Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · astro-ph/9910550

The infrared polarizations of high-redshift radio galaxies

Gareth Leyshon
View original source ↗Read source document ↗Export metadata ↓

Abstract

This thesis reports the K-band polarizations of a representative sample of nine radio galaxies: seven 3C objects at 0.7 < z < 1.3, and two other distinctive sources. Careful consideration is given to the accurate measurement and `debiasing' of faint polarizations, with recommendations for the function of polarimetric software. 3C 22 and 3C 41 both have 3% polarization perpendicular to their radio structures, consistent with suggestions that they may be obscured quasars. 3C 54 is polarized at 6%, parallel to its radio structure. 3C 65 and 3C 356 are faint: the noisy measurements give no firm evidence for polarization. MRC 0156-252 at z~2 is found to be unpolarized in K. 3C 114 has a complex structure of four bright knots, one offset from the radio structure and three along the axis. There is strong evidence for polarization in the source as a whole (12%) and the brightest knot (5%). 3C 441 lies in a rich field; one of its companions appears to be 18% polarized. The identification of the knot containing the active nucleus has been disputed, and is discussed. LBDS 53W091 was controversially reported to have a 40% H-band polarization. No firm evidence is found for non-zero K-band polarization in 53W091, though there is some evidence for its companion being polarized. The object is discussed in the context of other radio-weak galaxies. Simple spectral and spatial models for polarization in radio galaxies are discussed and used to interpret the measurements. The important cosmological question of the fraction of K-band light arising in radio galaxy nuclei is considered: in particular, the contribution of scattered nuclear light to the total K-band emission is estimated to be of order 7% in 3C 22 and 3C 41, 26% in 3C 114, and tentatively 25% or more in 3C 356.

Explore related subjects

astro-ph

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Gareth Leyshon. 1999-10-29. The infrared polarizations of high-redshift radio galaxies. https://arxiv.org/abs/astro-ph/9910550

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2023

Dark Energy is the Cosmological Quantum Vacuum Energy of Light Particles-The Axion and the Lightest Neutrino

We uncover the general mechanism producing the dark energy(DE). This is only based on well known quantum physics and cosmology. We show that the observed DE originates from the cosmological quantum vacuum of light particles which provides a continuous energy distribution able to reproduce the data. Bosons give positive contributions to the DE while fermions yield negative contributions. As usual in field theory, ultraviolet divergences are subtracted from the physical quantities. The subtractions respect the symmetries of the theory and we normalize the physical quantities to be zero for the Minkowski vacuum. The resulting finite contributions to the energy density and the pressure from the quantum vacuum grow as log a(t) where a(t) is the scale factor, while the particle contributions dilute as 1/a^3(t), as it must be for massive particles. The DE equation of state P = w(z)H turns to be w(z)<-1 with w(z) asymptotically reaching the value -1 from below.A scalar particle can produce the observed DE through its quantum cosmological vacuum provided:(i)its mass is of the order of 10^{-3} eV = 1 meV,(ii) it is very weakly coupled and (iii) it is stable on the time scale of the age of the universe. The axion vacuum thus appears as a natural candidate. The neutrino vacuum (especially the lightest mass eigenstate) can give negative contributions to the DE. We find that w(z=0) is slightly below -1 by an amount ranging from [-1.5 10^{-3}] to [-8 10^{-3}] and we predict the axion mass to be in the range between 4 and 5 meV. We find that the universe will expand in the future faster than the de Sitter universe, as an exponential in the square of the cosmic time. DE arises from the quantum vacua of light particles in FRW cosmological space time in an analogous way to the Casimir effect in Minkowski spacetime with non trivial boundaries.

astro-ph↗
arXiv2023

Scaling of Black Hole Accretion Discs from Gamma-Ray Bursts and Black Hole X-Ray Binaries to Active Galactic Nuclei

I consider how physical processes scale over eight orders of magnitude in black hole mass, from stellar masses in gamma-ray bursts (GRB) and black-hole X-ray binaries (BHXRB) to supermassive active galactic nuclei (AGN). Accretion rates onto stellar mass black holes range over more than sixteen orders of magnitude, from the lower luminosity BHXRB to GRB. These enormous parameter ranges correspond to qualitative as well as quantitative differences in behavior. The fundamental questions involve the balance between nonequilibrium and thermalized plasmas. When energy fluxes exceed a critical value $\sim 10^{29}$ erg/cm$^2$s, as in GRB, a black-body equilibrium pair plasma forms. At the lower fluxes found in AGN, BHXRB and microquasars, accretion power electrodynamically accelerates a small number of very energetic particles, explaining their non-thermal spectra and the high energy gamma-ray emission of blazars. Ultra-high energy cosmic rays may be accelerated by massive black holes, otherwise undetectable, with very low thermal luminosities. New-born fast high-field pulsars may be in the black-body equilibrium regime, resembling SGR in permanent outburst. I also consider the question, significant for the acceleration of nonthermal particles in GRB outflows, of whether collisionless plasmas interpenetrate rather than forming hydrodynamic shocks, and propose this as an alternative to internal shock models of GRB. A new appendix attempts to explain why AGN are, proportionally, more efficient accelerators of energetic particles than stellar mass black holes.

astro-ph↗