How do you calculate the radial velocity of a galaxy?
Rotational speed is directly correlated to a galaxy's luminosity.
Overall, line radiation from a spiral galaxy is "smeared out," or broadened, by its rotation; the faster the rotation, the greater the amount of broadening. Radiation from the galaxy where matter is generally approaching us is blueshifted by the Doppler effect; radiation on the other side is redshifted by a similar amount. This is known as the "Tully-Fisher relation."
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The Doppler shift equation, which is as follows: [ v = c \frac{\Delta \lambda}{\lambda} ] where: - ( v ) is the galaxy's radial velocity; - ( c ) is the speed of light (roughly ( 3 \times 10^8 ) meters per second); - ( \Delta \lambda ) is the wavelength change of the galaxy's light emission relative to its rest wavelength; and - ( \lambda ) is the galaxy's rest wavelength.
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When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.
When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.
When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.
When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.
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