adsabs/AstroCLIMB huggingface dataset:
Paper: JWST and Ground-based Observations of the Type Iax Supernovae SN 2024pxl and SN 2024vjm: Evidence for Weak Deflagration Explosions
Authors: Lindsey A. Kwok, Mridweeka Singh, Saurabh W. Jha, Stéphane Blondin, Raya Dastidar, Conor Larison, Adam A. Miller, Jennifer E. Andrews, Moira Andrews, G. C. Anupama, Katie Auchettl, Dominik Bánhidi, Barnabas Barna, K. Azalee Bostroem, Thomas G. Brink, Régis Cartier, Ping Chen, Collin T. Christy, David A. Coulter, Sofia Covarrubias, Kyle W. Davis, Connor B. Dickinson, Yize Dong, Joseph R. Farah, Alexei V. Filippenko, Andreas Flörs, Ryan J. Foley, Noah Franz, Christoffer Fremling, Lluís Galbany, Anjasha Gangopadhyay, Aarna Garg, Peter Garnavich, Elinor L. Gates, Or Graur, Alexa C. Gordon, Daichi Hiramatsu, Emily Hoang, D. Andrew Howell, Brian Hsu, Joel Johansson, Arti Joshi, Lordrick A. Kahinga, Ravjit Kaur, Sahana Kumar, Piramon Kumnurdmanee, Hanindyo Kuncarayakti, Natalie LeBaron, Chang Liu, Keiichi Maeda, Kate Maguire, Curtis McCully, Darshana Mehta, Luca M. Menotti, Anne J. Metevier, Kuntal Misra, C. Tanner Murphey, Megan Newsome, Estefania Padilla Gonzalez, Kishore C. Patra, Jeniveve Pearson, Anthony L. Piro, Abigail Polin, Aravind P. Ravi, Armin Rest, Nabeel Rehemtulla, Nicolas Meza Retamal, Olivia M. Robinson, César Rojas-Bravo, Devendra K. Sahu, David J. Sand, Brian P. Schmidt, Steve Schulze, Michaela Schwab, Manisha Shrestha, Matthew R. Siebert, Sunil Simha, Nathan Smith, Jesper Sollerman, Bhagya M. Subrayan, Tamás Szalai, Kirsty Taggart, Rishabh Singh Teja, Tea Temim, Jacco H. Terwel, Samaporn Tinyanont, Stefano Valenti, Jorge Anais Vilchez, József Vinkó, Aya L. Westerling, Yi Yang, WeiKang Zheng
Figure caption: The discrepancy in the LRS wavelength solution introduces some additional uncertainties to the measured line velocities and widths.
Paper: Electromagnetic Signatures from Pulsar Remnants of Binary Neutron Star Mergers: Prospects for Unique Identification Using Multiwavelength Signatures
Authors: Mainak Mukhopadhyay, Shigeo S. Kimura
Figure caption: Distance horizons (﹩{d}_{{\rm{lim}}}﹩; see Equation (5)) for various survey and pointing telescopes for the fiducial scenario. The upcoming telescopes are shown with dashed lines. See Table 1 for details about the telescopes. Note that for EP-FXT, AMEGO, and NuSTAR the sudden jump is a result of the long integration time ΔTint = 106 s. Note that Tobs is the time elapsed from the GW detection of the BNS merger.
Paper: Electromagnetic Signatures from Pulsar Remnants of Binary Neutron Star Mergers: Prospects for Unique Identification Using Multiwavelength Signatures
Authors: Mainak Mukhopadhyay, Shigeo S. Kimura
Figure caption: Left: same as Figure 3, but for the optimistic case. Right: same as Figure 4, but for the optimistic case.
Paper: Electromagnetic Signatures from Pulsar Remnants of Binary Neutron Star Mergers: Prospects for Unique Identification Using Multiwavelength Signatures
Authors: Mainak Mukhopadhyay, Shigeo S. Kimura
Figure caption: Time evolution of ﹩{ \mathcal A }﹩ for the fiducial (solid red-orange) and the optimistic (dotted–dashed purple) scenarios.
