ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters

Autores: Galván Madrid, Roberto; Díaz González, Daniel J.; Motte, Frédérique; Ginsburg, Adam; Cunningham, Nichol; Menten, Karl M.; Armante, Mélanie; Castaingts, Mélisse; Braine, Jonathan; Csengeri, Timea; Dell'Ova, Pierre; Louvet, Fabien; Nony, Thomas; Rivera-Soto, Rudy; Sanhueza, Patricio; Stutz, Amelia M.; Wyrowski, Friedrich; Álvarez Gutiérrez, Rodrigo H.; Baug, Tapas; Bontemps, Sylvain; Bronfman, Leonardo; Fernandez Lopez, Manuel; Gusdorf, Antoine; Koley, Atanu; Liu, Hong Li; Salinas, Javiera; Towner, Allison P. M.; Whitworth, Anthony P.
Año de publicación: 2024
Idioma: inglés
Tipo de recurso: artículo
Estado: versión publicada
Descripción: We use the H41α recombination line to create templates of the millimeter free–free emission in the ALMA-IMF continuum maps, which allows us to separate it from dust emission. This method complements spectral-index information and extrapolation from centimeter-wavelength maps. We use the derived maps to estimate the properties of up to 34 H II regions across the ALMA-IMF protoclusters. The hydrogen ionizing photon rate Q 0 and spectral types follow the evolutionary trend proposed by Motte et al. The youngest protoclusters lack detectable ionized gas, followed by protoclusters with increasing numbers of OB stars. The total Q 0 increases from ∼1045 s‑1 to >1049 s‑1. We used the adjacent He41α line to measure the relative number abundances of helium, finding values consistent with the Galactic interstellar medium, although a few outliers are discussed. A search for sites of maser amplification of the H41α line returned negative results. We looked for possible correlations between the electron densities, emission measures, and Q 0 with H II region size D. The latter is the best correlated, with Q 0 ∝ D 2.49 ± 0.18. This favors interpretations in which smaller ultracompact H II regions are not necessarily the less dynamically evolved versions of larger ones but rather are ionized by less massive stars. Moderate correlations were found between the dynamical width ΔV dyn with D and Q 0. ΔV dyn increases from about 1 to 2 times the ionized-gas sound speed. Finally, an outlier H II region south of W43-MM2 is discussed. We suggest that this source could harbor an embedded stellar or disk wind.
Fil: Galván Madrid, Roberto. Universidad Nacional Autónoma de México; México
Fil: Díaz González, Daniel J.. Universidad Nacional Autónoma de México; México
Fil: Motte, Frédérique. Universite Grenoble Alpes; Francia
Fil: Ginsburg, Adam. University of Florida; Estados Unidos
Fil: Cunningham, Nichol. Universite Grenoble Alpes; Francia
Fil: Menten, Karl M.. Max Planck Institute for Radio Astronomy; Alemania
Fil: Armante, Mélanie. Ecole Normale Supérieure; Francia
Fil: Castaingts, Mélisse. University of Virginia; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Braine, Jonathan. Universite de Bordeaux; Francia
Fil: Csengeri, Timea. Universite de Bordeaux; Francia
Fil: Dell'Ova, Pierre. Ecole Normale Supérieure; Francia
Fil: Louvet, Fabien. Universite Grenoble Alpes; Francia
Fil: Nony, Thomas. Universidad Nacional Autónoma de México; México
Fil: Rivera-Soto, Rudy. Universidad Nacional Autónoma de México; México
Fil: Sanhueza, Patricio. National Astronomical Observatory of Japan; Japón
Fil: Stutz, Amelia M.. Universidad de Concepción; Chile
Fil: Wyrowski, Friedrich. Max Planck Institute for Radio Astronomy; Alemania
Fil: Álvarez Gutiérrez, Rodrigo H.. Universidad de Concepción; Chile
Fil: Baug, Tapas. S.N. Bose National Centre For Basic Sciences; India
Fil: Bontemps, Sylvain. Universite de Bordeaux; Francia
Fil: Bronfman, Leonardo. Universidad de Chile; Chile
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Gusdorf, Antoine. Ecole Normale Supérieure; Francia
Fil: Koley, Atanu. Universidad de Concepción; Chile
Fil: Liu, Hong Li. Universidad de Concepción; Chile
Fil: Salinas, Javiera. Universidad de Concepción; Chile
Fil: Towner, Allison P. M.. University of Arizona; Estados Unidos
Fil: Whitworth, Anthony P.. Cardiff University; Reino Unido
Materia: H II regions
Star forming regions
Nivel de accesibilidad: acceso abierto
Condiciones de uso: https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
Institución: Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador: oai:ri.conicet.gov.ar:11336/268645

Acceder

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network_name_str	CONICET Digital (CONICET)
