Defensa digital: repositorio de publicaciones de Defensa iberoamericanas

Español
Português

Está en:  › Datos de registro

A few StePS forward in unveiling the complexity of galaxy evolution: light-weighted stellar ages of intermediate-redshift galaxies with WEAVE

Identificadores del recurso

Astronomy and Astrophysics 632: A9(2019)

0004-6361

https://www.aanda.org/articles/aa/abs/2019/12/aa36550-19/aa36550-19.html

http://hdl.handle.net/20.500.12666/420

10.1051/0004-6361/201936550

1432-0746

Procedencia

(Digital.INTA - Repositorio institucional del INTA)

Ficha

Título:: A few StePS forward in unveiling the complexity of galaxy evolution: light-weighted stellar ages of intermediate-redshift galaxies with WEAVE
Tema:: Galaxies: evolution; Galaxies: formation; Galaxies: fundamental parameters; Galaxies: star formation; Galaxies: stellar content
Descripción:: Context. The upcoming new generation of optical spectrographs on four-meter-class telescopes, with their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage, will provide invaluable information for reconstructing the history of star formation in individual galaxies up to redshifts of about 0.7. Aims. We aim at defining simple but robust and meaningful physical parameters that can be used to trace the coexistence of widely diverse stellar components: younger stellar populations superimposed on the bulk of older ones. Methods. We produced spectra of galaxies closely mimicking data from the forthcoming Stellar Populations at intermediate redshifts Survey (StePS), a survey that uses the WEAVE spectrograph on the William Herschel Telescope. First, we assessed our ability to reliably measure both ultraviolet and optical spectral indices in galaxies of different spectral types for typically expected signal-to-noise ratios. We then analyzed such mock spectra with a Bayesian approach, deriving the probability density function of r- and u-band light-weighted ages as well as of their difference. Results. We find that the ultraviolet indices significantly narrow the uncertainties in estimating the r- and u-band light-weighted ages and their difference in individual galaxies. These diagnostics, robustly retrievable for large galaxy samples even when observed at moderate signal-to-noise ratios, allow us to identify secondary episodes of star formation up to an age of ∼0.1 Gyr for stellar populations older than ∼1.5 Gyr, pushing up to an age of ∼1 Gyr for stellar populations older than ∼5 Gyr. Conclusions. The difference between r-band and u-band light-weighted ages is shown to be a powerful diagnostic to characterize and constrain extended star-formation histories and the presence of young stellar populations on top of older ones. This parameter can be used to explore the interplay between different galaxy star-formation histories and physical parameters such as galaxy mass, size, morphology, and environment.; We thank the anonymous referee for carefully reading the manuscript and for the