Paper: Electromagnetic Signatures from Pulsar Remnants of Binary Neutron Star Mergers: Prospects for Unique Identification Using Multiwavelength Signatures
Authors: Mainak Mukhopadhyay, Shigeo S. Kimura
Figure caption: Same as Figure 5, but for the optimistic case.
Paper: Electromagnetic Signatures from Pulsar Remnants of Binary Neutron Star Mergers: Prospects for Unique Identification Using Multiwavelength Signatures
Authors: Mainak Mukhopadhyay, Shigeo S. Kimura
Figure caption: Same as Figure 1, but for the optimistic case.
Paper: Electromagnetic Signatures from Pulsar Remnants of Binary Neutron Star Mergers: Prospects for Unique Identification Using Multiwavelength Signatures
Authors: Mainak Mukhopadhyay, Shigeo S. Kimura
Figure caption: Same as Figure 2, but for the optimistic case.
Paper: Pivot of the Emerging Bipolar Magnetic Region in the Birth of Sigmoidal Solar Active Regions
Authors: Ronald L. Moore, Sanjiv K. Tiwari, V. Aparna, Navdeep K. Panesar, Alphonse C. Sterling, Talwinder Singh
Figure caption: Four sequential schematic drawings depicting the production of an S-shaped sigmoidal AR by the emergence of an Ω-loop flux rope in which the magnetic field has a right-handed twist about the flux rope’s central field line. Top left: sketch of a buoyantly rising east–west preemergent Ω-loop flux rope viewed horizontally from the south. The thick black straight horizontal line close above the rising Ω loop is the Sun’s photosphere surface. Only the outline of the flux rope’s surface, the flux rope’s central field line, and a field line on the flux rope’s surface are drawn. The pitch of the surface field’s twist with respect to the central field line is drawn to be 45°. We assume that the field’s twist pitch angle monotonically decreases inward to 0 at the central field line. We also assume that the Ω-loop flux rope’s two opposite-polarity vertical legs each sit in a downflow at opposite edges of a convection cell. Top right, bottom left, and bottom right: three sequential sketches of the emerging Ω loop in the corona, viewed vertically from above. The growing red disk and blue disk represent the emerging BMR’s growing positive and negative magnetic flux domains. The black lines connecting the two disks represent the emerging AR’s coronal magnetic field lines. As the Ω-loop flux rope emerges through the photosphere into the corona, the BMR initially tilts 45° clockwise of east–west and then pivots counterclockwise to become directed east–west as its two growing opposite-polarity flux domains spread apart and the AR’s coronal field becomes S-shaped. At the end of emergence, the BMR is directed east–west as in the bottom right panel, and each of the BMR’s two opposite-polarity flux domains is centered on the downflow in which its leg of the Ω loop is trapped. Each is centered on the position of the vertical portion of its leg of the Ω loop in the top left panel, as a comparison of those two panels shows.
Paper: Flares on TRAPPIST-1 Reveal the Spectrum of Magnetic Features on Its Surface
Authors: Valeriy Vasilyev, Nadiia Kostogryz, Alexander I. Shapiro, Astrid M. Veronig, Benjamin V. Rackham, Christoph Schirninger, Julien de Wit, Ward Howard, Jeff Valenti, Adina D. Feinstein, Olivia Lim, Sara Seager, Laurent Gizon, Sami K. Solanki
Figure caption: Stellar flares observed in JWST/NIRISS time-series spectroscopy of TRAPPIST-1. Each column shows one flare event during transits of the TRAPPIST-1c or TRAPPIST-1f planets. Top row: light curves with the total flux (integrated over the full spectral range and normalized to the mean out-of-transit flux). Colored points indicate preflare (green), flare (orange), maximum flare light (red), and postflare (blue) phases. Green and blue dashed lines mark the average pre- and postflare flux levels. Middle row: light curves of the normalized Hα flux. Bottom row: time-resolved spectrograms (wavelength vs. time) normalized to the preflare spectrum. The shaded blue region shows the drop in flux caused by the planetary transit. For comparison, the time axes in all panels are aligned such that t = 0 corresponds to the beginning of the maximum flare light phase. In all four events, the total flux in the postflare phase is systematically elevated relative to the preflare level.
