Results from Hα + continuum and Johnson UBVI imaging for HCG 95 are presented in order to study the star formation history of the galaxies in the group. Based on the spatial distribution of the stellar populations, as well as the morphology of the three-galaxy system A-C1-C2, we propose two possible scenarios for the dynamical evolution of this system: In one of them, each of the nuclei C1 and C2 interacted with the elliptical galaxy at different times, and we are seeing both nuclei together as a projection effect. The other scenario suggests that both nuclei are involved in a merging process, with the resulting merger remnant interacting with the elliptical galaxy. The recent star formation of the system is strongly balanced toward the northern tidal tail and the nucleus C1. We note the presence of a candidate of a young dwarf galaxy which would have been created at the tip of one of the northern tidal tails. A very young population and no signs of an underlying population were detected for this object. Recent spectroscopic observations of the galaxy HCG 95 B yielded a value for its radial velocity of 8000 km s-1, that is, more than 3000 km s-1 less than the rest of galaxies in the group. This new result would imply that galaxy B is a foreground galaxy instead of being physically associated with the group HCG 95. This galaxy appears distorted probably as a result of the close passage of a dwarf satellite that has been detected in the broadband frames and in Hα.
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机译：提出了Hα+连续谱和HCG 95的Johnson UBVI成像的结果，以研究该组星系的恒星形成历史。基于恒星种群的空间分布以及三星系系统A-C1-C2的形态，我们为该系统的动力学演化提出了两种可能的方案：在其中一种中，每个核C1 C2和C2在不同时间与椭圆星系相互作用，我们将两个原子核一起视为投影效应。另一种情况表明，两个原子核都参与了合并过程，导致合并后的残余物与椭圆星系相互作用。该系统最近的恒星形成在北潮汐尾和C1原子核之间具有很强的平衡。我们注意到存在一个年轻的矮星系，该星系可能是在北潮汐尾部之一的尖端产生的。没有发现此对象非常年轻的人口，也没有潜在人口的迹象。最近对HCG 95 B星系的光谱观察得出的径向速度值为8000 km s-1，即比该组中其余星系小3000 km s-1。这一新结果将暗示星系B是一个前景星系，而不是与HCG 95族物理相关。这个星系似乎是扭曲的，这可能是由于在宽带帧和Hα中检测到的矮卫星的近距离通过造成的。 。
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