\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}