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1. Revealing the Progenitor of SN 2021zby through Analysis of the TESS Shock-cooling Light Curve

Author

Qinan Wang, Patrick Armstrong, Yossef Zenati, Ryan Ridden-Harper, Armin Rest, Iair Arcavi, Charles D. Kilpatrick, Ryan J. Foley, Brad E. Tucker, Chris Lidman, Thomas L. Killestein, Melissa Shahbandeh, Joseph P Anderson, Rodrigo Angulo, Chris Ashall, Jamison Burke, Ting-Wan Chen, Sophie von Coelln, Kyle A. Dalrymple, Kyle W. Davis, Michael D. Fulton, Lluís Galbany, Estefania Padilla Gonzalez, Bore Gao, Mariusz Gromadzki, D. Andrew Howell, Nada Ihanec, Jacob E. Jencson, David O. Jones, Joseph D. Lyman, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Matt Nicholl, David O’Neill, Craig Pellegrino, Sofia Rest, Stephen J. Smartt, Ken Smith, Shubham Srivastav, Giacomo Terreran, Samaporn Tinyanont, David R. Young, and Alfredo Zenteno

Subjects
Core-collapse supernovae, Supernovae, Astrophysics, QB460-466
Abstract

We present early observations and analysis of the double-peaked Type IIb supernova (SN IIb) SN 2021zby. TESS captured the prominent early shock-cooling peak of SN 2021zby within the first ∼10 days after explosion with a 30 minute cadence. We present optical and near-infrared spectral series of SN 2021zby, including three spectra during the shock-cooling phase. Using a multiband model fit, we find that the inferred properties of its progenitor are consistent with a red supergiant or yellow supergiant, with an envelope mass of ∼0.30–0.65 M _⊙ and an envelope radius of ∼120–300 R _⊙ . These inferred progenitor properties are similar to those of other SNe IIb with a double-peaked feature, such as SNe 1993J, 2011dh, 2016gkg, and 2017jgh. This study further validates the importance of the high cadence and early coverage in resolving the shape of the shock-cooling light curve, while the multiband observations, particularly UV, are also necessary to fully constrain the progenitor properties.

Published
2023
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2. SN 2022acko: The First Early Far-ultraviolet Spectra of a Type IIP Supernova

Author

K. Azalee Bostroem, Luc Dessart, D. John Hillier, Michael Lundquist, Jennifer E. Andrews, David J. Sand, Yize Dong, Stefano Valenti, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, Vladimir Kouprianov, Jeniveve Pearson, Nicolas E. Meza Retamal, Daniel E. Reichart, Manisha Shrestha, Christopher Ashall, E. Baron, Peter J. Brown, James M. DerKacy, Joseph Farah, Lluís Galbany, J. I. González Hernández, Elizabeth Green, Peter Hoeflich, D. Andrew Howell, Lindsey A. Kwok, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Jeonghee Rho, Micalyn Rowe, Michaela Schwab, Melissa Shahbandeh, Nathan Smith, Jay Strader, Giacomo Terreran, Schuyler D. Van Dyk, and Samuel Wyatt

Subjects
Type II supernovae, Core-collapse supernovae, Ultraviolet astronomy, Ultraviolet transient sources, Astrophysics, QB460-466
Abstract

We present five far- and near-ultraviolet spectra of the Type II plateau supernova, SN 2022acko, obtained 5, 6, 7, 19, and 21 days after explosion, all observed with the Hubble Space Telescope/Space Telescope Imaging Spectrograph. The first three epochs are earlier than any Type II plateau supernova has been observed in the far-ultraviolet revealing unprecedented characteristics. These three spectra are dominated by strong lines, primarily from metals, which contrasts with the featureless early optical spectra. The flux decreases over the initial time series as the ejecta cool and line blanketing takes effect. We model this unique data set with the non–local thermodynamic equilibrium radiation transport code CMFGEN , finding a good match to the explosion of a low-mass red supergiant with energy E _kin = 6 × 10 ^50 erg. With these models we identify, for the first time, the ions that dominate the early ultraviolet spectra. We present optical photometry and spectroscopy, showing that SN 2022acko has a peak absolute magnitude of V = − 15.4 mag and plateau length of ∼115 days. The spectra closely resemble those of SN 2005cs and SN 2012A. Using the combined optical and ultraviolet spectra, we report the fraction of flux as a function of bluest wavelength on days 5, 7, and 19. We create a spectral time-series of Type II supernovae in the ultraviolet, demonstrating the rapid decline of flux over the first few weeks of evolution. Future observations of Type II supernovae are required to map out the landscape of exploding red supergiants, with and without circumstellar material, which is best revealed in high-quality ultraviolet spectra.

