We report the detection of a new satellite of M31, projected close to M32. And VIII is tidally distorted, with length ~10 kpc and width a few kpc. It contains 5-12 planetary nebulae (PNe) and 1-3 globular clusters, and has a velocity of -204 km/s with respect to M31, some 350 km/s away from M32's velocity. There are also about 4 x 10^5 solar masses of HI, well-separated from the disk, at the same position and velocity. The satellite has luminosity of 1.2-2.4 x 10^8 solar luminosities, and a central surface brightness of order \mu_V=24. Both these values are typical of Local Group dwarf galaxies. Its surface brightness is some 6 magnitudes brighter than any of the stellar streams found in the Milky Way or M31. The three associated globular clusters have reddening consistent with foreground reddening from the Milky Way only, making it likely that the satellite is in front of M31, unlike the giant tidal stream of Ibata et al.(2001), which is behind M31 in the SE quadrant. However, the major axis of And VIII is aligned with the western edge of this giant stream, and we suggest that its unusual fan shape is caused by superposition of two streams, the westernmost of which was tidally stripped from And VIII.
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机译：我们报告检测到一颗新的M31卫星，预计接近M32。 VIII扭曲变形，长度约10 kpc，宽度约几kpc。它包含5-12个行星状星云（PNe）和1-3个球状星团，相对于M31的速度为-204 km / s，与M32的速度相差约350 km / s。在相同的位置和速度下，还有大约4 x 10 ^ 5个太阳质量的HI与磁盘完全分开。卫星的光度为1.2-2.4 x 10 ^ 8太阳光度，中心表面亮度为\ mu_V = 24。这两个值都是本地群矮星系的典型值。它的表面亮度比银河系或M31中发现的任何恒星流都要亮6个数量级。三个相关的球状星团的变红与仅来自银河系的前景变红相一致，这很可能使卫星位于M31的前方，这与Ibata等人（2001）的巨大潮汐流（位于东南SE的M31的后方）不同。象限。但是，And VIII的主轴线与这条大溪流的西边对齐，因此我们建议其异常的扇形是由两股溪流的叠加所引起的，其中最西端的溪流是从And VIII剥离的。
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