Near-IR Spectra of Red Supergiants and Giants. I- Models with Solar and with Mixing-Induced Surface Abundance Ratios

TL;DR

This study presents a grid of near-IR spectra models for red giants and supergiants, incorporating surface abundance modifications to better match observations and assess their impact on stellar parameter estimates.

Contribution

First models with modified surface abundances of C, N, and O are provided, enabling improved spectral fitting and understanding of abundance effects on stellar parameters.

Findings

Models fit observed spectra well at solar metallicity for giants down to 3400K.

Modified abundances improve CN band reproduction but do not resolve all spectral fitting issues.

Abundance changes can alter temperature estimates by several hundred Kelvin.

Abstract

We provide a grid of PHOENIX spectra of red giant and supergiant stars, that extend through optical and near-IR wavelengths. For the first time, models are also provided with modified surface abundances of C, N and O, as a step towards accounting for the changes known to occur due to convective dredge-up (and to be enhanced in the case of rotation). The aims are (i) to assess how well current models reproduce observed spectra, (ii) to quantify the effects of the abundance changes on the spectra, and (iii) to determine how these changes affect estimates of fundamental stellar parameters. Observed giant star spectra can be fitted very well at solar metallicity down to about 3400K. Modified surface abundances are preferred in only a minority of cases for luminosity class II, possibly indicating mixing in excess of standard first dredge-up. Supergiant stars show a larger variety of near-IR spectra, and good fits are currently obtained for about one third of the observations only. Modified surface abundances help reproducing strong CN bands, but do not suffice to resolve all the difficulties. The effect of the abundance changes on the estimated Teff depends on the wavelength range of observation and can amount several 100K. Reasons for the remaining discrepancies are discussed.