Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr
- Autores
- Whitmore, Bradley C.; Chandar, Rupali; Lee, Janice C.; Henny, Kiana F.; Rodriguez, Maria Jimena; Baron, Dalya; Bigiel, F.; Boquien, Médéric; Chevance, Mélanie; Chown, Ryan; Dale, Daniel A.; Floyd, Matthew; Grasha, Kathryn; Glover, Simon C. O.; Gnedin, Oleg; Hassani, Hamid; Indebetouw, Remy; Kapoor, Anand Utsav; Larson, Kirsten L.; Leroy, Adam K.; Maschmann, Daniel; Scheuermann, Fabian; Sutter, Jessica; Schinnerer, Eva; Sarbadhicary, Sumit K.; Thilker, David A.; Williams, Thomas G.; Wofford, Aida
- Año de publicación
- 2025
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- JWST observations, when combined with Hubble Space Telescope (HST) data, promise to improve age estimates of star clusters in nearby spiral galaxies. However, feedback from young cluster stars pushes out the natal gas and dust, making cluster formation and evolution a challenge to model. Here, we use JWST+ HST observations of the nearby spiral galaxy NGC 628 to produce spectral energy distribution (SED) templates of compact star clusters spanning 275 nm through 21 μm. These preliminary SEDs capture the cluster stars and associated gas and dust within radii of ≍0 12─0 67 (corresponding to ≍6─33 pc at the distance of NGC 628). One important finding is that the SEDs of 1, 2, 3, and 4 Myr clusters can be differentiated in the infrared. Another is that, in 80%─90% of the cases we study, the polycyclic aromatic hydrocarbon (PAH) and Hα emission track one another, with the dust responsible for the 3.3 μm PAH emission largely removed by 4 Myr, consistent with pre-supernova stellar feedback acting quickly on the surrounding gas and dust. Nearly embedded cluster candidates have infrared SEDs that are quite similar to optically visible 1─3 Myr clusters. In nearly all cases, we find there is a young star cluster within a few tenths of an arcsec (10─30 pc) of the nearly embedded cluster, suggesting the formation of the cluster was triggered by its presence. The resulting age estimates from the empirical templates are compatible both with dynamical estimates based on CO superbubble expansion velocities, as well as the TODDLERS models, which track spherical evolution of homogeneous gas clouds around young stellar clusters.
Fil: Whitmore, Bradley C.. Space Telescope Science Institute; Estados Unidos
Fil: Chandar, Rupali. The University Of Toledo; España
Fil: Lee, Janice C.. Space Telescope Science Institute; Estados Unidos
Fil: Henny, Kiana F.. University Of Wyoming; Estados Unidos
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: Baron, Dalya. No especifíca;
Fil: Bigiel, F.. Universitat Bonn; Alemania
Fil: Boquien, Médéric. Université Côte D'azur; Francia
Fil: Chevance, Mélanie. Ruprecht Karls Universitat Heidelberg; Alemania
Fil: Chown, Ryan. Ohio University; Estados Unidos
Fil: Dale, Daniel A.. University Of Wyoming; Estados Unidos
Fil: Floyd, Matthew. University Of Toledo (utoledo); Estados Unidos
Fil: Grasha, Kathryn. Australian National University; Australia
Fil: Glover, Simon C. O.. Ruprecht Karls Universitat Heidelberg; Alemania
Fil: Gnedin, Oleg. University of Michigan; Estados Unidos
Fil: Hassani, Hamid. University of Alberta; Canadá
Fil: Indebetouw, Remy. University of Virginia; Estados Unidos
Fil: Kapoor, Anand Utsav. Universiteit Gent; Bélgica
Fil: Larson, Kirsten L.. Space Telescope Science Institute; Estados Unidos
Fil: Leroy, Adam K.. Ohio University; Estados Unidos
Fil: Maschmann, Daniel. Arizona State University; Estados Unidos
Fil: Scheuermann, Fabian. University of California; Estados Unidos
Fil: Sutter, Jessica. University of California; Estados Unidos
Fil: Schinnerer, Eva. Max Planck Institut für Astronomie; Alemania
Fil: Sarbadhicary, Sumit K.. Ohio State University; Estados Unidos
Fil: Thilker, David A.. University Johns Hopkins; Estados Unidos
Fil: Williams, Thomas G.. University of Oxford; Reino Unido
Fil: Wofford, Aida. Universidad Nacional Autónoma de México; México - Materia
-
Young star clusters
Spiral galaxies
Spectral energy distribution
HST photometry - 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:11336/290779
Ver los metadatos del registro completo
| id |
CONICETDig_d3402922b05a84abe14748005dc911b1 |
|---|---|
| oai_identifier_str |
oai:ri.conicet.gov.ar:11336/290779 |
| network_acronym_str |
CONICETDig |
| repository_id_str |
3498 |
| network_name_str |
CONICET Digital (CONICET) |
| spelling |
Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 MyrWhitmore, Bradley C.Chandar, RupaliLee, Janice C.Henny, Kiana F.Rodriguez, Maria JimenaBaron, DalyaBigiel, F.Boquien, MédéricChevance, MélanieChown, RyanDale, Daniel A.Floyd, MatthewGrasha, KathrynGlover, Simon C. O.Gnedin, OlegHassani, HamidIndebetouw, RemyKapoor, Anand UtsavLarson, Kirsten L.Leroy, Adam K.Maschmann, DanielScheuermann, FabianSutter, JessicaSchinnerer, EvaSarbadhicary, Sumit K.Thilker, David A.Williams, Thomas G.Wofford, AidaYoung star clustersSpiral galaxiesSpectral energy distributionHST photometryhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1JWST observations, when combined with Hubble Space Telescope (HST) data, promise to improve age estimates of star clusters in nearby spiral galaxies. However, feedback from young cluster stars pushes out the natal gas and dust, making cluster formation and evolution a challenge to model. Here, we use JWST+ HST observations of the nearby spiral galaxy NGC 628 to produce spectral energy distribution (SED) templates of compact star clusters spanning 275 nm through 21 μm. These preliminary SEDs capture the cluster stars and associated gas and dust within radii of ≍0 12─0 67 (corresponding to ≍6─33 pc at the distance of NGC 628). One important finding is that the SEDs of 1, 2, 3, and 4 Myr clusters can be differentiated in the infrared. Another is that, in 80%─90% of the cases we study, the polycyclic aromatic hydrocarbon (PAH) and Hα emission track one another, with the dust responsible for the 3.3 μm PAH emission largely removed by 4 Myr, consistent with pre-supernova stellar feedback acting quickly on the surrounding gas and dust. Nearly embedded cluster candidates have infrared SEDs that are quite similar to optically visible 1─3 Myr clusters. In nearly all cases, we find there is a young star cluster within a few tenths of an arcsec (10─30 pc) of the nearly embedded cluster, suggesting the formation of the cluster was triggered by its presence. The resulting age estimates from the empirical templates are compatible both with dynamical estimates based on CO superbubble expansion velocities, as well as the TODDLERS models, which track spherical evolution of homogeneous gas clouds around young stellar clusters.Fil: Whitmore, Bradley C.. Space Telescope Science Institute; Estados UnidosFil: Chandar, Rupali. The University Of Toledo; EspañaFil: Lee, Janice C.. Space Telescope Science Institute; Estados UnidosFil: Henny, Kiana F.. University Of Wyoming; Estados UnidosFil: 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: Baron, Dalya. No especifíca;Fil: Bigiel, F.. Universitat Bonn; AlemaniaFil: Boquien, Médéric. Université Côte D'azur; FranciaFil: Chevance, Mélanie. Ruprecht Karls Universitat Heidelberg; AlemaniaFil: Chown, Ryan. Ohio University; Estados UnidosFil: Dale, Daniel A.. University Of Wyoming; Estados UnidosFil: Floyd, Matthew. University Of Toledo (utoledo); Estados UnidosFil: Grasha, Kathryn. Australian National University; AustraliaFil: Glover, Simon C. O.. Ruprecht Karls Universitat Heidelberg; AlemaniaFil: Gnedin, Oleg. University of Michigan; Estados UnidosFil: Hassani, Hamid. University of Alberta; CanadáFil: Indebetouw, Remy. University of Virginia; Estados UnidosFil: Kapoor, Anand Utsav. Universiteit Gent; BélgicaFil: Larson, Kirsten L.. Space Telescope Science Institute; Estados UnidosFil: Leroy, Adam K.. Ohio University; Estados UnidosFil: Maschmann, Daniel. Arizona State University; Estados UnidosFil: Scheuermann, Fabian. University of California; Estados UnidosFil: Sutter, Jessica. University of California; Estados UnidosFil: Schinnerer, Eva. Max Planck Institut für Astronomie; AlemaniaFil: Sarbadhicary, Sumit K.. Ohio State University; Estados UnidosFil: Thilker, David A.. University Johns Hopkins; Estados UnidosFil: Williams, Thomas G.. University of Oxford; Reino UnidoFil: Wofford, Aida. Universidad Nacional Autónoma de México; MéxicoIOP Publishing2025-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/290779Whitmore, Bradley C.; Chandar, Rupali; Lee, Janice C.; Henny, Kiana F.; Rodriguez, Maria Jimena; et al.; Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr; IOP Publishing; Astrophysical Journal; 982; 1; 3-2025; 1-290004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/adb3a2info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/adb3a2info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-08-25T14:49:06Zoai:ri.conicet.gov.ar:11336/290779instacron: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:34982026-08-25 14:49:07.563CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr |
| title |
Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr |
| spellingShingle |
Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr Whitmore, Bradley C. Young star clusters Spiral galaxies Spectral energy distribution HST photometry |
| title_short |
Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr |
| title_full |
Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr |
| title_fullStr |
Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr |
| title_full_unstemmed |
Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr |
| title_sort |
Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr |
| dc.creator.none.fl_str_mv |
Whitmore, Bradley C. Chandar, Rupali Lee, Janice C. Henny, Kiana F. Rodriguez, Maria Jimena Baron, Dalya Bigiel, F. Boquien, Médéric Chevance, Mélanie Chown, Ryan Dale, Daniel A. Floyd, Matthew Grasha, Kathryn Glover, Simon C. O. Gnedin, Oleg Hassani, Hamid Indebetouw, Remy Kapoor, Anand Utsav Larson, Kirsten L. Leroy, Adam K. Maschmann, Daniel Scheuermann, Fabian Sutter, Jessica Schinnerer, Eva Sarbadhicary, Sumit K. Thilker, David A. Williams, Thomas G. Wofford, Aida |
| author |
Whitmore, Bradley C. |
| author_facet |
Whitmore, Bradley C. Chandar, Rupali Lee, Janice C. Henny, Kiana F. Rodriguez, Maria Jimena Baron, Dalya Bigiel, F. Boquien, Médéric Chevance, Mélanie Chown, Ryan Dale, Daniel A. Floyd, Matthew Grasha, Kathryn Glover, Simon C. O. Gnedin, Oleg Hassani, Hamid Indebetouw, Remy Kapoor, Anand Utsav Larson, Kirsten L. Leroy, Adam K. Maschmann, Daniel Scheuermann, Fabian Sutter, Jessica Schinnerer, Eva Sarbadhicary, Sumit K. Thilker, David A. Williams, Thomas G. Wofford, Aida |
| author_role |
author |
| author2 |
Chandar, Rupali Lee, Janice C. Henny, Kiana F. Rodriguez, Maria Jimena Baron, Dalya Bigiel, F. Boquien, Médéric Chevance, Mélanie Chown, Ryan Dale, Daniel A. Floyd, Matthew Grasha, Kathryn Glover, Simon C. O. Gnedin, Oleg Hassani, Hamid Indebetouw, Remy Kapoor, Anand Utsav Larson, Kirsten L. Leroy, Adam K. Maschmann, Daniel Scheuermann, Fabian Sutter, Jessica Schinnerer, Eva Sarbadhicary, Sumit K. Thilker, David A. Williams, Thomas G. Wofford, Aida |
| 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 |
| dc.subject.none.fl_str_mv |
Young star clusters Spiral galaxies Spectral energy distribution HST photometry |
| topic |
Young star clusters Spiral galaxies Spectral energy distribution HST photometry |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
JWST observations, when combined with Hubble Space Telescope (HST) data, promise to improve age estimates of star clusters in nearby spiral galaxies. However, feedback from young cluster stars pushes out the natal gas and dust, making cluster formation and evolution a challenge to model. Here, we use JWST+ HST observations of the nearby spiral galaxy NGC 628 to produce spectral energy distribution (SED) templates of compact star clusters spanning 275 nm through 21 μm. These preliminary SEDs capture the cluster stars and associated gas and dust within radii of ≍0 12─0 67 (corresponding to ≍6─33 pc at the distance of NGC 628). One important finding is that the SEDs of 1, 2, 3, and 4 Myr clusters can be differentiated in the infrared. Another is that, in 80%─90% of the cases we study, the polycyclic aromatic hydrocarbon (PAH) and Hα emission track one another, with the dust responsible for the 3.3 μm PAH emission largely removed by 4 Myr, consistent with pre-supernova stellar feedback acting quickly on the surrounding gas and dust. Nearly embedded cluster candidates have infrared SEDs that are quite similar to optically visible 1─3 Myr clusters. In nearly all cases, we find there is a young star cluster within a few tenths of an arcsec (10─30 pc) of the nearly embedded cluster, suggesting the formation of the cluster was triggered by its presence. The resulting age estimates from the empirical templates are compatible both with dynamical estimates based on CO superbubble expansion velocities, as well as the TODDLERS models, which track spherical evolution of homogeneous gas clouds around young stellar clusters. Fil: Whitmore, Bradley C.. Space Telescope Science Institute; Estados Unidos Fil: Chandar, Rupali. The University Of Toledo; España Fil: Lee, Janice C.. Space Telescope Science Institute; Estados Unidos Fil: Henny, Kiana F.. University Of Wyoming; Estados Unidos 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: Baron, Dalya. No especifíca; Fil: Bigiel, F.. Universitat