The Gas-Star Formation Cycle in Nearby Star-forming Galaxies. II. Resolved Distributions of CO and H α Emission for 49 PHANGS Galaxies

Hsi An Pan; Eva Schinnerer; Annie Hughes; Adam Leroy; Brent Groves; Ashley Thomas Barnes; Francesco Belfiore; Frank Bigiel; Guillermo A. Blanc; Yixian Cao; Mélanie Chevance; Enrico Congiu; Daniel A. Dale; Cosima Eibensteiner; Eric Emsellem; Christopher M. Faesi; Simon C.O. Glover; Kathryn Grasha; Cinthya N. Herrera; I. Ting Ho; Ralf S. Klessen; J. M.Diederik Kruijssen; Philipp Lang; Daizhong Liu; Rebecca McElroy; Sharon E. Meidt; Eric J. Murphy; Jérôme Pety; Miguel Querejeta; Alessandro Razza; Erik Rosolowsky; Toshiki Saito; Francesco Santoro; Andreas Schruba; Jiayi Sun; Neven Tomičić; Antonio Usero; Dyas Utomo; Thomas G. Williams

doi:10.3847/1538-4357/ac474f

The Gas-Star Formation Cycle in Nearby Star-forming Galaxies. II. Resolved Distributions of CO and H α Emission for 49 PHANGS Galaxies

Hsi An Pan
, Eva Schinnerer
, Annie Hughes
, Adam Leroy
, Brent Groves
, Ashley Thomas Barnes
, Francesco Belfiore
, Frank Bigiel
, Guillermo A. Blanc
, Yixian Cao
, Mélanie Chevance
, Enrico Congiu
, Daniel A. Dale
, Cosima Eibensteiner
, Eric Emsellem
, Christopher M. Faesi
, Simon C.O. Glover
, Kathryn Grasha
, Cinthya N. Herrera
, I. Ting Ho

Ralf S. Klessen, J. M.Diederik Kruijssen, Philipp Lang, Daizhong Liu, Rebecca McElroy, Sharon E. Meidt, Eric J. Murphy, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Erik Rosolowsky, Toshiki Saito, Francesco Santoro, Andreas Schruba, Jiayi Sun, Neven Tomičić, Antonio Usero, Dyas Utomo, Thomas G. Williams

Physics And Astronomy

Producción científica: Article › revisión exhaustiva

35 Citas (Scopus)

Resumen

The relative distribution of molecular gas and star formation in galaxies gives insight into the physical processes and timescales of the cycle between gas and stars. In this work, we track the relative spatial configuration of CO and Hα emission at high resolution in each of our galaxy targets and use these measurements to quantify the distributions of regions in different evolutionary stages of star formation: from molecular gas without star formation traced by Hα to star-forming gas, and to H ii regions. The large sample, drawn from the Physics at High Angular resolution in Nearby GalaxieS ALMA and narrowband Hα (PHANGS-ALMA and PHANGS-Hα) surveys, spans a wide range of stellar masses and morphological types, allowing us to investigate the dependencies of the gas-star formation cycle on global galaxy properties. At a resolution of 150 pc, the incidence of regions in different stages shows a dependence on stellar mass and Hubble type of galaxies over the radial range probed. Massive and/or earlier-type galaxies in our sample exhibit a significant reservoir of molecular gas without star formation traced by Hα, while lower-mass galaxies harbor substantial H ii regions that may have dispersed their birth clouds or formed from low-mass, more isolated clouds. Galactic structures add a further layer of complexity to the relative distribution of CO and Hα emission. Trends between galaxy properties and distributions of gas traced by CO and Hα are visible only when the observed spatial scale is ≪500 pc, reflecting the critical resolution requirement to distinguish stages of the star formation process.

Idioma original	English
Número de artículo	9
Publicación	Astrophysical Journal
Volumen	927
N.º	1
DOI	https://doi.org/10.3847/1538-4357/ac474f
Estado	Published - mar 1 2022

Nota bibliográfica

Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.

