be able to use the equation, intensity \(I = \dfrac{L}{4πd^2}\) where L is luminosity and d is distance from the source

understand how astronomical distances can be determined using trigonometric parallax

understand how astronomical distances can be determined using measurements of intensity received from standard candles (objects of known luminosity)

be able to sketch and interpret a simple Hertzsprung-Russell diagram that relates stellar luminosity to surface temperature

understand how to relate the Hertzsprung-Russell diagram to the life cycle of stars

understand how the movement of a source of waves relative to an observer/detector gives rise to a shift in frequency (Doppler effect)

be able to use the equations for redshift \(z = \dfrac{∆λ}{λ} ≈ \dfrac{∆f}{f} ≈ \dfrac{v}{c}\) for a source of electromagnetic radiation moving relative to an observer and \(v = H_0d\) for objects at cosmological distances

understand the controversy over the age and ultimate fate of the universe associated with the value of the Hubble constant and the possible existence of dark matter.