All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa8901f1.ps}\end{figure}$ Figure 1: Section of the ESO-3.6 m plus EFOSC2 R-band acquisition image (exposure time: 20 s) of the field of Swift J1656.3-3302, with superimposed the X-ray 0.3-10 keV band Swift/XRT (larger circle) and the radio 1.4 GHz NVSS (smaller circle) positions. The actual optical counterpart, identified through optical spectroscopy at the same telescope, is indicated by the black arrows. In the image, North is at top, East is to the left.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{aa8901f2.ps}\end{figure}$ Figure 2: 3700-8500 Å optical spectrum of Swift J1656.3-3302 obtained with the ESO-3.6 m telescope. The spectrum shows broad emission lines of Lyman- $\alpha$ , Si IV, He II, C IV and C III] with redshift $z = 2.40 \pm 0.01$ . Telluric absorption bands are marked with the symbol $\oplus$ . The spectrum has been smoothed with a running boxcar of 5 pixels ( $\sim$ 14 Å).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa8901f3.ps}\end{figure}$ Figure 3: Swift/XRT 0.3-10 keV image of the field of Swift J1656.3-3302 acquired on 13 June 2006. The larger circle indicates the BAT positional uncertainty and the smaller circle the IBIS one. Swift J1656.3-3302 is the brightest source in the image.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{aa8901f4u.ps}\\ [2... ...}\\ [2.5mm] \includegraphics[angle=-90,width=8cm,clip]{aa8901f4l.ps}\end{figure}$ Figure 4: Averaged 0.7-200 keV X-ray spectrum of Swift J1656.3-3302 obtained from the XRT and ISGRI data described in the text and fitted with a power law absorbed only by the Galactic hydrogen column ( upper panel), a power law absorbed by Galactic plus neutral hydrogen local to the blazar ( central panel), and a broken power law absorbed by the Galactic hydrogen column only ( lower panel). The fit residuals using the best-fit models reported in Table 2 are shown in each panel.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{aa8901f5.ps}\end{figure}$ Figure 5: Broadband non-simultaneous observational radio to gamma-ray SED of Swift J1656.3-3302, constructed with the measurements collected from the literature and with those presented in this paper (see text for details). Moving towards higher energies, the following information was used: the 1.4 GHz NVSS radio flux, the ESO 3.6 m optical spectrum, the ROSAT 0.1-2.4 keV flux, and the XRT+IBIS 0.7-200 keV spectrum. The IRAS upper limits in the mid-infrared bands and the upper limit at MeV energies from the EGRET survey are also reported. The dashed line indicates an example of the application of the log-parabolic model (Massaro et al. 2006; Tramacere et al. 2007) briefly described in the text.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{aa8901f2.ps}\end{figure}$	Figure 2: 3700-8500 Å optical spectrum of Swift J1656.3-3302 obtained with the ESO-3.6 m telescope. The spectrum shows broad emission lines of Lyman- $\alpha$ , Si IV, He II, C IV and C III] with redshift $z = 2.40 \pm 0.01$ . Telluric absorption bands are marked with the symbol $\oplus$ . The spectrum has been smoothed with a running boxcar of 5 pixels ( $\sim$ 14 Å).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa8901f3.ps}\end{figure}$	Figure 3: Swift/XRT 0.3-10 keV image of the field of Swift J1656.3-3302 acquired on 13 June 2006. The larger circle indicates the BAT positional uncertainty and the smaller circle the IBIS one. Swift J1656.3-3302 is the brightest source in the image.
Open with DEXTER