\begin{table}%t1
\caption{\label{tab-sourcedata}The 20 objects investigated in this study and the properties of the corresponding datasets.} 
\small%\centerline
 {
  \begin{tabular}{llllcccc}
    \hline\hline
&&&&&&& \\[-8pt]
 Object name$^a$& Object type$^b$ & RA, Dec (FK5)&galactic $l$, $b$& elapsed & \multicolumn{1}{c}{effective}& var.$^d$ &  Data\\
         &            &                       &              & time & \multicolumn{1}{c}{SPI exposure$^c$} &       &   Set\\ 
         &           & \multicolumn{1}{c}{$[^\circ]$}    & \multicolumn{1}{c}{$[^\circ]$}    & $[$Ms$]$ &  \multicolumn{1}{c}{$[$10$^6$ cm$^2$ s$]$} & $[$ks$]$ & \\
\hline                                                                                               Crab              & PWN       & 083.6332, +22.0145 & 184.5575, --05.7843 & 1.33 & 22.7 &  --                         &   1 \\
Vela Pulsar       & PWN       & 128.8361, --45.1764 & 263.5520, --02.7873 & 3.48 & 68.9 &  --                         &   2 \\
NGC 4151          & Seyfert 1.5 & 182.6364, +39.4054 & 155.0765, +75.0637 & 0.085 & 5.2 &  --                         &  3 \\
NGC 4945          & Seyfert 2 & 196.3587,  --49.4708  & 305.2681, +13.3374 & 0.53 &  9.1  & --                       &  4 \\
Cen A             & Radio Gal., Seyf.2 & 201.3651, --43.01911 & 309.5159, +19.4173 & 0.56 & 11.5  & --               &  5 \\
XTE J1550-564     & LMXB, BHC, $\mu$Q&237.7446, --56.4767& 325.8822, --01.8271 & 2.56 & 42.4 & --                        &  6 \\
4U 1630-47        & LMXB, BHC  & 248.5017, --47.3942   & 336.9081, +00.2519 & 3.97 & 154  & --                        &  7 \\
Swift J1656.3-3302& Blazar    & 254.0690, --33.0359   & 350.5993 +06.3581  & 10.1 & 151  & --                        &  10\\
OAO 1657-415      & HMXB, Pulsar & 255.1996, --41.6731   & 344.3538, +00.3111 & 3.97 & 110 &  --                        &  7 \\
GX 339-4          & LMXB, BHC, $\mu$Q & 255.7062, --48.7897   & 338.9394, --04.3267 & 3.36 & 123 &  --                        &  8 \\
4U 1700-377       & HMXB, NS  & 255.9866, --37.8441   & 347.7544, +02.1735 & 3.97 & 73.5&  90, --                    &  7 \\
IGR J17091-3624   & LMXB?, BHC   & 257.275,  --36.410    & 349.519,  +02.215  & 7.08 & 214 &  --                        &  9 \\
GX 354-0          & LMXB, NS  & 262.9892, --33.8347   & 354.3022, --00.1501  & 7.08 & 130 &  --                       &  9 \\
1E 1740.7-2942    & LMXB?, BHC, $\mu$Q& 265.9785, --29.7452   & 359.1160, --00.1057 & 7.08 & 134 &  --                        &  9 \\
IGR J17464-3213   & LMXB?, BHC, $\mu$Q  & 266.5650, --32.2335   & 357.2552, --01.8330  & 7.08 & 114 &  90, --                   &  9 \\
GRS 1758-258      & LMXB, BHC, $\mu$Q& 270.3012, --25.7433 & 004.5076, --01.3607 & 10.1 & 403 &  --                        &  10\\
Ginga 1826-24     & LMXB, NS    & 277.3675, --23.7969   & 009.2724, --06.0878 & 10.1 & 239 &  --                        &  10\\
GRS 1915+105      & LMXB, BHC, $\mu$Q& 288.7983, +10.9456 & 045.3656, --00.2194 & 2.83 & 53.1&  90, --                    &  11\\
Cyg X-1           & HMXB, BHC, $\mu$Q  & 299.5903, +35.2016   & 071.3350, +03.0668  & 1.94 & 32.9 &  90, 180                 &  12\\   
Cyg X-3           & HMXB, BHC, $\mu$Q  & 308.1074, +40.9578   & 079.8455, +00.7001  & 2.79 & 50.2 &  90, --                   &  13\\
Control1$^e$      & --              & 259.5000, --40.3500   & 347.7000, --02.1000  & 7.08 & 181 & -- & 9 \\ 
\hline
\end{tabular}}
\medskip
$^a$ See Sect.~\ref{sec-selection} for the selection criteria and Sect.~\ref{secresults} for
references concerning the source properties. \\
$^b$ PWN~= pulsar wind nebula, $\mu$Q~= microquasar, NS~= binary containing a neutron star,          BHC~= containing a black hole candidate, ?~= classification uncertain. \\
$^c$ Calculated at 30~keV and taking into account the SPI response. \\
$^d$ Assumed variability timescale in the analysis at $E < 144$~keV (first number) and at $E > 144$~keV (second number); ``$-$''~= the source was assumed constant either because it is known to be steady or because the variability timescale and/or amplitude is too small for SPI to detect significant variability. \\
$^e$ Control position for the assessment of systematic errors in the analysis of crowded fields
(see Sects.~\ref{sec-syserr} and~\ref{sec-control1}).
\end{table}