Paper: Flares on TRAPPIST-1 Reveal the Spectrum of Magnetic Features on Its Surface
Authors: Valeriy Vasilyev, Nadiia Kostogryz, Alexander I. Shapiro, Astrid M. Veronig, Benjamin V. Rackham, Christoph Schirninger, Julien de Wit, Ward Howard, Jeff Valenti, Adina D. Feinstein, Olivia Lim, Sara Seager, Laurent Gizon, Sami K. Solanki
Figure caption: Spectral variations during and after the flare, relative to the preflare state. Panels (a)–(d): each panel shows one flare event (Flares 1-4). The red curves represent the flare spectrum (maximum flare light minus preflare), and the blue curves show the postflare spectrum relative to the preflare level, reflecting the spectral energy distributions of a disappearing active region. Vertical dashed lines indicate emission lines observed during the flare. All spectra are binned in wavelength by averaging over 20 points per bin for clarity. The spectral profile of the postflare flux enhancement is substantially different from that observed during the flare maximum. In particular, it is not accompanied by the strong emission lines seen during the flare phase.
Paper: Flares on TRAPPIST-1 Reveal the Spectrum of Magnetic Features on Its Surface
Authors: Valeriy Vasilyev, Nadiia Kostogryz, Alexander I. Shapiro, Astrid M. Veronig, Benjamin V. Rackham, Christoph Schirninger, Julien de Wit, Ward Howard, Jeff Valenti, Adina D. Feinstein, Olivia Lim, Sara Seager, Laurent Gizon, Sami K. Solanki
Figure caption: Correlation between total and Hα fluxes. Each panel shows the normalized Hα flux vs. normalized total flux for one of the four observed flares. Data are separated into three temporal phases: preflare (green), flare (orange), and postflare (blue). Linear fits are shown for the flare phase (orange line) and for the combined pre- and postflare data (blue line), with shaded regions indicating ±1σ confidence intervals. Pearson correlation coefficients (R) are listed in matching colors. There is a tight correlation between the Hα flux and the total flux during the flare, and this correlation breaks down in the pre- and postflare periods. This decoupling supports our conclusion that the postflare flux enhancement is not due to a lingering flare decay.
Paper: Pivot of the Emerging Bipolar Magnetic Region in the Birth of Sigmoidal Solar Active Regions
Authors: Ronald L. Moore, Sanjiv K. Tiwari, V. Aparna, Navdeep K. Panesar, Alphonse C. Sterling, Talwinder Singh
Figure caption: Scatter plot of the measured end-of-pivot tilt vs. measured pivot-amount angle at the end of the emergence (both from Table 1) for our 42 single-BMR sigmoidal ARs. The pivot-amount angle is taken to be positive for a counterclockwise pivot and negative for a clockwise pivot. The red line is the linear least-squares fit to the 42 points. The slope and 1σ uncertainty of the fit are −0.08 ± 0.08.
Paper: Pivot of the Emerging Bipolar Magnetic Region in the Birth of Sigmoidal Solar Active Regions
Authors: Ronald L. Moore, Sanjiv K. Tiwari, V. Aparna, Navdeep K. Panesar, Alphonse C. Sterling, Talwinder Singh
Figure caption: Histogram of the measured pivot amount for our 42 emerging sigmoidal ARs. Each colored square is for an AR that has a pivot amount in the pivot-amount range of that square. Each AR’s measured pivot amount is listed in Table 1. Red squares are for ARs in which the emerging BMR pivots counterclockwise as the AR’s coronal magnetic field becomes overall S-shaped. Blue squares are for ARs in which the emerging BMR pivots clockwise as the AR’s coronal magnetic field becomes overall Z-shaped.