Financiación

The work of A.K.L., J.S., and D.U. is partially supported by the National Science Foundation under grants No. 1615105, 1615109, and 1653300. E.R. acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference number RGPIN-2017-03987. M.Q. acknowledges support from the research project PID2019-106027GA-C44 from the Spanish Ministerio de Ciencia e Innovación. A.B. and F.B. acknowledge funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 726384/Empire). E.S., P.L., D.L., R.Mc.E., T.S., F.S., and T.G.W. acknowledge funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 694343). H.A.P. acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 694343), and the Ministry of Science and Technology (MOST) of Taiwan under grant 110-2112-M-032-020-MY3. A.U. acknowledges support from the Spanish funding grants PGC2018-094671-B-I00 (MCIU/AEI/FEDER) and PID2019-108765GB-I00 (MICINN). M.C. gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG) through an Emmy Noether Research Group, grant No. KR4801/1-1 and the DFG Sachbeihilfe, grant No. KR4801/2-1, and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program via the ERC Starting Grant MUSTANG (grant agreement No. 714907). J.M.D.K. gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG) in the form of an Emmy Noether Research Group (grant No. KR4801/1-1) and the DFG Sachbeihilfe (grant No. KR4801/2-1), and from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program via the ERC Starting Grant MUSTANG (grant agreement No. 714907). A.H. was supported by the Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES, and by the Programme National “Physique et Chimie du Milieu Interstellaire” (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES. J.P. acknowledges support from the Programme National “Physique et Chimie du Milieu Interstellaire” (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES. C.E. acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG) Sachbeihilfe, grant No. BI1546/3-1. S.C.O.G. and R.S.K. acknowledge financial support from the German Research Foundation (DFG) via the collaborative research center (SFB 881, Project-ID 138713538) “The Milky Way System” (subprojects A1, B1, B2, and B8). They also acknowledge funding from the Heidelberg Cluster of Excellence “STRUCTURES” in the framework of Germany's Excellence Strategy (grant EXC-2181/1, Project-ID 390900948) and from the European Research Council via the ERC Synergy Grant “ECOGAL” (grant 855130). C.M.F. is supported by the National Science Foundation under award No. 1903946 and acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 694343). E.C. acknowledges support from ANID project Basal AFB-170002.

Financiadores	Número del financiador
ANID Fondecyt	AFB-170002
DFG Sachbeihilfe	KR4801/2-1
German Excellence Strategy in the Heidelberg Cluster of Excellence STRUCTURES	EXC-2181/1, 390900948
INSU
CNRS Programme National Physique Chimie du Milieu Interstellaire
Spanish Ministerio de Ciencia e innovación
National Science Foundation Arctic Social Science Program	1903946, 1615109, 1653300, 1615105
Horizon 2020 Framework Programme	694343, 714907, 855130, 726384/Empire
Ministerio de Ciencia, Innovación y Universidades
Natural Sciences and Engineering Research Council of Canada	RGPIN-2017-03987
H2020 European Research Council
Deutsche Forschungsgemeinschaft	138713538, BI1546/3-1, KR4801/1-1
Centre National d’Etudes Spatiales
Ministry of Science and Technology, Taiwan	110-2112-M-032-020-MY3
CNRS Centre National de la Recherche Scientifique
Commissariat à l'Énergie Atomique et aux Énergies Alternatives
European Regional Development Fund	PID2019-108765GB-I00
Agencia Estatal de Investigación
Institut national de physique nucléaire et de physique des particules

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.3847/1538-4357/ac474f

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Pan, H. A., Schinnerer, E., Hughes, A., Leroy, A., Groves, B., Barnes, A. T., Belfiore, F., Bigiel, F., Blanc, G. A., Cao, Y., Chevance, M., Congiu, E., Dale, D. A., Eibensteiner, C., Emsellem, E., Faesi, C. M., Glover, S. C. O., Grasha, K., Herrera, C. N., ... Williams, T. G. (2022). The Gas-Star Formation Cycle in Nearby Star-forming Galaxies. II. Resolved Distributions of CO and H α Emission for 49 PHANGS Galaxies. Astrophysical Journal, 927(1), Artículo 9. https://doi.org/10.3847/1538-4357/ac474f

