Cosmology (Observables-Inflation). Obtain:

a)

b)

HInt:

Amplitude for scalar perturbations, In(1010A3) = 3.094 0.034 = Slightly red scalar index ng = 0.9645 + 0.0049 Amplitude for scalar perturbations, In(1010A,) = 3.094 = 0.034 [2] As discussed at the end of the last section, this corresponds to the ampli- tude for the fluctuations in the spatial curvature which can be related to the anisotropies in the CMB. This amplitude has been known since the COBE satellite measured it, but we provide the most recent measurement of it from the Planck satellite Slightly red scalar index ns = 0.9645 +0.0049 [2] Even though the amplitude for scalar perturbations is nearly constant for all wavelengths, there is a slight tilt to the 'red' end of the spectrum. This means that there is slightly more power for longer wavelength than for shorter ones. One of the general predictions of inflation is a slightly red spectrum. Amplitude for scalar perturbations, In(1010A3) = 3.094 0.034 = Slightly red scalar index ng = 0.9645 + 0.0049 Amplitude for scalar perturbations, In(1010A,) = 3.094 = 0.034 [2] As discussed at the end of the last section, this corresponds to the ampli- tude for the fluctuations in the spatial curvature which can be related to the anisotropies in the CMB. This amplitude has been known since the COBE satellite measured it, but we provide the most recent measurement of it from the Planck satellite Slightly red scalar index ns = 0.9645 +0.0049 [2] Even though the amplitude for scalar perturbations is nearly constant for all wavelengths, there is a slight tilt to the 'red' end of the spectrum. This means that there is slightly more power for longer wavelength than for shorter ones. One of the general predictions of inflation is a slightly red spectrum