We introduce the cosmological principle and the geometry of homogeneous and isotropic spacetimes with three spatial dimensions. This will allow us to go on to calculate distance-related observables, a...We introduce the cosmological principle and the geometry of homogeneous and isotropic spacetimes with three spatial dimensions. This will allow us to go on to calculate distance-related observables, an important step toward predicting observable consequences of the expansion.
We begin to work out observational consequences of living in an expanding spatially homogeneous and isotropic universe. In this and the next two chapters we derive Hubble's Law, \(v = H_0 d\), and a m...We begin to work out observational consequences of living in an expanding spatially homogeneous and isotropic universe. In this and the next two chapters we derive Hubble's Law, \(v = H_0 d\), and a more general version of it valid for arbitrarily large distances.
We begin to work out observational consequences of living in an expanding spatially homogeneous and isotropic universe. In this chapter we introduce the concept of redshift and work out the relationsh...We begin to work out observational consequences of living in an expanding spatially homogeneous and isotropic universe. In this chapter we introduce the concept of redshift and work out the relationship between it and the history of the expansion.
