\begin{table}%t5
\caption{\label{phot_table}Overview of the infrared photometry of $\ell$~Car and RS~Pup from the present work and bibliography. All flux densities are corrected for interstellar extinction, except longwards of 30~$\mu$m, where it is considered negligible. The ``$\bullet$'' symbols in the ``Fit'' column indicate the photometry used for the synthetic spectrum fitting. $\lambda_0$~is the average of the half maximum extreme wavelengths of each instrument/filter combination, and $\Delta \lambda$ the half-bandwidth. $\lambda_{\rm eff}$~is the effective wavelength of the measurement considering the spectral energy distribution of the star. The ``Ap.''~column lists the effective radius of the aperture over which the flux density was measured, when this parameter was available. In the ``Ref.''~column, the references are the following: F07~= Fouqu\'e et~al. (\cite{fouque07}), I86~= IPAC (\cite{ipac86}), H88~= Helou \& Walker (\cite{helou88}), K08~= present work, S04~= Smith et~al. (\cite{smith04}). ``$\alpha$''~is the measured flux density excess, expressed in percentage of the photospheric flux (see Sect.~\ref{sed-section} for details), except for RS~Pup's three longest wavelengths, where it is expressed in stellar flux units, followed by~``$\times$''. The last column~``$N\sigma$'' gives the detection level in number of times the rms~uncertainty.} 
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\small%\centerline
 {
\begin{tabular}{lcclccclllr}
\hline \hline
Inst.~/ & Band  & Fit & $\lambda_0 \pm \Delta \lambda$ & $\lambda_{\rm eff}$ & Ap. & Flux density & Flux density & Ref. & $\alpha \pm \sigma(\alpha)$ & $N\sigma$\\
{\it System} & &  & [$\mu$m] & [$\mu$m]  & [\arcsec] & [${\rm W/m}^{2}/\mu{\rm m}$] & [Jy] & & [\%] & \\
\hline
 $\mathbf{\ell}$~{\bf Car} \\
{\it Johnson} & $B$ & $\bullet$ & $0.44 \pm 0.05$ & 0.44 & $-$ & $1.13 \pm 0.03$~$\times$ $10^{-09}$  &  $72.6 \pm 2.0$ & F07 & $-1.5 \pm 2.8$ & --0.5 \\
{\it Johnson} & $V$ & $\bullet$ & $0.55 \pm 0.04$ & 0.56 & $-$  & $1.80 \pm 0.05$~$\times$ $10^{-09}$  &  $181 \pm 5.1$  & F07 & $1.0 \pm 2.8$ & 0.3 \\
{\it Cousins}  & $I_{\rm c}$ & $\bullet$ & $0.75 \pm 0.11$ & 0.75 & $-$  & $1.47 \pm 0.04$~$\times$ $10^{-09}$  &  $274 \pm 7.7$  & F07 & $3.5 \pm 2.9$ & 1.2 \\
{\it 2MASS} & $J$ & $\bullet$ & $1.25 \pm 0.15$ & 1.22 & $-$  & $7.34 \pm 0.35$~$\times$ $10^{-10}$  &  $382 \pm 18$  &  F07 & $4.3 \pm 4.9$ & 0.9 \\
 {\it 2MASS} & $H$ & $\bullet$ & $1.62 \pm 0.10$ & 1.65 & $-$  & $3.91 \pm 0.18$~$\times$ $10^{-10}$  &  $342 \pm 16$   &  F07 & $-4.5 \pm 4.7$ & --1.0 \\
 {\it 2MASS} & $K$ & $\bullet$ & $2.20 \pm 0.30$ & 2.16 & $-$  & $1.67 \pm 0.08$~$\times$ $10^{-10}$  &  $269 \pm 13$ &  F07 & $-1.1 \pm 4.7$ & --0.2 \\
