High-resolution spectroscopy of the high velocity hot post-AGB star IRAS 18379-1707 (LS 5112)

TL;DR

This study presents a detailed high-resolution spectral analysis of the post-AGB star IRAS 18379-1707, revealing its atmospheric parameters, chemical composition, and evidence of mass loss, contributing to understanding late stellar evolution.

Contribution

First detailed spectral identification and chemical analysis of IRAS 18379-1707, including atmospheric parameters and mass-loss indicators, using non-LTE models and high-resolution spectroscopy.

Findings

Metal-deficient ([M/H]≈-0.6) post-AGB star.

Overabundance of CNO elements indicating third dredge-up.

Detection of P-Cygni profiles in Balmer lines indicating mass loss.

Abstract

The high-resolution ($R\sim48\,000$) optical spectrum of the B-type supergiant LS 5112, identified as the optical counterpart of the post-AGB candidate IRAS 18379-1707, is analysed. We report the detailed identifications of the observed absorption and emission features in the wavelength range 3700-9200 A for the first time. The absorption line spectrum has been analysed using non-LTE model atmosphere techniques to determine stellar atmospheric parameters and chemical composition. We estimate $T_\text{eff}=18~000\pm1000$ K, $\log g=2.25\pm0.08$, $\xi_{\rm t}=10\pm4$ km/s and $v \sin i=37\pm6$ km/s, and the derived abundances indicate a metal-deficient ([M/H]$\approx-0.6)$ post-AGB star. Chemical abundances of eight different elements were obtained. The estimates of the CNO abundances in IRAS 18379-1707 indicate that these elements are overabundant with [(C+N+O)/S]=+0.5$\pm$0.2 suggesting that the products of helium burning have been brought to the surface as a result of third dredge-up on the AGB. From the absorption lines, we derived heliocentric radial velocity of $V_\text{r}=-124.0\pm0.4$ km/s. We have identified permitted emission lines of O I, N I, Na I, S II, Si II, C II, Mg II and Fe III. The nebula forbidden lines of [N I], [O I], [Fe II], [N II], [S II], [Ni II] and [Cr II] have also been identified. The Balmer lines H$\alpha$, H$\beta$ and H$\gamma$ show P-Cygni behaviour clearly indicating post-AGB mass-loss process in the object with the wind velocity up to 170 km/s.