The Red Supergiant Progenitor of Type II Supernova 2024ggi
We present a detailed analysis of the progenitor and its local environment for the recently discovered Type II supernova (SN) 2024ggi at a distance of about 6.7 Mpc, by utilizing the pre-explosion images from the Hubble Space Telescope and Spitzer Space Telescope. The progenitor is identified as a r...
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| Veröffentlicht in: | Astrophysical journal. Letters 2024-07, Vol.969 (1), p.L15 |
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| container_title | Astrophysical journal. Letters |
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| creator | Xiang, Danfeng Mo, Jun Wang, Xiaofeng Wang, Lingzhi Zhang, Jujia Lin, Han Chen, Liyang Song, Cuiying Liu, Liang-Duan Wang, Zhenyu Li, Gaici |
| description | We present a detailed analysis of the progenitor and its local environment for the recently discovered Type II supernova (SN) 2024ggi at a distance of about 6.7 Mpc, by utilizing the pre-explosion images from the Hubble Space Telescope and Spitzer Space Telescope. The progenitor is identified as a red bright variable star, with absolute F814W-band magnitudes being −6.2 mag in 1995 to −7.2 mag in 2003, respectively, consistent with that of a normal red supergiant star. Combining with the historical mid-infrared light curves, a pulsational period of about 379 days can be inferred for the progenitor star. Fitting its spectral energy distribution with stellar spectral models yields the stellar parameters of temperature, radius, and bolometric luminosity as
T
*
=
3290
−
27
+
19
K,
R
*
=
887
−
51
+
60
R
⊙
, and log(
L
/
L
⊙
)
=
4.92
−
0.04
+
0.05
, respectively. The above parameters indicate that the progenitor of SN 2024ggi is consistent with the stellar evolutionary track of a solar-metallicity massive star with an initial mass of
13
−
1
+
1
M
⊙
. Moreover, our analysis indicates a relatively low mass-loss rate (i.e., |
| doi_str_mv | 10.3847/2041-8213/ad54b3 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_iop_j</sourceid><recordid>TN_cdi_proquest_journals_3073222407</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><doaj_id>oai_doaj_org_article_9347ae819d774f60a10c402bc8d918ef</doaj_id><sourcerecordid>3073222407</sourcerecordid><originalsourceid>FETCH-LOGICAL-c369t-f9b6a3d011d6ab379ef85e2e136e5b00d8adf84febea1c100fb4eb74d5c0be7e3</originalsourceid><addsrcrecordid>eNp1kM1Lw0AQxRdRsFbvHgNejZ39SHbjTcSPQEHRel52s7MxpXbjJhX635saqSdPMzze-83wCDmncMWVkDMGgqaKUT4zLhOWH5DJXjrc75Adk5OuWwIwyKmakOvFOyYv6JLXTYuxbsy6T55jqHHd9CEmwSeLbYtJWY6GdfgyCQMm6ro5JUferDo8-51T8nZ_t7h9TOdPD-XtzTyteF70qS9sbrgDSl1uLJcFepUhQ8pzzCyAU8Z5JTxaNLSiAN4KtFK4rAKLEvmUlCPXBbPUbWw-TNzqYBr9I4RYaxP7plqhLriQBhUtnJTC52AoVAKYrZQrqEI_sC5GVhvD5wa7Xi_DJq6H9zUHyRljYhhTAqOriqHrIvr9VQp617be1al31eqx7SFyOUaa0P4x_7V_A2nrfm8</addsrcrecordid><sourcetype>Open Website</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>3073222407</pqid></control><display><type>article</type><title>The Red Supergiant Progenitor of Type II Supernova 2024ggi</title><source>IOP Publishing Free Content</source><source>DOAJ Directory of Open Access Journals</source><source>EZB-FREE-00999 freely available EZB journals</source><source>Alma/SFX Local Collection</source><creator>Xiang, Danfeng ; Mo, Jun ; Wang, Xiaofeng ; Wang, Lingzhi ; Zhang, Jujia ; Lin, Han ; Chen, Liyang ; Song, Cuiying ; Liu, Liang-Duan ; Wang, Zhenyu ; Li, Gaici</creator><creatorcontrib>Xiang, Danfeng ; Mo, Jun ; Wang, Xiaofeng ; Wang, Lingzhi ; Zhang, Jujia ; Lin, Han ; Chen, Liyang ; Song, Cuiying ; Liu, Liang-Duan ; Wang, Zhenyu ; Li, Gaici</creatorcontrib><description>We present a detailed analysis of the progenitor and its local environment for the recently discovered Type