Published
2023
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3. Early Spectroscopy and Dense Circumstellar Medium Interaction in SN 2023ixf

Author

K. Azalee Bostroem, Jeniveve Pearson, Manisha Shrestha, David J. Sand, Stefano Valenti, Saurabh W. Jha, Jennifer E. Andrews, Nathan Smith, Giacomo Terreran, Elizabeth Green, Yize Dong, Michael Lundquist, Joshua Haislip, Emily T. Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Vladimir Kouprianov, Emmy Paraskeva, Nicolas E. Meza Retamal, Daniel E. Reichart, Iair Arcavi, Alceste Z. Bonanos, Michael W. Coughlin, Ross Dobson, Joseph Farah, Lluís Galbany, Claudia Gutiérrez, Suzanne Hawley, Leslie Hebb, Daichi Hiramatsu, D. Andrew Howell, Takashi Iijima, Ilya Ilyin, Kiran Jhass, Curtis McCully, Sean Moran, Brett M. Morris, Alessandra C. Mura, Tomás E. Müller-Bravo, James Munday, Megan Newsome, Maria Th. Pabst, Paolo Ochner, Estefania Padilla Gonzalez, Andrea Pastorello, Craig Pellegrino, Lara Piscarreta, Aravind P. Ravi, Andrea Reguitti, Laura Salo, József Vinkó, Kellie de Vos, J. C. Wheeler, G. Grant Williams, and Samuel Wyatt

Subjects
Core-collapse supernovae, Type II supernovae, Circumstellar matter, Stellar mass loss, Red supergiant stars, Astrophysics, QB460-466
Abstract

We present the optical spectroscopic evolution of SN 2023ixf seen in subnight cadence spectra from 1.18 to 15 days after explosion. We identify high-ionization emission features, signatures of interaction with material surrounding the progenitor star, that fade over the first 7 days, with rapid evolution between spectra observed within the same night. We compare the emission lines present and their relative strength to those of other supernovae with early interaction, finding a close match to SN 2020pni and SN 2017ahn in the first spectrum and SN 2014G at later epochs. To physically interpret our observations, we compare them to CMFGEN models with confined, dense circumstellar material around a red supergiant (RSG) progenitor from the literature. We find that very few models reproduce the blended N iii ( λλ 4634.0,4640.6)/C iii ( λλ 4647.5,4650.0) emission lines observed in the first few spectra and their rapid disappearance thereafter, making this a unique diagnostic. From the best models, we find a mass-loss rate of 10 ^−3 –10 ^−2 M _⊙ yr ^−1 , which far exceeds the mass-loss rate for any steady wind, especially for an RSG in the initial mass range of the detected progenitor. These mass-loss rates are, however, similar to rates inferred for other supernovae with early circumstellar interaction. Using the phase when the narrow emission features disappear, we calculate an outer dense radius of circumstellar material R _CSM,out ≈ 5 × 10 ^14 cm, and a mean circumstellar material density of ρ = 5.6 × 10 ^−14 g cm ^−3 . This is consistent with the lower limit on the outer radius of the circumstellar material we calculate from the peak H α emission flux, R _CSM,out ≳ 9 × 10 ^13 cm.

