SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material

Ido Irani; Ping Chen; Jonathan Morag; Steve Schulze; Avishay Gal-Yam; Nora L. Strotjohann; Ofer Yaron; Erez A. Zimmerman; Amir Sharon; Daniel A. Perley; J. Sollerman; Aaron Tohuvavohu; Kaustav K. Das; Mansi M. Kasliwal; Rachel Bruch; Thomas G. Brink; Wei Kang Zheng; Alexei V. Filippenko; Kishore C. Patra; Sergiy S. Vasylyev; Yi Yang; Matthew J. Graham; Joshua S. Bloom; Paolo Mazzali; Josiah Purdum; Russ R. Laher; Avery Wold; Yashvi Sharma; Leander Lacroix; Michael S. Medford

doi:10.3847/1538-4357/ad04d7

SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material

Ido Irani^*, Ping Chen, Jonathan Morag, Steve Schulze, Avishay Gal-Yam, Nora L. Strotjohann, Ofer Yaron, Erez A. Zimmerman, Amir Sharon, Daniel A. Perley, J. Sollerman, Aaron Tohuvavohu, Kaustav K. Das, Mansi M. Kasliwal, Rachel Bruch, Thomas G. Brink, Wei Kang Zheng, Alexei V. Filippenko, Kishore C. Patra, Sergiy S. VasylyevYi Yang, Matthew J. Graham, Joshua S. Bloom, Paolo Mazzali, Josiah Purdum, Russ R. Laher, Avery Wold, Yashvi Sharma, Leander Lacroix, Michael S. Medford

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

1 Citation (Scopus)

Abstract

We present the discovery and analysis of SN 2022oqm, a Type Ic supernova (SN) detected <1 day after the explosion. The SN rises to a blue and short-lived (2 days) initial peak. Early-time spectral observations of SN 2022oqm show a hot (40,000 K) continuum with high ionization C and O absorption features at velocities of 4000 km s⁻¹, while its photospheric radius expands at 20,000 km s⁻¹, indicating a pre-existing distribution of expanding C/O material. After ∼2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of ∼10,000 km s⁻¹, in agreement with the evolution of the photospheric radius. The optical light curves reach a second peak at t ≈ 15 days. By t = 60 days, the spectrum of SN 2022oqm becomes nearly nebular, displaying strong Ca ii and [Ca ii] emission with no detectable [O i], marking this event as Ca-rich. The early behavior can be explained by 10⁻³ M _⊙ of optically thin circumstellar material (CSM) surrounding either (1) a massive compact progenitor such as a Wolf-Rayet star, (2) a massive stripped progenitor with an extended envelope, or (3) a binary system with a white dwarf. We propose that the early-time light curve is powered by both the interaction of the ejecta with the optically thin CSM and shock cooling (in the massive star scenario). The observations can be explained by CSM that is optically thick to X-ray photons, is optically thick in the lines as seen in the spectra, and is optically thin to visible-light continuum photons that come either from downscattered X-rays or from the shock-heated ejecta. Calculations show that this scenario is self-consistent.

Original language	English
Article number	109
Number of pages	29
Journal	Astrophysical Journal
Volume	962
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/ad04d7
Publication status	Published - 1 Feb 2024

Bibliographical note

A.G-Y.'s research is supported by the EU via ERC grant 725161, the ISF GW excellence center, an IMOS space infrastructure grant and BSF/Transformative and GIF grants, as well as the André Deloro Institute for Advanced Research in Space and Optics, The Helen Kimmel Center for Planetary Science, the Schwartz/Reisman Collaborative Science Program and the Norman E Alexander Family Foundation ULTRASAT Data Center Fund, Minerva and Yeda-Sela; A.G.-Y. is the incumbent of the Arlyn Imberman Professorial Chair. S. Schulze acknowledges support from the G.R.E.A.T research environment, funded by Vetenskapsrådet, the Swedish Research Council, project 2016-06012. N.L.S. is funded by the Deutsche Forschungsgemeinschaft (DFG; German Research Foundation) via the Walter Benjamin program—461903330. A.V.F.'s SN group at UC Berkeley has been supported by Steven Nelson, Landon Noll, Sunil Nagaraj, Sandy Otellini, Gary and Cynthia Bengier, Clark and Sharon Winslow, Sanford Robertson, the Christopher R. Redlich Fund, the Miller Institute for Basic Research in Science (in which A.V.F. was a Miller Senior Fellow), and numerous individual donors.

Publisher Copyright:
© 2024. The Author(s). Published by the American Astronomical Society.