Paper: Flares on TRAPPIST-1 Reveal the Spectrum of Magnetic Features on Its Surface
Authors: Valeriy Vasilyev, Nadiia Kostogryz, Alexander I. Shapiro, Astrid M. Veronig, Benjamin V. Rackham, Christoph Schirninger, Julien de Wit, Ward Howard, Jeff Valenti, Adina D. Feinstein, Olivia Lim, Sara Seager, Laurent Gizon, Sami K. Solanki
Figure caption: Magnetic surface features vanishing during flares on TRAPPIST-1. (a) Schematic representation of the inferred projected surface areas of magnetic features that disappeared during four flare events on TRAPPIST-1. The colored circles illustrate the projected surface areas required to explain the observed postflare flux enhancement, assuming three limiting cases for the brightness contrast of the vanished region: a completely black spot (darkest), an umbra-like region (medium gray), and a penumbra-like region (light gray). Limb darkening, spatial distribution, and foreshortening are not considered. We note that these projected surface areas represent only the vanished part of the active region. The total size of the original active region may be larger. (b) Spectra of the vanishing active regions shown in panel (a). Each colored curve shows the difference between the postflare and preflare spectra for one of the four analyzed flares (AR 1–4), interpreted as the spectral energy distribution of a magnetic active surface feature that vanished during the flare. The spectra are binned over 40 wavelength intervals for clarity. The black curve shows the quiescent spectrum of TRAPPIST-1, obtained by time-averaging the data during the TRAPPIST-1f visit. The spectrum is scaled for comparison. The figure shows that the spectral profile of the vanished magnetic features does not differ substantially from that of TRAPPIST-1.
Paper: Flares on TRAPPIST-1 Reveal the Spectrum of Magnetic Features on Its Surface
Authors: Valeriy Vasilyev, Nadiia Kostogryz, Alexander I. Shapiro, Astrid M. Veronig, Benjamin V. Rackham, Christoph Schirninger, Julien de Wit, Ward Howard, Jeff Valenti, Adina D. Feinstein, Olivia Lim, Sara Seager, Laurent Gizon, Sami K. Solanki
Figure caption: Line profiles of flare-induced emission features in normalized JWST/NIRISS spectra. Each column corresponds to a different flare event. Rows show zoomed-in views of selected spectral lines typically associated with flare activity: the hydrogen Balmer (Hα), Paschen (Paγ, Paβ), and Brackett (Brγ) series, as well as the He I triplet at 1.083 μm. The red curves represent spectra averaged at the flare peak, and the blue curves show postflare spectra, both normalized to the preflare level.
Paper: Flares on TRAPPIST-1 Reveal the Spectrum of Magnetic Features on Its Surface
Authors: Valeriy Vasilyev, Nadiia Kostogryz, Alexander I. Shapiro, Astrid M. Veronig, Benjamin V. Rackham, Christoph Schirninger, Julien de Wit, Ward Howard, Jeff Valenti, Adina D. Feinstein, Olivia Lim, Sara Seager, Laurent Gizon, Sami K. Solanki
Figure caption: Temperature estimates of the vanishing dark features. Each panel shows the flux difference between post- and preflare spectra, interpreted as the spectral energy distribution of the vanished active region (binned over 40 points; bold markers). The black dashed line shows the Planck function that best fits this spectrum, used to estimate the temperature of the vanished region. The temperature and its 1σ uncertainty are indicated in the legend.
