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- W1613181055 abstract "Aiming at picking up suitable theoretical tools to break the agemetallicity degeneracy in simple stellar populations (SSPs), we explore here the properties of a set of 17 synthetic mid-UV spectroscopic indices relying on the Uvblue synthetic stellar library and the Buzzoni population synthesis code. 1. The Theoretical Mid-UV Spectroscopic Indices Spectroscopic indices are widely used to extract information on the physical properties of astronomical objects from low or mid-resolution spectroscopic observations. In the ultraviolet region Fanelli et al. (1990) defined a set of 25 narrow-band indices based on International Ultraviolet Explorer (IUE) stellar spectra, covering the wavelength interval 1230–3200 A. Several authors have used this system to study evolved populations, such as globular clusters and elliptical galaxies (e.g. Ponder et al. 1998; Lotz et al. 2000). In order to compute theoretical indices in the standard Fanelli system, we implemented the UVBLUE high-resolution synthetic stellar library (RodriguezMerino et al. 2005) in the Buzzoni’s code (1989) to produce integrated spectral energy distributions (SED) of SSPs at the IUE original resolution (namely 6 A FWHM). Model grid spans an age interval from 2 to 15 Gyr at five different metallicities ([Fe/H]= −2.27,−1.27,−0.25,−0.02,+0.22). The models are computed for three different exponents of a standard power-law Initial Mass Function, IMF (i.e. N(M∗) ∝ M −s ∗ , with s = 1.35, 2.35 the Salpeter case, and 3.35), and explore three horizontal branch (HB) morphologies (red, intermediate, blue), for two values of Reimers’ (1975) mass loss parameter (i.e. η=0.3, 0.5). According to Fanelli’s et al. (1990) original prescriptions, as summarized in Table 1 of Chavez et al. (2006), we computed a set of 17 indices, which measure the strength of either prominent mid-UV absorption features or pseudo-continuum slope. Two general trend can be identified from the analysis of the whole data set: (i) some indices, like Fe ii 2332, Fe ii 2402 and, partly, Mg ii 2800, better trace young (t < 3 Gyr) stellar populations, showing a much more entangled behaviour at older ages and usually reversing their metallicity dependence in the latter range; (ii) all the other indices increase with increasing age and/or metal abundance, though with very different age sensitivity. The two behaviours can" @default.
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- W1613181055 date "2007-12-01" @default.
- W1613181055 modified "2023-10-17" @default.
- W1613181055 title "Theoretical Mid-UV Spectroscopic Indices for Evolved Stellar Populations" @default.
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