Published
2023
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4. Strong Carbon Features and a Red Early Color in the Underluminous Type Ia SN 2022xkq

Author

Jeniveve Pearson, David J. Sand, Peter Lundqvist, Lluís Galbany, Jennifer E. Andrews, K. Azalee Bostroem, Yize Dong, Emily Hoang, Griffin Hosseinzadeh, Daryl Janzen, Jacob E. Jencson, Michael J. Lundquist, Darshana Mehta, Nicolás Meza Retamal, Manisha Shrestha, Stefano Valenti, Samuel Wyatt, Joseph P. Anderson, Chris Ashall, Katie Auchettl, Eddie Baron, Stéphane Blondin, Christopher R. Burns, Yongzhi Cai, Ting-Wan Chen, Laura Chomiuk, David A. Coulter, Dane Cross, Kyle W. Davis, Thomas de Jaeger, James M. DerKacy, Dhvanil D. Desai, Georgios Dimitriadis, Aaron Do, Joseph R. Farah, Ryan J. Foley, Mariusz Gromadzki, Claudia P. Gutiérrez, Joshua Haislip, Jonay I. González Hernández, Jason T. Hinkle, Willem B. Hoogendam, D. Andrew Howell, Peter Hoeflich, Eric Hsiao, Mark E. Huber, Saurabh W. Jha, Cristina Jiménez Palau, Charles D. Kilpatrick, Vladimir Kouprianov, Sahana Kumar, Lindsey A. Kwok, Conor Larison, Natalie LeBaron, Xavier Le Saux, Jing Lu, Curtis McCully, Tycho Mera Evans, Peter Milne, Maryam Modjaz, Nidia Morrell, Tomás E. Müller-Bravo, Megan Newsome, Matt Nicholl, Estefania Padilla Gonzalez, Anna V. Payne, Craig Pellegrino, Kim Phan, Jonathan Pineda-García, Anthony L. Piro, Lara Piscarreta, Abigail Polin, Daniel E. Reichart, César Rojas-Bravo, Stuart D. Ryder, Irene Salmaso, Michaela Schwab, Melissa Shahbandeh, Benjamin J. Shappee, Matthew R. Siebert, Nathan Smith, Jay Strader, Kirsty Taggart, Giacomo Terreran, Samaporn Tinyanont, M. A. Tucker, Giorgio Valerin, and D. R. Young

Subjects
Supernovae, White dwarf stars, Type Ia supernovae, Astrophysics, QB460-466
Abstract

We present optical, infrared, ultraviolet, and radio observations of SN 2022xkq, an underluminous fast-declining Type Ia supernova (SN Ia) in NGC 1784 ( D ≈ 31 Mpc), from

Published
2023
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5. Corrigendum: Applications and techniques for fast machine learning in science.

Author

Allison McCarn Deiana, Nhan Tran, Joshua Agar, Michaela Blott, Giuseppe Di Guglielmo, Javier M. Duarte, Philip C. Harris, Scott Hauck, Mia Liu, Mark S. Neubauer, Jennifer Ngadiuba, Seda Ogrenci-Memik, Maurizio Pierini, Thea Aarrestad, Steffen Bähr, Jürgen Becker 0001, Anne-Sophie Berthold, Richard J. Bonventre, Tomás E. Müller-Bravo, Markus Diefenthaler, Zhen Dong 0003, Nick Fritzsche, Amir Gholami, Ekaterina Govorkova, Dongning Guo, Kyle J. Hazelwood, Christian Herwig, Babar Khan, Sehoon Kim, Thomas Klijnsma, Yaling Liu, Kin Ho Lo, Tri Nguyen, Gianantonio Pezzullo, Seyedramin Rasoulinezhad, Ryan A. Rivera, Kate Scholberg, Justin Selig, Sougata Sen, Dmitri Strukov, William Tang 0002, Savannah Thais, Kai Lukas Unger, Ricardo Vilalta, Belinavon Krosigk, Shen Wang 0007, and Thomas K. Warburton

Published
2024
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6. SN 2019hcc: a Type II supernova displaying early O ii lines

Author

Eleonora Parrag, Cosimo Inserra, Steve Schulze, Joseph Anderson, Ting-Wan Chen, Giorgios Leloudas, Lluis Galbany, Claudia P Gutiérrez, Daichi Hiramatsu, Erkki Kankare, Tomás E Müller-Bravo, Matt Nicholl, Giuliano Pignata, Regis Cartier, Mariusz Gromadzki, Alexandra Kozyreva, Arne Rau, Jamison Burke, D Andrew Howell, Curtis McCully, and Craig Pellegrino

Published
2021
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7. Applications and Techniques for Fast Machine Learning in Science.