suggestions that helped us to improve the way we presented our results. We wish to thank M. Irwin for very useful discussions and valuable suggestions. L. C. wish to acknowledge financial support from Premiale 2015 MITiC, program 1.05.06.10 and Comunidad de Madrid under Atraccion de Talento grant 2018-T2/TIC-11612. A. I., S. Z., M. L., A. G., A. M., and C. T. acknowledge the financial support from the INAF PRIN-SKA 2017 program 1.05.01.88.04.ESKAPE-HI. I. L. acknowledges financial support from INAF-WEAVE funds, program 1.05.03.04.05. R. G. B. acknowledges support from the Spanish Ministry of Economy and Competitiveness through grant 205 AYA2016-77846-P and the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to 2017 the Instituto de Astrofisica de Andalucia (SEV-2017-0709). A. F. M. has received financial support through the Postdoctoral Junior Leader Fellowship Programme from "La Caixa" Banking Foundation (LCF/BQ/LI18/11630007). B. V. acknowledges the financial support from INAF Main Stream 2018 (P. I.: B. Vulcani); With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).; Peer review
Idioma:: English
Relación:: info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-77846-P/ES/EVOLUCION DE GALAXIAS/
Autor/Productor:: Costantin, L.; Lovino, A.; Zibetti, S.; Longhetti, M.; Gallazzi, A.; Mercurio, A.; Lonoce, I.; Balcells, M.; Bolzonella, M.; Busarello, G.; Dalton, G.; Ferré Mateu, A.; García Benito, R.; Gargiulo, A.; Haines, C.; Jin, S.; La Barbera, F.; McGee, S.; Merluzzi, P.; Morelli, L.; Murphy, D. N. A.; Peralta de Arriba, L.; Pizzella, A.; Poggianti, B. M.; Pozzetti, L.; Sánchez Blázquez, P.; Talia, M.; Tortora, C.; Trager, S. C.; Vazdekis, A.; Vergani, D.; Vulcani, B.
Editor:: EDP Sciences
Otros colaboradores/productores:: Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; Vulcani, B. [0000-0003-0980-1499]; De Arribas, L. P. [0000-0002-3084-084X]; Zibetti, S. [0000-0003-1734-8356]; Talia, M. [0000-0003-4352-2063]; Tortora, C. [0000-0001-7958-6531]; Pizzella, A. [0000-0001-9585-417X]; Ferré Mateu, A. [0000-0002-6411-220X]; McGee, S. [0000-0003-3255-3139]; Gargiulo, A. [0000-0002-3351-1216]; Longhetti, M. [0000-0002-6142-4822]; Gallazzi, A. [0000-0002-9656-1800]; Vergani, D. [0000-0003-0898-2216]; Haines, C. [0000-0002-8814-8960]; Costantin, L. [0000-0001-6820-0015]; Pozzetti, L. [0000-0001-7085-0412]; Dalton, G. [0000-0002-3031-2588]; Iovino, A. [0000-0001-6958-0304]; Sánchez Blázquez, P. [0000-0003-0651-0098]; Merluzzi, P. [0000-0003-3966-2397]; Istituto Nazionale di Astrofisica (INAF); Comunidad de Madrid; Fundación Caixa; Agencia Estatal de Investigación (AEI)
Derechos:: Attribution-NonCommercial-NoDerivatives 4.0 International; © ESO 2019; https://creativecommons.org/licenses/by-nc-nd/4.0/; info:eu-repo/semantics/openAccess
Fecha:: 2021-04-19T10:06:39Z; 2019-11-21
Tipo de recurso:: info:eu-repo/semantics/article; info:eu-repo/semantics/publishedVersion; http://purl.org/coar/resource_type/c_6501
Formato:: application/pdf

