adsabs/AstroCLIMB huggingface dataset:
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: Best-fit SED models from EAzY for the off-center emission. The measured flux densities for solid detections are presented by filled green dots with error bars, while upper limits are marked as green triangles. The spectroscopic redshift for the LRD point source (zLRD) and the redshift of the off-center blob with the highest probability (zblob) are given in each panel. The inset panel shows the probability distribution function [p(z)] of the redshift, with the orange shaded regions representing the original probability derived by EAzY and the cyan shaded regions representing the probability rescaled by the overlapping probability that the off-center blobs correspond to galaxies at redshifts different from the LRD point sources.
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: Dynamical timescale (left vertical axis) and the corresponding baryonic mass accretion rate (right vertical axis) as functions of halo virial mass at z = 6 for a 108 M⊙ gas cloud infalling from 1 kpc. The blue solid (dashed) line represents the result for halo concentration c = 3 (c = 15).
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: Same as Figure 3 but for the nebular models generated with CLOUDY. Redshift as well as best-fit density and metallicity are given in each panel.
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: Same as Figure 1 but for MSA13821.
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: Same as Figure 1 but for MSA45924.
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: Same as Figure 1 but for MSA41225.
Paper: Uniform Reanalysis of JWST MIRI 15 μm Exoplanet Eclipse Observations Using Frame-normalized Principal Component Analysis
Authors: Nicholas J. Connors, Christopher Monaghan, Björn Benneke, Lisa Dang
Figure caption: (Left) Detector-settling time per visit was taken as the time for 99% of the detector-settling component eigenvalue (fit with an exponential) to decay. Three individual visits of planets orbiting high-, medium-, and low-magnitude stars (TRAPPIST-1 b, LHS 1478 b, and HD 260655 b, respectively) are shown as examples of detector-settling fitting. (Right) Best-fit model between detector-settling time and star Ks-band magnitude for all planets with available MIRI 15 μm data. Each data point represents the average settling time across all available visits for that planet, with the error bars taken from the standard deviation of the settling time for all visits (for planets with only a single available visit the error is 0). These data points are generated from the following: four visits of GJ 3473 b; three visits of LHS 1140 c; two visits of LHS 1478 b; four visits of TOI 270 b; five visits of TRAPPIST-1 b; three visits of TRAPPIST-1 c (we discard one of the four available visits as an outlier); one visit of GJ 357 b; two visits of HD 260655 b; two visits of LTT 3780 b; three visits of TOI 1468 b; one visit of TOI 175 c; and one visit of LP 791-18 d. We label these components as representing detector settling due to their exponential shape and strong dependence on photon flux. For TRAPPIST-1 b (top left) the settling time is greater than the duration of the observation, for LHS 1478 b (middle left) the settling time is greater than the midpoint of the observation, and for HD 260655 b (bottom left) the settling time is near immediate. The best fit for the detector-settling time relationship is ﹩{T}_{\mathrm{settling}}=0.063{e}^{0.427{m}_{K}}-0.657﹩ hr.
Paper: Uniform Reanalysis of JWST MIRI 15 μm Exoplanet Eclipse Observations Using Frame-normalized Principal Component Analysis
Authors: Nicholas J. Connors, Christopher Monaghan, Björn Benneke, Lisa Dang
Figure caption: Simulated emission spectra for LHS 1478 b, TOI-1468 b, LHS 1140 c, TRAPPIST-1 b, and TRAPPIST-1 c compared to the measured eclipse depths from our FN-PCA calculation, alongside the previous literature results reported in Table 2 (in addition to the values calculated by E. Ducrot et al. (2025) for TRAPPIST-1 b). The joint fit results are plotted for all planets except for LHS 1478 b, which only plots the measured eclipse depth from the first visit. The Ultramafic Dunite spectra were modeled using the dunite xenolith wavelength-dependent spherical reflectance from K. Paragas et al. (2025).
Paper: Dark Star Clusters or Ultrafaint Dwarf Galaxies? Revisiting UMa3/U1
Authors: Ali Rostami-Shirazi, Hosein Haghi, Akram Hasani Zonoozi, Pavel Kroupa
Figure caption: Evolutionary tracks of five simulated clusters, benchmarked against UMa3/U1. Left: cluster trajectories in the M*–Rh plane. Right: progression of MDyn/L1/2 with stellar mass loss. Dynamical masses are computed from bound stellar sums within Rh; for model M5, an additional estimate using Equation (3) based on the mock-observed velocity dispersion from the UNIONS range is shown as the red dashed line. Statistical smoothing is applied in both panels to reduce snapshot-to-snapshot fluctuations. Faint (solid) segments indicate evolutionary stages before (after) entering the DSC phase.
