Hostname: page-component-78c5997874-ndw9j Total loading time: 0 Render date: 2024-11-19T08:49:46.767Z Has data issue: false hasContentIssue false
  • English
  • Français

BL Lacertae objects as an evolutionary population*

Published online by Cambridge University Press:  19 July 2016

A. Cavaliere ,
E. Giallongo  and
F. Vagnetti
A. Cavaliere
Affiliation:
Astrofisica, Dip. Fisica, II Univ. Roma, Italy
E. Giallongo
Affiliation:
Ist. Astronomia, Univ. Padova, Italy
F. Vagnetti
Affiliation:
Ist. Astronomico, I Univ. Roma, Italy

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

If the BL Lac Objects are active nuclei with a beamed component that is dominant when directed at us, their observed luminosity function must comprise a flat faint branch: N(L)dL ∝ L1+1/pdL with p=4.5 (Urry and Shafer 1984). If this is flatter than the LF NP(L) of the parent objects at equal observed L, then we expect the counts of BL Lacs to flatten out in turn at fluxes quite higher than the counts of the parents, even when both populations evolve strongly and uniformly with comparable timescales (Cavaliere, Giallongo and Vagnetti 1985).

Type
V. Cosmological Studies, Clustering, Isotropy etc
Information
Symposium - International Astronomical Union , Volume 119: Quasars , 1986 , pp. 491 - 492
Copyright
Copyright © Reidel 1986 

References

Cavaliere, A., Giallongo, E., Vagnetti, F. 1985, Astr. Ap., in press (CGV).Google Scholar
Cheng, F.Z. et al. 1985, M.N.R.A.S. 212, 857.Google Scholar
Maccacaro, T. et al. 1984, Ap. J. (Letters) 284, L23.Google Scholar
Setti, G., and Woltjer, L. 1982, in ‘Astrophysical Cosmology’, Pont. Acad. Scientiarum Scripta Varia 48, 315.Google Scholar
Urry, C.M. 1984, , Johns Hopkins University.Google Scholar
Urry, C.M. and Shafer, R.A. 1984, Ap. J. 280, 569.Google Scholar