  IGR J17091-3624 is a low mass X-ray binary (LMXB) which received wide
attention from the community thanks to its similarities with the bright black
hole system GRS 1915+105. Both systems exhibit a wide range of highly
structured X-ray variability during outburst, with time scales from few seconds
to tens of minutes, which make them unique in the study of mass accretion in
LMXBs. In this work we present a general overview into the long-term evolution
of IGR J17091-3624, using Swift/XRT observations from the onset of the
2011-2013 outburst in February 2011 to the end of the last bright outburst in
November 2016. We found 4 re-flares during the decay of the 2011 outburst, but
no similar re-flares appear to be present in the latter one. We studied in
detail the period with the lowest flux observed in the last 10 years, just at
the tail end of the 2011-2013 outburst, using Chandra and XMM-Newton
observations. We observed changes in flux as high as a factor of 10 during this
period of relative quiescence, without strong evidence of softening in the
spectra. This result suggests that the source has not been observed at its true
quiescence so far. By comparing the spectral properties at low luminosities of
IGR J17091-3624 and those observed for a well studied population of LMXBs, we
concluded that IGR J17091-3624 is most likely to host a black hole as a compact
companion rather than a neutron star.