oai_dc

Descargar XML

<?xml version="1.0" encoding="UTF-8" ?>

< oai_dc:dc schemaLocation =" http://www.openarchives.org/OAI/2.0/oai_dc/ http://www.openarchives.org/OAI/2.0/oai_dc.xsd " >
1. < dc:title > A few StePS forward in unveiling the complexity of galaxy evolution: light-weighted stellar ages of intermediate-redshift galaxies with WEAVE </ dc:title >
2. < dc:creator > Costantin, L. </ dc:creator >
3. < dc:creator > Lovino, A. </ dc:creator >
4. < dc:creator > Zibetti, S. </ dc:creator >
5. < dc:creator > Longhetti, M. </ dc:creator >
6. < dc:creator > Gallazzi, A. </ dc:creator >
7. < dc:creator > Mercurio, A. </ dc:creator >
8. < dc:creator > Lonoce, I. </ dc:creator >
9. < dc:creator > Balcells, M. </ dc:creator >
10. < dc:creator > Bolzonella, M. </ dc:creator >
11. < dc:creator > Busarello, G. </ dc:creator >
12. < dc:creator > Dalton, G. </ dc:creator >
13. < dc:creator > Ferré Mateu, A. </ dc:creator >
14. < dc:creator > García Benito, R. </ dc:creator >
15. < dc:creator > Gargiulo, A. </ dc:creator >
16. < dc:creator > Haines, C. </ dc:creator >
17. < dc:creator > Jin, S. </ dc:creator >
18. < dc:creator > La Barbera, F. </ dc:creator >
19. < dc:creator > McGee, S. </ dc:creator >
20. < dc:creator > Merluzzi, P. </ dc:creator >
21. < dc:creator > Morelli, L. </ dc:creator >
22. < dc:creator > Murphy, D. N. A. </ dc:creator >
23. < dc:creator > Peralta de Arriba, L. </ dc:creator >
24. < dc:creator > Pizzella, A. </ dc:creator >
25. < dc:creator > Poggianti, B. M. </ dc:creator >
26. < dc:creator > Pozzetti, L. </ dc:creator >
27. < dc:creator > Sánchez Blázquez, P. </ dc:creator >
28. < dc:creator > Talia, M. </ dc:creator >
29. < dc:creator > Tortora, C. </ dc:creator >
30. < dc:creator > Trager, S. C. </ dc:creator >
31. < dc:creator > Vazdekis, A. </ dc:creator >
32. < dc:creator > Vergani, D. </ dc:creator >
33. < dc:creator > Vulcani, B. </ dc:creator >
34. < dc:contributor > Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709 </ dc:contributor >
35. < dc:contributor > Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737 </ dc:contributor >
36. < dc:contributor > Vulcani, B. [0000-0003-0980-1499] </ dc:contributor >
37. < dc:contributor > De Arribas, L. P. [0000-0002-3084-084X] </ dc:contributor >
38. < dc:contributor > Zibetti, S. [0000-0003-1734-8356] </ dc:contributor >
39. < dc:contributor > Talia, M. [0000-0003-4352-2063] </ dc:contributor >
40. < dc:contributor > Tortora, C. [0000-0001-7958-6531] </ dc:contributor >
41. < dc:contributor > Pizzella, A. [0000-0001-9585-417X] </ dc:contributor >
42. < dc:contributor > Ferré Mateu, A. [0000-0002-6411-220X] </ dc:contributor >
43. < dc:contributor > McGee, S. [0000-0003-3255-3139] </ dc:contributor >
44. < dc:contributor > Gargiulo, A. [0000-0002-3351-1216] </ dc:contributor >
45. < dc:contributor > Longhetti, M. [0000-0002-6142-4822] </ dc:contributor >
46. < dc:contributor > Gallazzi, A. [0000-0002-9656-1800] </ dc:contributor >
47. < dc:contributor > Vergani, D. [0000-0003-0898-2216] </ dc:contributor >
48. < dc:contributor > Haines, C. [0000-0002-8814-8960] </ dc:contributor >
49. < dc:contributor > Costantin, L. [0000-0001-6820-0015] </ dc:contributor >
50. < dc:contributor > Pozzetti, L. [0000-0001-7085-0412] </ dc:contributor >
51. < dc:contributor > Dalton, G. [0000-0002-3031-2588] </ dc:contributor >
52. < dc:contributor > Iovino, A. [0000-0001-6958-0304] </ dc:contributor >
53. < dc:contributor > Sánchez Blázquez, P. [0000-0003-0651-0098] </ dc:contributor >
54. < dc:contributor > Merluzzi, P. [0000-0003-3966-2397] </ dc:contributor >
55. < dc:contributor > Istituto Nazionale di Astrofisica (INAF) </ dc:contributor >
56. < dc:contributor > Comunidad de Madrid </ dc:contributor >
57. < dc:contributor > Fundación Caixa </ dc:contributor >
58. < dc:contributor > Agencia Estatal de Investigación (AEI) </ dc:contributor >
59. < dc:subject > Galaxies: evolution </ dc:subject >
60. < dc:subject > Galaxies: formation </ dc:subject >
61. < dc:subject > Galaxies: fundamental parameters </ dc:subject >
62. < dc:subject > Galaxies: star formation </ dc:subject >
63. < dc:subject > Galaxies: stellar content </ dc:subject >
