M dwarfs with masses 0.1 = 66.67 mas) from which we have created a sample of 413 M dwarfs for spectroscopic study. We present the mass function for these 512 M dwarfs, which increases with decreasing stellar mass in linear mass space, but is flat in logarithmic mass space. As part of this sample, we present new VRI photometry for 17 targets, measured as a result of the RECONS group's long-term work at the CTIO/SMARTS 0.9m telescope. We also note the details of targets that are known to be members of multiple systems and find a preliminary multiplicity rate of 21 +/- 2% for the primary M dwarfs in our sample, when considering known stellar and brown dwarf companions at all separations from their primaries. We further find that 43 +/- 2% of all M dwarfs with masses 0.1 <= M/M_sol <= 0.3 are found in multiple systems with primary stars of all masses within 15 pc.

中文翻译：

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质量为 0.1 ≤ M/M ⊙ ≤ 0.3 的 M 个矮星的体积完整样本在 15 秒差距内

质量为 0.1 = 66.67 mas 的 M 矮星），我们从中创建了 413 M 矮星的样本用于光谱研究。我们展示了这 512 M 矮星的质量函数，它在线性质量空间中随着恒星质量的减少而增加，但在对数质量空间中是平坦的。作为这个样本的一部分，我们展示了 17 个目标的新 VRI 光度测量，这是 RECONS 小组在 CTIO/SMARTS 0.9m 望远镜的长期工作的结果。我们还注意到已知是多个系统成员的目标的详细信息，并在我们的样本中发现原始 M 矮星的初步多重率为 21 +/- 2%，当考虑已知的恒星和棕矮星伴星时他们的初选。我们进一步发现，质量为 0.1 <= M/M_sol <= 0 的所有 M 矮星中有 43 +/- 2%。