\begin{table}%t1 %\centering \par \caption{\label{tab:lines}Detected gas lines within the PACS spectrum of DK Cha.} \tiny \begin{tabular}{l l r r r r} \hline \hline\noalign{\smallskip} Species & Transition & $\lambda$\tablefootmark{a}& $E_u$& $FWHM$ & Flux\tablefootmark{b} \\ & & $\mu$m & $K$ & $\mu$m & W m$^{-2}$ \\ \hline [\ion{O}{i}] & $^3$P$_1$-$^3$P$_2$ & 63.18 & 227.72 & 0.08 & 3657.7\\ OH 3/2-3/2 & 9/2- -- 7/2+ & 65.13 & 512.1 & 0.05 & 56.0$^2$ \\ OH 3/2-3/2 & 9/2+ -- 7/2- & 65.28 & 510.9 & 0.07 & 52.3$^2$\\ CO & 38-37 & 69.07 & 4079.98 & 0.06 & 42.1$^2$ \\ CO & 37-36 & 70.91 & 3871.88 & 0.09 & 59.6$^2$ \\ o-H$_2$O$^3$& 7$_{07}$--6$_{16}$& 71.95 & 843.5 & 0.06 & 37.1$^2$\\ CO & 36--35 & 72.84 & 3668.96 & 0.06 & 40.1$^2$\\ CO & 35--34 & 74.89 & 3471.44 & 0.1 & 57.0$^2$\\ o-H$_2$O& 4$_{23}$-3$_{12}$& 78.74 & 432.2 & 0.04 & 19.8$^2$ \\ OH 1/2-3/2 & 1/2- -- 3/2+ & 79.12 & 181.7 & 0.06 & 28$^2$\\ CO & 33--32 & 79.36 & 3092.45 & 0.03 & 17.5$^2$\\ CO & 32-31 & 81.81 & 2911.15 & 0.05 & 126.2\\ o-H$_2$O & 6$_{16}$-5$_{05}$ & 82.09 & 643.5 & 0.03 & 96.2\\ CO & 31--30 & 84.41 & 2735.28 & 0.09 & 336.0 \\ OH 3/2-3/2 & 7/2+ -- 5/2- & 84.42$^1$ & 291.2 & -- & --\\ OH 3/2-3/2 & 7/2- -- 5/2+ & 84.60 & 290.5 & 0.09 & 301.4\\ CO & 30--29 & 87.19 & 2564.94 & 0.09 & 317.5\\ CO & 29--28 & 90.16 & 2399.93 & 0.14 & 545.8\\ CO & 28--27 & 93.35 & 2240.30 & 0.07 & 261.4\\ CO & 27--26 & 96.77 & 2086.22 & 0.10 & 330.1\\ CO & 25--24 & 104.44 & 1794.23 & 0.2 & 314.5\\ o-H$_2$O & 2$_{21}$--1$_{10}$& 108.08 & 194.1 & 0.15 & 126.9\\ CO & 24--23 & 108.76 & 1656.55 & 0.15 & 260.0\\ CO & 23--22 & 113.46 & 1524.19 & 0.2 & 477.4\\ o-H$_2$O & 4$_{14}$--3$_{03}$ & 113.54$^1$& 323.5 & -- & -- \\ CO & 22--21 & 118.58 & 1397.43 & 0.17 & 285.2\\ OH 3/2-3/2 & 5/2- -- 3/2+ & 119.23 & 120.7 & 0.18 & $<$40\\ OH 3/2-3/2 & 5/2+ -- 3/2- & 119.44 & 120.5 & 0.17 & $<$72.3\\ \protect{[\ion{N}{ii}}] & $^3$P$_2$--$^3$P$_1$ & 121.90 & 188.20 & 0.12 & 45.7\\ CO & 21--20 & 124.19 & 1276.10 & 0.17 & 357.1\\ p-H$_2$O & 4$_{04}$--3$_{13}$ & 125.35 & 319.5 & 0.12 & 42.8 \\ CO & 20--19 & 130.37 & 1160.24 & 0.16 & 319.0\\ CO & 19--18 & 137.20 & 1049.89 & 0.18 & 338.7\\ p-H$_2$O & 3$_{13}$--2$_{02}$& 138.53 & 204.7 & 0.17 & 103.0\\ CO & 18--17 & 144.78 & 945.01 & 0.15 & 350.4\\ \par [\ion{O}{i}] & $^3$P$_0$--$^3$P$_2$ & 145.53 & 326.58 & 0.16 & 146.7\\ CO & 17--16 & 153.27 & 845.63 & 0.15 & 386.0\\ CO & 16--15 & 162.81 & 751.76 & 0.18 & 466.5\\ OH 1/2-1/2 & 3/2+ -- 1/2- & 163.12 & 270.2 & 0.24 & 91.0\\ OH 1/2-1/2 & 3/2+ -- 1/2- & 163.40 & 269.8 & 0.19 & 90.0\\ CO & 15--14 & 173.63 & 663.37 & 0.16 & 413.0\\ o-H$_2$O &3$_{03}$--2$_{12}$& 174.63 & 196.8 & 0.19 & 208.0\\ o-H$_2$O &2$_{12}$--1$_{01}$& 179.53 & 114.4 & 0.11 & 31.0\\ o-H$_2$O &2$_{21}$--2$_{12}$ & 180.49 & 194.1 & 0.12 & 34.9 \\ CO & 14--13 & 186.00 & 580.51 & 0.20 & 437.2\\ \hline \end{tabular} \tablefoot{\tablefoottext{a}{Laboratory wavelength;} \tablefoottext{b}{flux summed over all pixels in 10$^{-18}$~W~m$^{-2}$. Typical line flux uncertainties are dominated by calibration uncertainties ($\sim$30--50\%) and fringing (0.1~Jy at the longest wavelengths to 0.6~Jy at the shortest);} \tablefoottext{1}{lines blended with above line;} \tablefoottext{2}{Line detected only in central spaxel and should not be compared to the fluxes of the summed spaxels;} \tablefoottext{3}{doublet unresolved.}} \end{table}