The Boötis stars are population I A-type stars which show marked deficiencies in the iron-peak elements. Spectral analysis indicates that the most extreme of these stars can have metal deficiencies of nearly 2 dex below the sun. Interestingly, they show nearly solar abundances of C, N, O, and S. These stars are recognized spectroscopically by their weak Mg II 4481 lines. However, since many peculiar types near A0 have weak 4481 lines, to confirm a star as a Boötis star, it is also necessary to show that it is metal-weak. This can be done by first ascertaining the hydrogen-line type of the star, as the hydrogen lines are probably the best indicators of the effective temperature. Notice that the hydrogen lines of HD 142703 are best matched by the F0 V standard, HD 23585, whereas the metallic-line spectrum is only slightly stronger than A0. This clearly indicates that the star is metal-weak. The very broad hydrogen lines of the type star, Boo itself, indicate that it is an early A-type star, near to the ZAMS. Many Boötis stars are young; a few have been discovered in the Orion Association, including HD 37411, which is an Ae star. Many Boötis stars show evidence of circumstellar material, either in the form of dust, or shell absorption.