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/ad04d7

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Irani, I., Chen, P., Morag, J., Schulze, S., Gal-Yam, A., Strotjohann, N. L., Yaron, O., Zimmerman, E. A., Sharon, A., Perley, D. A., Sollerman, J., Tohuvavohu, A., Das, K. K., Kasliwal, M. M., Bruch, R., Brink, T. G., Zheng, W. K., Filippenko, A. V., Patra, K. C., ... Medford, M. S. (2024). SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material. Astrophysical Journal, 962(2), Article 109. https://doi.org/10.3847/1538-4357/ad04d7

@article{90bc7bf20a364fafa966ded2652c67b1,

title = "SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material",

abstract = "We present the discovery and analysis of SN 2022oqm, a Type Ic supernova (SN) detected <1 day after the explosion. The SN rises to a blue and short-lived (2 days) initial peak. Early-time spectral observations of SN 2022oqm show a hot (40,000 K) continuum with high ionization C and O absorption features at velocities of 4000 km s−1, while its photospheric radius expands at 20,000 km s−1, indicating a pre-existing distribution of expanding C/O material. After ∼2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of ∼10,000 km s−1, in agreement with the evolution of the photospheric radius. The optical light curves reach a second peak at t ≈ 15 days. By t = 60 days, the spectrum of SN 2022oqm becomes nearly nebular, displaying strong Ca ii and [Ca ii] emission with no detectable [O i], marking this event as Ca-rich. The early behavior can be explained by 10−3 M ⊙ of optically thin circumstellar material (CSM) surrounding either (1) a massive compact progenitor such as a Wolf-Rayet star, (2) a massive stripped progenitor with an extended envelope, or (3) a binary system with a white dwarf. We propose that the early-time light curve is powered by both the interaction of the ejecta with the optically thin CSM and shock cooling (in the massive star scenario). The observations can be explained by CSM that is optically thick to X-ray photons, is optically thick in the lines as seen in the spectra, and is optically thin to visible-light continuum photons that come either from downscattered X-rays or from the shock-heated ejecta. Calculations show that this scenario is self-consistent.",

author = "Ido Irani and Ping Chen and Jonathan Morag and Steve Schulze and Avishay Gal-Yam and Strotjohann, {Nora L.} and Ofer Yaron and Zimmerman, {Erez A.} and Amir Sharon and Perley, {Daniel A.} and J. Sollerman and Aaron Tohuvavohu and Das, {Kaustav K.} and Kasliwal, {Mansi M.} and Rachel Bruch and Brink, {Thomas G.} and Zheng, {Wei Kang} and Filippenko, {Alexei V.} and Patra, {Kishore C.} and Vasylyev, {Sergiy S.} and Yi Yang and Graham, {Matthew J.} and Bloom, {Joshua S.} and Paolo Mazzali and Josiah Purdum and Laher, {Russ R.} and Avery Wold and Yashvi Sharma and Leander Lacroix and Medford, {Michael S.}",

note = "A.G-Y.'s research is supported by the EU via ERC grant 725161, the ISF GW excellence center, an IMOS space infrastructure grant and BSF/Transformative and GIF grants, as well as the Andr{\'e} Deloro Institute for Advanced Research in Space and Optics, The Helen Kimmel Center for Planetary Science, the Schwartz/Reisman Collaborative Science Program and the Norman E Alexander Family Foundation ULTRASAT Data Center Fund, Minerva and Yeda-Sela; A.G.-Y. is the incumbent of the Arlyn Imberman Professorial Chair. S. Schulze acknowledges support from the G.R.E.A.T research environment, funded by Vetenskapsr{\aa}det, the Swedish Research Council, project 2016-06012. N.L.S. is funded by the Deutsche Forschungsgemeinschaft (DFG; German Research Foundation) via the Walter Benjamin program—461903330. A.V.F.'s SN group at UC Berkeley has been supported by Steven Nelson, Landon Noll, Sunil Nagaraj, Sandy Otellini, Gary and Cynthia Bengier, Clark and Sharon Winslow, Sanford Robertson, the Christopher R. Redlich Fund, the Miller Institute for Basic Research in Science (in which A.V.F. was a Miller Senior Fellow), and numerous individual donors. Publisher Copyright: {\textcopyright} 2024. The Author(s). Published by the American Astronomical Society.",

year = "2024",

month = feb,

day = "1",

doi = "10.3847/1538-4357/ad04d7",

language = "English",

volume = "962",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "Institute of Physics Publishing",

number = "2",

}

Irani, I , Chen, P, Morag, J, Schulze, S, Gal-Yam, A, Strotjohann, NL, Yaron, O, Zimmerman, EA, Sharon, A, Perley, DA, Sollerman, J, Tohuvavohu, A, Das, KK, Kasliwal, MM, Bruch, R, Brink, TG, Zheng, WK, Filippenko, AV, Patra, KC, Vasylyev, SS, Yang, Y, Graham, MJ, Bloom, JS, Mazzali, P, Purdum, J, Laher, RR, Wold, A, Sharma, Y, Lacroix, L & Medford, MS 2024, 'SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material', Astrophysical Journal, vol. 962, no. 2, 109. https://doi.org/10.3847/1538-4357/ad04d7

TY - JOUR

T1 - SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material

AU - Irani, Ido

AU - Chen, Ping

AU - Morag, Jonathan

AU - Schulze, Steve

AU - Gal-Yam, Avishay

AU - Strotjohann, Nora L.

AU - Yaron, Ofer

AU - Zimmerman, Erez A.

AU - Sharon, Amir

AU - Perley, Daniel A.

AU - Sollerman, J.

AU - Tohuvavohu, Aaron

AU - Das, Kaustav K.

AU - Kasliwal, Mansi M.

