English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Here we present the results of the long-term (1995-2007) spectral monitoringof the broad line radio galaxy \object{3C~390.3}, a well known AGN with thedouble peaked broad emission lines, usually assumed to be emitted from anaccretion disk. To explore dimensions and structure of the BLR, we analyze thelight curves of the broad H$\alpha$ and H$\beta$ line fluxes and the continuumflux. In order to find changes in the BLR, we analyze the H$\alpha$ andH$\beta$ line profiles, as well as the change in the line profiles during themonitoring period. First we try to find a periodicity in the continuum andH$\beta$ light curves, finding that there is a good chance for quasi-periodicaloscillations. Using the line shapes and their characteristics (as e.g. peaksseparation and their intensity ratio, or FWHM) of broad H$\beta$ and H$\alpha$lines, we discuss the structure of the BLR. Also, we cross-correlate thecontinuum flux with H$\beta$ and H$\alpha$ lines to find dimensions of the BLR.We found that during the monitoring period the broad emission component of theH$\alpha$ and H$\beta$ lines, and the continuum flux varied by a factor of$\approx $4-5. Also, we detected different structure in the line profiles ofH$\alpha$ and H$\beta$. It seems that an additional central component ispresent and superposed to the disk emission. In the period of high activity(after 2002), H$\beta$ became broader than H$\alpha$ and red wing of H$\beta$was higher than the one of H$\alpha$. We found time lags of $\sim$95 daysbetween the continuum and H$\beta$ flux, and about 120 days between thecontinuum and H$\alpha$ flux. Variation in the line profiles, as well ascorrelation between the line and continuum flux during the monitoring period isin the favor of the disk origin of the broad lines with the possiblecontribution of some additional region and/or some kind of perturbation in thedisk.

Spectral optical monitoring of 3C390.3 in 1995-2007: I. Light curves and flux variation of the continuum and broad lines