Perseus-Pisces Supercluster: Difference between revisions
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[[File:LaniPP2.png|thumb|left|400px|A representation of Mass Lanes in Laniakea and Perseus-Pisces, and their relative position in space]]The '''Perseus-Pisces Supercluster''' is sometimes referred to as the [[Laniakea Supercluster]]'s mirror image. Several galactic filaments connect the two superclusters around several different voids. The Taurus Void is the main void that separates the two superclusters where they have their nearest concentrations of mass. Perseus-Pisces is the closest supercluster to Laniakea, going by the distance between the centers of mass of the two superclusters. | [[File:LaniPP2.png|thumb|left|400px|A representation of Mass Lanes in Laniakea and Perseus-Pisces, and their relative position in space]]The '''Perseus-Pisces Supercluster''' is sometimes referred to as the [[Laniakea Supercluster]]'s mirror image. Several galactic filaments connect the two superclusters around several different voids. The Taurus Void is the main void that separates the two superclusters where they have their nearest concentrations of mass. Perseus-Pisces is the closest supercluster to Laniakea, going by the distance between the centers of mass of the two superclusters. | ||
Perseus-Pisces was the first supercluster outside of Laniakea to be reached by humankind. it has subsequently been subject to colonization along the edge of the Taurus Void opposite the Virgo Cluster. The total human population in Perseus-Pisces numbers in the low trillions, with several hundred colonies having been established across several galaxies. Explorers have found large swaths of intraclustural plasma and a number of powerful X-ray sources throughout Perseus-Pisces, and have observed a small ratio of planets orbiting stars than in Laniakea. Furthermore, the galaxies in Perseus-Pisces appear to have a lower proportion of red dwarf stars relative to the galaxies in Laniakea. In a qualitative sense, Perseus-Pisces seems to exhibit greater entropy and less overall stability than Laniakea. The reasons for these discrepancies are as yet undetermined. | Perseus-Pisces was the first supercluster outside of Laniakea to be reached by humankind. it has subsequently been subject to [[Colonization of the Universe | colonization]] along the edge of the Taurus Void opposite the Virgo Cluster. The total human population in Perseus-Pisces numbers in the low trillions, with several hundred colonies having been established across several galaxies. Explorers have found large swaths of intraclustural plasma and a number of powerful X-ray sources throughout Perseus-Pisces, and have observed a small ratio of planets orbiting stars than in Laniakea. Furthermore, the galaxies in Perseus-Pisces appear to have a lower proportion of red dwarf stars relative to the galaxies in Laniakea. In a qualitative sense, Perseus-Pisces seems to exhibit greater entropy and less overall stability than Laniakea. The reasons for these discrepancies are as yet undetermined. | ||
[[File:TaurusVoid.png|thumb|right|400px|The Taurus Void between Laniakea and Perseus-Pisces]] | [[File:TaurusVoid.png|thumb|right|400px|The Taurus Void between Laniakea and Perseus-Pisces]] | ||
[[Category: GURPS: Dark Energy]] | [[Category: GURPS: Dark Energy]] | ||
Latest revision as of 21:34, 19 October 2016
The Perseus-Pisces Supercluster is sometimes referred to as the Laniakea Supercluster's mirror image. Several galactic filaments connect the two superclusters around several different voids. The Taurus Void is the main void that separates the two superclusters where they have their nearest concentrations of mass. Perseus-Pisces is the closest supercluster to Laniakea, going by the distance between the centers of mass of the two superclusters.
Perseus-Pisces was the first supercluster outside of Laniakea to be reached by humankind. it has subsequently been subject to colonization along the edge of the Taurus Void opposite the Virgo Cluster. The total human population in Perseus-Pisces numbers in the low trillions, with several hundred colonies having been established across several galaxies. Explorers have found large swaths of intraclustural plasma and a number of powerful X-ray sources throughout Perseus-Pisces, and have observed a small ratio of planets orbiting stars than in Laniakea. Furthermore, the galaxies in Perseus-Pisces appear to have a lower proportion of red dwarf stars relative to the galaxies in Laniakea. In a qualitative sense, Perseus-Pisces seems to exhibit greater entropy and less overall stability than Laniakea. The reasons for these discrepancies are as yet undetermined.
