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We have established an internally consistent Local Group distance framework,using the Galactic Center, the Large Magellanic Cloud, and Messier 31 (M31) asimportant stepping stones. At greater distances, few distance benchmarks areavailable. As a consequence, M87 and/or Virgo cluster distances are ofteninvoked as the next rung on the ladder to more distant objects such as theFornax and Coma clusters. Therefore, we extensively mined the publishedliterature for independently derived distance estimates to either M87 or thecenter of the Virgo cluster. Based on our newly compiled, comprehensivedatabase of 213 such distances, published between 1929 and 2017 July, werecommend an outward extension to our distance framework, $(m-M)_0^{\rm M87} =31.03 \pm 0.14$ mag ($D = 16.07 \pm 1.03$ Mpc; where the uncertainty representsthe Gaussian $\sigma$ of the distribution), based on a subset of recent(post-1990) M87/Virgo cluster distance measurements. The most stable distancetracers employed here were derived from analysis of both primary and secondarydistance indicators. Among the former, we preferentially rely on Cepheidperiod--luminosity relations and red-giant-branch terminal magnitudes; ourpreferred secondary distance tracers are surface brightness fluctuations. Ourupdated distance modulus to M87 implies a slightly reduced black hole mass of$(5.9 \pm 0.6) \times 10^9 M_\odot$ with respect to that determined by theEvent Horizon Telescope collaboration.

Clustering of Local Group distances: publication bias or correlated measurements? VI. Extending to Virgo cluster distances