All Tables

Table 1: List of sources in the INTEGRAL Galactic bulge monitoring program, ordered by Galactic longitude (from left to right in the Hammer-Aitoff projection, i.e., from 180 $^{\circ }$ -0 $^{\circ }$ , 360 $^{\circ }$ -180 $^{\circ }$ ).
Table 2: Sources monitored by the OMC in the Galactic bulge region. The ordering is the same as Table 1. Listed are the source name, OMC identifier and the period of monitoring (period I covers the revolutions before 421, period II covers revolution 421 and onwards). Revolution 421 corresponds to 2006, March 25 or MJD 53819. The results for IGR J17544-2619 are shown in Fig. 17.
Table 3: This table lists the maximum detection significance reached during the hexagonal dither observations (Sig $_{\rm rev,~max}$ ), the detection significance per season (Sig $_{\rm sX}$ ; where X=1, 2, 3 for the three seasons) and the detection significance for all observations together (Sig $_{\rm all}$ ), together with the corresponding fluxes ( $F_{\rm s,~X}$ ) and errors in the fluxes for the IBIS/ISGRI 20-60 keV band. The ordering of sources is the same as used for Table 1. When a source was not detected it is indicated with "-''; we then provide a 3 $\sigma$ (statistical) upper limit on the flux. Whenever Sig $_{\rm rev,~max}$ exceeds 7, the source long-term light curves are discussed in Sect. 4.2.
Table 4: This table lists the maximum detection significance reached during the hexagonal dither observations (Sig $_{\rm rev,~max}$ ), the detection significance per season (Sig $_{\rm sX}$ ; where X=1, 2, 3 for the three seasons) and the detection significance for all observations together (Sig $_{\rm all}$ ), together with the corresponding fluxes ( $F_{\rm sX}$ ) and errors in the fluxes for the IBIS/ISGRI 60-150 keV band. The ordering of sources is the same as used for Table 1. We only list those sources for which either Sig $_{\rm rev,~max}$ , Sig $_{\rm sX}$ or Sig $_{\rm all}$ reached a value higher than 7. When a source was not detected it is indicated with "-''; we then provide a 3 $\sigma$ (statistical) upper limit on the flux. Whenever Sig $_{\rm rev, max}$ exceeds 7, the source long-term light curves are discussed in Sect. 4.2.
Table 5: Compilation of information for each of the JEM-X mosaic images per season and for the whole program (Fig. 4). We report the season which is refered to, the INTEGRAL revolutions corresponding to the season, the total number of single pointings (ScWs), the total exposure time at the center of each mosaic ( $t_{\rm exp}$ ), the effective exposure time ( $t_{\rm eff}$ ) when taking into account vignetting and other effects inherent to the JEM-X instrument (see Lund et al. 2003), and the list of sources which are detected above the 3 $\sigma$ level in the 3-10 keV and 10-25 keV bands during a season or in the average over the whole program. When the detection significance is lower than 3 or a source is not detected we indicate it with (-). The ordering of the sources is the same as in Table 1.
Table 6: Mean ( $\overline {F}$ ) observed fluxes in the 20-60 keV (denoted by A) and 60-150 keV (denoted by B) bands, respectively, over the whole AO-3 monitoring program. The error given for $\overline {F}$ is the error in the mean. " $\sigma$ '' denotes the standard deviation of the averaged values and gives a measure of the variability of a source. The ordering of sources is the same as used for Table 1.
Table 7: New INTEGRAL sources detected through our monitoring program. We give the source position (J2000.0) with its 90% confidence error, whether the source was detected by JEM-X (J) and/or IBIS/ISGRI (I) or not, and the reference in which the detection was first noted. References: [1] Kuulkers et al. (2006c); [2] this paper; [3] Turler et al. (2006); [4] Chenevez et al. (2006b).