Imprints of galaxy evolution on H II regions: memory of the past uncovered by the CALIFA survey

S. F. Sánchez, E. Pérez, F. F. Rosales-Ortega, D. Miralles-Caballero, A. R. López-Sánchez, J. Iglesias-Páramo, R. A. Marino, L. Sánchez-Menguiano, R. García-Benito, D. Mast, M. A. Mendoza, P. Papaderos, S. Ellis, L. Galbany, C. Kehrig, A. Monreal-Ibero, R. González Delgado, M. Mollá, B. Ziegler, A. De Lorenzo-Cáceres & 10 others J. Mendez-Abreu, J. Bland-Hawthorn, S. Bekeraitė, M. M. Roth, A. Pasquali, A. Díaz, D. Bomans, G. Van De Ven, L. Wisotzki, CALIFA collaboration

Research output: Contribution to journalArticleResearchpeer-review

Abstract

Context. H II regions in galaxies are the sites of star formation, so they are special places for understanding the build-up of stellar mass in the universe. The line ratios of this ionized gas are frequently used to characterize the ionization conditions. In particular, the oxygen abundances are assumed to trace the chemical enrichment of galaxies. Aims. We explore the connections between the ionization conditions and the properties of the overall underlying stellar population (ionizing or not-ionizing) in H II regions, in order to uncover the actual physical connection between them. Methods. We use the H II regions catalog from the CALIFA survey, which is the largest in existence with more than 5000 H II regions, to explore their distribution across the classical [O III] λ5007/Hβ vs. [N II] λ6583/α diagnostic diagram, and the way it depends on the oxygen abundance, ionization parameter, electron density, and dust attenuation. The location of H II regions within this diagram is compared with predictions from photoionization models. Finally, we explore the dependence of the location within the diagnostic diagram on the properties of the host galaxies, the galactocentric distances, and the properties of the underlying stellar population. Results. The H II regions with weaker ionization strengths and more metal-rich are located in the bottom righthand area of the diagram. In contrast, those regions with stronger ionization strengths and more metal poor are located in the upper lefthand end of the diagram. Photoionization models per se do not predict these correlations between the parameters and the line ratios. The H II regions located in earlier-type galaxies, closer to the center and formed in older and more metal-rich regions of the galaxies are located in the bottom-right area of the diagram. On the other hand, those regions located in late-type galaxies in the outer regions of the disks and formed on younger and more metal-poor regions lie in the top lefthand area of the diagram. The two explored line ratios show strong correlations with the age and metallicity of the underlying stellar population. Conclusions. These results indicate that although H II regions are short-lived events, they are aff ected by the total underlying stellar population. One may say that H II regions keep a memory of the stellar evolution and chemical enrichment that have left an imprint on both the ionizing stellar population and the ionized gas.

LanguageEnglish
Article numberA47
Pages1-17
Number of pages17
JournalAstronomy and Astrophysics
Volume574
DOIs
Publication statusPublished - 1 Jan 2015

Fingerprint

H II regions
galaxies
diagrams
diagram
ionization
ionized gases
metals
photoionization
metal
stellar evolution
oxygen
stellar mass
metallicity
catalogs
star formation
universe
dust
attenuation
gas
electron density

Bibliographical note

Copyright 2015 ESO. First published in Astronomy and Astrophysics, 587, A55, 2016, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/201424873.

Keywords

  • Galaxies: abundances
  • Galaxies: evolution galaxies: ISM
  • Galaxies: star formation

