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	Figure 1: Composite X-ray spectrum of GRS 1734-292 obtained from nonsimultaneous INTEGRAL, GRANAT and ASCA observations. The dashed lines indicate the best-fit (absorbed power-law+reflection) model defined by parameters given in Table 1 (the last set), scaled to match the different data sets.
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In the text

	Figure 2: Upper panel: time history of the observed X-ray flux from GRS 1734-292 in 1990-2004 assuming that its broadband X-ray spectrum remained invariably as that shown in Fig. 1. Lower panel: light curve of GRS 1734-292 in August-September 2003 measured with INTEGRAL/IBIS.
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In the text

Figure 3: Comparison of the broadband spectral energy distribution of GRS 1734-292 (in solid) with those of NGC 4151 (in dotted) and of BL Lac objects (in dashed). The data for GRS 1734-292 include the radio spectrum and near infrared measurements (K and H bands) adopted from Martí et al. (1998), X-ray spectrum at 5-200 keV from GRANAT/ART-P and INTEGRAL/IBIS and the gamma-ray flux measured from 3EG J1736-2908 with CGRO/EGRET in July-August, 1992 (Hartman et al. 1999). For NGC 4151, the radio to optical spectrum is approximated from multifrequency data taken from the NED database, the X-ray spectrum above 10 keV is adopted from Finoguenov et al. (1995), the upper limit on the flux above 100 MeV is taken from Lin et al. (1993), and a distance of 20 Mpc is assumed. The composite SED for BL Lac objects is adopted from Fossati et al. (1998), specifically from the sample characterized by radio luminosities of 1042-1043 erg s-1, which closely matches the SED of GRS 1734-292 in the X-ray range; these data were recalculated to our adopted value H0=75 km s-1 Mpc-1.

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In the text