Paper: FRB 20250316A: A Brilliant and Nearby One-off Fast Radio Burst Localized to 13 pc Precision
Authors: Thomas C. Abbott, Daniel Amouyal, Bridget C. Andersen, Shion E. Andrew, Kevin Bandura, Mohit Bhardwaj, Kalyani Bhopi, Yash Bhusare, Charanjot Brar, Alice Cai, Tomas Cassanelli, Shami Chatterjee, Jean-François Cliche, Amanda M. Cook, Alice P. Curtin, Evan Davies-Velie, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Nina Gusinskaia, Jason W. T. Hessels, Danté M. Hewitt, Jeff Huang, Naman Jain, Ronniy. C. Joseph, Lordrick Kahinga, Victoria M. Kaspi, Afrasiyab (Afrokk) Khan, Bikash Kharel, Adam E. Lanman, Magnus L'Argent, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Kyle McGregor, Ryan Mckinven, Juan Mena-Parra, Daniele Michilli, Nicole Mulyk, Mason Ng, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Scott M. Ransom, Gurman Sachdeva, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, David C. Stenning, Haochen Wang, Thomas Boles, Ismaël Cognard, Tammo Jan Dijkema, Alexei V. Filippenko, Marcin P. Gawroński, Wolfgang Herrmann, Charles D. Kilpatrick, Franz Kirsten, Shawn Knabel, Omar S. Ould-Boukattine, Hadrien Paugnat, Weronika Puchalska, William Sheu, Aswin Suresh, Aaron Tohuvavohu, Tommaso Treu, WeiKang Zheng
Figure caption: KCWI narrowband images of the burst location. The top panels show [O II] 3726, 3729 Å and Hα images extracted from the coadded cubes of the blue and red arms of KCWI, respectively. The solid black ellipse shows the 2σ localization region of the FRB, placing its center at 190 pc projected separation (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩9 angular offset) from the emission peak of the nearby star-forming region, which is marked by the dashed blue ellipse. The middle panel shows the combined blue and red side 1D spectrum of the star-forming clump extracted within the dashed ellipse. The bottom panel shows the spectrum extracted from the FRB localization ellipse. The gap in the spectra between 5500 and 5600 Å masks out the region where the dichroic splits the blue and red light. Both spectra show narrow nebular emission features, and we do not see any transient features at the location of the FRB.
Paper: FRB 20250316A: A Brilliant and Nearby One-off Fast Radio Burst Localized to 13 pc Precision
Authors: Thomas C. Abbott, Daniel Amouyal, Bridget C. Andersen, Shion E. Andrew, Kevin Bandura, Mohit Bhardwaj, Kalyani Bhopi, Yash Bhusare, Charanjot Brar, Alice Cai, Tomas Cassanelli, Shami Chatterjee, Jean-François Cliche, Amanda M. Cook, Alice P. Curtin, Evan Davies-Velie, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Nina Gusinskaia, Jason W. T. Hessels, Danté M. Hewitt, Jeff Huang, Naman Jain, Ronniy. C. Joseph, Lordrick Kahinga, Victoria M. Kaspi, Afrasiyab (Afrokk) Khan, Bikash Kharel, Adam E. Lanman, Magnus L'Argent, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Kyle McGregor, Ryan Mckinven, Juan Mena-Parra, Daniele Michilli, Nicole Mulyk, Mason Ng, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Scott M. Ransom, Gurman Sachdeva, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, David C. Stenning, Haochen Wang, Thomas Boles, Ismaël Cognard, Tammo Jan Dijkema, Alexei V. Filippenko, Marcin P. Gawroński, Wolfgang Herrmann, Charles D. Kilpatrick, Franz Kirsten, Shawn Knabel, Omar S. Ould-Boukattine, Hadrien Paugnat, Weronika Puchalska, William Sheu, Aswin Suresh, Aaron Tohuvavohu, Tommaso Treu, WeiKang Zheng
Figure caption: Left: linearly scaled MMT r-band image showing part of the host galaxy, NGC 4141, of FRB 20250316A with the CHIME Outrigger VLBI localization overlaid in red; the ellipse incorporates both positional and absolute astrometric tie uncertainties. The 3σ limiting magnitude of the image is r ≳ 25.6 mag (AB, corrected for Galactic extinction). The image is oriented north up and east left. Right: image zoomed in at the Outrigger position, 8″ × 8″, and additionally showing the 1σ, 2σ, and 3σ localization ellipses of FRB 20250316A.
