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\usepackage{supertabular}
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\begin{document}

\begin{table}
\caption[]{Atomic lines found in ultracool dwarf synthetic spectrum from 
10000 -- 25000\AA.
The columns are priority of the line (Pr), wavelength in \AA ($\lambda$ (\AA)),
element name (Atom),
residual flux in ``ultracool dwarf'' synthetic spectrum (UCD\_ss),
residual flux in ``Arcturus-like'' synthetic spectrum (Ar\_ss),
residual line intensity from hard copy of Arcturus atlas (Ar\_At),
residual line intensity from hard copy of Sunspot umbra atlas (Ss\_At).}
\end{table}
\footnotesize
\tablefirsthead{\hline 
 Pr & $\lambda$ (\AA) & Atom & UCD\_ss & Ar\_ss & Ar\_At & Ss\_At \\ \hline } 
\tablehead{\hline  
 Pr & $\lambda$ (\AA) & Atom & UCD\_ss & Ar\_ss & Ar\_At & Ss\_At \\ \hline }  
\tabletail{\hline }
\tablelasttail{\hline }
\begin{supertabular}{|c|c|c|c|c|c|c|}
    & 10003.086 & Ti~I & 0.909  & 0.716  & 0.75 &    --  \\
    & 10011.745 & Ti~I & 0.928  & 0.756  & 0.77 &    --  \\
    &{\it 10032.099} &{\it Ba~I} &{\it 0.887} &{\it 1.000} &{\it 0.97} &  --  \\
    & 10034.491 & Ti~I & 0.855  & 0.739  & 0.63 &    --  \\
    & 10048.826 & Ti~I & 0.845  & 0.730  & 0.65 &    --  \\
    & 10057.728 & Ti~I & 0.867  & 0.659  & 0.65 &    --  \\
    & 10059.904 & Ti~I & 0.868  & 0.779  & 0.72 &    --  \\
    & 10155.159 & Fe~I & 0.917  & 0.790  & 0.67 &    --  \\
    & 10167.463 & Fe~I & 0.893  & 0.753  & 0.65 &    --  \\
2   & 10340.880 & Fe~I & 0.772  & 0.608  & 0.55 &    --  \\
1   & 10343.820 & Ca~I & 0.365  & 0.420  & 0.44 &    --  \\
    & 10378.995 & Fe~I & 0.904  & 0.747  & 0.68 &    --  \\
3   & 10395.789 & Fe~I & 0.650  & 0.566  & 0.50 &    --  \\
1   & 10396.802 & Ti~I & 0.384  & 0.441  & 0.35 &    --  \\
    &{\it 10471.272} &{\it Ba~I} &{\it 0.936}  &{\it 1.000} &{\it 0.99} & --  \\
1   & 10496.114 & Ti~I & 0.403  & 0.445  & 0.35 &    --  \\
1   & 10584.633 & Ti~I & 0.425  & 0.449  & 0.38 &    --  \\
2   & 10607.718 & Ti~I & 0.677  & 0.639  & 0.70 &    --  \\
1   & 10661.623 & Ti~I & 0.455  & 0.475  & 0.41 &    --  \\
2   & 10677.047 & Ti~I & 0.621  & 0.581  & 0.61 &    --  \\
1   & 10726.391 & Ti~I & 0.489  & 0.490  & 0.45 &    --  \\
2   & 10732.864 & Ti~I & 0.615  & 0.591  & 0.60 &    --  \\
2   & 10746.440 & Na~I & 0.783  & 0.840  & 0.94 &    --  \\
    & 10749.293 & Na~I & 0.880  & 0.749  & 1.00 &    --  \\
2   & 10774.866 & Ti~I & 0.652  & 0.622  & 0.63 &    --  \\
2   & 10821.176 & S~I  & 0.696  & 0.451  & 0.85 &    --  \\
    & 10827.896 & Ti~I & 0.928  & 0.924  & 0.97 &    --  \\
