%
%       TABLE with Results
% 
\begin{deluxetable}{lccccccccl}
\rotate
\tabletypesize{\scriptsize}
\tablewidth{0pt}
\tablecaption{Spectral parameters\label{tab:spec}}
\tablehead{
\colhead{NAME}           & \colhead{RA}     & \colhead{DEC}     & \colhead{Type}   &\colhead{$\Gamma$/E[kT]\tablenotemark{a}}   & \colhead{N$_H$}   &
\colhead{MODEL}          & \colhead{INSTR.\tablenotemark{b}}             \\
%%%%%%%%%  units
\colhead{} & \colhead{\scriptsize (J2000)}  & \colhead{\scriptsize (J2000)}    &
\colhead{} & \colhead{}  & 
\colhead{\scriptsize ($10^{22}$atoms cm$^{-2}$) }

}
\startdata 
%

%%%
3C 105.0    &61.9178 &  3.6517  & Sy2
&$1.66^{+0.13}_{-0.13}$  &$29.4^{+5.7}_{-4.8}$ &wabs*pow &B, X\\
 


%%%
1AXG J042556-5711  &66.6021 &-57.1775 &Sy1 & $1.54^{+0.028}_{-0.027}$ & 0 & pow &  B, A \\

%%%
3C 120        & 68.2982 &  5.3374  & Sy1 &$ 1.80^{+0.04}_{-0.04}$/$0.27^{+0.026}_{-0.025}$  &  0 & wabs*pow+bb & B, A \\



%%%
 MCG -01-13-025 & 72.9205 &-3.8240 & Sy1.2 &
$ 1.6^{+0.48}_{-0.47}$  & $ <0.02$ (1) & pow & B \\


%%%
 SWIFT J0505.7-2348 & 76.4674 & -23.8666 & Sy2 &
$ 1.77^{+0.08}_{-0.07}$ &$ 4.8^{+0.9}_{-0.7}$ 
& wabs*pow & B, X\\


%%%
CSV 6150    & 77.7224 & 16.5265 & Sy1.5  & 1.94$^{+0.25}_{-0.23}$ 
& \nodata & pow & B \\


%%%
4U 0513-40      & 78.5146 & -40.0558 & LXB      & 29.7$^{+7.5}_{-5.8}$   
& \nodata &  brem &B\\


%%%
QSO B0513-002  & 79.0096 & -0.1332 & Sy1
&$1.83^{+0.02}_{-0.016}$/$0.27^{+0.02}_{-0.02}$ &$<0.01$ & wabs*pow+bb & B, A \\



%%%
SWIFT  J0517.1+1633 & 79.2839 & 16.5605 & \nodata
& 2.0$^{+0.23}_{-0.26}$  & \nodata & pow & B \\


%%%
 ESO 362- G 018  & 79.8844 & -32.6720  & Sy1.5
& $1.5^{+0.03}_{-0.02}$  & $<$0.01 & wabs*pow & B,X \\


%%%
 Pictor A   &  79.9460 &  -45.7557   &  Sy1
&$1.8^{+0.015}_{-0.014}$ &$0.12^{+0.007}_{-0.02}$ &wabs*pow &B, A\\


%%%
ESO 362-G021    &80.6581  &  -36.4233 & BL Lac 
   &$1.7^{+0.037}_{-0.036} $ &$ 0.1^{+0.0197}_{-0.0187}$ & wabs*pow & B, A, X\\



%%%
V* TV Col & 82.3541 & -32.7965  & CV-DQ* & $24.9^{+4.6}_{-3.8}$ 
& \nodata & bremss & B \\


%%%
V* TW Pic      & 83.6470 & -58.0200 & CV &  
13.5$^{+10.6}_{-5.6}$ & \nodata & bremss & B \\


%%%
LMC X-3         & 84.7717 & -64.1148 & HXB  & 2.0$^{+0.4}_{-0.3}$
&\nodata& pow &B\\


%%% 
LMC X-1         & 84.8917 & -69.7210 & HXB     & 2.3$^{+0.22}_{-0.20}$ & \nodata & pow &B\\

%%%%
PSR B0540-69.3 & 84.9878  & -69.3230 & Pulsar  & 1.85$^{+0.28}_{-0.26}$ 
&\nodata& pow &B\\

%%%
PKS 0537-286   & 84.9953  & -28.7029 & BLAZAR  &
$1.35^{+0.06}_{-0.08}$ &$<0.01$  &wabs*pow &B, A \\



%%%
PKS 0548-322    & 87.7165 & -32.2610  & BL Lac  
&  $ 1.8^{+0.032}_{-0.031}$ &$ 0.02^{+0.006}_{-0.005}$   & wabs*pow & B, X\\



%%%
NGC 2110      & 88.0411 & -7.4554 &  Sy2  & 
$1.62^{+0.01}_{-0.01}$/$0.47^{+0.02}_{-0.02}$  &
$4.0^{+0.13}_{-0.07}$ & wabs*(pow+ga) + bb & B, A, X\\



%%% 
 LEDA 75476  & 89.5237  & -38.3799 & Sy1 & $1.74^{+0.017}_{-0.025}$/
$0.25^{+0.08}_{-0.05}$ &
$2.5^{+0.11}_{-0.17} $& wabs*(pow+ga)+bb &  B, A\\



%%%
ESO 490- G 26   & 100.0031 & -25.8931 & Sy1.2  &
 1.90$^{+0.05}_{-0.04}$ & 0.27$^{+0.005}_{-0.005}$ & wabs*pow & B, X \\




%%%
SWIFT  J0727.5-2406 & 111.8951 & -24.1039 &\nodata &1.53$^{+0.55}_{-0.54}$
&\nodata & pow & B\\


