Kris Davidson and Hagai Netzer: Emission lines of quasars and similar objects those of galaxies. However, some quasars were seen to fluctuate in br ightness within a few years or less; this meant, according to arguments involving light- travel times, that the luminous souces must be smaller than a few light-years across, tiny compared with any galaxy and far too small to be resolved optically.
Quasar radiation is absorbed mainly along the entire line of sight of the “inter-galactic medium” (IGM), including intervening galaxies and the ISM of the Milky Way. PKS 0454+0339, z = 1.34 Typical moderate-z quasar spectrum showing the dominant Ly emission line and many absorption lines, especially many Ly .
10/15/2020 · Where are the missing emissions? While it may seem strange to not be able to detect broad emission lines of a quasar, in actuality, it is not uncommon if the quasar is obscured. This is because the broad lines can easily be absorbed by obscuring materials, such as gas and dust around the accretion disk. However, this is unlikely to be the case for PSO J083+11: first, because there is no clear.
Distributions of broad emission line equivalent widths (EWs) in SDSS quasars at z>3 WLQs were originally defined as quasars having EW ? 15.4 Å for the Ly?+N Vemission-line complex (EW ? 10 Å for C IV). The Inner Regions of Quasars, UT Austin, September 13, 2014 WLQs: History and Mystery, Margaret Burbidge, Yakov Zeldovich, Maarten Schmidt, Edwin Ernest Salpeter, John Gatenby Bolton, Pulsar, Active Galactic Nucleus, Neutron Star, Blazar, Supernova
