OPTICAL AND INFRARED OBSERVATIONS OF SGR 1806-20

摘要

The soft gamma-ray repeater (SGR) 1806 — 20 is associated with the center-brightened nonthermal nebula G10.0 —0.3, thought to be a plerion. As in other plerions, a steady X-ray source, AX 1805.7 — 2025, has been detected coincident with the peak of the nebular radio emission. Vasisht et al. have shown that the radio peak has a core-jet appearance and argue that the core marks the true position of the SGR. At optical wavelengths, we detect three objects in the vicinity of the radio core. Only for the star closest to the core, barely visible in the optical but bright in the infrared (K = 8.4 mag), the reddening is consistent with the high extinction (A_V approx= 30 mag) that has been inferred for AX 1805.7 — 2025. From the absence of CO band absorption, we infer that the spectral type of this star is earlier than late-G/early-K. The large extinction probably arises in a molecular cloud located at a distance of 6 kpc, which means that the star, just like AX 1805.7-2025, is in or behind this cloud. This implies that the star is a supergiant. Since supergiants are rare, a chance coincidence with the compact radio core is very unlikely. To our knowledge, there are only three other examples of luminous stars embedded in nonthermal radio nebulae: SS 433, Cir X-1, and G70.7+1.2. Given this and the low coincidence probability, we suggest that the bright star is physically associated with SGR 1806 — 20, making it the first stellar identification of a high-energy transient.