Author

Allison McCarn Deiana, Nhan Tran, Joshua Agar, Michaela Blott, Giuseppe Di Guglielmo, Javier M. Duarte, Philip C. Harris, Scott Hauck, Mia Liu, Mark S. Neubauer, Jennifer Ngadiuba, Seda Ogrenci Memik, Maurizio Pierini, Thea Aarrestad, Steffen Bähr, Jürgen Becker 0001, Anne-Sophie Berthold, Richard J. Bonventre, Tomás E. Müller-Bravo, Markus Diefenthaler, Zhen Dong 0003, Nick Fritzsche, Amir Gholami, Ekaterina Govorkova, Kyle J. Hazelwood, Christian Herwig, Babar Khan, Sehoon Kim, Thomas Klijnsma, Yaling Liu, Kin Ho Lo, Tri Nguyen, Gianantonio Pezzullo, Seyedramin Rasoulinezhad, Ryan A. Rivera, Kate Scholberg, Justin Selig, Sougata Sen, Dmitri Strukov, William Tang 0002, Savannah Thais, Kai Lukas Unger, Ricardo Vilalta, Belinavon Krosigk, Thomas K. Warburton, Maria Acosta Flechas, Anthony Aportela, Thomas Calvet, Leonardo Cristella, Daniel Diaz 0003, Caterina Doglioni, Maria Domenica Galati, Elham E Khoda, Farah Fahim, Davide Giri, Benjamin Hawks, Duc Hoang, Burt Holzman, Shih-Chieh Hsu, Sergo Jindariani, Iris Johnson, Raghav Kansal, Ryan Kastner, Erik Katsavounidis, Jeffrey D. Krupa, Pan Li 0005, Sandeep Madireddy, Ethan Marx, Patrick McCormack, Andres Meza 0001, Jovan Mitrevski, Mohammed Attia Mohammed, Farouk Mokhtar, Eric A. Moreno, Srishti Nagu, Rohin Narayan, Noah Palladino, Zhiqiang Que, Sang Eon Park, Subramanian Ramamoorthy, Dylan S. Rankin, Simon Rothman, Ashish Sharma, Sioni Summers, Pietro Vischia, Jean-Roch Vlimant, and Olivia Weng

Published
2021

9. Applications and Techniques for Fast Machine Learning in Science.

Author

Allison McCarn Deiana, Nhan Tran, Joshua Agar, Michaela Blott, Giuseppe Di Guglielmo, Javier M. Duarte, Philip C. Harris, Scott Hauck, Mia Liu, Mark S. Neubauer, Jennifer Ngadiuba, Seda Ogrenci Memik, Maurizio Pierini, Thea Aarrestad, Steffen Bähr, Jürgen Becker 0001, Anne-Sophie Berthold, Richard J. Bonventre, Tomás E. Müller-Bravo, Markus Diefenthaler, Zhen Dong 0003, Nick Fritzsche, Amir Gholami, Ekaterina Govorkova, Dongning Guo, Kyle J. Hazelwood, Christian Herwig, Babar Khan, Sehoon Kim, Thomas Klijnsma, Yaling Liu, Kin Ho Lo, Tri Nguyen, Gianantonio Pezzullo, Seyedramin Rasoulinezhad, Ryan A. Rivera, Kate Scholberg, Justin Selig, Sougata Sen, Dmitri Strukov, William Tang 0002, Savannah Thais, Kai Lukas Unger, Ricardo Vilalta, Belinavon Krosigk, Shen Wang 0007, and Thomas K. Warburton

Published
2022
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10. SN 2021zny: an early flux excess combined with late-time oxygen emission suggests a double white dwarf merger event