AU - Bruch, Rachel

AU - Brink, Thomas G.

AU - Zheng, Wei Kang

AU - Filippenko, Alexei V.

AU - Patra, Kishore C.

AU - Vasylyev, Sergiy S.

AU - Yang, Yi

AU - Graham, Matthew J.

AU - Bloom, Joshua S.

AU - Mazzali, Paolo

AU - Purdum, Josiah

AU - Laher, Russ R.

AU - Wold, Avery

AU - Sharma, Yashvi

AU - Lacroix, Leander

AU - Medford, Michael S.

N1 - A.G-Y.'s research is supported by the EU via ERC grant 725161, the ISF GW excellence center, an IMOS space infrastructure grant and BSF/Transformative and GIF grants, as well as the André Deloro Institute for Advanced Research in Space and Optics, The Helen Kimmel Center for Planetary Science, the Schwartz/Reisman Collaborative Science Program and the Norman E Alexander Family Foundation ULTRASAT Data Center Fund, Minerva and Yeda-Sela; A.G.-Y. is the incumbent of the Arlyn Imberman Professorial Chair. S. Schulze acknowledges support from the G.R.E.A.T research environment, funded by Vetenskapsrådet, the Swedish Research Council, project 2016-06012. N.L.S. is funded by the Deutsche Forschungsgemeinschaft (DFG; German Research Foundation) via the Walter Benjamin program—461903330. A.V.F.'s SN group at UC Berkeley has been supported by Steven Nelson, Landon Noll, Sunil Nagaraj, Sandy Otellini, Gary and Cynthia Bengier, Clark and Sharon Winslow, Sanford Robertson, the Christopher R. Redlich Fund, the Miller Institute for Basic Research in Science (in which A.V.F. was a Miller Senior Fellow), and numerous individual donors. Publisher Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

PY - 2024/2/1

Y1 - 2024/2/1

N2 - We present the discovery and analysis of SN 2022oqm, a Type Ic supernova (SN) detected <1 day after the explosion. The SN rises to a blue and short-lived (2 days) initial peak. Early-time spectral observations of SN 2022oqm show a hot (40,000 K) continuum with high ionization C and O absorption features at velocities of 4000 km s−1, while its photospheric radius expands at 20,000 km s−1, indicating a pre-existing distribution of expanding C/O material. After ∼2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of ∼10,000 km s−1, in agreement with the evolution of the photospheric radius. The optical light curves reach a second peak at t ≈ 15 days. By t = 60 days, the spectrum of SN 2022oqm becomes nearly nebular, displaying strong Ca ii and [Ca ii] emission with no detectable [O i], marking this event as Ca-rich. The early behavior can be explained by 10−3 M ⊙ of optically thin circumstellar material (CSM) surrounding either (1) a massive compact progenitor such as a Wolf-Rayet star, (2) a massive stripped progenitor with an extended envelope, or (3) a binary system with a white dwarf. We propose that the early-time light curve is powered by both the interaction of the ejecta with the optically thin CSM and shock cooling (in the massive star scenario). The observations can be explained by CSM that is optically thick to X-ray photons, is optically thick in the lines as seen in the spectra, and is optically thin to visible-light continuum photons that come either from downscattered X-rays or from the shock-heated ejecta. Calculations show that this scenario is self-consistent.

AB - We present the discovery and analysis of SN 2022oqm, a Type Ic supernova (SN) detected <1 day after the explosion. The SN rises to a blue and short-lived (2 days) initial peak. Early-time spectral observations of SN 2022oqm show a hot (40,000 K) continuum with high ionization C and O absorption features at velocities of 4000 km s−1, while its photospheric radius expands at 20,000 km s−1, indicating a pre-existing distribution of expanding C/O material. After ∼2.5 days, both the spectrum and light curves evolve into those of a typical SN Ic, with line velocities of ∼10,000 km s−1, in agreement with the evolution of the photospheric radius. The optical light curves reach a second peak at t ≈ 15 days. By t = 60 days, the spectrum of SN 2022oqm becomes nearly nebular, displaying strong Ca ii and [Ca ii] emission with no detectable [O i], marking this event as Ca-rich. The early behavior can be explained by 10−3 M ⊙ of optically thin circumstellar material (CSM) surrounding either (1) a massive compact progenitor such as a Wolf-Rayet star, (2) a massive stripped progenitor with an extended envelope, or (3) a binary system with a white dwarf. We propose that the early-time light curve is powered by both the interaction of the ejecta with the optically thin CSM and shock cooling (in the massive star scenario). The observations can be explained by CSM that is optically thick to X-ray photons, is optically thick in the lines as seen in the spectra, and is optically thin to visible-light continuum photons that come either from downscattered X-rays or from the shock-heated ejecta. Calculations show that this scenario is self-consistent.

UR - http://www.scopus.com/inward/record.url?scp=85184936369&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/ad04d7

DO - 10.3847/1538-4357/ad04d7

M3 - Article

AN - SCOPUS:85184936369

SN - 0004-637X

VL - 962

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 109

ER -

SN 2022oqm-A Ca-rich Explosion of a Compact Progenitor Embedded in C/O Circumstellar Material

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