dc.contributor.author | Dietrich, M | |
dc.contributor.author | Peterson, B. M | |
dc.contributor.author | Albrecht, P | |
dc.contributor.author | Altmann, M | |
dc.contributor.author | Barth, A. J | |
dc.contributor.author | Bennie, P. J | |
dc.contributor.author | Bertram, R. | |
dc.contributor.author | Bochkarev, N. G | |
dc.contributor.author | Bock, H | |
dc.contributor.author | Braun, J. M | |
dc.contributor.author | Burenkov, A | |
dc.contributor.author | Collier, S | |
dc.contributor.author | Fang, L. Z | |
dc.contributor.author | Francis, O. P | |
dc.contributor.author | Filippenko, A. V | |
dc.contributor.author | Foltz, C. B | |
dc.contributor.author | Gaessler, W | |
dc.contributor.author | Gaskell, C. M | |
dc.contributor.author | Geffert, M | |
dc.contributor.author | Ghosh, K. K | |
dc.contributor.author | Hilditch, R. W | |
dc.contributor.author | Honeycutt, R. K | |
dc.contributor.author | Horne, K | |
dc.contributor.author | Huchra, J. P | |
dc.contributor.author | Kaspi, S | |
dc.contributor.author | Kuemmel, M | |
dc.contributor.author | Leighly, K. M | |
dc.contributor.author | Leonard, D. C | |
dc.contributor.author | Malkov, Yu. F | |
dc.contributor.author | Mikhailov, V | |
dc.contributor.author | Miller, H. R | |
dc.contributor.author | Morrill, A. C | |
dc.contributor.author | Noble, J | |
dc.contributor.author | O'Brien, P. T | |
dc.contributor.author | Oswalt, T. D | |
dc.contributor.author | Pebley, S. P | |
dc.contributor.author | Pfeiffer, M | |
dc.contributor.author | Pronik, V. I | |
dc.contributor.author | Qian, B. C | |
dc.contributor.author | Robertson, J. W | |
dc.contributor.author | Robinson, A. | |
dc.contributor.author | Rumstay, K. S | |
dc.contributor.author | Schmoll, J | |
dc.contributor.author | Sergeev, S. G | |
dc.contributor.author | Sergeeva, E. A | |
dc.contributor.author | Shapovalova, A. I | |
dc.contributor.author | Skillman, D. R | |
dc.contributor.author | Snedden, S. A | |
dc.contributor.author | Soundararajaperumal, S | |
dc.contributor.author | Stirpe, G. M | |
dc.contributor.author | Tao, J | |
dc.contributor.author | Turner, G. W | |
dc.contributor.author | Wagner, R. M | |
dc.contributor.author | Wagner, S. J | |
dc.contributor.author | Wei, J. Y | |
dc.contributor.author | Wu, H. | |
dc.contributor.author | Zheng, W | |
dc.contributor.author | Zou, Z. L | |
dc.date.accessioned | 2008-08-18T11:01:55Z | |
dc.date.available | 2008-08-18T11:01:55Z | |
dc.date.issued | 1998-04 | |
dc.identifier.citation | Astrophysical Journal Supplement Vol. 115, No. 2, pp. 185 - 202 | en |
dc.identifier.issn | 0067-0049 | |
dc.identifier.uri | http://hdl.handle.net/2248/3181 | |
dc.description.abstract | Results of a ground-based optical monitoring campaign on 3C 390.3 in 1994-1995 are presented. The broadband fluxes (B, V, R, and I), the spectrophotometric optical continuum flux F lambda (5177 A), and the integrated emission-line fluxes of H alpha , H beta , H gamma , He I lambda 5876, and He II lambda 4686 all show a nearly monotonic increase with episodes of milder short-term variations superposed. The amplitude of the continuum variations increases with decreasing wavelength (4400-9000 A). The optical continuum variations follow the variations in the ultraviolet and X-ray with time delays, measured from the centroids of the cross-correlation functions, typically around 5 days, but with uncertainties also typically around 5 days; zero time delay between the high-energy and low-energy continuum variations cannot be ruled out. The strong optical emission lines H alpha , H beta , H gamma , and He I lambda 5876 respond to the high-energy continuum variations with time delays typically about 20 days, with uncertainties of about 8 days. There is some evidence that He II lambda 4686 responds somewhat more rapidly, with a time delay of around 10 days, but again, the uncertainties are quite large (~8 days). The mean and rms spectra of the H alpha and H beta line profiles provide indications for the existence of at least three distinct components located at +/-4000 and 0 km s-1 relative to the line peak. The emission-line profile variations are largest near line center. | en |
dc.format.extent | 1292201 bytes | |
dc.format.mimetype | application/pdf | |
dc.language.iso | en | en |
dc.publisher | The American Astronomical Society | en |
dc.relation.uri | http://www.journals.uchicago.edu/doi/abs/10.1086/313085 | en |
dc.subject | Galaxies: Active | en |
dc.subject | Galaxies: Individual Alphanumeric: 3c 390.3 | en |
dc.subject | Galaxies: Seyfert | en |
dc.title | Steps toward Determination of the Size and Structure of the Broad-Line Region in Active Galactic Nuclei. XII. Ground-based Monitoring of 3C 390.3 | en |
dc.type | Article | en |