On the absence of broad MgII emission-line variability in NGC3516 during 1996.

Details On the absence of broad MgII emission-line variability in NGC3516 during 1996. On the absence of broad MgII emission-line variability in NGC3516 during 1996.

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...191.7810g&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #78.10; Bulletin of the American Astronomical Society, Vol. 29, p.1335

Astronomy and Astrophysics

Astronomy

Scientific paper

We report the first results of an 11 month HST/FOS monitoring campaign of the broad emission-line region in the Seyfert 1 nucleus NGC 3516. During the campaign the UV continuum showed a factor of 5 variation; correspondingly the strongest broad UV emission-lines (e.g. Lyalpha , CIV) displayed a somewhat weaker, though still significant variation (a factor of 2). In contrast, no variation was detected in either the strong broad MgII emission-line or in the many strong blended lines of FeII from lambda lambda 2200--3400 Angstroms. While historically the flux in the broad MgII emission-line has varied (a factor of 2 within a few years), the profile shape has remained unchanged for at least a decade. In contrast, the high ionization lines (HILs, e.g. Lyalpha , CIV) show both emission-line flux and profile changes on relatively short timescales, which appear to be correlated with changes in the continuum level. Differences between the rms and steady-state profiles of the HILs suggests that the variable component originates in a distinct (both spatially and kinematically) region of the BLR. Significantly, on Feb 21st 1996, the profile shapes of the HILs and MgII were identical. This suggests that the non-variable component of these lines either (a) arises from the same cloud population, or (b) is formed in self-similar structures (e.g. a terminal wind).

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