Paper: FRB 20250316A: A Brilliant and Nearby One-off Fast Radio Burst Localized to 13 pc Precision
Authors: Thomas C. Abbott, Daniel Amouyal, Bridget C. Andersen, Shion E. Andrew, Kevin Bandura, Mohit Bhardwaj, Kalyani Bhopi, Yash Bhusare, Charanjot Brar, Alice Cai, Tomas Cassanelli, Shami Chatterjee, Jean-François Cliche, Amanda M. Cook, Alice P. Curtin, Evan Davies-Velie, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Nina Gusinskaia, Jason W. T. Hessels, Danté M. Hewitt, Jeff Huang, Naman Jain, Ronniy. C. Joseph, Lordrick Kahinga, Victoria M. Kaspi, Afrasiyab (Afrokk) Khan, Bikash Kharel, Adam E. Lanman, Magnus L'Argent, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Kyle McGregor, Ryan Mckinven, Juan Mena-Parra, Daniele Michilli, Nicole Mulyk, Mason Ng, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Scott M. Ransom, Gurman Sachdeva, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, David C. Stenning, Haochen Wang, Thomas Boles, Ismaël Cognard, Tammo Jan Dijkema, Alexei V. Filippenko, Marcin P. Gawroński, Wolfgang Herrmann, Charles D. Kilpatrick, Franz Kirsten, Shawn Knabel, Omar S. Ould-Boukattine, Hadrien Paugnat, Weronika Puchalska, William Sheu, Aswin Suresh, Aaron Tohuvavohu, Tommaso Treu, WeiKang Zheng
Figure caption: Bottom: total intensity waterfall dedispersed to the structure-optimized DM of 161.82 ± 0.02 pc cm−3 and temporal profiles of Stokes I (black line), ﹩L=\sqrt{{Q}^{2}+{U}^{2}}﹩ (red line), V (blue line), linear polarization fraction (L/I; red circles), circular polarization fraction (∣V∣/I; blue circles), and PA (black circles). Channels masked out due to RFI are highlighted by red streaks on the left-hand side of the total intensity waterfall. The preceding and subsequent parabolic sweeps are artifacts due to “spectral ghosts” related to the instrumental signal chain. Top: all points plotted on the L/I, ∣V∣/I, and PA profiles exceed a linearly polarized S/N of 5.
Paper: FRB 20250316A: A Brilliant and Nearby One-off Fast Radio Burst Localized to 13 pc Precision
Authors: Thomas C. Abbott, Daniel Amouyal, Bridget C. Andersen, Shion E. Andrew, Kevin Bandura, Mohit Bhardwaj, Kalyani Bhopi, Yash Bhusare, Charanjot Brar, Alice Cai, Tomas Cassanelli, Shami Chatterjee, Jean-François Cliche, Amanda M. Cook, Alice P. Curtin, Evan Davies-Velie, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Nina Gusinskaia, Jason W. T. Hessels, Danté M. Hewitt, Jeff Huang, Naman Jain, Ronniy. C. Joseph, Lordrick Kahinga, Victoria M. Kaspi, Afrasiyab (Afrokk) Khan, Bikash Kharel, Adam E. Lanman, Magnus L'Argent, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Kyle McGregor, Ryan Mckinven, Juan Mena-Parra, Daniele Michilli, Nicole Mulyk, Mason Ng, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ue-Li Pen, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Scott M. Ransom, Gurman Sachdeva, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, David C. Stenning, Haochen Wang, Thomas Boles, Ismaël Cognard, Tammo Jan Dijkema, Alexei V. Filippenko, Marcin P. Gawroński, Wolfgang Herrmann, Charles D. Kilpatrick, Franz Kirsten, Shawn Knabel, Omar S. Ould-Boukattine, Hadrien Paugnat, Weronika Puchalska, William Sheu, Aswin Suresh, Aaron Tohuvavohu, Tommaso Treu, WeiKang Zheng
Figure caption: PA profile of FRB 20250316A as a function of frequency over 400–800 MHz. The y-axis scale is arbitrary, and a red marker is used to indicate PA variation on a 30° scale. The central frequencies of some frequency subbands are indicated on the left as a guide.