Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351
- Autores
- Sun, Jiayi; He, Hao; Batschkun, Kyle; Levy, Rebecca C.; Emig, Kimberly; Rodriguez, Maria Jimena; Hassani, Hamid; Leroy, Adam K.; Schinnerer, Eva; Ostriker, Eve C.; Wilson, Christine D.; Bolatto, Alberto D.; Mills, Elisabeth A. C.; Rosolowsky, Erik; Lee, Janice C.; Dale, Daniel A.; Larson, Kirsten L.; Thilker, David A.; Ubeda, Leonardo; Whitmore, Bradley C.; Williams, Thomas G.; Barnes, Ashley T.; Bigiel, Frank; Chevance, Mélanie; Glover, Simon C. O.; Neumann, Justus; Pinna, Francesca; Querejeta, Miguel; Sormani, Mattia C.; Tress, Robin G.
- Año de publicación
- 2024
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We use 0.1 observations from the Atacama Large Millimeter Array (ALMA), Hubble Space Telescope (HST),and JWST to study young massive clusters (YMCs) in their embedded“infant” phase across the central starburstring in NGC 3351. Our new ALMA data reveal 18 bright and compact (sub-)millimeter continuum sources, ofwhich 8 have counterparts in JWST images and only 6 have counterparts in HST images. Based on the ALMAcontinuum and molecular line data, as well as ancillary measurements for the HST and JWST counterparts, weidentify 14 sources as infant star clusters with high stellar and/or gas masses (∼105 Me), small radii ( 5 pc), largeescape velocities (6–10 km s−1), and short freefall times (0.5–1 Myr). Their multiwavelength properties motivateus to divide them into four categories, likely corresponding to four evolutionary stages from starless clumps toexposed H II region–cluster complexes. Leveraging age estimates for HST-identi ed clusters in the same region,we infer an evolutionary timeline, ranging from∼1–2 Myr before cluster formation as starless clumps, to∼4–6 Myr after as exposed H II region–cluster complexes. Finally, we show that the YMCs make up a substantialfraction of recent star formation across the ring, exhibit a nonuniform azimuthal distribution without a verycoherent evolutionary trend along the ring, and are capable of driving large-scale gas out ows
Fil: Sun, Jiayi. University of Princeton; Estados Unidos
Fil: He, Hao. Mc Master University; Canadá
Fil: Batschkun, Kyle. Mc Master University; Canadá
Fil: Levy, Rebecca C.. University of Arizona; Estados Unidos
Fil: Emig, Kimberly. University of Alberta; Canadá
Fil: Rodriguez, Maria Jimena. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Hassani, Hamid. Ohio State University; Estados Unidos
Fil: Leroy, Adam K.. Max Planck Institute For Astronomy; Alemania
Fil: Schinnerer, Eva. University of Alberta; Canadá
Fil: Ostriker, Eve C.. Space Telescope Science Institute; Estados Unidos
Fil: Wilson, Christine D.. University Of Wyoming; Estados Unidos
Fil: Bolatto, Alberto D.. Space Telescope Science Institute; Estados Unidos
Fil: Mills, Elisabeth A. C.. Space Telescope Science Institute; Estados Unidos
Fil: Rosolowsky, Erik. Space Telescope Science Institute; Estados Unidos
Fil: Lee, Janice C.. Space Telescope Science Institute; Estados Unidos
Fil: Dale, Daniel A.. University of Wyoming; Estados Unidos
Fil: Larson, Kirsten L.. Space Telescope Science Institute; Estados Unidos
Fil: Thilker, David A.. University Johns Hopkins; Estados Unidos
Fil: Ubeda, Leonardo. Space Telescope Science Institute; Estados Unidos
Fil: Whitmore, Bradley C.. Space Telescope Science Institute; Estados Unidos
Fil: Williams, Thomas G.. University of Oxford; Reino Unido
Fil: Barnes, Ashley T.. European Southern Observatory; Alemania
Fil: Bigiel, Frank. Universitat Bonn; Alemania
Fil: Chevance, Mélanie. Ruprecht Karls Universitat Heidelberg; Alemania
Fil: Glover, Simon C. O.. Ruprecht Karls Universitat Heidelberg; Alemania
Fil: Neumann, Justus. Max-Planck-Institut für Astronomie; Alemania
Fil: Pinna, Francesca. Max-Planck-Institut für Astronomie; Alemania. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; España
Fil: Querejeta, Miguel. Universidad de Alcala. Observatorio Astronómico Nacional; España
Fil: Sormani, Mattia C.. University of Surrey; Reino Unido
Fil: Tress, Robin G.. Observatoire de Sauverny; Suiza - Materia
-
STAR CLUSTERS
INTERSTELLAR MEDIUM
STAR FORMATION
BARRED SPIRAL GALAXIES - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/276032
Ver los metadatos del registro completo
