Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase

Abstract

The spectral evolution of the nova V5587 Sgr has been monitored at Koyama Astronomical Observatory and HigashiHiroshima Observatory, Japan, from the early to nebula phase. The nova rebrightened several times. The spectra during the early phase showed emission lines of Hα, Hβ, O I, He I, He II, N II, Fe II. Nova V5587 Sgr is classified into the Fe II type. The helium abundance of the nova is estimated as N(He)/N(H) = 0.134 ± 0.09. The light curve, the spectral evolution, and the helium abundance in V5587 Sgr are similar to those of the nova PW Vul.