We report the results of a long-term spectroscopic monitoring of the A-type supergiant with the B[e] phenomenon 3 Pup = HD 62623. We confirm earlier findings that it is a binary system. The orbital parameters were derived using cross-correlation of the spectra in a range of 4460-4632 A, which contains over 30 absorption lines. The orbit was found circular with a period of $137.4\pm0.1$ days, radial velocity semi-amplitude $K_{1} = 5.0\pm0.8$ km s$^{-1}$, systemic radial velocity $\gamma = +26.4\pm2.0$ km s$^{-1}$, and the mass function $f(m) = (1.81^{+0.97}_{-0.76})\times10^{-3}$ M$_{\odot}$. The object may have evolved from a pair with initial masses of $\sim$6.0 M$_{\odot}$ and $\sim$3.6 M$_{\odot}$ with an initial orbital period of $\sim$5 days. Based on the fundamental parameters of the A-supergiant (luminosity $\log$ L/L$_{\odot} = 4.1\pm$0.1 and effective temperature T$_{\rm eff} = 8500\pm$500 K) and evolutionary tracks of mass-transferring binaries, we found current masses of the gainer M$_{2} = 8.8\pm$0.5 M$_{\odot}$ and donor M$_{1} = 0.75\pm0.25$ M$_{\odot}$. We also modeled the object's IR-excess and derived a dust mass of $\sim 5\,\times10^{-5}$ M$_{\odot}$ in the optically-thin dusty disk. The orbital parameters and properties of the H$\alpha$ line profile suggest that the circumstellar gaseous disk is predominantly circumbinary. The relatively low mass of the gainer led us to a suggestion that 3 Pup should be excluded from the B[e] supergiant group and moved to the FS CMa group. Overall these results further support our original suggestion that FS CMa objects are binary systems, where an earlier mass-transfer caused formation of the circumstellar envelope.

中文翻译：

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银河系 B[e] 超巨星的性质。V. 3 Pup——约束轨道参数和模拟环绕恒星环境

我们报告了对具有 B[e] 现象 3 Pup = HD 62623 的 A 型超巨星的长期光谱监测结果。我们证实了早期的发现，它是一个双星系统。轨道参数是使用 4460-4632 A 范围内光谱的互相关得出的，其中包含超过 30 条吸收线。发现轨道为圆形，周期为 $137.4\pm0.1$ 天，径向速度半幅度 $K_{1} = 5.0\pm0.8$ km s$^{-1}$，系统径向速度 $\gamma = +26.4\pm2.0$ km s$^{-1}$，质量函数 $f(m) = (1.81^{+0.97}_{-0.76})\times10^{-3}$ M $_{\dot}$。该物体可能是从一对初始质量为 $\sim$6.0 M$_{\odot}$ 和 $\sim$3.6 M$_{\odot}$ 的对演化而来，初始轨道周期为 $\sim$5 天。基于 A 超巨星的基本参数（光度 $\log$ L/L$_{\odot} = 4.1\pm$0. 1 和有效温度 T$_{\rm eff} = 8500\pm$500 K) 和传质双星的演化轨迹，我们发现增益器的当前质量 M$_{2} = 8.8\pm$0.5 M$_{ \odot}$ 和捐赠者 M$_{1} = 0.75\pm0.25$ M$_{\odot}$。我们还对物体的 IR 过剩进行了建模，并在光学薄的尘埃盘中推导出了 $\sim 5\,\times10^{-5}$ M$_{\odot}$ 的尘埃质量。H$\alpha$ 线剖面的轨道参数和性质表明，星际气体盘主要是环绕双星的。获得者相对较低的质量使我们建议将 3 Pup 排除在 B[e] 超巨星群之外，并移至 FS CMa 群。总的来说，这些结果进一步支持了我们最初的建议，即 FS CMa 天体是双星系统，其中较早的质量转移导致了星周包层的形成。