2   & 10834.848 & Na~I & 0.757  & 0.732  & 0.84 &    --  \\
    & 10847.634 & Ti~I & 0.926  & 0.926  & 0.95 &    --  \\
1   & 11019.848 & K~I  & 0.477  & 0.902  & 1.00 &    --  \\
1   & 11022.653 & K~I  & 0.550  & 0.934  & 0.95 &    --  \\
2   & 11119.798 & Fe~I & 0.764  & 0.536  & 0.52 &    --  \\ 
2   & 11251.116 & Fe~I & 0.766  & 0.546  & 0.98 &    --  \\
    & 11298.862 & Fe~I & 0.837  & 0.609  & 0.55 &    --  \\
    &{\it 11303.052} &{\it Ba~I} &{\it 0.488} &{\it 0.977} &{\it 1.00} & --  \\
3   & 11374.081 & Fe~I & 0.557  & 0.538  & 0.50 &    --  \\
1   & 11381.454 & Na~I & 0.094  & 0.416  & 0.35 &    --  \\
1   & 11403.779 & Na~I & 0.076  & 0.385  & 0.26 &    --  \\
3   & 11422.323 & Fe~I & 0.509  & 0.469  & 0.37 &    --  \\
2   & 11439.127 & Fe~I & 0.650  & 0.476  &  --  &    --  \\ 
1   & 11593.591 & Fe~I & 0.477  & 0.437  &  --  &   0.70 \\
1   & 11607.575 & Fe~I & 0.359  & 0.389  & 0.30 &   0.60 \\ 
    & 11610.522 & Cr~I & 0.899  & 0.557  & 0.52 &   0.70 \\
1   & 11638.264 & Fe~I & 0.395  & 0.411  & 0.33 & $\sim$0.55 \\
1   & 11689.976 & Fe~I & 0.021  & 0.388  & 0.31 &   0.45 \\
1   & 11690.220 & K~I  & 0.013  & 0.483  & 0.40bl & $\sim$0.48 \\
1   & 11769.639 & K~I  & 0.061  & 0.601  & 0.70 &   0.65 \\ 
1   & 11772.838 & K~I  & 0.004  & 0.468  & 0.42 &  $\sim$0.55 \\
3   & 11780.543 & Ti~I & 0.522  & 0.736  & 0.75 &   0.82 \\ 
3   & 11783.267 & Fe~I & 0.485  & 0.453  & 0.40 &   0.67 \\
3   & 11797.179 & Ti~I & 0.779  & 0.757  & 0.75 &   0.82 \\
2   & 11828.185 & Mg~I & 0.705  & 0.430  & 0.21 &   0.50 \\
1   & 11882.847 & Fe~I & 0.277  & 0.353  & 0.29 &   0.55 \\
1   & 11884.085 & Fe~I & 0.364  & 0.398  & 0.33 &   0.57 \\
2   & 11892.878 & Ti~I & 0.731  & 0.606  & 0.57 &   0.70 \\
2   & 11949.542 & Ti~I & 0.700  & 0.571  & 0.55 &   0.72 \\
    & 11955.955 & Ca~I & 0.878  & 0.620  & 0.85 &   0.82 \\
1   & 11973.050 & Fe~I & 0.225  & 0.334  & 0.28 &    --  \\
1   & 11973.848 & Ti~I & 0.498  & 0.574  & 0.53 &  $\sim$0.50 \\
1   & 12432.273 & K~I  & 0.080  & 0.582  & 0.67 &   0.65 \\
2   & 12484.618 & Ti~I & 0.793  & 0.661  & 0.98 &   0.98 \\
1   & 12522.134 & K~I  & 0.022  & 0.528  & 0.57 &   0.60 \\ 
3   & 12526.081 & K~I  & 0.429  & 0.989  & 0.97 &   0.99 \\
2   & 12556.999 & Fe~I & 0.790  & 0.606  & 0.62 &   0.80 \\
    & 12600.277 & Ti~I & 0.862  & 0.748  & 0.75 &   0.80 \\
    & 12671.092 & Ti~I & 0.864  & 0.746  & 0.75 &   0.83 \\
2   & 12679.144 & Na~I & 0.656  & 0.589  & 0.66 &   0.65 \\
2   & 12679.224 & Na~I & 0.658  & 0.604  & 0.66 &   0.65 \\
    & 12738.383 & Ti~I & 0.914  & 0.726  & 0.75 &   0.75 \\
    & 12816.046 & Ca~I & 0.857  & 0.615  & 0.79 &   0.76 \\