II supernova (SN) 2024ggi at a distance of about 6.7 Mpc, by utilizing the pre-explosion images from the Hubble Space Telescope and Spitzer Space Telescope. The progenitor is identified as a red bright variable star, with absolute F814W-band magnitudes being −6.2 mag in 1995 to −7.2 mag in 2003, respectively, consistent with that of a normal red supergiant star. Combining with the historical mid-infrared light curves, a pulsational period of about 379 days can be inferred for the progenitor star. Fitting its spectral energy distribution with stellar spectral models yields the stellar parameters of temperature, radius, and bolometric luminosity as
T
*
=
3290
−
27
+
19
K,
R
*
=
887
−
51
+
60
R
⊙
, and log(
L
/
L
⊙
)
=
4.92
−
0.04
+
0.05
, respectively. The above parameters indicate that the progenitor of SN 2024ggi is consistent with the stellar evolutionary track of a solar-metallicity massive star with an initial mass of
13
−
1
+
1
M
⊙
. Moreover, our analysis indicates a relatively low mass-loss rate (i.e., <3 × 10
−6
M
⊙
yr
−1
) for the progenitor compared to that inferred from flash spectroscopy and X-ray detection (i.e., 10
−2
–10
−5
M
⊙
yr
−1
), implying a significant enhancement in mass loss within a few years prior to the explosion.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/ad54b3</identifier><language>eng</language><publisher>Austin: The American Astronomical Society</publisher><subject>Astronomical models ; Hubble Space Telescope ; Light curve ; Luminosity ; Massive stars ; Metallicity ; Parameters ; Red giant stars ; Red supergiant stars ; Space telescopes ; Spectral energy distribution ; Spectroscopy ; Stars ; Stellar evolution ; Stellar mass loss ; Stellar models ; Supergiant stars ; Supernova ; Supernovae ; Type II supernovae ; Variable stars</subject><ispartof>Astrophysical journal. Letters, 2024-07, Vol.969 (1), p.L15</ispartof><rights>2024. The Author(s). Published by the American Astronomical Society.</rights><rights>2024. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c369t-f9b6a3d011d6ab379ef85e2e136e5b00d8adf84febea1c100fb4eb74d5c0be7e3</cites><orcidid>0000-0002-1089-1519 ; 0000-0002-8296-2590 ; 0000-0002-1094-3817 ; 0000-0002-7334-2357 ; 0000-0002-8708-0597 ; 0000-0001-8390-9962</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/2041-8213/ad54b3/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>314,776,780,860,2096,27901,27902,38867,53842</link.rule.ids></links><search><creatorcontrib>Xiang, Danfeng</creatorcontrib><creatorcontrib>Mo, Jun</creatorcontrib><creatorcontrib>Wang, Xiaofeng</creatorcontrib><creatorcontrib>Wang, Lingzhi</creatorcontrib><creatorcontrib>Zhang, Jujia</creatorcontrib><creatorcontrib>Lin, Han</creatorcontrib><creatorcontrib>Chen, Liyang</creatorcontrib><creatorcontrib>Song, Cuiying</creatorcontrib><creatorcontrib>Liu, Liang-Duan</creatorcontrib><creatorcontrib>Wang, Zhenyu</creatorcontrib><creatorcontrib>Li, Gaici</creatorcontrib><title>The Red Supergiant Progenitor of Type II Supernova 2024ggi</title><title>Astrophysical journal. Letters</title><addtitle>APJL</addtitle><addtitle>Astrophys. J. Lett</addtitle><description>We present a detailed analysis of the progenitor and its local environment for the recently discovered Type II supernova (SN) 2024ggi at a distance of about 6.7 Mpc, by utilizing the pre-explosion images from the Hubble Space Telescope and Spitzer Space Telescope. The progenitor is identified as a red bright variable star, with absolute F814W-band magnitudes being −6.2 mag in 1995 to −7.2 mag in 2003, respectively, consistent with that of a normal red supergiant star. Combining with the historical mid-infrared light curves, a pulsational period of about 379 days can be inferred for the progenitor star. Fitting its spectral energy distribution with stellar spectral models yields the stellar parameters of temperature, radius, and bolometric luminosity as
