Comparing the Locations of Supernovae to CO (2-1) Emission in Their Host Galaxies

Ness Mayker Chen; Adam K. Leroy; Laura A. Lopez; Samantha Benincasa; Mélanie Chevance; Simon C.O. Glover; Annie Hughes; Kathryn Kreckel; Sumit Sarbadhicary; Jiayi Sun; Todd A. Thompson; Dyas Utomo; Frank Bigiel; Guillermo A. Blanc; Daniel A. Dale; Kathryn Grasha; J. M.Diederik Kruijssen; Hsi An Pan; Miguel Querejeta; Eva Schinnerer; Elizabeth J. Watkins; Thomas G. Williams

doi:10.3847/1538-4357/acab00

Comparing the Locations of Supernovae to CO (2-1) Emission in Their Host Galaxies

Ness Mayker Chen
, Adam K. Leroy
, Laura A. Lopez
, Samantha Benincasa
, Mélanie Chevance
, Simon C.O. Glover
, Annie Hughes
, Kathryn Kreckel
, Sumit Sarbadhicary
, Jiayi Sun
, Todd A. Thompson
, Dyas Utomo
, Frank Bigiel
, Guillermo A. Blanc
, Daniel A. Dale
, Kathryn Grasha
, J. M.Diederik Kruijssen
, Hsi An Pan
, Miguel Querejeta
, Eva Schinnerer

Elizabeth J. Watkins, Thomas G. Williams

Physics And Astronomy

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

8 Scopus citations

Abstract

We measure the molecular gas environment near recent (<100 yr old) supernovae (SNe) using ∼1″ or ≤150 pc resolution CO (2-1) maps from the PHANGS-Atacama Large Millimeter/submillimeter Array (ALMA) survey of nearby star-forming galaxies. This is arguably the first such study to approach the scales of individual massive molecular clouds (M _mol ≳ 10^5.3 M _⊙). Using the Open Supernova Catalog, we identify 63 SNe within the PHANGS-ALMA footprint. We detect CO (2-1) emission near ∼60% of the sample at 150 pc resolution, compared to ∼35% of map pixels with CO (2-1) emission, and up to ∼95% of the SNe at 1 kpc resolution, compared to ∼80% of map pixels with CO (2-1) emission. We expect the ∼60% of SNe within the same 150 pc beam, as a giant molecular cloud will likely interact with these clouds in the future, consistent with the observation of widespread SN-molecular gas interaction in the Milky Way, while the other ∼40% of SNe without strong CO (2-1) detections will deposit their energy in the diffuse interstellar medium, perhaps helping drive large-scale turbulence or galactic outflows. Broken down by type, we detect CO (2-1) emission at the sites of ∼85% of our 9 stripped-envelope SNe (SESNe), ∼40% of our 34 Type II SNe, and ∼35% of our 13 Type Ia SNe, indicating that SESNe are most closely associated with the brightest CO (2-1) emitting regions in our sample. Our results confirm that SN explosions are not restricted to only the densest gas, and instead exert feedback across a wide range of molecular gas densities.

Original language	English
Article number	110
Journal	Astrophysical Journal
Volume	944
Issue number	1
DOIs	https://doi.org/10.3847/1538-4357/acab00
State	Published - Feb 1 2023

Bibliographical note

Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.

