\begin{table}%t3 \caption{\label{lbv_summary}Summary of the stellar properties of \object{AFGL~2998} and other LBVs observed to undergo giant eruptions.} \small%\centerline { \begin{tabular}{lcccccccl} \hline \hline &&&&&&&& \\[-8pt] Star & Epoch & $R_{\ast}$ & $T_{\rm eff}$ & log($L_{\ast}/L_{\odot}$) & H/He & $v_{\infty}$ & log $\dot M$ /$\sqrt f$ & Reference\\ & & ($R_{\odot}$) & (kK) & & & (km~s$^{-1}$) & $M_{\odot}$ yr$^{-1}$ & \\ \hline AFGL 2298 & 1996--9 & -- & -- & $>$6.4 & -- & -- & -- & a\\ & 2001 Jun. & 262 & 11.7 & 6.2 & {\em 5.0} & {\em 200} & --4.3 & a\\ & 2002 Aug. & 158 & 10.9 & 6.1 & {\em 5.0} & {\em 200} & --3.9 & a \\ & 2006 Jun. & 385 & 10.3 & 6.3 & {\em 5.0} & 125 & --4.3 & a \\ & 2007 May & 312 & 10.9 & 6.2 & {\em 5.0} & 125 & --4.4 & a \\ \hline NGC 2363-V1 &$<$1993 & -- & -- & $\leq${\em 5.9} & -- & -- & -- &b \\ &1997 Nov. & 356 & 13.5 & 6.58& {\em 4.0} & 325 & --3.3 & b, c\\ &1999 Jul. & 201 & 18.5 & 6.63& {\em 4.0} & 290 & --3.2 & b, c\\ &2000 Oct. & 225 & 17.5 & 6.63& {\em 4.0} & -- & --3.3 & c, d\\ &2001 Dec. & 223 & 18.5 & 6.72& {\em 4.0} & -- & --3.5 & c, d\\ &2003 May & 194 & 20.5 & 6.78& {\em 4.0} & -- & --3.8 & c, d\\ &2004 May & -- &{\em 26.0}& {\em 6.80}& -- & -- & {\em $<$--3.4} &c, d \\ \hline HD 5980 &1978--80 & -- &{\em 60.5} & {\em 6.4} & -- & -- & -- & e\\ &1993 Nov. & -- &{\em 52.0} & {\em 6.5} & -- & -- & -- & e\\ &1994 Sep. & 280 & 23 & 7.05& 0.7 & 500 & --3.1 & b\\ &1994 Dec. & 130 & 35 & 6.50& 2.5 & 600 & --3.0 & e\\ \hline $\eta$ Car & 1840's & -- & -- & {\em 7.5} & -- & {\em 650--3000} & {\em $\ga$--0.3} & f, g\\ & 1890's & -- & -- & -- & -- & {\em 200} & {\em --1.8} & h, i \\ & 1998.2 & 60--881 & 35.3--9.2 & 6.74 & 5.0 & 500 & --3.0 & j\\ \hline P Cygni & 1600's & -- & -- & -- & -- & {\em 137} &{\em --1.7} &k \\ & 1989--92 & 76 & 18.7 & 5.8 & 3.5 & 185 & --4.5 &l \\ \hline \end{tabular}} \medskip Note~2. Those parameters that are not directly determined from non-LTE~model atmosphere analysis~-- for example wind parameters derived from present day nebular properties~-- are given in italics. Due to the extreme mass loss rate for \object{$\eta$~Car} a degeneracy is present for the stellar radius and temperature (Hillier et~al. \cite{hillier}). References used in the construction of this table are $^a$~Clark et~al. (\cite{clark03a}) and this study; $^b$~Drissen et~al. (\cite{drissen}); $^c$~Petit et~al. (\cite{petit05}); $^d$~Petit et~al. (\cite{petit}); $^e$~Koenigsberger et~al. (\cite{koen}) $^f$~Humphreys et~al. (\cite{h99}); $^g$~Smith et~al. (\cite{smith03}); $^h$~Smith (\cite{smith05}); $^i$~Smith (\cite{nature}); $^j$~Hillier et~al. (\cite{hillier}); $^k$~Smith \& Hartigan (\cite{smith06b}); $^l$~Najarro (\cite{pacopcyg}). Volume filling factors, $f$, range from~0.1 (\object{HD~5980} and \object{$\eta$~Car}), through~0.3 (\object{NGC~2363$-$V1}) to~0.5 (\object{P~Cygni}). Time averaged mass loss rates for \object{$\eta$~Car} and \object{P~Cygni} derived from nebular masses are absolute (i.e.~$f$~=~1). Finally, note that the values of~$V_{\infty}$ presented for NGC~2363$-$V1 in 1997 \& 1999 are from Drissen et~al. (\cite{drissen}), while $R_*$, $T_{\rm eff}$, $\log(L_{*})$ and~$\dot {M}$ are from the updated models presented by Petit et~al. (\cite{petit05}). \end{table}