T
*
=
3290
−
27
+
19
K,
R
*
=
887
−
51
+
60
R
⊙
, and log(
L
/
L
⊙
)
=
4.92
−
0.04
+
0.05
, respectively. The above parameters indicate that the progenitor of SN 2024ggi is consistent with the stellar evolutionary track of a solar-metallicity massive star with an initial mass of
13
−
1
+
1
M
⊙
. Moreover, our analysis indicates a relatively low mass-loss rate (i.e., <3 × 10
−6
M
⊙
yr
−1
) for the progenitor compared to that inferred from flash spectroscopy and X-ray detection (i.e., 10
−2
–10
−5
M
⊙
yr
−1
), implying a significant enhancement in mass loss within a few years prior to the explosion.</description><subject>Astronomical models</subject><subject>Hubble Space Telescope</subject><subject>Light curve</subject><subject>Luminosity</subject><subject>Massive stars</subject><subject>Metallicity</subject><subject>Parameters</subject><subject>Red giant stars</subject><subject>Red supergiant stars</subject><subject>Space telescopes</subject><subject>Spectral energy distribution</subject><subject>Spectroscopy</subject><subject>Stars</subject><subject>Stellar evolution</subject><subject>Stellar mass loss</subject><subject>Stellar models</subject><subject>Supergiant stars</subject><subject>Supernova</subject><subject>Supernovae</subject><subject>Type II supernovae</subject><subject>Variable stars</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp1kM1Lw0AQxRdRsFbvHgNejZ39SHbjTcSPQEHRel52s7MxpXbjJhX635saqSdPMzze-83wCDmncMWVkDMGgqaKUT4zLhOWH5DJXjrc75Adk5OuWwIwyKmakOvFOyYv6JLXTYuxbsy6T55jqHHd9CEmwSeLbYtJWY6GdfgyCQMm6ro5JUferDo8-51T8nZ_t7h9TOdPD-XtzTyteF70qS9sbrgDSl1uLJcFepUhQ8pzzCyAU8Z5JTxaNLSiAN4KtFK4rAKLEvmUlCPXBbPUbWw-TNzqYBr9I4RYaxP7plqhLriQBhUtnJTC52AoVAKYrZQrqEI_sC5GVhvD5wa7Xi_DJq6H9zUHyRljYhhTAqOriqHrIvr9VQp617be1al31eqx7SFyOUaa0P4x_7V_A2nrfm8</recordid><startdate>20240701</startdate><enddate>20240701</enddate><creator>Xiang, Danfeng</creator><creator>Mo, Jun</creator><creator>Wang, Xiaofeng</creator><creator>Wang, Lingzhi</creator><creator>Zhang, Jujia</creator><creator>Lin, Han</creator><creator>Chen, Liyang</creator><creator>Song, Cuiying</creator><creator>Liu, Liang-Duan</creator><creator>Wang, Zhenyu</creator><creator>Li, Gaici</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0002-1089-1519</orcidid><orcidid>https://orcid.org/0000-0002-8296-2590</orcidid><orcidid>https://orcid.org/0000-0002-1094-3817</orcidid><orcidid>https://orcid.org/0000-0002-7334-2357</orcidid><orcidid>https://orcid.org/0000-0002-8708-0597</orcidid><orcidid>https://orcid.org/0000-0001-8390-9962</orcidid></search><sort><creationdate>20240701</creationdate><title>The Red Supergiant Progenitor of Type II Supernova 2024ggi</title><author>Xiang, Danfeng ; Mo, Jun ; Wang, Xiaofeng ; Wang, Lingzhi ; Zhang, Jujia ; Lin, Han ; Chen, Liyang ; Song, Cuiying ; Liu, Liang-Duan ; Wang, Zhenyu ; Li, Gaici</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c369t-f9b6a3d011d6ab379ef85e2e136e5b00d8adf84febea1c100fb4eb74d5c0be7e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Astronomical models</topic><topic>Hubble Space Telescope</topic><topic>Light curve</topic><topic>Luminosity</topic><topic>Massive stars</topic><topic>Metallicity</topic><topic>Parameters</topic><topic>Red giant stars</topic><topic>Red supergiant stars</topic><topic>Space telescopes</topic><topic>Spectral energy distribution</topic><topic>Spectroscopy</topic><topic>Stars</topic><topic>Stellar evolution</topic><topic>Stellar mass loss</topic><topic>Stellar models</topic><topic>Supergiant stars</topic><topic>Supernova</topic><topic>Supernovae</topic><topic>Type II supernovae</topic><topic>Variable