Spectroscopic and Photometric Monitoring of a Poorly Known Highly Luminous OH/IR Star: IRAS 18278+0931

Abstract

We present the time-dependent properties of a poorly known OH/IR star, IRAS 18278+0931 (hereafter IRAS 18+09), toward the Ophiuchus constellation. We have carried out long-term optical/near-infrared photometric and spectroscopic observations to study the object. From optical R - and I -band light curves, the period of IRAS 18+09 is estimated to be 575 ± 30 days and the variability amplitudes range from Δ R ∼ 4.0 mag to Δ I ∼ 3.5 mag. From the standard period–luminosity relations, the distance ( D ) to the object, 4.0 ± 1.3 kpc, is estimated. Applying this distance in the radiative transfer model, the spectral energy distribution is constructed from multiwavelength photometric and IRAS-LRS spectral data, which provide the luminosity, optical depth, and gas mass-loss rate of the object to be 9600 ± 500 L ⊙ , 9.1 ± 0.6 at 0.55 μ m, and 1.0 × 10 −6 M ⊙ yr −1 , respectively. The current mass of the object is inferred to be in the range 1.0−1.5 M ⊙ assuming solar metallicity. Notably, the temporal variation of atomic and molecular features (e.g., TiO, Na i , Ca i , CO, H 2 O) over the pulsation cycle of the OH/IR star illustrates the sensitivity of the spectral features to the dynamical atmosphere as observed in pulsating AGB stars.