Quasar mass function represents accretion.BH mass scaling relation at low-z still valid at.How fast can the most massive high-z BH grow? z6.42 quasar stronger dust emission with higher. But how about dust? Timescale problem running.? disk and emission line regions form in very Lack of evolution in UV, emission line and X-ray.normal stars existed at very high-z in quasar.Type Ia is not critical in Fe production.Normal IMF is sufficient (given high SFR).Metallicity in BLR of z6 quasars 1 - 10 solar.Question can we generalize the conclusion drawnįrom regions around central BHs to the whole.Fe II emission ? type II SNe some could be Pop.NV emission ? multiple generation of star.Strong metal emission ? consistent with.High-z quasars and their environments mature.Quasar env has supersolar metallicity - metal.Rapid chemical enrichment in quasar vicinity.The Lack of Evolution in Quasar Intrinsic IzJ composite (z_lim 26) Pentericci et al. Another hint of quasars at zgt3 being somewhat.The statistical properties of quasar host DM Clustering provides the most effective probe to.Bias factor of quasars ? average DM halo mass.Quasar Two-point Correlation Function from SDSS Similar to the early growth of massive galaxies?.Implies that more luminous quasars grow early in.Simple luminosity evolution clearly not a good.Spectroscopic follow-up using 300-fiber HectospecĮvolution of faint quasars in SDSS Deep Survey.Down to 25 mag in SDSS bands with repeated.270 deg along Fall Equator in the Southern.SDSS Southern Deep Spectroscopic Survey.Different formation mechanism at low and high-z?.Transition at z3 (where quasar density peaks in.Bright-end slope of QLF is a strong function of.How does optically-selected quasar population.At high-luminosity X-ray and optical traces the.Billion solar mass BH at z6 indicates very.Mass estimate using emission line width toĪpproximate gravitational velocity, accurate to a Quasars ? quasar BH estimate valid at high-z BH Lack of spectral evolution in high-redshift Little or no feedback to stop BH/galaxy growth.Initial assembly from seed BH at zgtgt10.How to assemble such mass BHs and their host.Much massive halos existed at z6, but.Even the largest N-body simulation not big enough.The largest halo in Millennium simulation (500.Assembly of massive dark matter halo environment?.rare, 5-6 sigma peaks at z6 (density of 1 per.Density declines by a factor of 40 from between.High redshift, different from normal galaxies, Dust and star formation in high-z quasar hostĤ6,420 Quasars from the SDSS Data Release Three.Evolution of quasar spectra and metallicity.High-z quasar clustering and environment.Complete sample for bright quasars at z6.Hennawi,Gunn,Becker,White,Rix,Pentericci, Walter, CollaboratorsStrauss,Schneider,Richards,.You may still register to attend the meeting until September 1st, 2018.Title: Evolution of High-Redshift Quasars This conference aims to bring together both theorists and observers working on the various astronomical passbands to discuss the latest developments in this exciting field.ĭeadlines: Abstract submission is now closed. In the next few years, advances in telescope instrumentation, the emergence of massive spectroscopic surveys, as well as developments in theory and computation will deepen our understanding of the IGM as a probe of cosmology and the cosmic reionization events. Observations of absorption lines in quasar and galaxy spectra from the present until redshift 7 provide a thermal and chemical record of the IGM, enable precision measurements of density fluctuations and the geometry of the early Universe, and provide invaluable insights into the physical processes shaping galaxy formation. The complex interplay of these processes determines the physical state of the intergalactic gas over cosmic time. The IGM evolves into the clumpy cosmic web, which is the source of gas that cools and accretes onto galaxies powering star-formation, and a sink for the metal enriched material, energy, and radiation which galaxies eject. The stars and black holes in the first galaxies emitted copious amounts of ionizing radiation, singly ionizing hydrogen and helium at z~10, and later doubly ionizing Helium at z~3, thus reheating and reionizing the cosmos. Overview: As the dominant reservoir of baryons in the Universe, the intergalactic medium (IGM) plays a crucial role in the history and evolution of cosmic structure.
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