Evolutionary population synthesis: models, analysis of the ingredients and application to high-z galaxies

Clicks: 1
ID: 291632
2005
Free PDF
Article Quality & Performance Metrics
Overall Quality
Not rated
Combines reader engagement with the AI quality analysis. This article has not been analysed, so there is no overall score — reader engagement is measured and shown alongside.
AI Quality Assessment
Not analyzed
Readership in this journal

Ranked #514 of 908 articles by views in monthly notices of the royal astronomical society

Most read Least read

Bar heights use a square-root scale. Only the 120 most-read articles are drawn; the journal has 908 in total.

Mint this article as an NFT
Not yet minted

Create a permanent, verifiable on-chain record of this article on the Scimatic Network. The NFT is held in your Journament account, and you can withdraw it to your own wallet at any time.

5 SUSD one-off · no wallet required
Sign in to mint
Abstract
Evolutionary population synthesis models for a wide range of metallicities, ages, star formation histories, and Horizontal Branch morphologies, including blue morphologies at high metallicity, are computed. The energetics of the post Main Sequence evolutionary phases are evaluated with the fuel consumption theorem. The impact on the models of the stellar evolutionary tracks is assessed. We find modest differences in synthetic broad-band colours as induced by the use of different tracks in our code (e.g. d(V-K) ~ 0.08 mag; d(B-V) ~ 0.03 mag). These differences are smaller than the scatter among other models in the literature, even when the latter adopt the same evolutionary tracks. The models are calibrated with globular cluster data from the Milky Way for old ages, and the Magellanic Clouds plus the merger remnant galaxy NGC 7252, for ages of ~ 0.1 - 2 Gyr, in a large wavelength range from U to K. Particular emphasis is put on the contribution from the Thermally-Pulsing Asymptotic Giant Branch phase. We show that this phase is crucial for the modelling of young stellar populations by the comparison with observed spectral energy distributions of Magellanic Clouds clusters, which are characterised by high fluxes both blueward and redward the V-band. We find that the combination of the near-IR spectral indices C2 and H2O can be used to determine the metallicity of ~ 1 Gyr stellar populations. We re-analyze the spectral energy distributions of some of the high-z galaxies (2.4 < z < 2.9) observed with the Spitzer Space Telescope by Yan et al. (2004). Their high rest-frame near-IR fluxes are reproduced very well with the models including Thermally-Pulsing Asymptotic Giant Branch stars for ages in the range 0.6-1.5 Gyr, suggesting formation redshifts around z ~ 3-6.
Reference Key
openalex_W1970333333 Use this key to autocite in the manuscript while using SciMatic Manuscript Manager or Thesis Manager
Authors Claudia Maraston
Journal monthly notices of the royal astronomical society
Year 2005
DOI
10.1111/j.1365-2966.2005.09270.x
URL
https://academic.oup.com/mnras/article-pdf/362/3/799/2986994/362-3-799.pdf
Keywords Keywords not found

Citations

No citations found. To add a citation, contact the admin at info@scimatic.org

Comments

No comments yet. Be the first to comment on this article.