2   & 12821.672 & Ti~I & 0.628  & 0.519  & 0.45 &   0.67 \\
    & 12823.868 & Ca~I & 0.889  & 0.671  & 0.83 &   0.78 \\
2   & 12831.442 & Ti~I & 0.645  & 0.527  & 0.50 &   0.70 \\
2   & 12847.033 & Ti~I & 0.621  & 0.512  & 0.50 &   0.70 \\
2   & 12879.769 & Fe~I & 0.740  & 0.571  & 0.55 &   0.75 \\
1   & 12899.764 & Mn~I & 0.468  & 0.444  & 0.22 &   0.57 \\
    & 12975.912 & Mn~I & 0.851  & 0.587  & 0.46 &   0.75 \\
    & 13011.895 & Ti~I & 0.852  & 0.729  & 0.75 &   0.77 \\
    & 13077.263 & Ti~I & 0.896  & 0.798  & 0.70 &   0.80 \\
1   & 13123.410 & Al~I & 0.433  & 0.390  & 0.21 &   0.45 \\
1   & 13150.753 & Al~I & 0.500  & 0.415  & 0.25 &   0.52 \\
    &{\it 13233.279} &{\it Rb~I} &{\it 0.642} &{\it 1.000} &{\it 1.00} &{\it 0.99} \\
    & 13281.485 & Mn~I & 0.902  & 0.632  & 0.55 &   0.82 \\
2   & 13293.795 & Mn~I & 0.619  & 0.497  & 0.33 &   0.72 \\
1   & 13318.944 & Mn~I & 0.547  & 0.465  & 0.27 &   0.67 \\
    &{\it 13371.782} &{\it Lu~I} &{\it 0.385} &{\it 0.749} &{\it 1.00} & --  \\
    & 13377.794 & K~I  & 0.854  & 0.989  & 1.00 &    --  \\
    & 13409.108 & Ti~I & 0.716  & 0.583  & 0.97 &   1.00 \\
    & 13600.372 & Mn~I & 0.818  & 0.627  & $\bigoplus$  & $\bigoplus$  \\
3   & 13626.696 & Mn~I & 0.593  & 0.477  & $\bigoplus$  & $\bigoplus$  \\
3   & 13642.930 & Mn~I & 0.672  & 0.519  & $\bigoplus$  & $\bigoplus$  \\
    &{\it 13662.993} &{\it Rb~I} &{\it 0.523} &{\it 0.989} & $\bigoplus$  & $\bigoplus$ \\
    & 13688.911 & Ti~I & 0.905  & 0.822  & $\bigoplus$  & $\bigoplus$  \\
    & 13787.736 & V~I  & 0.832  & 0.746  & $\bigoplus$  & $\bigoplus$  \\
3   & 13847.454 & Mn~I & 0.725  & 0.558  & $\bigoplus$  & $\bigoplus$  \\
3   & 13864.219 & Mn~I & 0.625  & 0.492  & $\bigoplus$  & $\bigoplus$  \\
3   & 13997.520 & Mn~I & 0.663  & 0.509  & $\bigoplus$  & $\bigoplus$  \\
    & 14040.849 & V~I  & 0.841  & 0.757  & $\bigoplus$  & $\bigoplus$  \\
    & 14253.141 & V~I  & 0.848  & 0.765  & $\bigoplus$  & $\bigoplus$  \\
    & 14270.253 & Ca~I & 0.850  & 0.531  & $\bigoplus$  & $\bigoplus$  \\
    & 14308.700 & Fe~I & 0.852  & 0.551  & $\bigoplus$  & $\bigoplus$  \\       
    & 14423.053 & V~I  & 0.875  & 0.807  & $\bigoplus$  & $\bigoplus$  \\
    &{\it 14752.870} &{\it Rb~I} &{\it 0.368} &{\it 0.968} & $\bigoplus$ & $\bigoplus$  \\
2   & 14767.484 & Na~I & 0.786  & 0.706  & $\bigoplus$  & $\bigoplus$  \\
2   & 14779.732 & Na~I & 0.706  & 0.615  & 0.99 &   0.57bl \\
    &{\it 14999.917} &{\it Ba~I} &{\it 0.435} &{\it 0.952} &{\it 1.00} &{\it 0.95} \\
2   & 15024.992 & Mg~I & 0.780  & 0.399  & 0.24 &   0.49 \\ 
    & 15040.246 & Mg~I & 0.815  & 0.412  & 0.24 &   0.55 \\