spelling	ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive ProtoclustersGalván Madrid, RobertoDíaz González, Daniel J.Motte, FrédériqueGinsburg, AdamCunningham, NicholMenten, Karl M.Armante, MélanieCastaingts, MélisseBraine, JonathanCsengeri, TimeaDell'Ova, PierreLouvet, FabienNony, ThomasRivera-Soto, RudySanhueza, PatricioStutz, Amelia M.Wyrowski, FriedrichÁlvarez Gutiérrez, Rodrigo H.Baug, TapasBontemps, SylvainBronfman, LeonardoFernandez Lopez, ManuelGusdorf, AntoineKoley, AtanuLiu, Hong LiSalinas, JavieraTowner, Allison P. M.Whitworth, Anthony P.H II regionsStar forming regionshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We use the H41α recombination line to create templates of the millimeter free–free emission in the ALMA-IMF continuum maps, which allows us to separate it from dust emission. This method complements spectral-index information and extrapolation from centimeter-wavelength maps. We use the derived maps to estimate the properties of up to 34 H II regions across the ALMA-IMF protoclusters. The hydrogen ionizing photon rate Q 0 and spectral types follow the evolutionary trend proposed by Motte et al. The youngest protoclusters lack detectable ionized gas, followed by protoclusters with increasing numbers of OB stars. The total Q 0 increases from ∼1045 s‑1 to >1049 s‑1. We used the adjacent He41α line to measure the relative number abundances of helium, finding values consistent with the Galactic interstellar medium, although a few outliers are discussed. A search for sites of maser amplification of the H41α line returned negative results. We looked for possible correlations between the electron densities, emission measures, and Q 0 with H II region size D. The latter is the best correlated, with Q 0 ∝ D 2.49 ± 0.18. This favors interpretations in which smaller ultracompact H II regions are not necessarily the less dynamically evolved versions of larger ones but rather are ionized by less massive stars. Moderate correlations were found between the dynamical width ΔV dyn with D and Q 0. ΔV dyn increases from about 1 to 2 times the ionized-gas sound speed. Finally, an outlier H II region south of W43-MM2 is discussed. We suggest that this source could harbor an embedded stellar or disk wind.Fil: Galván Madrid, Roberto. Universidad Nacional Autónoma de México; MéxicoFil: Díaz González, Daniel J.. Universidad Nacional Autónoma de México; MéxicoFil: Motte, Frédérique. Universite Grenoble Alpes; FranciaFil: Ginsburg, Adam. University of Florida; Estados UnidosFil: Cunningham, Nichol. Universite Grenoble Alpes; FranciaFil: Menten, Karl M.. Max Planck Institute for Radio Astronomy; AlemaniaFil: Armante, Mélanie. Ecole Normale Supérieure; FranciaFil: Castaingts, Mélisse. University of Virginia; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Braine, Jonathan. Universite de Bordeaux; FranciaFil: Csengeri, Timea. Universite de Bordeaux; FranciaFil: Dell'Ova, Pierre. Ecole Normale Supérieure; FranciaFil: Louvet, Fabien. Universite Grenoble Alpes; FranciaFil: Nony, Thomas. Universidad Nacional Autónoma de México; MéxicoFil: Rivera-Soto, Rudy. Universidad Nacional Autónoma de México; MéxicoFil: Sanhueza, Patricio. National Astronomical Observatory of Japan; JapónFil: Stutz, Amelia M.. Universidad de Concepción; ChileFil: Wyrowski, Friedrich. Max Planck Institute for Radio Astronomy; AlemaniaFil: Álvarez Gutiérrez, Rodrigo H.. Universidad de Concepción; ChileFil: Baug, Tapas. S.N. Bose National Centre For Basic Sciences; IndiaFil: Bontemps, Sylvain. Universite de Bordeaux; FranciaFil: Bronfman, Leonardo. Universidad de Chile; ChileFil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Gusdorf, Antoine. Ecole Normale Supérieure; FranciaFil: Koley, Atanu. Universidad de Concepción; ChileFil: Liu, Hong Li. Universidad de Concepción; ChileFil: Salinas, Javiera. Universidad de Concepción; ChileFil: Towner, Allison P. M.. University of Arizona; Estados UnidosFil: Whitworth, Anthony P.. Cardiff University; Reino UnidoIOP Publishing2024-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/268645Galván Madrid, Roberto; Díaz González, Daniel J.; Motte, Frédérique; Ginsburg, Adam; Cunningham, Nichol; et al.; ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters; IOP Publishing; Astrophysical Journal Supplement Series; 274; 1; 9-2024; 1-230067-0049CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4365/ad61e6info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4365/ad61e6info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:52:52Zoai:ri.conicet.gov.ar:11336/268645instacron: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:34982025-09-29 09:52:53.042CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv	ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