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Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351Sun, JiayiHe, HaoBatschkun, KyleLevy, Rebecca C.Emig, KimberlyRodriguez, Maria JimenaHassani, HamidLeroy, Adam K.Schinnerer, EvaOstriker, Eve C.Wilson, Christine D.Bolatto, Alberto D.Mills, Elisabeth A. C.Rosolowsky, ErikLee, Janice C.Dale, Daniel A.Larson, Kirsten L.Thilker, David A.Ubeda, LeonardoWhitmore, Bradley C.Williams, Thomas G.Barnes, Ashley T.Bigiel, FrankChevance, MélanieGlover, Simon C. O.Neumann, JustusPinna, FrancescaQuerejeta, MiguelSormani, Mattia C.Tress, Robin G.STAR CLUSTERSINTERSTELLAR MEDIUMSTAR FORMATIONBARRED SPIRAL GALAXIEShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We use 0.1 observations from the Atacama Large Millimeter Array (ALMA), Hubble Space Telescope (HST),and JWST to study young massive clusters (YMCs) in their embedded“infant” phase across the central starburstring in NGC 3351. Our new ALMA data reveal 18 bright and compact (sub-)millimeter continuum sources, ofwhich 8 have counterparts in JWST images and only 6 have counterparts in HST images. Based on the ALMAcontinuum and molecular line data, as well as ancillary measurements for the HST and JWST counterparts, weidentify 14 sources as infant star clusters with high stellar and/or gas masses (∼105 Me), small radii ( 5 pc), largeescape velocities (6–10 km s−1), and short freefall times (0.5–1 Myr). Their multiwavelength properties motivateus to divide them into four categories, likely corresponding to four evolutionary stages from starless clumps toexposed H II region–cluster complexes. Leveraging age estimates for HST-identi ed clusters in the same region,we infer an evolutionary timeline, ranging from∼1–2 Myr before cluster formation as starless clumps, to∼4–6 Myr after as exposed H II region–cluster complexes. Finally, we show that the YMCs make up a substantialfraction of recent star formation across the ring, exhibit a nonuniform azimuthal distribution without a verycoherent evolutionary trend along the ring, and are capable of driving large-scale gas out owsFil: Sun, Jiayi. University of Princeton; Estados UnidosFil: He, Hao. Mc Master University; CanadáFil: Batschkun, Kyle. Mc Master University; CanadáFil: Levy, Rebecca C.. University of Arizona; Estados UnidosFil: Emig, Kimberly. University of Alberta; CanadáFil: Rodriguez, Maria Jimena. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Hassani, Hamid. Ohio State University; Estados UnidosFil: Leroy, Adam K.. Max Planck Institute For Astronomy; AlemaniaFil: Schinnerer, Eva. University of Alberta; CanadáFil: Ostriker, Eve C.. Space Telescope Science Institute; Estados UnidosFil: Wilson, Christine D.. University Of Wyoming; Estados UnidosFil: Bolatto, Alberto D.. Space Telescope Science Institute; Estados UnidosFil: Mills, Elisabeth A. C.. Space Telescope Science Institute; Estados UnidosFil: Rosolowsky, Erik. Space Telescope Science Institute; Estados UnidosFil: Lee, Janice C.. Space Telescope Science Institute; Estados UnidosFil: Dale, Daniel A.. University of Wyoming; Estados UnidosFil: Larson, Kirsten L.. Space Telescope Science Institute; Estados UnidosFil: Thilker, David A.. University Johns Hopkins; Estados UnidosFil: Ubeda, Leonardo. Space Telescope Science Institute; Estados UnidosFil: Whitmore, Bradley C.. Space Telescope Science Institute; Estados UnidosFil: Williams, Thomas G.. University of Oxford; Reino UnidoFil: Barnes, Ashley T.. European Southern Observatory; AlemaniaFil: Bigiel, Frank. Universitat Bonn; AlemaniaFil: Chevance, Mélanie. Ruprecht Karls Universitat Heidelberg; AlemaniaFil: Glover, Simon C. O.. Ruprecht Karls Universitat Heidelberg; AlemaniaFil: Neumann, Justus. Max-Planck-Institut für Astronomie; AlemaniaFil: Pinna, Francesca. Max-Planck-Institut für Astronomie; Alemania. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; EspañaFil: Querejeta, Miguel. Universidad de Alcala. Observatorio Astronómico Nacional; EspañaFil: Sormani, Mattia C.. University of Surrey; Reino UnidoFil: Tress, Robin G.. Observatoire de Sauverny; SuizaIOP Publishing2024-05info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/276032Sun, Jiayi; He, Hao; Batschkun, Kyle; Levy, Rebecca C.; Emig, Kimberly; et al.; Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351; IOP Publishing; Astrophysical Journal; 967; 2; 5-2024; 1-230004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ad3de6info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad3de6info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-01-14T12:21:26Zoai:ri.conicet.gov.ar:11336/276032instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982026-01-14 12:21:26.581CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351 |