64. < dc:description > Context. The upcoming new generation of optical spectrographs on four-meter-class telescopes, with their huge multiplexing capabilities, excellent spectral resolution, and unprecedented wavelength coverage, will provide invaluable information for reconstructing the history of star formation in individual galaxies up to redshifts of about 0.7. Aims. We aim at defining simple but robust and meaningful physical parameters that can be used to trace the coexistence of widely diverse stellar components: younger stellar populations superimposed on the bulk of older ones. Methods. We produced spectra of galaxies closely mimicking data from the forthcoming Stellar Populations at intermediate redshifts Survey (StePS), a survey that uses the WEAVE spectrograph on the William Herschel Telescope. First, we assessed our ability to reliably measure both ultraviolet and optical spectral indices in galaxies of different spectral types for typically expected signal-to-noise ratios. We then analyzed such mock spectra with a Bayesian approach, deriving the probability density function of r- and u-band light-weighted ages as well as of their difference. Results. We find that the ultraviolet indices significantly narrow the uncertainties in estimating the r- and u-band light-weighted ages and their difference in individual galaxies. These diagnostics, robustly retrievable for large galaxy samples even when observed at moderate signal-to-noise ratios, allow us to identify secondary episodes of star formation up to an age of ∼0.1 Gyr for stellar populations older than ∼1.5 Gyr, pushing up to an age of ∼1 Gyr for stellar populations older than ∼5 Gyr. Conclusions. The difference between r-band and u-band light-weighted ages is shown to be a powerful diagnostic to characterize and constrain extended star-formation histories and the presence of young stellar populations on top of older ones. This parameter can be used to explore the interplay between different galaxy star-formation histories and physical parameters such as galaxy mass, size, morphology, and environment. </ dc:description >
65. < dc:description > We thank the anonymous referee for carefully reading the manuscript and for the suggestions that helped us to improve the way we presented our results. We wish to thank M. Irwin for very useful discussions and valuable suggestions. L. C. wish to acknowledge financial support from Premiale 2015 MITiC, program 1.05.06.10 and Comunidad de Madrid under Atraccion de Talento grant 2018-T2/TIC-11612. A. I., S. Z., M. L., A. G., A. M., and C. T. acknowledge the financial support from the INAF PRIN-SKA 2017 program 1.05.01.88.04.ESKAPE-HI. I. L. acknowledges financial support from INAF-WEAVE funds, program 1.05.03.04.05. R. G. B. acknowledges support from the Spanish Ministry of Economy and Competitiveness through grant 205 AYA2016-77846-P and the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to 2017 the Instituto de Astrofisica de Andalucia (SEV-2017-0709). A. F. M. has received financial support through the Postdoctoral Junior Leader Fellowship Programme from "La Caixa" Banking Foundation (LCF/BQ/LI18/11630007). B. V. acknowledges the financial support from INAF Main Stream 2018 (P. I.: B. Vulcani); With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737). </ dc:description >
66. < dc:description > Peer review </ dc:description >
67. < dc:date > 2021-04-19T10:06:39Z </ dc:date >
68. < dc:date > 2021-04-19T10:06:39Z </ dc:date >
69. < dc:date > 2019-11-21 </ dc:date >
70. < dc:type > info:eu-repo/semantics/article </ dc:type >
71. < dc:type > info:eu-repo/semantics/publishedVersion </ dc:type >
72. < dc:type > http://purl.org/coar/resource_type/c_6501 </ dc:type >
73. < dc:identifier > Astronomy and Astrophysics 632: A9(2019) </ dc:identifier >
74. < dc:identifier > 0004-6361 </ dc:identifier >
75. < dc:identifier > https://www.aanda.org/articles/aa/abs/2019/12/aa36550-19/aa36550-19.html </ dc:identifier >
76. < dc:identifier > http://hdl.handle.net/20.500.12666/420 </ dc:identifier >
77. < dc:identifier > 10.1051/0004-6361/201936550 </ dc:identifier >
78. < dc:identifier > 1432-0746 </ dc:identifier >
79. < dc:language > eng </ dc:language >
80. < dc:relation > info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2016-77846-P/ES/EVOLUCION DE GALAXIAS/ </ dc:relation >
81. < dc:rights > Attribution-NonCommercial-NoDerivatives 4.0 International </ dc:rights >
82. < dc:rights > © ESO 2019 </ dc:rights >
83. < dc:rights > https://creativecommons.org/licenses/by-nc-nd/4.0/ </ dc:rights >
84. < dc:rights > info:eu-repo/semantics/openAccess </ dc:rights >
85. < dc:format > application/pdf </ dc:format >
86. < dc:publisher > EDP Sciences </ dc:publisher >
</ oai_dc:dc >