Cite this

Sánchez, S. F., Pérez, E., Rosales-Ortega, F. F., Miralles-Caballero, D., López-Sánchez, A. R., Iglesias-Páramo, J., ... CALIFA collaboration (2015). Imprints of galaxy evolution on H II regions: memory of the past uncovered by the CALIFA survey. Astronomy and Astrophysics, 574, 1-17. [A47]. https://doi.org/10.1051/0004-6361/201424873
Sánchez, S. F. ; Pérez, E. ; Rosales-Ortega, F. F. ; Miralles-Caballero, D. ; López-Sánchez, A. R. ; Iglesias-Páramo, J. ; Marino, R. A. ; Sánchez-Menguiano, L. ; García-Benito, R. ; Mast, D. ; Mendoza, M. A. ; Papaderos, P. ; Ellis, S. ; Galbany, L. ; Kehrig, C. ; Monreal-Ibero, A. ; Delgado, R. González ; Mollá, M. ; Ziegler, B. ; De Lorenzo-Cáceres, A. ; Mendez-Abreu, J. ; Bland-Hawthorn, J. ; Bekeraitė, S. ; Roth, M. M. ; Pasquali, A. ; Díaz, A. ; Bomans, D. ; Van De Ven, G. ; Wisotzki, L. ; CALIFA collaboration. / Imprints of galaxy evolution on H II regions : memory of the past uncovered by the CALIFA survey. In: Astronomy and Astrophysics. 2015 ; Vol. 574. pp. 1-17.
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abstract = "Context. H II regions in galaxies are the sites of star formation, so they are special places for understanding the build-up of stellar mass in the universe. The line ratios of this ionized gas are frequently used to characterize the ionization conditions. In particular, the oxygen abundances are assumed to trace the chemical enrichment of galaxies. Aims. We explore the connections between the ionization conditions and the properties of the overall underlying stellar population (ionizing or not-ionizing) in H II regions, in order to uncover the actual physical connection between them. Methods. We use the H II regions catalog from the CALIFA survey, which is the largest in existence with more than 5000 H II regions, to explore their distribution across the classical [O III] λ5007/Hβ vs. [N II] λ6583/α diagnostic diagram, and the way it depends on the oxygen abundance, ionization parameter, electron density, and dust attenuation. The location of H II regions within this diagram is compared with predictions from photoionization models. Finally, we explore the dependence of the location within the diagnostic diagram on the properties of the host galaxies, the galactocentric distances, and the properties of the underlying stellar population. Results. The H II regions with weaker ionization strengths and more metal-rich are located in the bottom righthand area of the diagram. In contrast, those regions with stronger ionization strengths and more metal poor are located in the upper lefthand end of the diagram. Photoionization models per se do not predict these correlations between the parameters and the line ratios. The H II regions located in earlier-type galaxies, closer to the center and formed in older and more metal-rich regions of the galaxies are located in the bottom-right area of the diagram. On the other hand, those regions located in late-type galaxies in the outer regions of the disks and formed on younger and more metal-poor regions lie in the top lefthand area of the diagram. The two explored line ratios show strong correlations with the age and metallicity of the underlying stellar population. Conclusions. These results indicate that although H II regions are short-lived events, they are aff ected by the total underlying stellar population. One may say that H II regions keep a memory of the stellar evolution and chemical enrichment that have left an imprint on both the ionizing stellar population and the ionized gas.",
keywords = "Galaxies: abundances, Galaxies: evolution galaxies: ISM, Galaxies: star formation",
author = "S{\'a}nchez, {S. F.} and E. P{\'e}rez and Rosales-Ortega, {F. F.} and D. Miralles-Caballero and L{\'o}pez-S{\'a}nchez, {A. R.} and J. Iglesias-P{\'a}ramo and Marino, {R. A.} and L. S{\'a}nchez-Menguiano and R. Garc{\'i}a-Benito and D. Mast and Mendoza, {M. A.} and P. Papaderos and S. Ellis and L. Galbany and C. Kehrig and A. Monreal-Ibero and Delgado, {R. Gonz{\'a}lez} and M. Moll{\'a} and B. Ziegler and {De Lorenzo-C{\'a}ceres}, A. and J. Mendez-Abreu and J. Bland-Hawthorn and S. Bekeraitė and Roth, {M. M.} and A. Pasquali and A. D{\'i}az and D. Bomans and {Van De Ven}, G. and L. Wisotzki and {CALIFA collaboration}",
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Sánchez, SF, Pérez, E, Rosales-Ortega, FF, Miralles-Caballero, D, López-Sánchez, AR, Iglesias-Páramo, J, Marino, RA, Sánchez-Menguiano, L, García-Benito, R, Mast, D, Mendoza, MA, Papaderos, P, Ellis, S, Galbany, L, Kehrig, C, Monreal-Ibero, A, Delgado, RG, Mollá, M, Ziegler, B, De Lorenzo-Cáceres, A, Mendez-Abreu, J, Bland-Hawthorn, J, Bekeraitė, S, Roth, MM, Pasquali, A, Díaz, A, Bomans, D, Van De Ven, G, Wisotzki, L & CALIFA collaboration 2015, 'Imprints of galaxy evolution on H II regions: memory of the past uncovered by the CALIFA survey', Astronomy and Astrophysics, vol. 574, A47, pp. 1-17. https://doi.org/10.1051/0004-6361/201424873

Imprints of galaxy evolution on H II regions : memory of the past uncovered by the CALIFA survey. / Sánchez, S. F.; Pérez, E.; Rosales-Ortega, F. F.; Miralles-Caballero, D.; López-Sánchez, A. R.; Iglesias-Páramo, J.; Marino, R. A.; Sánchez-Menguiano, L.; García-Benito, R.; Mast, D.; Mendoza, M. A.; Papaderos, P.; Ellis, S.; Galbany, L.; Kehrig, C.; Monreal-Ibero, A.; Delgado, R. González; Mollá, M.; Ziegler, B.; De Lorenzo-Cáceres, A.; Mendez-Abreu, J.; Bland-Hawthorn, J.; Bekeraitė, S.; Roth, M. M.; Pasquali, A.; Díaz, A.; Bomans, D.; Van De Ven, G.; Wisotzki, L.; CALIFA collaboration.

In: Astronomy and Astrophysics, Vol. 574, A47, 01.01.2015, p. 1-17.

Research output: Contribution to journalArticleResearchpeer-review

TY - JOUR

T1 - Imprints of galaxy evolution on H II regions

T2 - Astronomy and Astrophysics

AU - Sánchez, S. F.

AU - Pérez, E.

AU - Rosales-Ortega, F. F.

AU - Miralles-Caballero, D.