| title |
Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351 |
| spellingShingle |
Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351 Sun, Jiayi STAR CLUSTERS INTERSTELLAR MEDIUM STAR FORMATION BARRED SPIRAL GALAXIES |
| title_short |
Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351 |
| title_full |
Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351 |
| title_fullStr |
Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351 |
| title_full_unstemmed |
Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351 |
| title_sort |
Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351 |
| dc.creator.none.fl_str_mv |
Sun, Jiayi He, Hao Batschkun, Kyle Levy, Rebecca C. Emig, Kimberly Rodriguez, Maria Jimena Hassani, Hamid Leroy, Adam K. Schinnerer, Eva Ostriker, Eve C. Wilson, Christine D. Bolatto, Alberto D. Mills, Elisabeth A. C. Rosolowsky, Erik Lee, Janice C. Dale, Daniel A. Larson, Kirsten L. Thilker, David A. Ubeda, Leonardo Whitmore, Bradley C. Williams, Thomas G. Barnes, Ashley T. Bigiel, Frank Chevance, Mélanie Glover, Simon C. O. Neumann, Justus Pinna, Francesca Querejeta, Miguel Sormani, Mattia C. Tress, Robin G. |
| author |
Sun, Jiayi |
| author_facet |
Sun, Jiayi He, Hao Batschkun, Kyle Levy, Rebecca C. Emig, Kimberly Rodriguez, Maria Jimena Hassani, Hamid Leroy, Adam K. Schinnerer, Eva Ostriker, Eve C. Wilson, Christine D. Bolatto, Alberto D. Mills, Elisabeth A. C. Rosolowsky, Erik Lee, Janice C. Dale, Daniel A. Larson, Kirsten L. Thilker, David A. Ubeda, Leonardo Whitmore, Bradley C. Williams, Thomas G. Barnes, Ashley T. Bigiel, Frank Chevance, Mélanie Glover, Simon C. O. Neumann, Justus Pinna, Francesca Querejeta, Miguel Sormani, Mattia C. Tress, Robin G. |
| author_role |
author |
| author2 |
He, Hao Batschkun, Kyle Levy, Rebecca C. Emig, Kimberly Rodriguez, Maria Jimena Hassani, Hamid Leroy, Adam K. Schinnerer, Eva Ostriker, Eve C. Wilson, Christine D. Bolatto, Alberto D. Mills, Elisabeth A. C. Rosolowsky, Erik Lee, Janice C. Dale, Daniel A. Larson, Kirsten L. Thilker, David A. Ubeda, Leonardo Whitmore, Bradley C. Williams, Thomas G. Barnes, Ashley T. Bigiel, Frank Chevance, Mélanie Glover, Simon C. O. Neumann, Justus Pinna, Francesca Querejeta, Miguel Sormani, Mattia C. Tress, Robin G. |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
STAR CLUSTERS INTERSTELLAR MEDIUM STAR FORMATION BARRED SPIRAL GALAXIES |
| topic |
STAR CLUSTERS INTERSTELLAR MEDIUM STAR FORMATION BARRED SPIRAL GALAXIES |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
We use 0.1 observations from the Atacama Large Millimeter Array (ALMA), Hubble Space Telescope (HST),and JWST to study young massive clusters (YMCs) in their embedded“infant” phase across the central starburstring in NGC 3351. Our new ALMA data reveal 18 bright and compact (sub-)millimeter continuum sources, ofwhich 8 have counterparts in JWST images and only 6 have counterparts in HST images. Based on the ALMAcontinuum and molecular line data, as well as ancillary measurements for the HST and JWST counterparts, weidentify 14 sources as infant star clusters with high stellar and/or gas masses (∼105 Me), small radii ( 5 pc), largeescape velocities (6–10 km s−1), and short freefall times (0.5–1 Myr). Their multiwavelength properties motivateus to divide them into four categories, likely corresponding to four evolutionary stages from starless clumps toexposed H II region–cluster complexes. Leveraging age estimates for HST-identi ed clusters in the same region,we infer an evolutionary timeline, ranging from∼1–2 Myr before cluster formation as starless clumps, to∼4–6 Myr after as exposed H II region–cluster complexes. Finally, we show that the YMCs make up a substantialfraction of recent star formation across the ring, exhibit a nonuniform azimuthal distribution without a verycoherent evolutionary trend along the ring, and are capable of driving large-scale gas out ows Fil: Sun, Jiayi. University of Princeton; Estados Unidos Fil: He, Hao. Mc Master University; Canadá Fil: Batschkun, Kyle. Mc Master University; Canadá Fil: Levy, Rebecca C.. University of Arizona; Estados Unidos Fil: Emig, Kimberly. University of Alberta; Canadá Fil: Rodriguez, Maria Jimena. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Hassani, Hamid. Ohio State University; Estados Unidos Fil: Leroy, Adam K.. Max Planck Institute For Astronomy; Alemania Fil: Schinnerer, Eva. University of Alberta; Canadá Fil: Ostriker, Eve C.. Space Telescope Science Institute; Estados Unidos Fil: Wilson, Christine D.. University Of Wyoming; Estados Unidos Fil: Bolatto, Alberto D.. Space Telescope Science Institute; Estados Unidos Fil: Mills, Elisabeth A. C.. Space Telescope Science Institute; Estados Unidos Fil: Rosolowsky, Erik. Space Telescope Science Institute; Estados Unidos Fil: Lee, Janice C.. Space Telescope Science Institute; Estados Unidos Fil: Dale, Daniel A.. University of Wyoming; Estados Unidos Fil: Larson, Kirsten L.. Space Telescope Science Institute; Estados Unidos Fil: Thilker, David A.. University Johns Hopkins; Estados Unidos Fil: Ubeda, Leonardo. Space Telescope Science Institute; Estados Unidos Fil: Whitmore, Bradley C.. Space Telescope Science Institute; Estados Unidos Fil: Williams, Thomas G.. University of Oxford; Reino Unido Fil: Barnes, Ashley T.. European Southern Observatory; Alemania Fil: Bigiel, Frank. Universitat Bonn; Alemania Fil: Chevance, Mélanie. Ruprecht Karls Universitat Heidelberg; Alemania Fil: Glover, Simon C. O.. Ruprecht Karls Universitat Heidelberg; Alemania Fil: Neumann, Justus. Max-Planck-Institut für Astronomie; Alemania Fil: Pinna, Francesca. Max-Planck-Institut für Astronomie; Alemania. Universidad de La Laguna; España. Instituto de Astrofísica de Canarias; España Fil: Querejeta, Miguel. Universidad de Alcala. Observatorio Astronómico Nacional; España Fil: Sormani, Mattia C.. University of Surrey; Reino Unido Fil: Tress, Robin G.. Observatoire de Sauverny; Suiza |
| description |
We use 0.1 observations from the Atacama Large Millimeter Array (ALMA), Hubble Space Telescope (HST),and JWST to study young massive clusters (YMCs) in their embedded“infant” phase across the central starburstring in NGC 3351. Our new ALMA data reveal 18 bright and compact (sub-)millimeter continuum sources, ofwhich 8 have counterparts in JWST images and only 6 have counterparts in HST images. Based on the ALMAcontinuum and molecular line data, as well as ancillary measurements for the HST and JWST counterparts, weidentify 14 sources as infant star clusters with high stellar and/or gas masses (∼105 Me), small radii ( 5 pc), largeescape velocities (6–10 km s−1), and short freefall times (0.5–1 Myr). Their multiwavelength properties motivateus to divide them into four categories, likely corresponding to four evolutionary stages from starless clumps toexposed H II region–cluster complexes. Leveraging age estimates for HST-identi ed clusters in the same region,we infer an evolutionary timeline, ranging from∼1–2 Myr before cluster formation as starless clumps, to∼4–6 Myr after as exposed H II region–cluster complexes. Finally, we show that the YMCs make up a substantialfraction of recent star formation across the ring, exhibit a nonuniform azimuthal distribution without a verycoherent evolutionary trend along the ring, and are capable of driving large-scale gas out ows |
| publishDate |
2024 |
| dc.date.none.fl_str_mv |
2024-05 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
| format |
article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/276032 Sun, Jiayi; He, Hao; Batschkun, Kyle; Levy, Rebecca C.; Emig, Kimberly; et al.; Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351; IOP Publishing; Astrophysical Journal; 967; 2; 5-2024; 1-23 0004-637X CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/276032 |
| identifier_str_mv |
Sun, Jiayi; He, Hao; Batschkun, Kyle; Levy, Rebecca C.; Emig, Kimberly; et al.; Hidden Gems on a Ring: Infant Massive Clusters and Their Formation Timeline Unveiled by ALMA, HST, and JWST in NGC 3351; IOP Publishing; Astrophysical Journal; 967; 2; 5-2024; 1-23 0004-637X CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
| dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ad3de6 info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad3de6 |
| dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by/2.5/ar/ |
| eu_rights_str_mv |
openAccess |
| rights_invalid_str_mv |
https://creativecommons.org/licenses/by/2.5/ar/ |
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application/pdf application/pdf |
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IOP Publishing |
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IOP Publishing |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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13.127887 |