@article{d82c159a6b9d436da3d1137caffc366a,

title = "The Gas-Star Formation Cycle in Nearby Star-forming Galaxies. II. Resolved Distributions of CO and H α Emission for 49 PHANGS Galaxies",

abstract = "The relative distribution of molecular gas and star formation in galaxies gives insight into the physical processes and timescales of the cycle between gas and stars. In this work, we track the relative spatial configuration of CO and Hα emission at high resolution in each of our galaxy targets and use these measurements to quantify the distributions of regions in different evolutionary stages of star formation: from molecular gas without star formation traced by Hα to star-forming gas, and to H ii regions. The large sample, drawn from the Physics at High Angular resolution in Nearby GalaxieS ALMA and narrowband Hα (PHANGS-ALMA and PHANGS-Hα) surveys, spans a wide range of stellar masses and morphological types, allowing us to investigate the dependencies of the gas-star formation cycle on global galaxy properties. At a resolution of 150 pc, the incidence of regions in different stages shows a dependence on stellar mass and Hubble type of galaxies over the radial range probed. Massive and/or earlier-type galaxies in our sample exhibit a significant reservoir of molecular gas without star formation traced by Hα, while lower-mass galaxies harbor substantial H ii regions that may have dispersed their birth clouds or formed from low-mass, more isolated clouds. Galactic structures add a further layer of complexity to the relative distribution of CO and Hα emission. Trends between galaxy properties and distributions of gas traced by CO and Hα are visible only when the observed spatial scale is ≪500 pc, reflecting the critical resolution requirement to distinguish stages of the star formation process.",

author = "Pan, \{Hsi An\} and Eva Schinnerer and Annie Hughes and Adam Leroy and Brent Groves and Barnes, \{Ashley Thomas\} and Francesco Belfiore and Frank Bigiel and Blanc, \{Guillermo A.\} and Yixian Cao and M{\'e}lanie Chevance and Enrico Congiu and Dale, \{Daniel A.\} and Cosima Eibensteiner and Eric Emsellem and Faesi, \{Christopher M.\} and Glover, \{Simon C.O.\} and Kathryn Grasha and Herrera, \{Cinthya N.\} and Ho, \{I. Ting\} and Klessen, \{Ralf S.\} and Kruijssen, \{J. M.Diederik\} and Philipp Lang and Daizhong Liu and Rebecca McElroy and Meidt, \{Sharon E.\} and Murphy, \{Eric J.\} and J{\'e}r{\^o}me Pety and Miguel Querejeta and Alessandro Razza and Erik Rosolowsky and Toshiki Saito and Francesco Santoro and Andreas Schruba and Jiayi Sun and Neven Tomi{\v c}i{\'c} and Antonio Usero and Dyas Utomo and Williams, \{Thomas G.\}",

note = "Publisher Copyright: {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society.",

year = "2022",

month = mar,

day = "1",

doi = "10.3847/1538-4357/ac474f",

language = "English",

volume = "927",

number = "1",

}

Pan, HA, Schinnerer, E, Hughes, A, Leroy, A, Groves, B, Barnes, AT, Belfiore, F, Bigiel, F, Blanc, GA, Cao, Y, Chevance, M, Congiu, E, Dale, DA, Eibensteiner, C, Emsellem, E, Faesi, CM, Glover, SCO, Grasha, K, Herrera, CN, Ho, IT, Klessen, RS, Kruijssen, JMD, Lang, P, Liu, D, McElroy, R, Meidt, SE, Murphy, EJ, Pety, J, Querejeta, M, Razza, A, Rosolowsky, E, Saito, T, Santoro, F, Schruba, A, Sun, J, Tomičić, N, Usero, A, Utomo, D & Williams, TG 2022, 'The Gas-Star Formation Cycle in Nearby Star-forming Galaxies. II. Resolved Distributions of CO and H α Emission for 49 PHANGS Galaxies', Astrophysical Journal, vol. 927, n.º 1, 9. https://doi.org/10.3847/1538-4357/ac474f

TY - JOUR

T1 - The Gas-Star Formation Cycle in Nearby Star-forming Galaxies. II. Resolved Distributions of CO and H α Emission for 49 PHANGS Galaxies

AU - Pan, Hsi An

AU - Schinnerer, Eva

AU - Hughes, Annie

AU - Leroy, Adam

AU - Groves, Brent

AU - Barnes, Ashley Thomas

AU - Belfiore, Francesco

AU - Bigiel, Frank

AU - Blanc, Guillermo A.

AU - Cao, Yixian

AU - Chevance, Mélanie

AU - Congiu, Enrico

AU - Dale, Daniel A.