Funding

K.G. is supported by the Australian Research Council through the Discovery Early Career Researcher Award (DECRA) Fellowship DE220100766 funded by the Australian Government. N.M.C. thanks the Ohio State University’s Galaxy and Supernova groups, including Christopher Kochanek, Kris Stanek, and Patrick Vallely, for useful discussions at several stages of the project. This work was carried out as part of the PHANGS collaboration. S.C.O.G. acknowledges financial support from the DFG via the collaborative research center (SFB 881, Project-ID 138713538) “The Milky Way System” (subprojects A1, B1, B2, B8, and P2). They also acknowledge funding from the Heidelberg Cluster of Excellence “STRUCTURES” in the framework of Germany's Excellence Strategy (grant EXC-2181/1, Project-ID 390900948) and from the European Research Council via the ERC Synergy Grant “ECOGAL” (grant 855130). The work of J.S. is partially supported by the Natural Sciences and Engineering Research Council of Canada (NSERC) through the Canadian Institute for Theoretical Astrophysics (CITA) National Fellowship. Support for this work was provided by the NSF through award SOSP SOSPADA-010 from the NRAO, which supported the work of N.M.C. The work of N.M.C., A.K.L., and J.S. was partially supported by the National Science Foundation (NSF) under grants No. 1615105, 1615109, and 1653300. E.S. and T.G.W. acknowledge funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 694343). The work of J.S. and A.K.L. is partially supported by the National Aeronautics and Space Administration (NASA) under ADAP grants NNX16AF48G and NNX17AF39G. M.C. and J.M.D.K. gratefully acknowledge funding from the DFG through an Emmy Noether Research Group (grant number KR4801/1-1) and the DFG Sachbeihilfe (grant number KR4801/2-1), as well as from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program via the ERC Starting Grant MUSTANG (grant agreement number 714907). M.C. gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) through an Emmy Noether Research Group (grant number CH2137/1-1). COOL Research DAO is a Decentralized Autonomous Organization supporting research in astrophysics aimed at uncovering our cosmic origins. GAB acknowledges support from the ANID BASAL FB210003 project. H.A.P. acknowledges support by the Ministry of Science and Technology of Taiwan under grant 110-2112-M-032-020-MY3.

Funders	Funder number
Australian Victorian Government
Ohio State University’s Galaxy and Supernova groups
Engineering Research Centers
Canadian Institute for Theoretical Astrophysics
Natural Sciences and Engineering Research Council of Canada
National Radio Astronomy Observatory
H2020 European Research Council
Horizon 2020
National Aeronautics and Space Administration	NNX16AF48G, NNX17AF39G
California Department of Fish and Game	138713538, KR4801/1-1
German Excellence Strategy in the Heidelberg Cluster of Excellence STRUCTURES	EXC-2181/1, 390900948
Horizon 2020 Framework Programme	694343, 726384, 714907, 855130
Australian Research Council	DE220100766
Deutsche Forschungsgemeinschaft	CH2137/1-1
Agencia Nacional de Investigación y Desarrollo	BASAL FB210003
Ministry of Science and Technology, Taiwan	110-2112-M-032-020-MY3
National Science Foundation Arctic Social Science Program	1615109, 1653300, 1615105
DFG Sachbeihilfe	KR4801/2-1

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.3847/1538-4357/acab00

Cite this

Mayker Chen, N., Leroy, A. K., Lopez, L. A., Benincasa, S., Chevance, M., Glover, S. C. O., Hughes, A., Kreckel, K., Sarbadhicary, S., Sun, J., Thompson, T. A., Utomo, D., Bigiel, F., Blanc, G. A., Dale, D. A., Grasha, K., Kruijssen, J. M. D., Pan, H. A., Querejeta, M., ... Williams, T. G. (2023). Comparing the Locations of Supernovae to CO (2-1) Emission in Their Host Galaxies. Astrophysical Journal, 944(1), Article 110. https://doi.org/10.3847/1538-4357/acab00

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title = "Comparing the Locations of Supernovae to CO (2-1) Emission in Their Host Galaxies",

abstract = "We measure the molecular gas environment near recent (<100 yr old) supernovae (SNe) using ∼1″ or ≤150 pc resolution CO (2-1) maps from the PHANGS-Atacama Large Millimeter/submillimeter Array (ALMA) survey of nearby star-forming galaxies. This is arguably the first such study to approach the scales of individual massive molecular clouds (M mol ≳ 105.3 M ⊙). Using the Open Supernova Catalog, we identify 63 SNe within the PHANGS-ALMA footprint. We detect CO (2-1) emission near ∼60\% of the sample at 150 pc resolution, compared to ∼35\% of map pixels with CO (2-1) emission, and up to ∼95\% of the SNe at 1 kpc resolution, compared to ∼80\% of map pixels with CO (2-1) emission. We expect the ∼60\% of SNe within the same 150 pc beam, as a giant molecular cloud will likely interact with these clouds in the future, consistent with the observation of widespread SN-molecular gas interaction in the Milky Way, while the other ∼40\% of SNe without strong CO (2-1) detections will deposit their energy in the diffuse interstellar medium, perhaps helping drive large-scale turbulence or galactic outflows. Broken down by type, we detect CO (2-1) emission at the sites of ∼85\% of our 9 stripped-envelope SNe (SESNe), ∼40\% of our 34 Type II SNe, and ∼35\% of our 13 Type Ia SNe, indicating that SESNe are most closely associated with the brightest CO (2-1) emitting regions in our sample. Our results confirm that SN explosions are not restricted to only the densest gas, and instead exert feedback across a wide range of molecular gas densities.",

