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: Comparison of selected relatively isolated permitted lines, some of which display a clear P-Cygni profile, in SN 2024pxl at +37 days (teal) and SN 2024vjm (pink) at +12 days. The features that are confidently associated with the label are given in full opacity. Regions that may be contaminated by other lines are shown in low opacity. The spectra have not been scaled or offset.
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: Evolution of Mg, Ni, and Co forbidden emission line profiles of SN 2024pxl at +11, +21, +37, and +42 days. For lines at wavelengths >5 μm, spectra from the different epochs are offset for clearer comparison.
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: Qualitative schematic showing that the O I line morphology in SN 2024pxl may reflect predictions from M. Fink et al. (2014) of weak one-sided deflagrations. The base O I emission (yellow, dotted lines) likely arises from the inner O-rich region (<5000 km s−1). The unburned channel (magenta, dashed lines) results from incomplete burning, and may correspond to the off-center narrow peak of the O I emission. Right panel adapted from the N20def 16O of Figure 9 from M. Fink et al. (2014).
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: Photospheric NIR Co II velocity and width measurements for the absorption component of the P-Cygni profile and their evolution. The dotted line represents an outer velocity edge of the ejecta where vouter ≈ vphot  +  FWHMphot.
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: N1def model spectrum at 50 day post explosion (black) compared with SN 2024pxl at +37 days, corresponding to 50 day post explosion (gray). The SN 2024pxl spectrum has been offset for clarity, and the flux is displayed using an arcsinh scaling to show details of weaker lines. Contributions from each ion to spectral features are shaded by color.
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 the MIR spectra of normal SN Ia 2021aefx (L. A. Kwok et al. 2023), 91bg-like SN Ia 2022xkq (J. M. DerKacy et al. 2024), and the SN Iax 2024pxl and 2024vjm. Notably, the SN Iax IME profiles are centrally peaked indicating well-mixed ejecta, whereas SN 2021aefx and SN 2022xkq IME profiles (particularly [Ar II] 6.89 μm, and [Ar III] 8.99 μm) are flat topped indicating stratified ejecta.
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: Evolution of the ratios between the flux density Fν at peak of the most prominent MIR Ni and Co lines in SN 2024pxl. The continuum was subtracted before measuring the value of the peaks.
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: Light curves from a source at 100 Mpc corresponding to the radio, optical, infrared, X-ray, and gamma-ray bands for the fiducial case. The characteristic spin-down (tsd), nebular diffusion (﹩{t}_{{\rm{diff}},{\rm{0}}}^{{\rm{neb}}}﹩), and ejecta diffusion (﹩{t}_{{\rm{diff}},{\rm{0}}}^{{\rm{ej}}}﹩) timescales are also shown. The representative frequencies (for radio), wavelengths (for optical and infrared), and energies (for X-ray and γ-rays) are motivated by relevant bands from observational telescopes shown in Table 1 and Figures 3 and 5. In the plots, Fν denotes spectral flux density; Lν is the spectral luminosity; the apparent and absolute magnitudes are shown by mAB and MAB, respectively; and νLν is the differential luminosity. Note that t is the time elapsed from the instance 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: Attenuation coefficients at different time snaps for γγ, SSA, and ejecta attenuations denoted by fγγ, fSSA, and fej, respectively. The plots are shown for radio, X-ray/MeV, and high-energy (HE) and very high energy (VHE) gamma rays for the fiducial case. The value of f = 1 corresponds to τ = 0.
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: Observed EM spectra from a source at 100 Mpc corresponding to the radio, X-ray, MeV, and gamma-ray bands for the fiducial case at different time snapshots. The sensitivity curves for the relevant detectors in the given EM bands are also shown (see Table 1). In the plots, Fν denotes spectral flux density, Lν is the spectral luminosity, and νLν is the differential luminosity. Note that the radio spectra (top panel) show flux density while the middle and bottom panels show flux.
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: SN 2024pxl at +11 days (23 day post explosion; indigo), +21 days (33 day post explosion; light blue), and +37 days (50 day post explosion; teal) compared to the N1def model at 23, 33, and 50 day post explosion (gray, light gray, and lightest gray, respectively). Adding illustrative modified ∼4000 K blackbodies to the model spectra (black, dark gray, and gray, respectively) improves the match of the continuum flux, potentially indicating needed effects from time-dependent models or additional energy input from a remnant. The modified blackbodies are added postradiative transfer and are therefore not physically accurate. The flux is displayed using an arcsinh scaling to show details of weaker lines. Models are scaled to a distance of 23 Mpc (M. Singh et al. 2025).
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: Photon energy density spectrum (νuν) of the nonthermal (solid) and thermal (dashed) photons in the nebula (comoving frame) after γγ and SSA attenuations, at different times for the fiducial case. The corresponding synchrotron (Synch.) and IC components are shown with thin dashed–dotted and dotted lines, 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: SN 2024vjm at +12 days (∼20 day post explosion; pink) compared to the N5def_hybrid C/O/Ne WD model (gray) and the N5def_hybrid C/O/Ne WD model + an illustrative 4500 K blackbody (black) at 20 day post explosion. The additional blackbody improves the match to the NIR + MIR continuum flux, but is added postradiative transfer and is therefore not physically accurate. The model overpredicts the optical flux at <1 μm. The model has been scaled to a distance of 7 Mpc.
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 the MRS spectrum of SN 2024pxl at +37 days (gray), the LRS spectrum at +42 days (black), and the LRS spectrum with our wavelength correction applied (red).