For the Milky Way, this quantity can be written as A r sin of 2 l where A is an Oort constant. Thecorrelation of the spread of this quantity with luminosity can be improved by including a parameter forsurface brightness, such as in the fundamental plane. This quantity is plotted against radius in a rotationcurve. The dispersion of this quantity is empirically correlated to the luminosity of an elliptical galaxy bythe Faber-Jackson relation. Small variations in a star's proper motion can be observed in one form of thisquantity, which forms the basis for a method for detecting extrasolar planets; that is the radial form of thisquantity, which i
For the Milky Way, this quantity can be written as A r sin of 2 l where A is an Oort constant. Thecorrelation of the spread of this quantity with luminosity can be improved by including a parameter forsurface brightness, such as in the fundamental plane. This quantity is plotted against radius in a rotationcurve. The dispersion of this quantity is empirically correlated to the luminosity of an elliptical galaxy bythe Faber-Jackson relation. Small variations in a star's proper motion can be observed in one form of thisquantity, which forms the basis for a method for detecting extrasolar planets; that is the radial form of thisquantity, which is usually measured with the Doppler effect. The Hubble constant relates this parameter ofa galaxy to its distance. For 10 points, identify this quantity whose escape form, for a black hole, is greaterthan the speed of light
For the Milky Way, this quantity can be written as A r sin of 2 l where A is an Oort constant.
radial velocity 