Hostname: page-component-7bb8b95d7b-dvmhs Total loading time: 0 Render date: 2024-09-11T03:08:28.107Z Has data issue: false hasContentIssue false
  • English
  • Français

Some Peculiarities of Variable Optical Spectra of 11 Low-Redshift Quasars

Published online by Cambridge University Press:  19 July 2016

I.I. Pronik
I.I. Pronik*
Affiliation:
Crimean Astrophysical Observatory, Ukraine

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.

The flux of narrow 5007 Å [OIII] forbidden line during last 20 years is accepted as a bench-mark for calibration of the continuum and broad-lines fluxes in AGN. But one can not get away from the problem of the forbidden lines variability in these objects. The first report were published by Bardin et al. (1967). Some of the results are revieved by V. Pronik, I. Pronik (1988, 1992). There were 4 years monitoring of [OIII] fluxes variability in the Seyfert galaxy NGC 1275 nucleus (Pronik et al., 1990). Now we reexamine the published data of W. Zheng et al. (1986, 1987, 1988), discussed earlier in supposition of forbidden lines constant in spectra of 11 low-redshifted QSOs. Maximal calibration coefficients adopted by W. Zheng et al. in supposition of [OIII] lines constant were in the interval 2.0–3.6. On the other hand the fluxes errors are about 15%. Disagreement is very high. This is one of the arguments in the forbidden lines variability Tightness.

Type
Poster contributions: Statistical Studies and Evolution
Information
Symposium - International Astronomical Union , Volume 159: Multi-Wavelength Continuum Emission of AGN , 1994 , pp. 518
Copyright
Copyright © Kluwer 1994 

References

Bardin, B., Chopinet, M., Duflot-Augarde, R.: 1967, Comp. Rendus Acad. Sci. Paris, vol. 265, Serie B, P.1149. Bochkarev, N.: 1987, Proceed. IAU Sym. 121 , eds. Khachikian, E. et al., Reidel Publ. Comp., P.223.Google Scholar
Fabrika, S.: 1987, In “Active nuclei and stars cosmology”, ed. Martinov, D., Moscow Univ. Press, P.107.Google Scholar
Pronik, I., Merkulova, N., Metik, L.: 1990, Astrophys. a. Space Sci , vol. 171, P.91.CrossRefGoogle Scholar
Pronik, I., Pronik, V.: 1992, Astronomical a. Astrophys. Trancac , Vol. 3, P.57.Google Scholar
Pronik, V. Pronik, I.: 1988, Russian Astron. J , Vol. 65, P.478.Google Scholar
Zheng, W.: 1988, Astrophys. J. , Vol. 324, P.801.Google Scholar
Zheng, W., Burbidge, E.M.: 1986, Astrophys. J. , Vol. 306, P. L 67.CrossRefGoogle Scholar
Zheng, W., Burbidge, E.M., Smith, H.E., Cohen, R.D., Bradley, S.E.: 1987, Astrophys. J. , Vol. 322, P.164.Google Scholar