Hostname: page-component-6bf8c574d5-w79xw Total loading time: 0 Render date: 2025-02-27T20:51:14.180Z Has data issue: false hasContentIssue false
  • English
  • Français

Exploring the star formation histories of galaxies in different environments from MaNGA spectra

Published online by Cambridge University Press:  10 June 2020

Maria Argudo-Fernández Open the ORCID record for Maria Argudo-Fernández [Opens in a new window] ,
Médéric Boquien ,
Shiyin Shen ,
Fangting Yuan ,
Jun Yin ,
Ruixiang Chang  and
Lei Hao
Maria Argudo-Fernández
Affiliation:
Instituto de Física, Pontificia Universidad Católica de Valparaíso, Casilla 4059, Valparaíso, Chile Centro de Astronomía (CITEVA), Universidad de Antofagasta, Avenida Angamos 601 Antofagasta, Chile email: maria.argudo@uantof.cl
Médéric Boquien
Affiliation:
Centro de Astronomía (CITEVA), Universidad de Antofagasta, Avenida Angamos 601 Antofagasta, Chile email: maria.argudo@uantof.cl
Shiyin Shen
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
Fangting Yuan
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
Jun Yin
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
Ruixiang Chang
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
Lei Hao
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The star formation history (SFH) of galaxies allow us to investigate when galaxies formed their stars and assembled their mass. We can constrain the SFH with high level of precision from galaxies with resolved stellar populations, since we are able to discriminate between stars of different ages from the spectrum they emit. However, the relative importance of secular evolution (nature) over nurture is not yet clear, and separating the effects of interaction-driven evolution in the observed galaxy properties is not trivial. The aim of this study is to use MaNGA (Mapping Nearby Galaxies at APO) Integral Field Unit (IFU) data, in combination with multi-wavelength data, to constrain the SFH of nearby isolated galaxies. We present here the new techniques we are developing to constrain the SFH with high level of precision from Spectral Energy Distribution (SED) fitting. This study is part of a China-Chile collaboration program where we are applying these new techniques to investigate how galaxies formed and evolve in different environments.

Keywords

galaxies: generalgalaxies: formationgalaxies: evolutiongalaxies: interactionsgalaxies: spiraltechniques: miscellaneous
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 60 - 64
Copyright
© International Astronomical Union 2020

References

Aguado, D. S., Ahumada, R., Almeida, A., Anderson, S. F., Andrews, B. H., Anguiano, B., Aquino Ortz, E., Aragón-Salamanca, A., et al. 2019, ApJS, 240, 23CrossRefGoogle Scholar
Argudo-Fernández, M., Verley, S., Bergond, G., Duarte Puertas, S., Ramos Carmona, E., Sabater, J., Fernández Lorenzo, M., Espada, D., et al. 2015, A&A, 578, A110Google Scholar
Blanton, M. R., Bershady, M. A., Abolfathi, B., Albareti, F. D., Allende Prieto, C., Almeida, A., Alonso-Garca, J., Anders, F., et al. 2017, AJ, 154, 2810.3847/1538-3881/aa7567CrossRefGoogle Scholar
Boquien, M., Burgarella, D., Roehlly, Y., Buat, V., Ciesla, L., Corre, D., Inoue, A. K., Salas, H., et al. 2018, arXiv:1811.03094Google Scholar
Bundy, K., Bershady, M. A., Law, D. R., Yan, R., Drory, N., MacDonald, N., Wake, D. A., Cherinka, B., et al. 2015, ApJ, 798, 7CrossRefGoogle Scholar
Cherinka, B., Andrews, B. H., Sánchez-Gallego, J., Brownstein, J., Argudo-Fernández, M., Blanton, M., Bundy, K., Jones, A., et al. 2018, arXiv:1812.03833Google Scholar
Gunn, J. E., Siegmund, W. A., Mannery, E. J., Owen, R. E., Hull, C. L., Leger, R. F., Carey, L. N., Knapp, G. R., et al. 2006, AJ, 131, 233210.1086/500975CrossRefGoogle Scholar
Strauss, M. A., Weinberg, D. H., Lupton, R. H., Narayanan, V. K., Annis, J., Bernardi, M., Blanton, M., Burles, S., et al. 2002, AJ, 124, 1810CrossRefGoogle Scholar
York, D. G., Adelman, J., Anderson, J. E. Jr, et al. 2000, AJ, 120, 157910.1086/301513CrossRefGoogle Scholar
Yuan, F.-T., Argudo-Fernández, M., Shen, S., Hao, L., Jiang, C., Yin, J., Boquien, M., and Lin, L., et al. 2018, A&A, 613, A13Google ScholarPubMed