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tokens: be considered constant between all the observations. A simple light-travel argument can then put constraints on the distance between the central source and the reflector. For an edge-on view of the system, , and yr, depending on when the source switched on (between the beginning of 1996 and the beginning of 2001). In this case, the distance between the source and the reflector is pc. First a fading, and then an increase in reflection is then expected to occur in the future, and monitoring of the source is the only way to keep track of its changes. Monitoring could also shed new light on the role of the X-ray absorber, which varies on much shorter temporal scales and seems to be associated with broad line region (BLR) clouds (see Risaliti et al. 2010) . If this is the case, the physical interpretation of our result applying the decoupled MYTorus model is straightforward: the l.o.s. is intercepting the variable (and presumably compact) Compton-thin absorber, while the reflector is located on larger scales and the photons reflecting back to our l.o.s. are “seeing” a Compton-thick column of gas. Risaliti et al. (2010) suggest that the absorber is a BLR cloud, assuming a central black hole (BH) mass of . In this picture, a second “screen” is required to obscure the broad lines in the optical spectrum, which is instead likely showing an outflow, resulting in the classification of Mrk 1210 as a Seyfert 2 (Mazzalay Rodríguez-Ardila 2007) . However, if the reflection component comes from photons reflecting off the far inner wall of the torus, delayed with respect to the intrinsic emission, a rather distant torus edge is needed with respect to the dust sublimation radius , which is usually thought to mark the inner wall of the torus, and in this case is 0.2 pc ( Gandhi et al. 2009 , and references therein, and adopting a bolometric correction of 20; Lusso et al. 2012 ). Table 3 ASCA best fit parameters compared with NuSTAR pexrav+zgauss only model. Notes. The NuSTAR line equivalent width is calculated with respect to the reflection continuum. Fig. 9 Observed 1040 keV flux ( top panel ) and iron line flux ( bottom panel ) of Mrk 1210, as a function of time. 4.2. Eclipsing event The ASCA data cannot distinguish between a Compton-thick eclipsing event and an intrinsic low-flux state of the central engine. A random pass of a Compton-thick cloud (or an alignment of clouds along the l.o.s.) during the ASCA observation is consistent with the known clumpiness of the gas surrounding obscured AGN. During the two observations by ASCA in 1995, separated by 25 days, Mrk 1210 was in a low-flux state. In an eclipsing scenario, this means that the putative eclipsing event lasted for at least 25 days. Assuming Keplerian motion of the clump, the linear size eclipsed by a moving Compton-thick cloud in a given time interval can be written as cm, where is the distance from the center in parsecs, and is the eclipse time interval in units of 25 days. This implies that the