 COBE$^{*}$ & 3.5~$\mu$m & & $3.57 \pm 0.49$ & 3.55 & $\infty$ & $3.03 \pm 0.41$~$\times$ $10^{-11}$  &  $127 \pm 17$ & S04 & $8.4 \pm 15$ & 0.6 \\
 IRAC & I1 & & $3.54 \pm 0.39$ & 3.55 & 24 & $2.78 \pm 0.08$~$\times$ $10^{-11}$  &  $117 \pm 4$ & K08 & $3.1 \pm 3.1$ & 1.0 \\
 IRAC & I2 & & $4.51 \pm 0.51$ & 4.49  & 24 & $1.01 \pm 0.03$~$\times$ $10^{-11}$  &  $68 \pm 2$ & K08 & $-0.3 \pm 3.0$ & --0.1 \\
COBE$^{*}$ & 4.9~$\mu$m & & $4.93 \pm 0.37$ & 4.90 & $\infty$ & $7.47 \pm 1.22$~$\times$ $10^{-12}$  &  $60 \pm 10$ & S04 & $11 \pm 18$ & 0.6 \\
 IRAC & I3 & & $5.73 \pm 0.70$ & 5.73  & 24 & $4.23 \pm 0.13$~$\times$ $10^{-12}$  &  $46.3 \pm 1.4$  & K08 & $4.3 \pm 3.1$ & 1.4 \\
 IRAC & I4 & & $7.89 \pm 1.44$ & 7.87 & 24 & $1.41 \pm 0.04$~$\times$ $10^{-12}$  &  $29.1 \pm 0.9$ & K08 & $8.6 \pm 3.3$ & 2.6 \\
 VISIR & PAH1 & & $8.59 \pm 0.42$ & 8.60 & 1.3 &  $9.96 \pm 0.38$~$\times$ $10^{-13}$  &  $24.6 \pm 0.9$ & K08 & $14.9 \pm 4.4$ & 3.4 \\
 IRAS$^{**}$  & 12~$\mu$m & & $11.5 \pm 3.5$ & 11.22 & 25 & $4.32 \pm 0.17$~$\times$ $10^{-13}$  &  $18.1 \pm 0.7$ & I86 & $17.1 \pm 4.7$ & 3.6 \\
 VISIR & PAH2 & & $11.25  \pm 0.59$ & 11.25 & 1.3 &  $3.46 \pm 0.12$~$\times$ $10^{-13}$  &  $14.6 \pm 0.5$ & K08 & $16.1 \pm 4.2$ & 3.9 \\
 VISIR & SiC & & $11.85  \pm 2.34$ & 11.79 & 1.3 & $3.00 \pm 0.07$~$\times$ $10^{-13}$  &  $13.9 \pm 0.3$ & K08 & $16.7 \pm 2.9$ & 5.8 \\
COBE$^{*}$ & 12~$\mu$m & & $12.71 \pm 4.08$ & 12.35 & $\infty$ & $3.64 \pm 2.89$~$\times$ $10^{-13}$  &  $19 \pm 15$ & S04 & $18.6 \pm 94$ & 0.2 \\
 IRAS$^{**}$  & 25~$\mu$m & & $24 \pm 6$ & 23.34 & 25 &  $2.37 \pm 0.14$~$\times$ $10^{-14}$  &  $4.31 \pm 0.26$ & I86 & $25.3 \pm 7.5$ & 3.4 \\	
 MIPS & M1 & & $23.5 \pm 2.7$ & 23.68 & 35 & $2.00 \pm 0.08$~$\times$ $10^{-14}$  &  $3.73 \pm 0.15$ & K08 & $23.4 \pm 4.9$ & 4.7 \\
 IRAS$^{**}$  & 60~$\mu$m & & $62 \pm 17$ & 59.32 & 60 & $7.63 \pm 0.69$~$\times$ $10^{-16}$  &  $0.90 \pm 0.08$ & I86 & $51.3 \pm 14$ & 3.8 \\	
 MIPS & M2 & & $70.4 \pm 9.54$ & 71.42 & 30 & $2.63 \pm 0.13$~$\times$ $10^{-16}$  &  $0.45 \pm 0.02$ & K08 & $30.5 \pm 6.5$ & 4.7 \\
\hline
{\bf RS~Pup} \\
 {\it Johnson} & $B$ & $\bullet$ & $0.44 \pm 0.05$ & 0.44 & $-$ & $1.56 \pm 0.04$~$\times$ $10^{-10}$  &  $10.1 \pm 0.3$ & F07 & $1.5 \pm 2.8$ & 0.5 \\
 {\it Johnson} & $V$ & $\bullet$ & $0.55 \pm 0.04$ & 0.56 & $-$  & $2.21 \pm 0.06$~$\times$ $10^{-10}$  &  $22.3 \pm 0.6$  & F07 & $-0.5 \pm 2.8$ & --0.2 \\
 {\it Cousins}  & $R_{\rm c}$ & $\bullet$ & $0.65 \pm 0.15$ & 0.65 & $-$  & $2.30 \pm 0.06$~$\times$ $10^{-10}$  &  $32.1 \pm 0.9$  & F07 & $7.7 \pm 3.0$ & 2.6 \\
