Optical Brightness Variations in a Sample of Nineteen Radio-Quiet Quasi-Stellar Objects

Cover Optical Brightness Variations in a Sample of Nineteen Radio-Quiet Quasi-Stellar Objects
Optical Brightness Variations in a Sample of Nineteen Radio-Quiet Quasi-Stellar Objects
Edwards, Patricia Louise
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Figure 55 shows variability index (V.I.) versus log z for the RQQSO sample. Redshift (z) is also marked along the horizontal axis. As is suggested by the graph, the more variable of the 139 ~1 CD, - ) C o CD *—, c u •H _J CD 71 0) X , CL CD u o o l0 d CD O r CD O D 0) O o CM H > m CM O 140 ~> CD o > CD O O _J m X , CL CD L 00 .
o O in o o 00 "6 o o o > I CD > n C\J O i O 141 —) CD —) O DO o u if) _J CD CD in o CD C O GO O o > o 3 CM CO H > CO CM O 142 143 o 00 6 CD 6 6 C\J d o d C\J d 144 N CO
...2 N "^ -CO - CM CD O d C\J O O lO o "o c 9' 145 objects have low redshifts. The linear correlation coefficient is 0.43 for V.I. versus z and 0.39 for V.I. versus log z. The closer RQQSOs are more likely to be variable. If the redshift is cosmological, the closer RQQSOs are also older and at a later stage in their evolution.
At low redshifts, objects can be observed which are fainter intrinsically than could be observed at greater distances. Since the correlation between V.I. and B suggested that objects fainter in apparent magnitude, which might be expected to be more distant, were more likely to vary, a relative intrinsic brightness (R.I.B.


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