    & 15057.099 & Ca~I & 0.829  & 0.895  & 0.97 &   0.77 \\
2   & 15077.291 & Fe~I & 0.771  & 0.545  & 0.98 &   0.79 \\
1   & 15163.067 & K~I  & 0.254  & 0.534  & 0.67 &   0.67 \\
1   & 15163.067 & K~I  & 0.254  & 0.534  & 0.67 &   0.67 \\
1   & 15168.376 & K~I  & 0.280  & 0.572  & 0.70 &   0.72 \\
    &{\it 15288.938} &{\it Rb~I} &{\it 0.501} &{\it 0.993} &{\it 1.00} &{\it 0.85} \\
    &{\it 15289.966} &{\it Rb~I} &{\it 0.299} &{\it 0.940} &{\it 1.00} &{\it 0.90} \\
2   & 15334.847 & Ti~I & 0.618  & 0.436  & 0.45 &   0.60 \\
    & 15490.339 & Fe~I & 0.858  & 0.642  & 0.64 &   1.00 \\
2   & 15543.756 & Ti~I & 0.628  & 0.451  & 0.47 &   0.65 \\
    & 15602.842 & Ti~I & 0.867  & 0.646  & 0.73 &   0.72 \\
    & 15698.979 & Ti~I & 0.855  & 0.699  & 0.70 &   0.75 \\
2   & 15715.573 & Ti~I & 0.629  & 0.446  & 0.50 &   0.67 \\
    & 15836.788 & Ti~I & 0.851  & 0.710  & 0.73 &   0.85 \\
2   & 16136.823 & Ca~I & 0.795  & 0.474  & 0.76 &   0.70 \\
2   & 16150.763 & Ca~I & 0.695  & 0.427  & 0.68 &   0.67 \\
    & 16155.236 & Ca~I & 0.829  & 0.496  & 0.80 &   0.80 \\
2   & 16157.364 & Ca~I & 0.674  & 0.416  & 0.67 &   0.62 \\
2   & 16197.075 & Ca~I & 0.635  & 0.398  & 0.55 &   0.56 \\
    & 16204.087 & Ca~I & 0.825  & 0.494  & 0.85 &    --  \\
2   & 16388.857 & Na~I & 0.771  & 0.770  & 0.95 &   0.87 \\
    & 16454.533 & Si~I & 0.868  & 0.585  & 0.98 &   0.93 \\
2   & 16718.957 & Al~I & 0.678  & 0.398  & 0.55 &   0.45bl \\
2   & 16750.564 & Al~I & 0.626  & 0.380  & 0.27 &   0.50 \\
2   & 17108.662 & Mg~I & 0.799  & 0.403  & 0.27 &   0.47 \\
    &{\it 17123.809} &{\it Y~I} &{\it 0.581} &{\it 0.699} &{\it 0.99} &{\it 0.96} \\
    &{\it 17422.836} &{\it Y~I} &{\it 0.537} &{\it 0.631} &{\it 1.00} &{\it 0.90} \\
    &{\it 17663.289} &{\it Y~I} &{\it 0.526} &{\it 0.625} &{\it 0.95} &{\it 0.98} \\
    &{\it 17903.229} &{\it Y~I} &{\it 0.489} &{\it 0.559} &{\it 1.00} &  --  \\
    &{\it 18049.807} &{\it Y~I} &{\it 0.473} &{\it 0.557} &{\it 1.00} &  --  \\
    &{\it 18115.295} &{\it Y~I} &{\it 0.458} &{\it 0.533} &{\it 1.00} &  --  \\
    &{\it 18181.758} &{\it Y~I} &{\it 0.450} &{\it 0.539} &  --  &    --  \\
    &{\it 18234.975} &{\it Lu~I} &{\it 0.377} &{\it 0.732} &{\it 1.00} &  --  \\
    &{\it 18293.682} &{\it Y~I}  &{\it 0.523} &{\it 0.641} & $\bigoplus$  & $\bigoplus$ \\
1   & 18465.312 & Na~I & 0.333  & 0.402  & $\bigoplus$  & $\bigoplus$  \\
1   & 18465.312 & Na~I & 0.333  & 0.402  & $\bigoplus$  & $\bigoplus$  \\
1   & 18465.484 & Na~I & 0.337  & 0.410  & $\bigoplus$  & $\bigoplus$  \\
3   & 18856.646 & Fe~I & 0.770  & 0.458  & $\bigoplus$  & $\bigoplus$  \\
    & 18987.010 & Fe~I & 0.830  & 0.495  & $\bigoplus$  & $\bigoplus$  \\