AU - Eibensteiner, Cosima

AU - Emsellem, Eric

AU - Faesi, Christopher M.

AU - Glover, Simon C.O.

AU - Grasha, Kathryn

AU - Herrera, Cinthya N.

AU - Ho, I. Ting

AU - Klessen, Ralf S.

AU - Kruijssen, J. M.Diederik

AU - Lang, Philipp

AU - Liu, Daizhong

AU - McElroy, Rebecca

AU - Meidt, Sharon E.

AU - Murphy, Eric J.

AU - Pety, Jérôme

AU - Querejeta, Miguel

AU - Razza, Alessandro

AU - Rosolowsky, Erik

AU - Saito, Toshiki

AU - Santoro, Francesco

AU - Schruba, Andreas

AU - Sun, Jiayi

AU - Tomičić, Neven

AU - Usero, Antonio

AU - Utomo, Dyas

AU - Williams, Thomas G.

PY - 2022/3/1

Y1 - 2022/3/1

N2 - The relative distribution of molecular gas and star formation in galaxies gives insight into the physical processes and timescales of the cycle between gas and stars. In this work, we track the relative spatial configuration of CO and Hα emission at high resolution in each of our galaxy targets and use these measurements to quantify the distributions of regions in different evolutionary stages of star formation: from molecular gas without star formation traced by Hα to star-forming gas, and to H ii regions. The large sample, drawn from the Physics at High Angular resolution in Nearby GalaxieS ALMA and narrowband Hα (PHANGS-ALMA and PHANGS-Hα) surveys, spans a wide range of stellar masses and morphological types, allowing us to investigate the dependencies of the gas-star formation cycle on global galaxy properties. At a resolution of 150 pc, the incidence of regions in different stages shows a dependence on stellar mass and Hubble type of galaxies over the radial range probed. Massive and/or earlier-type galaxies in our sample exhibit a significant reservoir of molecular gas without star formation traced by Hα, while lower-mass galaxies harbor substantial H ii regions that may have dispersed their birth clouds or formed from low-mass, more isolated clouds. Galactic structures add a further layer of complexity to the relative distribution of CO and Hα emission. Trends between galaxy properties and distributions of gas traced by CO and Hα are visible only when the observed spatial scale is ≪500 pc, reflecting the critical resolution requirement to distinguish stages of the star formation process.

AB - The relative distribution of molecular gas and star formation in galaxies gives insight into the physical processes and timescales of the cycle between gas and stars. In this work, we track the relative spatial configuration of CO and Hα emission at high resolution in each of our galaxy targets and use these measurements to quantify the distributions of regions in different evolutionary stages of star formation: from molecular gas without star formation traced by Hα to star-forming gas, and to H ii regions. The large sample, drawn from the Physics at High Angular resolution in Nearby GalaxieS ALMA and narrowband Hα (PHANGS-ALMA and PHANGS-Hα) surveys, spans a wide range of stellar masses and morphological types, allowing us to investigate the dependencies of the gas-star formation cycle on global galaxy properties. At a resolution of 150 pc, the incidence of regions in different stages shows a dependence on stellar mass and Hubble type of galaxies over the radial range probed. Massive and/or earlier-type galaxies in our sample exhibit a significant reservoir of molecular gas without star formation traced by Hα, while lower-mass galaxies harbor substantial H ii regions that may have dispersed their birth clouds or formed from low-mass, more isolated clouds. Galactic structures add a further layer of complexity to the relative distribution of CO and Hα emission. Trends between galaxy properties and distributions of gas traced by CO and Hα are visible only when the observed spatial scale is ≪500 pc, reflecting the critical resolution requirement to distinguish stages of the star formation process.

UR - https://www.scopus.com/pages/publications/85126298452

UR - https://www.scopus.com/pages/publications/85126298452#tab=citedBy

U2 - 10.3847/1538-4357/ac474f

DO - 10.3847/1538-4357/ac474f

M3 - Article

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SN - 0004-637X

VL - 927

JO - Astrophysical Journal

JF - Astrophysical Journal

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The Gas-Star Formation Cycle in Nearby Star-forming Galaxies. II. Resolved Distributions of CO and H α Emission for 49 PHANGS Galaxies

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