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
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In our eReader you can find the full English version of the book. Read Optical Brightness Variations in a Sample of Nineteen Radio-Quiet Quasi-Stellar Objects Online - link to read the book on full screen. Our eReader also allows you to upload and read Pdf, Txt, ePub and fb2 books. In the Mini eReder on the page below you can quickly view all pages of the book - Read Book Optical Brightness Variations in a Sample of Nineteen Radio-Quiet Quasi-Stellar Objects
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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.
What to read after Optical Brightness Variations in a Sample of Nineteen Radio-Quiet Quasi-Stellar Objects?
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To quickly assess the difficulty of the text, read a short excerpt:
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.
What to read after Optical Brightness Variations in a Sample of Nineteen Radio-Quiet Quasi-Stellar Objects?
You can find similar books in the "Read Also" column, or choose other free books by Edwards, Patricia Louise to read onlineMoreLess
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