    & 19046.178 & Ca~I & 0.828  & 0.555  & $\bigoplus$  & $\bigoplus$  \\
1   & 19309.223 & Ca~I & 0.144  & 0.326  & $\bigoplus$  & $\bigoplus$  \\
1   & 19452.982 & Ca~I & 0.125  & 0.311  & $\sim$0.20 &    -- \\
1   & 19505.738 & Ca~I & 0.142  & 0.337  & 0.22 &  $\sim$0.30 \\
    &{\it 19728.117} &{\it Y~I} &{\it 0.601} &{\it 0.726} &{\it 0.99} &{\it 0.95} \\
1   & 19776.771 & Ca~I & 0.074  & 0.306  & 0.16 &   0.30 \\
1   & 19853.092 & Ca~I & 0.516  & 0.428  & 0.45 &   0.50 \\
1   & 19862.191 & Ca~I & 0.162  & 0.345  & 0.25 &  $\sim$0.35 \\
1   & 19917.195 & Ca~I & 0.280  & 0.417  & 0.45 &   0.65 \\
1   & 19933.729 & Ca~I & 0.555  & 0.443  & 0.45 &   0.65 \\
2   & 19961.832 & Ca~I & 0.638  & 0.477  & $\sim$0.60 &    -- \\
    &{\it 20170.207} &{\it Y~I} &{\it 0.647} &{\it 0.778} &{\it 1.00} &{\it 1.00} \\
    &{\it 20831.520} &{\it Y~I} &{\it 0.624} &{\it 0.747} &{\it 1.00} &{\it 0.95} \\
    &{\it 20879.256} &{\it Y~I} &{\it 0.678} &{\it 0.812} &{\it 0.97} &{\it 0.90} \\
2   & 21163.756 & Al~I & 0.794  & 0.497  & 0.45 &   0.65 \\
    &{\it 21260.449} &{\it Y~I} &{\it 0.526} &{\it 0.617} &{\it 0.96} &{\it 1.00} \\
    &{\it 21574.170} &{\it Y~I} &{\it 0.605} &{\it 0.733} &{\it 1.00} &{\it 0.95} \\
    & 21730.506 & Sc~I & 0.821  & 0.904  & 0.95 &   0.98 \\
1   & 21782.926 & Ti~I & 0.532  & 0.467  & 0.50 &   0.70 \\
    & 21812.055 & Sc~I & 0.802  & 0.896  & 0.95 &   0.93 \\
2   & 21897.377 & Ti~I & 0.583  & 0.493  & 0.55 &   0.72 \\
2   & 22004.494 & Ti~I & 0.671  & 0.551  & 0.66 &   0.80 \\
1   & 22052.141 & Sc~I & 0.493  & 0.579  & 0.75 &   0.65 \\
1   & 22056.426 & Na~I & 0.342  & 0.469  & 0.50 &   0.50 \\
1   & 22065.232 & Sc~I & 0.544  & 0.635  & 0.83 &   0.75 \\
1   & 22083.662 & Na~I & 0.383  & 0.487  & 0.56 &   0.60 \\
1   & 22211.229 & Ti~I & 0.650  & 0.537  & 0.63 &   0.80 \\
1   & 22232.838 & Ti~I & 0.628  & 0.521  & 0.61 &   0.76 \\
2   & 22266.729 & Sc~I & 0.648  & 0.756  & 0.90 &   0.85 \\
1   & 22274.012 & Ti~I & 0.654  & 0.540  & 0.64 &   0.75 \\
3   & 22310.617 & Ti~I & 0.682  & 0.613  & 0.75 &   0.80 \\
    &{\it 22311.588} &{\it Ba~I} &{\it 0.475} &{\it 0.980} &{\it 0.98} &{\it 0.96} \\
2   & 22394.670 & Sc~I & 0.587  & 0.686  & 0.89 &   0.81 \\ 
2   & 22443.904 & Ti~I & 0.773  & 0.657  & 0.77 &   0.85 \\
    &{\it 22543.826} &{\it Y~I} &{\it 0.538} &{\it 0.647} &{\it 1.00} &{\it 0.97} \\
    & 22656.963 & Sc~I & 0.844  & 0.919  & 0.97 &   0.90 \\
2   & 22963.336 & Ti~I & 0.675  & 0.547  & 0.65 &   0.75 \\
2   & 22986.250 & Sc~I & 0.605  & 0.697  & 0.89 &   0.87 \\
    &{\it 23204.070} &{\it Y~I} &{\it 0.686} &{\it 0.826} &{\it 1.00} &{\it 0.96} \\ 