author = "\{Mayker Chen\}, Ness and Leroy, \{Adam K.\} and Lopez, \{Laura A.\} and Samantha Benincasa and M{\'e}lanie Chevance and Glover, \{Simon C.O.\} and Annie Hughes and Kathryn Kreckel and Sumit Sarbadhicary and Jiayi Sun and Thompson, \{Todd A.\} and Dyas Utomo and Frank Bigiel and Blanc, \{Guillermo A.\} and Dale, \{Daniel A.\} and Kathryn Grasha and Kruijssen, \{J. M.Diederik\} and Pan, \{Hsi An\} and Miguel Querejeta and Eva Schinnerer and Watkins, \{Elizabeth J.\} and Williams, \{Thomas G.\}",

note = "Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = feb,

day = "1",

doi = "10.3847/1538-4357/acab00",

language = "English",

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Mayker Chen, N, Leroy, AK, Lopez, LA, Benincasa, S, Chevance, M, Glover, SCO, Hughes, A, Kreckel, K, Sarbadhicary, S, Sun, J, Thompson, TA, Utomo, D, Bigiel, F, Blanc, GA, Dale, DA, Grasha, K, Kruijssen, JMD, Pan, HA, Querejeta, M, Schinnerer, E, Watkins, EJ & Williams, TG 2023, 'Comparing the Locations of Supernovae to CO (2-1) Emission in Their Host Galaxies', Astrophysical Journal, vol. 944, no. 1, 110. https://doi.org/10.3847/1538-4357/acab00

TY - JOUR

T1 - Comparing the Locations of Supernovae to CO (2-1) Emission in Their Host Galaxies

AU - Mayker Chen, Ness

AU - Leroy, Adam K.

AU - Lopez, Laura A.

AU - Benincasa, Samantha

AU - Chevance, Mélanie

AU - Glover, Simon C.O.

AU - Hughes, Annie

AU - Kreckel, Kathryn

AU - Sarbadhicary, Sumit

AU - Sun, Jiayi

AU - Thompson, Todd A.

AU - Utomo, Dyas

AU - Bigiel, Frank

AU - Blanc, Guillermo A.

AU - Dale, Daniel A.

AU - Grasha, Kathryn

AU - Kruijssen, J. M.Diederik

AU - Pan, Hsi An

AU - Querejeta, Miguel

AU - Schinnerer, Eva

AU - Watkins, Elizabeth J.

AU - Williams, Thomas G.

PY - 2023/2/1

Y1 - 2023/2/1

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AB - We measure the molecular gas environment near recent (<100 yr old) supernovae (SNe) using ∼1″ or ≤150 pc resolution CO (2-1) maps from the PHANGS-Atacama Large Millimeter/submillimeter Array (ALMA) survey of nearby star-forming galaxies. This is arguably the first such study to approach the scales of individual massive molecular clouds (M mol ≳ 105.3 M ⊙). Using the Open Supernova Catalog, we identify 63 SNe within the PHANGS-ALMA footprint. We detect CO (2-1) emission near ∼60% of the sample at 150 pc resolution, compared to ∼35% of map pixels with CO (2-1) emission, and up to ∼95% of the SNe at 1 kpc resolution, compared to ∼80% of map pixels with CO (2-1) emission. We expect the ∼60% of SNe within the same 150 pc beam, as a giant molecular cloud will likely interact with these clouds in the future, consistent with the observation of widespread SN-molecular gas interaction in the Milky Way, while the other ∼40% of SNe without strong CO (2-1) detections will deposit their energy in the diffuse interstellar medium, perhaps helping drive large-scale turbulence or galactic outflows. Broken down by type, we detect CO (2-1) emission at the sites of ∼85% of our 9 stripped-envelope SNe (SESNe), ∼40% of our 34 Type II SNe, and ∼35% of our 13 Type Ia SNe, indicating that SESNe are most closely associated with the brightest CO (2-1) emitting regions in our sample. Our results confirm that SN explosions are not restricted to only the densest gas, and instead exert feedback across a wide range of molecular gas densities.

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Comparing the Locations of Supernovae to CO (2-1) Emission in Their Host Galaxies

Abstract

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