Bonn; Alemania Fil: Boquien, Médéric. Université Côte D'azur; Francia Fil: Chevance, Mélanie. Ruprecht Karls Universitat Heidelberg; Alemania Fil: Chown, Ryan. Ohio University; Estados Unidos Fil: Dale, Daniel A.. University Of Wyoming; Estados Unidos Fil: Floyd, Matthew. University Of Toledo (utoledo); Estados Unidos Fil: Grasha, Kathryn. Australian National University; Australia Fil: Glover, Simon C. O.. Ruprecht Karls Universitat Heidelberg; Alemania Fil: Gnedin, Oleg. University of Michigan; Estados Unidos Fil: Hassani, Hamid. University of Alberta; Canadá Fil: Indebetouw, Remy. University of Virginia; Estados Unidos Fil: Kapoor, Anand Utsav. Universiteit Gent; Bélgica Fil: Larson, Kirsten L.. Space Telescope Science Institute; Estados Unidos Fil: Leroy, Adam K.. Ohio University; Estados Unidos Fil: Maschmann, Daniel. Arizona State University; Estados Unidos Fil: Scheuermann, Fabian. University of California; Estados Unidos Fil: Sutter, Jessica. University of California; Estados Unidos Fil: Schinnerer, Eva. Max Planck Institut für Astronomie; Alemania Fil: Sarbadhicary, Sumit K.. Ohio State University; Estados Unidos Fil: Thilker, David A.. University Johns Hopkins; Estados Unidos Fil: Williams, Thomas G.. University of Oxford; Reino Unido Fil: Wofford, Aida. Universidad Nacional Autónoma de México; México |
| description |
JWST observations, when combined with Hubble Space Telescope (HST) data, promise to improve age estimates of star clusters in nearby spiral galaxies. However, feedback from young cluster stars pushes out the natal gas and dust, making cluster formation and evolution a challenge to model. Here, we use JWST+ HST observations of the nearby spiral galaxy NGC 628 to produce spectral energy distribution (SED) templates of compact star clusters spanning 275 nm through 21 μm. These preliminary SEDs capture the cluster stars and associated gas and dust within radii of ≍0 12─0 67 (corresponding to ≍6─33 pc at the distance of NGC 628). One important finding is that the SEDs of 1, 2, 3, and 4 Myr clusters can be differentiated in the infrared. Another is that, in 80%─90% of the cases we study, the polycyclic aromatic hydrocarbon (PAH) and Hα emission track one another, with the dust responsible for the 3.3 μm PAH emission largely removed by 4 Myr, consistent with pre-supernova stellar feedback acting quickly on the surrounding gas and dust. Nearly embedded cluster candidates have infrared SEDs that are quite similar to optically visible 1─3 Myr clusters. In nearly all cases, we find there is a young star cluster within a few tenths of an arcsec (10─30 pc) of the nearly embedded cluster, suggesting the formation of the cluster was triggered by its presence. The resulting age estimates from the empirical templates are compatible both with dynamical estimates based on CO superbubble expansion velocities, as well as the TODDLERS models, which track spherical evolution of homogeneous gas clouds around young stellar clusters. |
| publishDate |
2025 |
| dc.date.none.fl_str_mv |
2025-03 |
| 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/11336/290779 Whitmore, Bradley C.; Chandar, Rupali; Lee, Janice C.; Henny, Kiana F.; Rodriguez, Maria Jimena; et al.; Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr; IOP Publishing; Astrophysical Journal; 982; 1; 3-2025; 1-29 0004-637X CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/290779 |
| identifier_str_mv |
Whitmore, Bradley C.; Chandar, Rupali; Lee, Janice C.; Henny, Kiana F.; Rodriguez, Maria Jimena; et al.; Empirical SED Templates for Star Clusters Observed with HST and JWST: No Strong PAH or IR Dust Emission after 5 Myr; IOP Publishing; Astrophysical Journal; 982; 1; 3-2025; 1-29 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/adb3a2 info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/adb3a2 |
| 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/ |
| dc.format.none.fl_str_mv |
application/pdf application/pdf |
| dc.publisher.none.fl_str_mv |
IOP Publishing |
| publisher.none.fl_str_mv |
IOP Publishing |
| dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
| reponame_str |
CONICET Digital (CONICET) |
| collection |
CONICET Digital (CONICET) |
| instname_str |
Consejo Nacional de Investigaciones Científicas y Técnicas |
| repository.name.fl_str_mv |
CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
| repository.mail.fl_str_mv |
dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
| _version_ |
1874774720428113920 |
| score |
13.24418 |