Author

Georgios Dimitriadis, Kate Maguire, Viraj R Karambelkar, Ryan J Lebron, Chang Liu (刘 畅), Alexandra Kozyreva, Adam A Miller, Ryan Ridden-Harper, Joseph P Anderson, Ting-Wan Chen, Michael Coughlin, Massimo Della Valle, Andrew Drake, Lluís Galbany, Mariusz Gromadzki, Steven L Groom, Claudia P Gutiérrez, Nada Ihanec, Cosimo Inserra, Joel Johansson, Tomás E Müller-Bravo, Matt Nicholl, Abigail Polin, Ben Rusholme, Steve Schulze, Jesper Sollerman, Shubham Srivastav, Kirsty Taggart, Qinan Wang, Yi Yang (杨 轶), and David R Young

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a photometric and spectroscopic analysis of the ultra-luminous and slowly evolving 03fg-like Type Ia SN 2021zny. Our observational campaign starts from $\sim5.3$ hours after explosion (making SN 2021zny one of the earliest observed members of its class), with dense multi-wavelength coverage from a variety of ground- and space-based telescopes, and is concluded with a nebular spectrum $\sim10$ months after peak brightness. SN 2021zny displayed several characteristics of its class, such as the peak brightness ($M_{B}=-19.95$ mag), the slow decline ($\Delta m_{15}(B) = 0.62$ mag), the blue early-time colours, the low ejecta velocities and the presence of significant unburned material above the photosphere. However, a flux excess for the first $\sim1.5$ days after explosion is observed in four photometric bands, making SN 2021zny the third 03fg-like event with this distinct behavior, while its $+313$ d spectrum shows prominent [O I] lines, a very unusual characteristic of thermonuclear SNe. The early flux excess can be explained as the outcome of the interaction of the ejecta with $\sim0.04\:\mathrm{M_{\odot}}$ of H/He-poor circumstellar material at a distance of $\sim10^{12}$ cm, while the low ionization state of the late-time spectrum reveals low abundances of stable iron-peak elements. All our observations are in accordance with a progenitor system of two carbon/oxygen white dwarfs that undergo a merger event, with the disrupted white dwarf ejecting carbon-rich circumstellar material prior to the primary white dwarf detonation., Comment: 19 pages, 16 figures, accepted for publication in MNRAS

Published
2023
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11. Luminous Type II Short-Plateau Supernovae 2006Y, 2006ai, and 2016egz: A Transitional Class from Stripped Massive Red Supergiants

Author

Daichi Hiramatsu, D. Andrew Howell, Takashi J. Moriya, Jared A. Goldberg, Griffin Hosseinzadeh, Iair Arcavi, Joseph P. Anderson, Claudia P. Gutiérrez, Jamison Burke, Curtis McCully, Stefano Valenti, Lluís Galbany, Qiliang Fang, Keiichi Maeda, Gastón Folatelli, Eric Y. Hsiao, Nidia I. Morrell, Mark M. Phillips, Maximilian D. Stritzinger, Nicholas B. Suntzeff, Mariusz Gromadzki, Kate Maguire, Tomás E. Müller-Bravo, and David R. Young

Published
2021
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12. Revealing the progenitor of SN 2021zby through analysis of the $TESS$ shock-cooling light curve

Author

Qinan Wang, Patrick Armstrong, Yossef Zenati, Ryan Ridden-Harper, Armin Rest, Iair Arcavi, Charles D. Kilpatrick, Ryan J. Foley, Brad E. Tucker, Chris Lidman, Thomas L. Killestein, Melissa Shahbandeh, Joseph P Anderson, Rodrigo Angulo, Chris Ashall, Jamison Burke, Ting-Wan Chen, Sophie von Coelln, Kyle A. Dalrymple, Kyle W. Davis, Michael D. Fulton, Lluís Galbany, Estefania Padilla Gonzalez, Bore Gao, Mariusz Gromadzki, D. Andrew Howell, Nada Ihanec, Jacob E. Jencson, David O. Jones, Joseph D. Lyman, Curtis McCully, Tomás E. Müller-Bravo, Megan Newsome, Matt Nicholl, David O’Neill, Craig Pellegrino, Sofia Rest, Stephen J. Smartt, Ken Smith, Shubham Srivastav, Giacomo Terreran, Samaporn Tinyanont, David R. Young, and Alfredo Zenteno

