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Mrk926 is known to be a highly variable AGN with very broad line profiles. Westudied the continuum and line profile variations of this object with hightemporal resolution in order to determine its broad-line region structure andto derive its BH mass. We carried out a high-cadence spectroscopic variabilitycampaign of Mrk926 with the 10m HET telescope, aided by photometric V-band datataken at the Wise Observatory, over a period of about five months. We extractedspectroscopic continuum and line light curves, and computed CCFs as well asvelocity-resolved CCFs with respect to the combined continuum V-band lightcurve. The continuum luminosity of Mrk926 showed a drastic decrease during ourcampaign: it dropped to less than 50% of its original value within only 2.5months. The spectra show complex and very broad Balmer line profiles, includingouter Balmer satellites ranging from +-5000 to +-13,000 kms-1. The Ha, Hb, andHeI5876 line light curves are delayed relative to the continuum light curve.The Ha and Hb lines show two velocity-delay structures in the central part oftheir line profile (within +- 5000 kms-1), at ~10 and ~57 ld and at ~5 and ~48ld, respectively. These structures might be interpreted as the signature of aline-emitting ring, inclined by ~50 deg to the line of sight and orbiting theBH at radii, R, of 33.5 and 26.5 ld. We determined continuum luminosities,log(lambda\,L_(lambda)/erg s-1), of 43.68 to 44.13, which are in good agreementwith the established R_(BLR)-L_(AGN) relation. We derive a black hole mass of1.1 +- 0.2 * 10^8 M_solar; this indicates a low Eddington ratio, whichdecreased from 8 to 3 percent during our campaign. The Balmer satellitecomponents show a response to the continuum variations on the order of only 3-5days. We attribute this to the central line segment and the Balmer satelliteshaving different, spatially distinct regions of origin.

The Great Slump: Mrk926 reveals discrete and varying Balmer line satellite components during a drastic phase of decline