stars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Xiang, Danfeng</creatorcontrib><creatorcontrib>Mo, Jun</creatorcontrib><creatorcontrib>Wang, Xiaofeng</creatorcontrib><creatorcontrib>Wang, Lingzhi</creatorcontrib><creatorcontrib>Zhang, Jujia</creatorcontrib><creatorcontrib>Lin, Han</creatorcontrib><creatorcontrib>Chen, Liyang</creatorcontrib><creatorcontrib>Song, Cuiying</creatorcontrib><creatorcontrib>Liu, Liang-Duan</creatorcontrib><creatorcontrib>Wang, Zhenyu</creatorcontrib><creatorcontrib>Li, Gaici</creatorcontrib><collection>IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>DOAJ Directory of Open Access Journals</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Xiang, Danfeng</au><au>Mo, Jun</au><au>Wang, Xiaofeng</au><au>Wang, Lingzhi</au><au>Zhang, Jujia</au><au>Lin, Han</au><au>Chen, Liyang</au><au>Song, Cuiying</au><au>Liu, Liang-Duan</au><au>Wang, Zhenyu</au><au>Li, Gaici</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Red Supergiant Progenitor of Type II Supernova 2024ggi</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2024-07-01</date><risdate>2024</risdate><volume>969</volume><issue>1</issue><spage>L15</spage><pages>L15-</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>We present a detailed analysis of the progenitor and its local environment for the recently discovered Type II supernova (SN) 2024ggi at a distance of about 6.7 Mpc, by utilizing the pre-explosion images from the Hubble Space Telescope and Spitzer Space Telescope. The progenitor is identified as a red bright variable star, with absolute F814W-band magnitudes being −6.2 mag in 1995 to −7.2 mag in 2003, respectively, consistent with that of a normal red supergiant star. Combining with the historical mid-infrared light curves, a pulsational period of about 379 days can be inferred for the progenitor star. Fitting its spectral energy distribution with stellar spectral models yields the stellar parameters of temperature, radius, and bolometric luminosity as
T
*
=
3290
−
27
+
19
K,
R
*
=
887
−
51
+
60
R
⊙
, and log(
L
/
L
⊙
)
=
4.92
−
0.04
+
0.05
, respectively. The above parameters indicate that the progenitor of SN 2024ggi is consistent with the stellar evolutionary track of a solar-metallicity massive star with an initial mass of
13
−
1
+
1
M
⊙
. Moreover, our analysis indicates a relatively low mass-loss rate (i.e., <3 × 10
−6
M
⊙
yr
−1
) for the progenitor compared to that inferred from flash spectroscopy and X-ray detection (i.e., 10
−2
–10
−5
M
⊙
yr
−1
), implying a significant enhancement in mass loss within a few years prior to the explosion.</abstract><cop>Austin</cop><pub>The American Astronomical Society</pub><doi>10.3847/2041-8213/ad54b3</doi><tpages>10</tpages><orcidid>https://orcid.org/0000-0002-1089-1519</orcidid><orcidid>https://orcid.org/0000-0002-8296-2590</orcidid><orcidid>https://orcid.org/0000-0002-1094-3817</orcidid><orcidid>https://orcid.org/0000-0002-7334-2357</orcidid><orcidid>https://orcid.org/0000-0002-8708-0597</orcidid><orcidid>https://orcid.org/0000-0001-8390-9962</orcidid><oa>free_for_read</oa></addata></record> |
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| source | IOP Publishing Free Content; DOAJ Directory of Open Access Journals; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Astronomical models Hubble Space Telescope Light curve Luminosity Massive stars Metallicity Parameters Red giant stars Red supergiant stars Space telescopes Spectral energy distribution Spectroscopy Stars Stellar evolution Stellar mass loss Stellar models Supergiant stars Supernova Supernovae Type II supernovae Variable stars |
| title | The Red Supergiant Progenitor of Type II Supernova 2024ggi |
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