AU - López-Sánchez, A. R.

AU - Iglesias-Páramo, J.

AU - Marino, R. A.

AU - Sánchez-Menguiano, L.

AU - García-Benito, R.

AU - Mast, D.

AU - Mendoza, M. A.

AU - Papaderos, P.

AU - Ellis, S.

AU - Galbany, L.

AU - Kehrig, C.

AU - Monreal-Ibero, A.

AU - Delgado, R. González

AU - Mollá, M.

AU - Ziegler, B.

AU - De Lorenzo-Cáceres, A.

AU - Mendez-Abreu, J.

AU - Bland-Hawthorn, J.

AU - Bekeraitė, S.

AU - Roth, M. M.

AU - Pasquali, A.

AU - Díaz, A.

AU - Bomans, D.

AU - Van De Ven, G.

AU - Wisotzki, L.

AU - CALIFA collaboration

N1 - Copyright 2015 ESO. First published in Astronomy and Astrophysics, 587, A55, 2016, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/201424873.

PY - 2015/1/1

Y1 - 2015/1/1

N2 - Context. H II regions in galaxies are the sites of star formation, so they are special places for understanding the build-up of stellar mass in the universe. The line ratios of this ionized gas are frequently used to characterize the ionization conditions. In particular, the oxygen abundances are assumed to trace the chemical enrichment of galaxies. Aims. We explore the connections between the ionization conditions and the properties of the overall underlying stellar population (ionizing or not-ionizing) in H II regions, in order to uncover the actual physical connection between them. Methods. We use the H II regions catalog from the CALIFA survey, which is the largest in existence with more than 5000 H II regions, to explore their distribution across the classical [O III] λ5007/Hβ vs. [N II] λ6583/α diagnostic diagram, and the way it depends on the oxygen abundance, ionization parameter, electron density, and dust attenuation. The location of H II regions within this diagram is compared with predictions from photoionization models. Finally, we explore the dependence of the location within the diagnostic diagram on the properties of the host galaxies, the galactocentric distances, and the properties of the underlying stellar population. Results. The H II regions with weaker ionization strengths and more metal-rich are located in the bottom righthand area of the diagram. In contrast, those regions with stronger ionization strengths and more metal poor are located in the upper lefthand end of the diagram. Photoionization models per se do not predict these correlations between the parameters and the line ratios. The H II regions located in earlier-type galaxies, closer to the center and formed in older and more metal-rich regions of the galaxies are located in the bottom-right area of the diagram. On the other hand, those regions located in late-type galaxies in the outer regions of the disks and formed on younger and more metal-poor regions lie in the top lefthand area of the diagram. The two explored line ratios show strong correlations with the age and metallicity of the underlying stellar population. Conclusions. These results indicate that although H II regions are short-lived events, they are aff ected by the total underlying stellar population. One may say that H II regions keep a memory of the stellar evolution and chemical enrichment that have left an imprint on both the ionizing stellar population and the ionized gas.

AB - Context. H II regions in galaxies are the sites of star formation, so they are special places for understanding the build-up of stellar mass in the universe. The line ratios of this ionized gas are frequently used to characterize the ionization conditions. In particular, the oxygen abundances are assumed to trace the chemical enrichment of galaxies. Aims. We explore the connections between the ionization conditions and the properties of the overall underlying stellar population (ionizing or not-ionizing) in H II regions, in order to uncover the actual physical connection between them. Methods. We use the H II regions catalog from the CALIFA survey, which is the largest in existence with more than 5000 H II regions, to explore their distribution across the classical [O III] λ5007/Hβ vs. [N II] λ6583/α diagnostic diagram, and the way it depends on the oxygen abundance, ionization parameter, electron density, and dust attenuation. The location of H II regions within this diagram is compared with predictions from photoionization models. Finally, we explore the dependence of the location within the diagnostic diagram on the properties of the host galaxies, the galactocentric distances, and the properties of the underlying stellar population. Results. The H II regions with weaker ionization strengths and more metal-rich are located in the bottom righthand area of the diagram. In contrast, those regions with stronger ionization strengths and more metal poor are located in the upper lefthand end of the diagram. Photoionization models per se do not predict these correlations between the parameters and the line ratios. The H II regions located in earlier-type galaxies, closer to the center and formed in older and more metal-rich regions of the galaxies are located in the bottom-right area of the diagram. On the other hand, those regions located in late-type galaxies in the outer regions of the disks and formed on younger and more metal-poor regions lie in the top lefthand area of the diagram. The two explored line ratios show strong correlations with the age and metallicity of the underlying stellar population. Conclusions. These results indicate that although H II regions are short-lived events, they are aff ected by the total underlying stellar population. One may say that H II regions keep a memory of the stellar evolution and chemical enrichment that have left an imprint on both the ionizing stellar population and the ionized gas.

KW - Galaxies: abundances

KW - Galaxies: evolution galaxies: ISM

KW - Galaxies: star formation

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U2 - 10.1051/0004-6361/201424873

DO - 10.1051/0004-6361/201424873

M3 - Article

VL - 574

SP - 1

EP - 17

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A47

ER -