The Masses of Supernova Remnant Progenitors in M33
Using resolved optical stellar photometry from the Panchromatic Hubble Andromeda Treasury Triangulum Extended Region survey, we measured the star formation history near the position of 85 supernova remnants (SNRs) in M33. We constrained the progenitor masses for 60 of these SNRs, finding that the re...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acc249 |
| _version_ | 1797698911708643328 |
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| author | Brad Koplitz Jared Johnson Benjamin F. Williams Mariangelly Díaz-Rodríguez Jeremiah W. Murphy Margaret Lazzarini Joseph Guzman Julianne J. Dalcanton Andrew Dolphin Meredith Durbin |
| author_facet | Brad Koplitz Jared Johnson Benjamin F. Williams Mariangelly Díaz-Rodríguez Jeremiah W. Murphy Margaret Lazzarini Joseph Guzman Julianne J. Dalcanton Andrew Dolphin Meredith Durbin |
| author_sort | Brad Koplitz |
| collection | DOAJ |
| description | Using resolved optical stellar photometry from the Panchromatic Hubble Andromeda Treasury Triangulum Extended Region survey, we measured the star formation history near the position of 85 supernova remnants (SNRs) in M33. We constrained the progenitor masses for 60 of these SNRs, finding that the remaining 25 remnants had no local star formation in the last 56 Myr, consistent with core-collapse supernovae, making them potential Type Ia candidates. We then infer a progenitor mass distribution from the age distribution, assuming single star evolution. We find that the progenitor mass distribution is consistent with being drawn from a power law with an index of $-{2.9}_{-1.0}^{+1.2}$ . Additionally, we infer a minimum progenitor mass of ${7.1}_{-0.2}^{+0.1}$ M _⊙ from this sample, consistent with several previous studies, providing further evidence that stars with ages older than the lifetimes of single 8 M _⊙ stars are producing supernovae. |
| first_indexed | 2024-03-12T04:00:57Z |
| format | Article |
| id | doaj.art-b4b0d69d696c49e194495f030e8ba395 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T04:00:57Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-b4b0d69d696c49e194495f030e8ba3952023-09-03T11:41:28ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0194913210.3847/1538-4357/acc249The Masses of Supernova Remnant Progenitors in M33Brad Koplitz0https://orcid.org/0000-0001-5530-2872Jared Johnson1https://orcid.org/0000-0002-2630-9490Benjamin F. Williams2https://orcid.org/0000-0002-7502-0597Mariangelly Díaz-Rodríguez3https://orcid.org/0000-0002-4652-5983Jeremiah W. Murphy4Margaret Lazzarini5https://orcid.org/0000-0003-3252-352XJoseph Guzman6https://orcid.org/0000-0001-8878-4994Julianne J. Dalcanton7https://orcid.org/0000-0002-1264-2006Andrew Dolphin8https://orcid.org/0000-0001-8416-4093Meredith Durbin9https://orcid.org/0000-0001-7531-9815Department of Astronomy, Box 351580, University of Washington , Seattle, WA 98195, USA ; bmk12@uw.eduDepartment of Astronomy, Box 351580, University of Washington , Seattle, WA 98195, USA ; bmk12@uw.eduDepartment of Astronomy, Box 351580, University of Washington , Seattle, WA 98195, USA ; bmk12@uw.eduDepartment of Physics, Florida State University , 77 Chieftan Way, Tallahassee, FL 32306, USADepartment of Physics, Florida State University , 77 Chieftan Way, Tallahassee, FL 32306, USACalifornia Institute of Technology , 1200 E California Boulevard, Pasadena, CA 91125, USADepartment of Physics, Florida State University , 77 Chieftan Way, Tallahassee, FL 32306, USADepartment of Astronomy, Box 351580, University of Washington , Seattle, WA 98195, USA ; bmk12@uw.edu; Center for Computational Astrophysics , Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USARaytheon Technologies , 1151 E. Hermans Road, Tucson, AZ 85706, USA; Steward Observatory, University of Arizona , 933 N. Cherry Avenue, Tucson, AZ 85719, USADepartment of Astronomy, Box 351580, University of Washington , Seattle, WA 98195, USA ; bmk12@uw.eduUsing resolved optical stellar photometry from the Panchromatic Hubble Andromeda Treasury Triangulum Extended Region survey, we measured the star formation history near the position of 85 supernova remnants (SNRs) in M33. We constrained the progenitor masses for 60 of these SNRs, finding that the remaining 25 remnants had no local star formation in the last 56 Myr, consistent with core-collapse supernovae, making them potential Type Ia candidates. We then infer a progenitor mass distribution from the age distribution, assuming single star evolution. We find that the progenitor mass distribution is consistent with being drawn from a power law with an index of $-{2.9}_{-1.0}^{+1.2}$ . Additionally, we infer a minimum progenitor mass of ${7.1}_{-0.2}^{+0.1}$ M _⊙ from this sample, consistent with several previous studies, providing further evidence that stars with ages older than the lifetimes of single 8 M _⊙ stars are producing supernovae.https://doi.org/10.3847/1538-4357/acc249SupernovaeStellar evolutionMassive starsStellar populations |
| spellingShingle | Brad Koplitz Jared Johnson Benjamin F. Williams Mariangelly Díaz-Rodríguez Jeremiah W. Murphy Margaret Lazzarini Joseph Guzman Julianne J. Dalcanton Andrew Dolphin Meredith Durbin The Masses of Supernova Remnant Progenitors in M33 The Astrophysical Journal Supernovae Stellar evolution Massive stars Stellar populations |
| title | The Masses of Supernova Remnant Progenitors in M33 |
| title_full | The Masses of Supernova Remnant Progenitors in M33 |
| title_fullStr | The Masses of Supernova Remnant Progenitors in M33 |
| title_full_unstemmed | The Masses of Supernova Remnant Progenitors in M33 |
| title_short | The Masses of Supernova Remnant Progenitors in M33 |
| title_sort | masses of supernova remnant progenitors in m33 |
| topic | Supernovae Stellar evolution Massive stars Stellar populations |
| url | https://doi.org/10.3847/1538-4357/acc249 |
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