Paper: Uniform Reanalysis of JWST MIRI 15 μm Exoplanet Eclipse Observations Using Frame-normalized Principal Component Analysis
Authors: Nicholas J. Connors, Christopher Monaghan, Björn Benneke, Lisa Dang
Figure caption: The detector-settling component either decays with a wide eigenimage covering most of the PSF (top) or ramps up with a more narrow eigenimage (bottom). The ramp-up component is less common and can have a lesser effect on the lightcurve depending on the size of the aperture and of the affected portion of the PSF due to it being narrower in general, despite being a stronger signal that explains more of the total variance found by PCA.
Paper: Uniform Reanalysis of JWST MIRI 15 μm Exoplanet Eclipse Observations Using Frame-normalized Principal Component Analysis
Authors: Nicholas J. Connors, Christopher Monaghan, Björn Benneke, Lisa Dang
Figure caption: The number of integrations for the detector to settle as a function of the star’s Ks-band magnitude for all planets with available MIRI 15 μm data. Moreover, 525 ± 203 integrations are required for the detector to settle, which is marked as the red region. TOI175 c appears as a notable outlier; however, this data point is based solely on a single available visit and does not take into account possible flux contributions by the two other planets in its star system (R. Cloutier et al. 2019).
Paper: Uniform Reanalysis of JWST MIRI 15 μm Exoplanet Eclipse Observations Using Frame-normalized Principal Component Analysis
Authors: Nicholas J. Connors, Christopher Monaghan, Björn Benneke, Lisa Dang
Figure caption: The first and fourth principal components of TOI-1468 b visit 1 show the Gaussian centroid moving along two perpendicular axes. The positive diagonal explains 13.9% of the total variance and the negative diagonal explains only 3.6%.
Paper: Uniform Reanalysis of JWST MIRI 15 μm Exoplanet Eclipse Observations Using Frame-normalized Principal Component Analysis
Authors: Nicholas J. Connors, Christopher Monaghan, Björn Benneke, Lisa Dang
Figure caption: Pixel-dominated principal components from visits of TRAPPIST-1 c (left) and TOI-1468 b (right).
Paper: Uniform Reanalysis of JWST MIRI 15 μm Exoplanet Eclipse Observations Using Frame-normalized Principal Component Analysis
Authors: Nicholas J. Connors, Christopher Monaghan, Björn Benneke, Lisa Dang
Figure caption: Random principal components from two visits of TRAPPIST-1 b.
Paper: Dark Star Clusters or Ultrafaint Dwarf Galaxies? Revisiting UMa3/U1
Authors: Ali Rostami-Shirazi, Hosein Haghi, Akram Hasani Zonoozi, Pavel Kroupa
Figure caption: Compilation of Local Group dGs (A. W. McConnachie 2012; version 2021 January), GCs (W. E. Harris 1996; version 2010 December), and faint, ambiguous satellites (W. Cerny et al. 2023c, 2023c; S. E. T. Smith et al. 2024; J. D. Simon et al. 2024) in the Rh–L (left) and MDyn/L1/2–L (right) parameter spaces. Solid lines trace the tidal evolutionary tracks of DSC models (Section 3.2) on circular orbits at RG = 8 kpc (green) and RG = 16 kpc (orange). The gray-shaded region spans the full parameter space swept by the DSC models along their evolutionary tracks. The darker portion marks the period during which the clusters are in the DSC phase (Q* ≥ 1). Dynamical mass is obtained by summing bound stellar plus remnant masses within Rh in both models. Filled symbols indicate observed ambiguous satellites with velocity dispersion measurements.
Paper: Dark Star Clusters or Ultrafaint Dwarf Galaxies? Revisiting UMa3/U1
Authors: Ali Rostami-Shirazi, Hosein Haghi, Akram Hasani Zonoozi, Pavel Kroupa
Figure caption: Time-resolved evolution of the model shown in Figure 3 (orange line), located at RG = 16 kpc. The black curve (left axis) shows the cluster’s luminosity as a function of normalized evolutionary time (t/τDiss), indicating the fraction of its lifetime spent at each luminosity level. The gray curve (right axis) shows the instantaneous mass-loss rate of luminous stars (﹩{\mathop{M}\limits^{\cdot }}_{* }﹩) throughout the cluster’s evolution. The green shaded band highlights the transitional luminosity regime (103 < L/L⊙ < 104), where the cluster evolves rapidly, while the orange band marks the faint regime (L < 103 L⊙), where evolution proceeds more slowly.