%%%
V* 441 Pup      & 112.1626 & -26.0696 & CV & 
$12.4^{+13.6}_{-5.6}$ & \nodata & bremss & B \\


%%%
V* BG CMi      & 112.8752 & 9.9214  & CV  &  31.3$^{+41.2}_{-14.2}$& \nodata & bremss& B \\


%%%
SWIFT J0732.5-1331 & 113.1328 & -13.5037 & CV  & $33.2^{+50.1}_{-14.2}$ 
& \nodata & bremss & B \\


%%%
SWIFT J0739.6-3144 & 114.9127 & -31.7496 & Sy2\tablenotemark{d}   &$1.77^{+0.51}_{-0.43}$ 
& $>$2\tablenotemark{c} & pow & B\\

%%%
SWIFT J0743.0-2543 & 115.7501 & -25.7314 & \nodata & $1.78^{+0.69}_{-0.56}$ & 
\nodata & pow & B \\



%%%
IGR J07597-3842 & 119.9822 & -38.7422 & Sy1.2 & 
$1.8^{+0.08}_{-0.07}$& $<$0.01 &  wabs*pow &B, X\\


%%%
UGC 4203       & 121.0552 & 5.1203 & Sy2 &
1.68$^{+0.09}_{-0.10}$/ $0.31^{+0.08}_{-0.05}$ 
&12.5$^{+5.0}_{-3.7}$\tablenotemark{f} & wabs(pexrav+ga)+bb
 &B, A, X \\


%%%
SWIFT J0811.5+0937 &  122.8750 &  9.6214  &  XBONG\tablenotemark{d} &
$2.2^{+2.1}_{-0.9}$ & 
{$ ~0$}\tablenotemark{e} & pow &  B \\



%%%
SWIFT J0823.4-0457 & 125.8271 &  -4.9401 &  Sy2 &
$1.84^{+0.28}_{-0.22}$ 
&$19.3^{+6.8}_{-5.4}$ & wabs*pow & B, X\\



%%%
Vela PSR   & 128.8308 & -45.1771  & PSR & 1.88$^{+0.20}_{-0.26}$ & \nodata
& pow &B\\


%%%
FRL 1146        & 129.6151 & -35.9976  & Sy1  
& $1.88^{+0.37}_{-0.31}$ & \nodata & pow & B \\


%%%
3C 206 & 129.9556 &  -12.2467 &  QSO  &
$1.95^{+0.43}_{-0.39}$ & $0$\tablenotemark{e} 
& wabs*pow &  B \\



%%%
SWFIT  J0844.9-3531 & 131.2411 & -35.5313  &\nodata& $1.91^{+0.46}_{-0.68}$
 &\nodata & pow & B \\




%%%
SWIFT J0854.7+1502 & 133.6828 &  15.0371 & Sy2\tablenotemark{d}
  &$1.41^{+0.7}_{-0.9}$ &$  >0.5$\tablenotemark{c} & pow & B\\



%%%
SWIFT J0917.2-6221     & 139.112 & -62.359 & Sy1 & $1.87^{+0.07}_{-0.04}$/ 0.14$^{+0.02}_{-0.02}$
 & 1.33$^{+0.18}_{-0.10}$ & bb+wabs*pow & B \\


%%%
Mrk 0704  &  139.6505 & 16.2987 & Sy1.5
&$ 1.36^{+0.1}_{-0.07}$ & $15.0^{+6.3}_{-3.5}$ & pcfabs*(pow+ga) & B, A, X \\


%%%
4U 0919-54      & 140.0753 & -55.2135 & LXB & 45.11$^{+26.13}_{-9.8}$
 & \nodata & bremss &B\\


%%%
MCG -01-24-012 & 140.2134 & -8.0872 &  Sy2 &
$ 1.7^{+0.08}_{-0.07}$  & $6.5^{+0.8}_{-0.7}$ & wabs*pow & B, X\\


%%%
NGC 2992  & 146.4060 & -14.3007  & Sy1.9
 &$1.24^{+0.06}_{-0.05}$ 
&$0.17^{-0.03}_{-0.03}$ & wabs*(pow+ga)& B, A, X\\


%%%
ESO 434- G 040  & 146.9151 &-30.9388 &  Sy2  &
$1.77^{+0.006}_{-0.07}$/ $0.15^{+0.011}_{-0.016}$
 &$1.5^{+0.026}_{-0.09}$ &wabs*(pow+ga)+bb & B, A, X\\


%%%
3C 227   & 146.9447 & 7.4191 & Sy1 &
$2.11^{+0.14}_{-0.24}$ & $ 3.6$ & pexrav+wa*pow & B, C \\


%%%
NGC 3081  &  149.8805 &  -22.8561  &  Sy2   &
$1.9^{+0.02}_{-0.04}$/ $0.58^{+0.15}_{-0.11}$ 
&$60^{+3.1}_{-3.1}$ &wabs*(pow+ga) +bb  & B, A, S \\




\enddata
\tablenotetext{a}{Photon index and/or plasma temperature for the model,
specified in column ``Model'', to fit the data.}

\tablenotetext{b}{Instrumenst used for spectral analysis are: 
B = BAT, X = Swift/XRT, A = ASCA, C = Chandra, and S = BeppoSAX.}

\tablenotetext{c}{\ Lower limit on absorption estimated through 
the non detection by ROSAT}.


\tablenotetext{d}{Proposed identification in \cite{rau07}.}

\tablenotetext{e}{Order of magnitude of the absorption estimated imposing
that the extrapolated source flux match the ROSAT-PSPC count rates.}

\tablenotetext{f}{UGC 4203 exhibits transition between reflection-dominated
and a trasmission-dominated spectrum. The absorption is estimated in the
latter case using XRT data (see text for details).}


\tablerefs{References: (1) Gallo et al. (2005). }
\end{deluxetable}
