Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · astro-ph/0309149

Completion of a Survey and Detailed Study of Double-Peaked Emission Lines in Radio-Loud AGNs

M. Eracleous·J. P. Halpern
View original source ↗Read source document ↗Export metadata ↓

Abstract

We report the completion of a survey of radio-loud AGNs begun in an earlier paper, aimed finding and studying broad, double-peaked Balmer lines. We present Ha spectra of 13 broad-lined objects (3 with double-peaked Ha profiles). The final sample includes 106 radio-loud AGNs. 20% of the objects have Ha lines with double peaks or twin shoulders and of these, 60% can be fitted quite well with a model attributing the emission to a circular, relativistic, disk. We also compare the Hb and MgII profiles of 4 objects with models of photoionized accretion disks and find them to be in reasonable agreement. Double-peaked emitters stand out on the basis of the following properties: (1) unusually large contribution of starlight to the optical continuum around Ha, (2) unusually large equivalent widths of low-ionization lines ([OI] and [SII]), (3) unusually large [OI]/[OIII] ratios, and (4) Balmer lines on average twice as broad as in other radio-loud AGNs. We evaluate models for the origin of the lines and we find accretion-disk emission to be the most successful one because it can explain the double-peaked line profiles and it also offers an interpretation of the spectroscopic properties of these objects. Aternative suggestions (binary broad-line regions, bipolar outflows, anisotropically illuminated spherical broad-line regions) are unsatisfactory because (a) they fail direct observational tests, (b) they cannot explain the unusual properties of double-peaked emitters self-consistently, or (c) their physical foundations appear to be unsound. We suggest that in double-peaked emitters and accretion- powered LINERs the accretion rate is considerably lower than the Eddington rate with the consequence that the inner accretion disk takes the form of an ion torus and the wind that normally enshrouds the disk proper is absent.

Explore related subjects

astro-ph

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

M. Eracleous, J. P. Halpern. 2003-09-17. Completion of a Survey and Detailed Study of Double-Peaked Emission Lines in Radio-Loud AGNs. https://doi.org/10.1086/379540

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↗