å images. Black dashed lines indicate the crossing flaring loops. (b) Time–distance plots taken along the orange dashed lines plotted on panel (a). White dashed lines represent the peak times of the first three flares, respectively. The plane-of-sky velocities of tiny ejections E1–E11, appearing as inclined bright bands on panel (b), are measured as approximately 232, 154, 229, 216, 221, 339, 248, 261, 317, 226, and 211km s−1, respectively.
Paper: The Discovery of a 41 s Radio Pulsar PSR J0311+1402 with ASKAP
Authors: Yuanming Wang, 远明 王, Pavan A. Uttarkar, Ryan M. Shannon, Yu Wing Joshua Lee, Dougal Dobie, Ziteng Wang, Keith W. Bannister, Manisha Caleb, Adam T. Deller, Marcin Glowacki, Joscha N. Jahns-Schindler, Tara Murphy, Reshma Anna-Thomas, N. D. R. Bhat, Xinping Deng, Vivek Gupta, Akhil Jaini, Clancy W. James, John Tuthill
Figure caption: A sample of folded radio pulses from PSR J0311+1402. For each observation, the top panel shows the linear polarization position angle (PA) for detections of linear polarization greater than 3 times the off-pulse noise. The middle panel presents the average intensity vs. phase: the total intensity is shown as a black solid line, linear polarization is shown as the red solid line, and circular polarization is shown as the blue solid line. The bottom panel shows the pulse dynamic spectrum. “a.u.” stands for arbitrary units. The dark horizontal regions represent flagged data due to RFI. The number of averaged pulses are 58 for the MeerKAT observations and 136 for the GBT observation. The PAs in MeerKAT epoch 2 are different from those in other epochs, possibly due to low SNR and inadequate number of averaged pulses.
Paper: Moving Plasma Structures and Possible Driving Mechanisms of Solar Microflares Observed with High-resolution Coronal Imaging
Authors: Qingmei Wang, Yi Bi, Hongfei Liang, JiaYan Yang, Liufan Gong
Figure caption: (a) The average SDO/HMI magnetogram from 00:00 UT to 00:43:45 UT within the red box in Figure 1(e). The orange arrow indicates the average horizontal velocity field traced from the SDO/HMI magnetograms. (b) The sum of the helicity flux from 00:00 UT to 01:00 UT within the region in panel (a). (c) The evolution of HMI magnetograms covering the dipolar field associated with solar flares. The red, violet, and black curves represent the temporal profiles of positive, negative, and unsigned magnetic fluxes, respectively, from 00:00:00 UT to an hour later. The unsigned flux is defined as the summation of positive flux and the absolute value of negative flux. (d) The temporal profile of helicity flux and the accumulated helicity flux. The black and red curves represent the accumulated helicity flux and the helicity flux, respectively, from 00:00:00 UT to one hour later. The black arrows in panels (c) and (d) indicate the times of the 11 tiny ejections.
Paper: The Discovery of a 41 s Radio Pulsar PSR J0311+1402 with ASKAP
Authors: Yuanming Wang, 远明 王, Pavan A. Uttarkar, Ryan M. Shannon, Yu Wing Joshua Lee, Dougal Dobie, Ziteng Wang, Keith W. Bannister, Manisha Caleb, Adam T. Deller, Marcin Glowacki, Joscha N. Jahns-Schindler, Tara Murphy, Reshma Anna-Thomas, N. D. R. Bhat, Xinping Deng, Vivek Gupta, Akhil Jaini, Clancy W. James, John Tuthill
Figure caption: Pulsar period vs. duty cycle. The dots represent pulsars from the ATNF pulsar catalog (R. N. Manchester et al. 2005), while the dotted line shows the empirical relationship between pulsar spin period and pulse profile width (S. Johnston & A. Karastergiou 2019). The gray lines represent the theoretical relationship between pulsar period and pulse width, assuming an inclination angle of 45° and an impact parameter of 0°. The two lines correspond to emission heights of R (the neutron star radius) and 0.01rLC, where rLC is the light cylinder radius. PSR J0311+1402 is marked with a red star, and known LPTs from literature are also included (S. D. Hyman et al. 2005; C. M. Tan et al. 2018; M. P. Surnis et al. 2023; M. Caleb et al. 2022, 2024; N. Hurley-Walker et al. 2022, 2024; Z. Wang et al. 2024).
Paper: Moving Plasma Structures and Possible Driving Mechanisms of Solar Microflares Observed with High-resolution Coronal Imaging
Authors: Qingmei Wang, Yi Bi, Hongfei Liang, JiaYan Yang, Liufan Gong
Figure caption: (a)–(f) The EUI/HRIEUV 174 Å images displaying the detailed evolution of several tiny ejections. Red arrows mark tiny ejections, while black circles indicate the initial dot-like structure of tiny ejections. (g) SDO/AIA 171 Å images corresponding to the time and location of panel (c). In each panel, the left four images are raw, while the right four images show their base difference version (a), (b), (c), (d), and (g) or high-pass filtered version (e) and (f).
Paper: The Discovery of a 41 s Radio Pulsar PSR J0311+1402 with ASKAP
Authors: Yuanming Wang, 远明 王, Pavan A. Uttarkar, Ryan M. Shannon, Yu Wing Joshua Lee, Dougal Dobie, Ziteng Wang, Keith W. Bannister, Manisha Caleb, Adam T. Deller, Marcin Glowacki, Joscha N. Jahns-Schindler, Tara Murphy, Reshma Anna-Thomas, N. D. R. Bhat, Xinping Deng, Vivek Gupta, Akhil Jaini, Clancy W. James, John Tuthill
Figure caption: Diagram of spin period vs. period derivatives for pulsars and LPTs. The star outlined in red marks PSR J0311+1402. Dots represent radio pulsars from the ATNF pulsar catalog (R. N. Manchester et al. 2005), and circles represent recently discovered LPTs (N. Hurley-Walker et al. 2022, 2023; M. Caleb et al. 2022, 2024). Markers are colored by surface dipolar magnetic field at the pole, assuming spin-down due to dipolar losses. Dashed lines correspond to theoretical death lines for a pure dipole (K. Chen & M. Ruderman 1993; B. Zhang et al. 2000), dotted lines for a twisted dipole (K. Chen & M. Ruderman 1993; B. Zhang et al. 2000), and solid lines for a twisted multipole configuration (K. Chen & M. Ruderman 1993). Figure adapted from N. Hurley-Walker et al. (2023).