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), spectra, iib supernova, FOS: Physical sciences, Astronomy and Astrophysics, mass-loss, 2011dh, Yellow supergiant progenitor, wolf-rayet stars, ia supernova, Space and Planetary Science, emission, spectrograph, early evolution, Astrophysics - High Energy Astrophysical Phenomena, High-Energy Phenomena and Fundamental Physics
Abstract

We present early observations and analysis of the double-peaked Type IIb supernova (SN IIb) 2021zby. $TESS$ captured the prominent early shock cooling peak of SN 2021zby within the first $\sim$10 days after explosion with a 30-minute cadence. We present optical and near-infrared spectral series of SN 2021zby, including three spectra during the shock cooling phase. Using a multi-band model fit, we find that the inferred properties of its progenitor are consistent with a red supergiant or yellow supergiant, with an envelope mass of $\sim$0.3-3.0 M$_\odot$ and an envelope radius of $\sim$50-350$ R_\odot$. These inferred progenitor properties are similar to those of other SNe IIb with double-peak feature, such as SNe 1993J, 2011dh, 2016gkg and 2017jgh. This study further validates the importance of the high cadence and early coverage in resolving the shape of the shock cooling light curve, while the multi-band observations, especially UV, is also necessary to fully constrain the progenitor properties., Comment: 12 pages, 5 figures, 2 tables, submitted to ApJL

Published
2022
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13. The Tidal Disruption Event AT 2018hyz II: Light Curve Modeling of a Partially Disrupted Star

Author

L. Patton, P. K. Blanchard, Tanmoy Laskar, Iair Arcavi, Tomás E. Müller Bravo, Ryan Chornock, Steve Schulze, P. Short, Giacomo Terreran, Edo Berger, Philip S. Cowperthwaite, Tarraneh Eftekhari, Matt Nicholl, Griffin Hosseinzadeh, Kate D. Alexander, Raffaella Margutti, Joseph P. Anderson, Lluís Galbany, Daichi Hiramatsu, Laura J. Herzog, and Sebastian Gomez

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, 01 natural sciences, Spectral line, Redshift, Galaxy, Photometry (optics), Tidal disruption event, Supernova, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Impact parameter, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

AT 2018hyz (=ASASSN-18zj) is a tidal disruption event (TDE) located in the nucleus of a quiescent E+A galaxy at a redshift of $z = 0.04573$, first detected by the All-Sky Automated Survey for Supernovae (ASAS-SN). We present optical+UV photometry of the transient, as well as an X-ray spectrum and radio upper limits. The bolometric light curve of AT 2018hyz is comparable to other known TDEs and declines at a rate consistent with a $t^{-5/3}$ at early times, emitting a total radiated energy of $E = 9\times10^{50}$ erg. An excess bump appears in the UV light curve about 50 days after bolometric peak, followed by a flattening beyond 250 days. The light curve shows an excess bump in the UV about 50 days after bolometric peak lasting for at least 100 days, which may be related to an outflow. We detect a constant X-ray source present for at least 86 days. The X-ray spectrum shows a total unabsorbed flux of $\sim 4\times10^{-14}$ erg cm$^{-2}$ s$^{-1}$ and is best fit by a blackbody plus power-law model with a photon index of $\Gamma = 0.8$. A thermal X-ray model is unable to account for photons $> 1$ keV, while the radio non-detection favors inverse-Compton scattering rather than a jet for the non-thermal component. We model the optical and UV light curves using the Modular Open-Source Fitter for Transients (MOSFiT) and find a best fit for a black hole of $5.2\times10^6$ M$_\odot$ partially disrupting a $0.1$ M$_\odot$ star (stripping a mass of $\sim 0.01$ M$_\odot$ for the inferred impact parameter, $\beta=0.6$). The low optical depth implied by the small debris mass may explain how we are able to see hydrogen emission with disk-like line profiles in the spectra of AT 2018hyz (see our companion paper, Short et al.~2020)., Comment: 10 pages, 10 figures, published in MNRAS

Published
2020
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14. Weak Mass Loss from the Red Supergiant Progenitor of the Type II SN 2021yja