title	ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
spellingShingle	ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters Galván Madrid, Roberto H II regions Star forming regions
title_short	ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
title_full	ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
title_fullStr	ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
title_full_unstemmed	ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
title_sort	ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters
dc.creator.none.fl_str_mv	Galván Madrid, Roberto Díaz González, Daniel J. Motte, Frédérique Ginsburg, Adam Cunningham, Nichol Menten, Karl M. Armante, Mélanie Castaingts, Mélisse Braine, Jonathan Csengeri, Timea Dell'Ova, Pierre Louvet, Fabien Nony, Thomas Rivera-Soto, Rudy Sanhueza, Patricio Stutz, Amelia M. Wyrowski, Friedrich Álvarez Gutiérrez, Rodrigo H. Baug, Tapas Bontemps, Sylvain Bronfman, Leonardo Fernandez Lopez, Manuel Gusdorf, Antoine Koley, Atanu Liu, Hong Li Salinas, Javiera Towner, Allison P. M. Whitworth, Anthony P.
author	Galván Madrid, Roberto
author_facet	Galván Madrid, Roberto Díaz González, Daniel J. Motte, Frédérique Ginsburg, Adam Cunningham, Nichol Menten, Karl M. Armante, Mélanie Castaingts, Mélisse Braine, Jonathan Csengeri, Timea Dell'Ova, Pierre Louvet, Fabien Nony, Thomas Rivera-Soto, Rudy Sanhueza, Patricio Stutz, Amelia M. Wyrowski, Friedrich Álvarez Gutiérrez, Rodrigo H. Baug, Tapas Bontemps, Sylvain Bronfman, Leonardo Fernandez Lopez, Manuel Gusdorf, Antoine Koley, Atanu Liu, Hong Li Salinas, Javiera Towner, Allison P. M. Whitworth, Anthony P.
author_role	author
author2	Díaz González, Daniel J. Motte, Frédérique Ginsburg, Adam Cunningham, Nichol Menten, Karl M. Armante, Mélanie Castaingts, Mélisse Braine, Jonathan Csengeri, Timea Dell'Ova, Pierre Louvet, Fabien Nony, Thomas Rivera-Soto, Rudy Sanhueza, Patricio Stutz, Amelia M. Wyrowski, Friedrich Álvarez Gutiérrez, Rodrigo H. Baug, Tapas Bontemps, Sylvain Bronfman, Leonardo Fernandez Lopez, Manuel Gusdorf, Antoine Koley, Atanu Liu, Hong Li Salinas, Javiera Towner, Allison P. M. Whitworth, Anthony P.
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	H II regions Star forming regions
topic	H II regions Star forming regions
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 the H41α recombination line to create templates of the millimeter free–free emission in the ALMA-IMF continuum maps, which allows us to separate it from dust emission. This method complements spectral-index information and extrapolation from centimeter-wavelength maps. We use the derived maps to estimate the properties of up to 34 H II regions across the ALMA-IMF protoclusters. The hydrogen ionizing photon rate Q 0 and spectral types follow the evolutionary trend proposed by Motte et al. The youngest protoclusters lack detectable ionized gas, followed by protoclusters with increasing numbers of OB stars. The total Q 0 increases from ∼1045 s‑1 to >1049 s‑1. We used the adjacent He41α line to measure the relative number abundances of helium, finding values consistent with the Galactic interstellar medium, although a few outliers are discussed. A search for sites of maser amplification of the H41α line returned negative results. We looked for possible correlations between the electron densities, emission measures, and Q 0 with H II region size D. The latter is the best correlated, with Q 0 ∝ D 2.49 ± 0.18. This favors interpretations in which smaller ultracompact H II regions are not necessarily the less dynamically evolved versions of larger ones but rather are ionized by less massive stars. Moderate correlations were found between the dynamical width ΔV dyn with D and Q 0. ΔV dyn increases from about 1 to 2 times the ionized-gas sound speed. Finally, an outlier H II region south of W43-MM2 is discussed. We suggest that this source could harbor an embedded stellar or disk wind. Fil: Galván Madrid, Roberto. Universidad Nacional Autónoma de México; México Fil: Díaz González, Daniel J.. Universidad Nacional Autónoma de México; México Fil: Motte, Frédérique. Universite Grenoble Alpes; Francia Fil: Ginsburg, Adam. University of Florida; Estados Unidos Fil: Cunningham, Nichol. Universite Grenoble Alpes; Francia Fil: Menten, Karl M.. Max Planck Institute for Radio Astronomy; Alemania Fil: Armante, Mélanie. Ecole Normale Supérieure; Francia Fil: Castaingts, Mélisse. University of Virginia; Estados Unidos. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina Fil: Braine, Jonathan. Universite de Bordeaux; Francia Fil: Csengeri, Timea. Universite de Bordeaux; Francia Fil: Dell'Ova, Pierre. Ecole Normale Supérieure; Francia Fil: Louvet, Fabien. Universite Grenoble Alpes; Francia Fil: Nony, Thomas. Universidad Nacional Autónoma de México; México Fil: Rivera-Soto, Rudy. Universidad Nacional Autónoma de México; México Fil: Sanhueza, Patricio. National Astronomical Observatory of Japan; Japón Fil: Stutz, Amelia M.. Universidad de Concepción; Chile Fil: Wyrowski, Friedrich. Max Planck Institute for Radio Astronomy; Alemania Fil: Álvarez Gutiérrez, Rodrigo H.. Universidad de Concepción; Chile Fil: Baug, Tapas. S.N. Bose National Centre For Basic Sciences; India Fil: Bontemps, Sylvain. Universite de Bordeaux; Francia Fil: Bronfman, Leonardo. Universidad de Chile; Chile Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina Fil: Gusdorf, Antoine. Ecole Normale Supérieure; Francia Fil: Koley, Atanu. Universidad de Concepción; Chile Fil: Liu, Hong Li. Universidad de Concepción; Chile Fil: Salinas, Javiera. Universidad de Concepción; Chile Fil: Towner, Allison P. M.. University of Arizona; Estados Unidos Fil: Whitworth, Anthony P.. Cardiff University; Reino Unido
description	We use the H41α recombination line to create templates of the millimeter free–free emission in the ALMA-IMF continuum maps, which allows us to separate it from dust emission. This method complements spectral-index information and extrapolation from centimeter-wavelength maps. We use the derived maps to estimate the properties of up to 34 H II regions across the ALMA-IMF protoclusters. The hydrogen ionizing photon rate Q 0 and spectral types follow the evolutionary trend proposed by Motte et al. The youngest protoclusters lack detectable ionized gas, followed by protoclusters with increasing numbers of OB stars. The total Q 0 increases from ∼1045 s‑1 to >1049 s‑1. We used the adjacent He41α line to measure the relative number abundances of helium, finding values consistent with the Galactic interstellar medium, although a few outliers are discussed. A search for sites of maser amplification of the H41α line returned negative results. We looked for possible correlations between the electron densities, emission measures, and Q 0 with H II region size D. The latter is the best correlated, with Q 0 ∝ D 2.49 ± 0.18. This favors interpretations in which smaller ultracompact H II regions are not necessarily the less dynamically evolved versions of larger ones but rather are ionized by less massive stars. Moderate correlations were found between the dynamical width ΔV dyn with D and Q 0. ΔV dyn increases from about 1 to 2 times the ionized-gas sound speed. Finally, an outlier H II region south of W43-MM2 is discussed. We suggest that this source could harbor an embedded stellar or disk wind.
publishDate	2024
dc.date.none.fl_str_mv	2024-09
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/11336/268645 Galván Madrid, Roberto; Díaz González, Daniel J.; Motte, Frédérique; Ginsburg, Adam; Cunningham, Nichol; et al.; ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters; IOP Publishing; Astrophysical Journal Supplement Series; 274; 1; 9-2024; 1-23 0067-0049 CONICET Digital CONICET
url	http://hdl.handle.net/11336/268645
identifier_str_mv	Galván Madrid, Roberto; Díaz González, Daniel J.; Motte, Frédérique; Ginsburg, Adam; Cunningham, Nichol; et al.; ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters; IOP Publishing; Astrophysical Journal Supplement Series; 274; 1; 9-2024; 1-23 0067-0049 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/10.3847/1538-4365/ad61e6 info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4365/ad61e6
dc.rights.none.fl_str_mv	info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv	openAccess
rights_invalid_str_mv	https://creativecommons.org/licenses/by-nc-sa/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
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score	13.070432

ALMA-IMF. XIV: Free–Free Templates Derived from H41α and Ionized Gas Content in 15 Massive Protoclusters

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