Constraining variability of coupling constants with bright and extreme quasars

The 'extreme Population A (xA) quasars' approaching, sometimes exceeding the Eddington limit, are a type of quasars that could serve as standard candle to measure distances too large for supernovae Ia (SNe Ia) be observable. For using xA candles, it would beneficial know how their luminosities vary if coupling constants varied over cosmic time. Alternatively, when calibrated SN candle, quasar observations constrain variation constants. We show Hubble diagram provides same constraint on constants' SNe from Pantheon data. concurrently in our model, i.e., speed light $c$, gravitational constant $G$, Planck $h$, and Boltzmann $k$, interrelated $G\thicksim c^{3}\thicksim h^{3}\thicksim k^{3/2}$. thus determined can expressed terms $H_{0}$ $(\dot{G}/G)_{0}=3(\dot{c}/c)_{0}=3(\dot{h}/h)_{0}=1.5 (\dot{k}/k)_{0}=5.4H_{0} =3.90(\pm 0.04)\times 10^{-10} yr^{-1}$, where subscript 0 is current This conclusion corroborated with analysis data correlated UV X-ray emissions.