Author

Griffin Hosseinzadeh, Charles D. Kilpatrick, Yize Dong, David J. Sand, Jennifer E. Andrews, K. Azalee Bostroem, Daryl Janzen, Jacob E. Jencson, Michael Lundquist, Nicolas E. Meza Retamal, Jeniveve Pearson, Stefano Valenti, Samuel Wyatt, Jamison Burke, Daichi Hiramatsu, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran, Katie Auchettl, Kyle W. Davis, Ryan J. Foley, Hao-Yu Miao, Yen-Chen Pan, Armin Rest, Matthew R. Siebert, Kirsty Taggart, Brad E. Tucker, Feng Lin Cyrus Leung, Jonathan J. Swift, Grace Yang, Joseph P. Anderson, Chris Ashall, Stefano Benetti, Peter J. Brown, Régis Cartier, Ting-Wan Chen, Massimo Della Valle, Lluís Galbany, Sebastian Gomez, Mariusz Gromadzki, Joshua Haislip, Eric Y. Hsiao, Cosimo Inserra, Saurabh W. Jha, Thomas L. Killestein, Vladimir Kouprianov, Alexandra Kozyreva, Tomás E. Müller-Bravo, Matt Nicholl, Emmy Paraskeva, Daniel E. Reichart, Stuart Ryder, Melissa Shahbandeh, Ben Shappee, Nathan Smith, and David R. Young

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High-Energy Phenomena and Fundamental Physics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We present high-cadence optical, ultraviolet (UV), and near-infrared data of the nearby ($D\approx23$ Mpc) Type II supernova (SN) 2021yja. Many Type II SNe show signs of interaction with circumstellar material (CSM) during the first few days after explosion, implying that their red supergiant (RSG) progenitors experience episodic or eruptive mass loss. However, because it is difficult to discover SNe early, the diversity of CSM configurations in RSGs has not been fully mapped. SN 2021yja, first detected within ${\approx}5.4$ hours of explosion, shows some signatures of CSM interaction (high UV luminosity, radio and x-ray emission) but without the narrow emission lines or early light curve peak that can accompany CSM. Here we analyze the densely sampled early light curve and spectral series of this nearby SN to infer the properties of its progenitor and CSM. We find that the most likely progenitor was an RSG with an extended envelope, encompassed by low-density CSM. We also present archival Hubble Space Telescope imaging of the host galaxy of SN 2021yja, which allows us to place a stringent upper limit of ${\lesssim}9\ M_\odot$ on the progenitor mass. However, this is in tension with some aspects of the SN evolution, which point to a more massive progenitor. Our analysis highlights the need to consider progenitor structure when making inferences about CSM properties, and that a comprehensive view of CSM tracers should be made to give a fuller view of the last years of RSG evolution., Comment: updated to match accepted version

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15. Corrigendum: Applications and techniques for fast machine learning in science

Author

Allison McCarn Deiana, Nhan Tran, Joshua Agar, Michaela Blott, Giuseppe Di Guglielmo, Javier Duarte, Philip Harris, Scott Hauck, Mia Liu, Mark S. Neubauer, Jennifer Ngadiuba, Seda Ogrenci-Memik, Maurizio Pierini, Thea Aarrestad, Steffen Bähr, Jürgen Becker, Anne-Sophie Berthold, Richard J. Bonventre, Tomás E. Müller Bravo, Markus Diefenthaler, Zhen Dong, Nick Fritzsche, Amir Gholami, Ekaterina Govorkova, Dongning Guo, Kyle J. Hazelwood, Christian Herwig, Babar Khan, Sehoon Kim, Thomas Klijnsma, Yaling Liu, Kin Ho Lo, Tri Nguyen, Gianantonio Pezzullo, Seyedramin Rasoulinezhad, Ryan A. Rivera, Kate Scholberg, Justin Selig, Sougata Sen, Dmitri Strukov, William Tang, Savannah Thais, Kai Lukas Unger, Ricardo Vilalta, Belina von Krosigk, Shen Wang, and Thomas K. Warburton

Subjects
machine learning for science, big data, particle physics, codesign, coprocessors, heterogeneous computing, Information technology, T58.5-58.64
Published
2023
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