Variability in Quasar Light Curves: using quasars as standard candles. (arXiv:2110.03671v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Solomon_R/0/1/0/all/0/1">Rance Solomon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stojkovic_D/0/1/0/all/0/1">Dejan Stojkovic</a>
A relation between the variational slope, $s_F$, and the mean flux, $langle
F rangle$, in the light curves of 59 spectroscopically confirmed quasars is
measured with a dispersion of 0.14dex ranging over three orders of magnitude in
$langle F rangle$. Assuming it holds for quasars in general, not only does
this relation add to our working knowledge of quasar variability but it may
also be used to determine the luminosity distance of a quasar in a model
independent way. Accurately obtaining the luminosity distance would allow
quasars to be added to the cosmic distance ladder, easily extending the ladder
out far beyond the redshifts accessible to type Ia supernovae where
cosmological parameters can be better constrained.
A relation between the variational slope, $s_F$, and the mean flux, $langle
F rangle$, in the light curves of 59 spectroscopically confirmed quasars is
measured with a dispersion of 0.14dex ranging over three orders of magnitude in
$langle F rangle$. Assuming it holds for quasars in general, not only does
this relation add to our working knowledge of quasar variability but it may
also be used to determine the luminosity distance of a quasar in a model
independent way. Accurately obtaining the luminosity distance would allow
quasars to be added to the cosmic distance ladder, easily extending the ladder
out far beyond the redshifts accessible to type Ia supernovae where
cosmological parameters can be better constrained.
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