Paper: Dark Star Clusters or Ultrafaint Dwarf Galaxies? Revisiting UMa3/U1
Authors: Ali Rostami-Shirazi, Hosein Haghi, Akram Hasani Zonoozi, Pavel Kroupa
Figure caption: Temporal evolution of the M5 model’s stellar content: luminous stars (red), subset within the UNIONS detection limits (green), white dwarfs (blue), and black holes (black). The shaded pink band marks the remaining lifetime of bound luminous stars. The gray curve (right axis) represents the instantaneous escape rate of luminous stars (﹩{\mathop{N}\limits^{\cdot }}_{* }﹩), which drops sharply after 12.5 Gyr as the remaining stars become deeply bound within the BHSub.
Paper: A Flare-related Decimetric Type-IV Radio Burst Induced by the X2 Radiation of Electron Cyclotron Maser Emission
Authors: Maoshui Lv, Ze Zhong, Xiangliang Kong, Hao Ning, Feiyu Yu, Bing Wang, Baolin Tan, Victor Melnikov, Alexey Kuznetsov, Hongqiang Song, Ruisheng Zheng, Yao Chen
Figure caption: Overview of the t-IVdm radio burst observed on 2011 September 24. (a) GOES soft X-ray fluxes of the M7.1-class flare at 1.0–8.0 Å. (b) The dynamic spectra observed from 12:40 to 14:00 UT, combining the data from the San Vito observatory (100–175 MHz), the Bleien observatory (175–870 MHz), and the Ondrejov observatory (870–2000 MHz). Bursts I and II are two components of the t-IVdm event. (c) The temporal profiles of the maximum TB and the degree of polarization (d) with a 10 s cadence at eight NRH frequencies from 228 to 445 MHz. The polarization level is obtained by taking an average over the 85% contours of the maximum TB.
Paper: A Flare-related Decimetric Type-IV Radio Burst Induced by the X2 Radiation of Electron Cyclotron Maser Emission
Authors: Maoshui Lv, Ze Zhong, Xiangliang Kong, Hao Ning, Feiyu Yu, Bing Wang, Baolin Tan, Victor Melnikov, Alexey Kuznetsov, Hongqiang Song, Ruisheng Zheng, Yao Chen
Figure caption: The AR polarization at four NRH frequencies before (a) and after (b) the t-IVdm burst. The box indicates where the radio sources were observed during the burst, and the plus indicates the sunspot location close to the radio sources.
Paper: A Flare-related Decimetric Type-IV Radio Burst Induced by the X2 Radiation of Electron Cyclotron Maser Emission
Authors: Maoshui Lv, Ze Zhong, Xiangliang Kong, Hao Ning, Feiyu Yu, Bing Wang, Baolin Tan, Victor Melnikov, Alexey Kuznetsov, Hongqiang Song, Ruisheng Zheng, Yao Chen
Figure caption: Velocity distribution of energetic electrons at altitudes between 20 and 100 Mm at 2 s (a) and 3 s (b) postinjection, respectively.
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: Line identifications for SN 2024vjm from 1.0 to 20 μm. Permitted transitions are marked by yellow dashed lines, semiforbidden transitions are marked by purple dashed–dotted lines, and forbidden transitions are marked by gray dotted lines. Only the most dominant lines contributing to each feature are labeled. For comparison, SN 2024pxl at +37 days is plotted in light teal.
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: Panchromatic spectra of SN 2024pxl at +11, +21, +37, and +42 day post-﹩{B}_{\max }﹩ compared to SN 2024vjm at +12 day post-﹩{B}_{\max }﹩. Flux density is shown in an arcsinh scaling for display purposes over a large range, and each spectrum is offset for visual clarity. Each is a combination of ground-based optical and NIR spectra with NIR and MIR spectra from JWST at similar phases. Details are given in Table 1.
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: Line identifications for SN 2024pxl from 1.0 to 20 μm. Permitted transitions are marked by yellow dashed lines, semiforbidden transitions are marked by purple dashed–dotted lines, and forbidden transitions are marked by gray dotted lines. Only the most dominant lines contributing to each feature are labeled.
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: Left: FWHM vs. kinematic offset, voff, of MIR forbidden emission lines of SN 2024pxl at +42 days and SN 2024vjm at +12 days. Heavy crosses represent the uncertainty-weighted average of all lines, and shaded regions represent the standard deviation. Middle: evolution of the bulk motion in SN 2024pxl (teal), which remains constant, and the Ar lines, which show an ionization offset. Right: forbidden-line profiles of [Ar II] (medium gray, thick line width), [Ni II] (light gray), and [Ne II] (black, thin line width) with color panels showing the average FWHM and standard deviation. The lines have similar profile shapes and widths, indicating the ejecta are well mixed.
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: Comparison of selected relatively isolated forbidden emission lines in SN 2024pxl at +37 days (teal) and SN 2024vjm (pink) at +12 days. The low opacity lines show the unbinned data. The spectra have not been scaled or offset.