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ABSTRACT  We present spectral and temporal results from  INTEGRAL  long‐term monitoring of the unidentified X‐ray source IGR J17354−3255. We show that it is a weak persistent hard X‐ray source spending a major fraction of the time in an out‐of‐outburst state with an average of 18–60 keV X‐ray flux of ∼1.1 milliCrab, occasionally interspersed with fast X‐ray flares (duration from a few hours to a few days) with a dynamic range as high as ∼200. From archival  Swift /X‐ray telescope observations, we also show that the dynamic range from non‐detection to highest level of measured X‐ray activity is &gt;300. Our imager on board the lntegral satellite (IBIS) timing analysis strongly confirms the ∼8.4 d orbital period previously detected with  Swift /burst alert telescope (BAT); in addition we show that the shape of the orbital profile is rather smooth and appears to be dominated by low‐level X‐ray emission rather than by bright outbursts; the measured degree of outburst recurrence is ∼25 per cent. The spectral and temporal characteristics of IGR J17354−3255 are highly indicative of a supergiant high‐mass X‐ray binary (SGXB) nature. However, our inferred dynamic ranges in both soft and hard X‐rays are significantly greater than those of classical SGXB systems, but instead are typical of intermediate supergiant fast X‐ray transients (SFXTs). Finally, we note for the first time that the observed fast flaring X‐ray behaviour of IGR J17354−3255 is very similar to that detected with  AGILE  from the spatially associated MeV source AGL J1734−3310, suggesting a possible physical link between the two objects.

IGR J17354−3255 as a candidate intermediate supergiant fast X‐ray transient possibly associated with the transient MeV AGL J1734−3310