 {\it Cousins}  & $I_{\rm c}$ & $\bullet$ & $0.75 \pm 0.11$ & 0.75 & $-$  & $1.76 \pm 0.05$~$\times$ $10^{-10}$  &  $32.8 \pm 0.9$  & F07 & $4.6 \pm 2.9$ & 1.6 \\
 {\it 2MASS} & $J$ & $\bullet$ & $1.25 \pm 0.15$ & 1.22 & $-$  & $8.40 \pm 0.40$~$\times$ $10^{-11}$  &  $43.7 \pm 2.1$ & F07 & $6.3 \pm 5.0$ & 1.3 \\
 {\it 2MASS} & $H$ & $\bullet$ & $1.62 \pm 0.10$ & 1.65 & $-$  & $4.28 \pm 0.20$~$\times$ $10^{-11}$  &  $37.4 \pm 1.8$  & F07 & $-3.0 \pm 4.6$ & --0.7 \\
 {\it 2MASS} & $K$ & $\bullet$ & $2.20 \pm0.30$ & 2.16 & $-$  & $1.82 \pm 0.09$~$\times$ $10^{-11}$  &  $29.4 \pm 1.4$ & F07 & $0.9 \pm 4.8$ & 0.2 \\
  IRAC & I1 & & $3.54 \pm 0.39$ & 3.55 & 6.1 &  $3.41 \pm 0.10$~$\times$ $10^{-12}$ &  $14.3 \pm 0.4$ & K08 & $19.2 \pm 3.6$ & 5.4 \\
 IRAC & I2 & & $4.51 \pm 0.51$ & 4.49  & 6.1 &  $1.31 \pm 0.04$~$\times$ $10^{-12}$  &  $8.82 \pm 0.26$ & K08 & $20.8 \pm 3.6$ & 5.7 \\
 IRAC & I3 & & $5.73 \pm 0.70$ & 5.73 & 6.1 &  $5.16 \pm 0.16$~$\times$ $10^{-13}$  &  $5.22 \pm 0.17$ & K08 & $18.7 \pm 3.6$ & 5.3 \\
 IRAC & I4 & & $7.89 \pm 1.44$ & 7.87 & 6.1 &  $1.49 \pm 0.05$~$\times$ $10^{-13}$  &  $3.08 \pm 0.09$ & K08 & $8.2 \pm 3.2$ & 2.5 \\
 VISIR & PAH1 & & $8.59  \pm 0.42$ & 8.60 & 1.3 &  $1.03 \pm 0.02$~$\times$ $10^{-13}$  &  $2.53 \pm 0.06$ & K08 & $11.4 \pm 2.5$ & 4.5 \\
 IRAS$^{**}$  & 12~$\mu$m & & $11.5 \pm3.5$ & 11.22 & 25 & $5.15 \pm 0.36$~$\times$ $10^{-14}$  &  $2.16 \pm 0.15$ & I86 & $31 \pm 9.2$ & 3.4 \\	
 VISIR & PAH2 & & $11.25 \pm 0.59$ & 11.27 & 1.3 &  $3.76 \pm 0.16$~$\times$ $10^{-14}$  &  $1.59 \pm 0.16$ & K08 & $18.8 \pm 5.2$ & 3.6 \\
  IRAS$^{**}$  & 25~$\mu$m & & $24 \pm 6$ & 23.34 & 25 &  $3.96 \pm 0.28$~$\times$ $10^{-15}$  & $0.72 \pm 0.05$ & I86 & $96 \pm 14$ & 7.0 \\	
 MIPS & M1 & & $23.5 \pm 2.7$ & 23.68 & 180 & $4.21 \pm 0.17$~$\times$ $10^{-15}$  &  $0.79 \pm 0.03$ & K08 & $145 \pm 9.8$ & 15 \\
 IRAS  & 60~$\mu$m & & $62 \pm 17$ & 59.32 & $\infty$ &  $1.19 \pm 0.26$~$\times$ $10^{-14}$  &  $13.9 \pm 3.1$ & H88 & $220 \pm 49\times$ & 4.5 \\
 MIPS$^{***}$ & M2 & & $70.4 \pm 9.5$ & 71.42 & $\infty$ & $9.94 \pm 0.50$~$\times$ $10^{-15}$  &  $16.9 \pm 0.9$ & K08 & $463 \pm 23\times$ & 20 \\
 IRAS  & 100~$\mu$m & & $103 \pm 18$ & 100.3 & $\infty$ & $7.87 \pm 1.57$~$\times$ $10^{-15}$  &  $26.4 \pm 5.3$ & H88 & $1~430 \pm 290\times$ & 5 \\	
\hline
\end{tabular}}
\medskip
$^{*}$ The angular resolution of COBE/DIRBE is $\approx$$0.7^\circ$, its aperture is thus considered as infinitely large. \\
$^{**}$ The IRAS Point Source Catalogue (IPAC \cite{ipac86}) apertures were taken as the 80\% encircled energy from Beichman et~al. (\cite{beichman88}). \\
$^{***}$ The MIPS/M2 flux density of RS~Pup's CSE is the integral of the Gaussian profile adjusted in Sect.~\ref{cse-sb}.
\end{table}