MIUSCAT: extended MILES spectral coverage. I. Stellar populations synthesis models

TL;DR

This paper extends stellar population synthesis models by combining multiple spectral libraries to cover a broader wavelength range, enabling improved analysis of stellar populations and IMF sensitivity in galaxy spectra.

Contribution

The authors develop extended spectral models using combined empirical libraries, introducing a new IMF-sensitive index and demonstrating their application to spectral fitting and stellar population analysis.

Findings

Composite SSP SEDs cover 3465-9469 Å at high resolution.

Colors involving red filters are highly sensitive to the IMF.

A new IMF-sensitive index based on NaI doublet at 8200 Å is proposed.

Abstract

We extend the spectral range of our stellar population synthesis models based on the MILES and CaT empirical stellar spectral libraries. For this purpose we combine these two libraries with the Indo-U.S. to construct composite stellar spectra to feed our models. The spectral energy distributions (SEDs) computed with these models and the originally published models are combined to construct composite SEDs for single-age, single-metallicity stellar populations (SSPs) covering the range 3465 - 9469\AA at moderately high, and uniform, resolution (FWHM=2.51\AA). The colours derived from these SSP SEDs provide good fits to Galactic globular cluster data. We find that the colours involving redder filters are very sensitive to the IMF, as well as a number of features and molecular bands throughout the spectra. To illustrate the potential use of these models we focus on the NaI doublet at 8200 \AA and with the aid of the newly synthesized SSP model SEDs we define a new IMF-sensitive index that is based on this feature, which overcomes various limitations from previous index definitions for low velocity dispersion stellar systems. We propose an index-index diagram based on this feature and the neighboring CaII triplet at 8600 \AA, to constrain the IMF if the age and [Na/Fe] abundance are known. Finally we also show a survey-oriented spectrophotometric application which evidences the accurate flux calibration of these models for carrying out reliable spectral fitting techniques. These models are available through our user-friendly website.