Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3181
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dc.contributor.authorDietrich, M-
dc.contributor.authorPeterson, B. M-
dc.contributor.authorAlbrecht, P-
dc.contributor.authorAltmann, M-
dc.contributor.authorBarth, A. J-
dc.contributor.authorBennie, P. J-
dc.contributor.authorBertram, R.-
dc.contributor.authorBochkarev, N. G-
dc.contributor.authorBock, H-
dc.contributor.authorBraun, J. M-
dc.contributor.authorBurenkov, A-
dc.contributor.authorCollier, S-
dc.contributor.authorFang, L. Z-
dc.contributor.authorFrancis, O. P-
dc.contributor.authorFilippenko, A. V-
dc.contributor.authorFoltz, C. B-
dc.contributor.authorGaessler, W-
dc.contributor.authorGaskell, C. M-
dc.contributor.authorGeffert, M-
dc.contributor.authorGhosh, K. K-
dc.contributor.authorHilditch, R. W-
dc.contributor.authorHoneycutt, R. K-
dc.contributor.authorHorne, K-
dc.contributor.authorHuchra, J. P-
dc.contributor.authorKaspi, S-
dc.contributor.authorKuemmel, M-
dc.contributor.authorLeighly, K. M-
dc.contributor.authorLeonard, D. C-
dc.contributor.authorMalkov, Yu. F-
dc.contributor.authorMikhailov, V-
dc.contributor.authorMiller, H. R-
dc.contributor.authorMorrill, A. C-
dc.contributor.authorNoble, J-
dc.contributor.authorO'Brien, P. T-
dc.contributor.authorOswalt, T. D-
dc.contributor.authorPebley, S. P-
dc.contributor.authorPfeiffer, M-
dc.contributor.authorPronik, V. I-
dc.contributor.authorQian, B. C-
dc.contributor.authorRobertson, J. W-
dc.contributor.authorRobinson, A.-
dc.contributor.authorRumstay, K. S-
dc.contributor.authorSchmoll, J-
dc.contributor.authorSergeev, S. G-
dc.contributor.authorSergeeva, E. A-
dc.contributor.authorShapovalova, A. I-
dc.contributor.authorSkillman, D. R-
dc.contributor.authorSnedden, S. A-
dc.contributor.authorSoundararajaperumal, S-
dc.contributor.authorStirpe, G. M-
dc.contributor.authorTao, J-
dc.contributor.authorTurner, G. W-
dc.contributor.authorWagner, R. M-
dc.contributor.authorWagner, S. J-
dc.contributor.authorWei, J. Y-
dc.contributor.authorWu, H.-
dc.contributor.authorZheng, W-
dc.contributor.authorZou, Z. L-
dc.date.accessioned2008-08-18T11:01:55Z-
dc.date.available2008-08-18T11:01:55Z-
dc.date.issued1998-04-
dc.identifier.citationAstrophysical Journal Supplement Vol. 115, No. 2, pp. 185 - 202en
dc.identifier.issn0067-0049-
dc.identifier.urihttp://hdl.handle.net/2248/3181-
dc.description.abstractResults 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.extent1292201 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherThe American Astronomical Societyen
dc.relation.urihttp://www.journals.uchicago.edu/doi/abs/10.1086/313085en
dc.subjectGalaxies: Activeen
dc.subjectGalaxies: Individual Alphanumeric: 3c 390.3en
dc.subjectGalaxies: Seyferten
dc.titleSteps toward Determination of the Size and Structure of the Broad-Line Region in Active Galactic Nuclei. XII. Ground-based Monitoring of 3C 390.3en
dc.typeArticleen
Appears in Collections:IIAP Publications

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