\begin{table}%t1
\caption{\label{tab:sample}Object designations and general characteristics. Star with their
names printed in italic have luminosities which also allow an AGB~star identification. The bolometric magnitudes were computed from  the dereddened $K$~band magnitudes, using the bolometric corrections of \cite{Levesque2005}.}
%\centerline
 {\small  \begin{tabular}{lcccccccc}
\hline \hline\noalign{\smallskip}
Source & ISO TDT  & Spectral & Variability$^{a}$ & Period$^{a}$ & Kraemer$^{b}$ &  Distance$^{c}$ & $A_{\rm{V}}$$^{d}$ & $M_{\rm bol}$ \\
& number   & type & type & [d] & class &  [pc] &  & \\
\hline
HD 14242       & 61~301~202 & M2Iab      & Lc   &      & 2.SEa:  & 2290 & 1.63 & --6.93\\
  AD PER         & 78~800~921 & M2.5Iab    & SRc  & 363  & 2.SEa:  & 2290 & 1.63 & --7.42\\
  HD 14404       & 45~501~704 & M1Iab      & Lc   &      & 2.SEap: & 2290 & 1.63 & --7.23\\
  SU PER         & 43~306~303 & M3Iab      & SRc  & 533  & 2.SEc   & 2290 & 1.63 & --7.90\\
  RS PER         & 45~501~805 & M4Iab      & SRc  & 245  & 2.SEc   & 2290 & 1.63 & --7.74\\
  S PER          & 42~500~605 & M4.5Iab    & SRc  & 822  & 3.SE    & 2290 & 1.63 & --8.18\\
  HD 14580       & 42~701~401 & M1Iab      & Lc   &      & 1.NO:   & 2290 & 1.63 & --6.49\\
  HD 14826       & 61~601~203 & M2Iab      & Lc   &      & 2.SEa:  & 2290 & 1.63 & --7.36\\
  YZ PER         & 47~301~604 & M2Iab      & SRb  & 378  & 2.SEc   & 2290 & 1.63 & --7.50\\
  W PER          & 63~702~662 & M4.5Iab    & SRc  & 485  & 2.SEc   & 2290 & 1.63 & --7.74\\
  {\it $\rho$ PER}  & 79~501~105 & M4II       & SRb  & 50   & 1.NO    & 100  & 0.82 & --4.20\\
  {\it HR 1939} & 86~603~434 & M2Iab      & Lc   &      & 2.SEa   & 420  & 0.66 & --4.51\\
  $\alpha$ ORI   & 69~201~980 & M2Iab      & SRc  & 2335 & 2.SEcp  & 131  & 0.09 & --7.19\\
  {\it HD 90586}& 25~400~410 & M2Iab/Ib   &      &      & 2.SEc   & 641  & 0.40 & --4.76\\
  R CEN          & 07~903~010 & M5IIevar   & M    & 546  & 2.SEap  & 641  & 0.95 & --6.94\\
  $\alpha$ SCO  & 08~200~369 & M1.5Iabb   & Lc   &      & 2.SEcp  & 185  & 0.72 & --7.86\\
  $\alpha$ HER  & 28~101~115 & M5Iab      & SRc  &      & 1.NOp   & 117  & 0.42 & --5.99\\
  {\it $\sigma$ OPH}  & 10~200~835 & K3Iab      &      &      & 1.NO    & 360  & 0.68 & --4.33\\
  HR 7475        & 31~601~515 & K4Ib       & N:   &      & 1.NO    & 704  & 0.91 & --5.87\\
  NR VUL         & 53~701~751 & K3Iab      & Lc   &      & 2.SEc   & 2000 & 2.98 & --8.01\\
  BD+35 4077     & 73~000~622 & M2.5Iab    & Lc   &      & 2.SEb   & 1820 & 2.61 & --7.48\\
  RW CYG         & 12~701~432 & M3Iab      & SRc  & 550  & 2.SEc   & 1200 & 3.54 & --7.77\\
  IRC +40427     & 53~000~406 & M1:Iab     &      &      & 2.SEap: & 2000 & 1.79 & --6.89\\
  $\mu$ CEP         & 08~001~274 & M2Ia       & SRc  & 730  & 2.SEc   & 830  & 1.84 & --8.86\\
  V354 CEP       & 41~300~101 & M2.5Iab    & Lc   &      & 2.SEc   & 3500 & 2.00 & --8.51\\
  U LAC          & 41~400~406 & M4Iab:e    & SRc  &      & 2.SEc   & 3470 & 1.74 & --8.30\\
  PZ CAS         & 09~502~846 & M3Iab      & SRc  & 925  & 2.SEc   & 2510 & 2.11 & --8.89\\
\hline
\end{tabular}}
\medskip		  	      
$^a$ Combined General Catalogue of Variable Stars \citep{Kholopov1998}; $^b$~\cite{Kraemer2002}; $^c$~distances below 1~kpc come from parallax measurements with {\sc hipparcos} \citep{Perryman1997}. Distances equal to 2~kpc are actually unknown and distances greater than 1~kpc are cluster distances from \cite{Humphreys1978}. $\mu$~Cep is an exception: we use the distance of \cite{Humphreys1978} instead of the poor parallax measurement; $^d$~ISM extinction estimates for stars within 1~kpc come from the galactic model of \cite{Arenou1992}. All other stars and $\mu$~Cep have estimates based on the extinction toward early-type stars in the corresponding clusters.
\end{table}