Wolfram Language & System 11.0 (2016)|Legacy Documentation

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UniverseModelData

UniverseModelData[spec]
returns properties of the universe based on the default model at specification defined by the time after the Big Bang, the distance to the comoving object, or the redshift of such an object.

UniverseModelData[spec,model]
returns properties of universe model at spec.

UniverseModelData[spec,property]
returns the specified property at the time or distance spec.

UniverseModelData[spec,property,model]
returns the specified property at the time or distance spec for the universe model.

DetailsDetails

  • The specification spec can be a Quantity object with units of times and distances, or it can be an association with the key "Time" for the age of the universe, "TimeAgo" for the time in the past measured from the present time, "Distance" for the distance to an object, or "Redshift" for the redshift of a distant object. For the keys "Time", "TimeAgo", and "Distance", the values must be Quantity objects.
  • Results are limited to after the epoch of cosmic inflation.
  • UniverseModelData["Models"] returns the list of available models. Use UniverseModelData[model] to learn the values for specific models.
  • UniverseModelData["Properties"] gives the list of all properties available.
  • Properties are returned using Quantity where appropriate.
  • General universe properties include:
  • "UniverseCurvature"curvature of the universe
  • Properties referring to an object seen at a distance that corresponds to a time after the Big Bang include:
  • "AngularDiameterDistance"distance determined by angular diameter
    "ComovingDistance"distance measure not affected by the expansion or contraction of space
    "ComovingVolume"volume of space within the comoving distance
    "ConformalTime"time measure not affected by the expansion or contraction of space
    "DarkEnergyDensityRatio"ratio of dark energy density to the total energy density in the universe
    "Epoch"overall composition of the universe model
    "EventHorizon"maximum distance from which light emitted at a given time can reach the observer in the future
    "HubbleDistance"distance to objects receding from observer at light speed
    "HubbleParameter"rate of expansion of the universe model
    "LuminosityDistance"distance determined by luminosity
    "MatterEnergyDensityRatio"ratio of matter density to the total energy density in the universe
    "MaximumUniverseAge"maximum age the universe can ever reach
    "ParticleHorizon"maximum distance traveled by light from the Big Bang to a given time
    "RadiationEnergyDensityRatio"ratio of radiation density to the total energy density in the universe
    "RadiationTemperature"temperature of background radiation
    "Redshift"shift in wavelength due to expansion or contraction of space
    "ScaleFactor"change in distance due to expansion or contraction of space
    "TimeAgo"time in past measured from the present time
    "TotalObservableRadiusFraction"fraction of the universe seen out of total possible for all time
    "TransverseComovingDistance"comoving distance between two objects located at the same redshift
  • model can be specified by one of the available models, by supplying the parameters for the composition of the universe, or by supplying the model and the parameters that diverge from it.
  • The default universe model is "LambdaCDM".
  • Parameters include:
  • "HubbleH0"Hubble constant H
    "OmegaLambda"ratio of dark energy density to the critical density
    "OmegaMatter"ratio of matter density to the critical density
    "OmegaRadiation"ratio of radiation density to the critical density
    "OmegaK"ratio of curvature density to the critical density
  • All parameters refer to their values now.
  • "HubbleH0" should be a Quantity with dimension of inverse time. All other parameters should be dimensionless or percentage quantities.
  • Parameters should be supplied as an association.
  • Calculations use the FriedmannLemaîtreRobertsonWalker (FLRW) metric, the Friedmann equations, and the equations of state for the matter, radiation, and dark energy components.

ExamplesExamplesopen allclose all

Basic Examples  (3)Basic Examples  (3)

Calculate the scale factor of the universe 100 million years after the Big Bang:

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Determine the redshift of a comoving object a billion light years away:

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Explore properties of cosmological models of arbitrary composition:

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Introduced in 2016
(10.4)