This publication (_publish isn't a noun, guys_) is just a markdown file with a few words about my new LBRY wallet server, which has the "variable decay" trending algorithm running on it. It gives the IP address of the server in case you want to connect to it, and I'm charging a modest fee so that the wallet server doesn't get too many users. I can't guarantee that I'll maintain the server long term, but you can expect it to be up for at least the next couple of months. This server might be of interest to you if: (a) you use the LBRY desktop app (i.e., real LBRY ;)); (b) you're located near Sydney, Australia, where the server is physically located; and (c) you want a more interesting (hopefully) trending list.

This is the authors' version of a Letter published in Nature on October 3rd, 2019. The official version is available [here](https://www.nature.com/articles/s41586-019-1597-1). This is an HTML file. It's probably best read in a web browser, but if you have a big monitor or good eyesight you can probably read it in LBRY. It has also been covered in the press: * [ABC News](https://www.abc.net.au/news/2019-10-03/cannibal-andromeda-galaxy-on-path-to-collide-with-milky-way/11565238) * [The Daily Mail](https://www.dailymail.co.uk/sciencetech/article-7529887/Earth-one-day-swallowed-cannibal-galaxy-envelops-Milky-Way.html)

ABSTRACT: Large galaxies grow through the accumulation of dwarf galaxies1,2. In principle it is possible to trace this growth history using the properties of a galaxy’s stellar halo3,4,5. Previous investigations of the galaxy M31 (Andromeda) have shown that outside a radius of 25 kpc the population of halo globular clusters is rotating in alignment with the stellar disk6,7, as are more centrally located clusters8,9. The M31 halo also contains coherent stellar substructures, along with a smoothly distributed stellar component10,11,12. Many of the globular clusters outside 25 kpc are associated with the most prominent substructures, while others are part of the smooth halo13. Here we report a new analysis of the kinematics of these globular clusters. We find that the two distinct populations are rotating with perpendicular orientations. The rotation axis for the population associated with the smooth halo is aligned with the rotation axis for the plane of dwarf galaxies14 that encircles M31. We interpret these separate cluster populations as arising from two major accretion epochs, likely separated by billions of years. Stellar substructures from the first epoch are gone, but those from the more recent second epoch still remain.