    &{\it 23253.688} &{\it Ba~I} &{\it 0.467} &{\it 0.966} &{\it 0.98} &{\it 0.98} \\ 
1   & 23348.424 & Na~I & 0.563  & 0.548  & 0.60bl & 0.64 \\
1   & 23378.945 & Na~I & 0.516  & 0.535  &  --  &   0.60 \\
1   & 23379.137 & Na~I & 0.513  & 0.525  & $\sim$0.60 &  0.60 \\
2   & 23404.758 & Sc~I & 0.646  & 0.755  & 0.90  &  0.95 \\
2   & 23441.471 & Ti~I & 0.702  & 0.572  & 0.60bl & 0.70 \\
2   & 23719.029 & Ti~I & 0.736  & 0.595  &  --  &   0.98 \\
    & 23809.379 & Sc~I & 0.694  & 0.801  & 0.96 &   0.95 \\
    &{\it 23990.445} &{\it Y~I} &{\it 0.554} &{\it 0.675} &{\it 1.00} &  --  \\ 
    & 24074.787 & Sc~I & 0.734  & 0.839  & 0.93 &   0.87 \\
    &{\it 24170.594} &{\it Lu~I} &{\it 0.190} &{\it 0.630} &{\it 0.97} &{\it 0.95} \\
2   & 24281.809 & Ti~I & 0.788  & 0.611  & 1.00 &   0.70 \\ 
\end{supertabular}

\clearpage

\begin{table}
\caption[]{ Sensitivity of first priority lines to temperature, gravity and 
metallicity.
The columns are wavelength in \AA ($\lambda$ (\AA)), name of element (Atom), 
central line intensity in the 2000/5.0/0.0 synthetic spectrum (LD),
temperature sensitivity in \% ($\Delta r_{\nu}^{\rm (Teff)}$),
log~g sensitivity in \% ($\Delta r_{\nu}^{\rm (log~g)}$), 
metallicity sensitivity in \% ($\Delta r_{\nu}^{\rm ([M/H])}$). }
\end{table}
\footnotesize
\tablefirsthead{\hline 
$\lambda$ (\AA) & Atom & LD &$\Delta r_{\nu}^{\rm (Teff)}$ & $\Delta r_{\nu}^{\rm (log~g)}$ & $\Delta r_{\nu}^{\rm ([M/H])}$\\ 
\hline }  
\tablehead{\hline 
$\lambda$ (\AA) & Atom & LD &$\Delta r_{\nu}^{\rm (Teff)}$ & $\Delta r_{\nu}^{\rm (log~g)}$ & $\Delta r_{\nu}^{\rm ([M/H])}$\\ 
\hline }
\tabletail{\hline }
\tablelasttail{\hline }
\begin{supertabular}{|c|c|c|c|c|c|} 
 10343.820 & Ca~I & 0.172 & -1.22 &  -6.86 &   19.49 \\ 
 10396.802 & Ti~I & 0.115 &  4.27 &  -2.01 &  -19.01 \\ 
 10496.114 & Ti~I & 0.125 &  4.24 &  -2.08 &  -18.65 \\ 
 10584.633 & Ti~I & 0.138 &  4.06 &  -2.18 &  -18.21 \\ 
 10661.623 & Ti~I & 0.155 &  3.56 &  -2.33 &  -17.85 \\ 
 10726.391 & Ti~I & 0.176 &  3.02 &  -2.50 &  -17.36 \\ 
 11019.848 & K~I  & 0.423 & -4.75 & -26.12 &   55.45 \\ 
 11022.653 & K~I  & 0.489 & -4.11 & -25.90 &   48.95 \\ 
 11381.454 & Na~I & 0.039 &  5.94 &  -8.27 &   27.39 \\ 
 11403.779 & Na~I & 0.030 &  6.98 &  -7.64 &   23.92 \\ 
 11593.591 & Fe~I & 0.186 &  3.70 &  -3.38 &   25.00 \\ 
 11607.575 & Fe~I & 0.119 &  5.42 &  -3.17 &   22.44 \\ 
 11638.264 & Fe~I & 0.136 &  5.22 &  -3.23 &   23.51 \\ 
 11689.976 & Fe~I & 0.135 &  5.12 &  -3.04 &   23.01 \\ 
 11690.220 & K~I  & 0.013 & 14.39 &  -7.58 &   18.94 \\ 
 11769.639 & K~I  & 0.027 & 11.44 &  -7.75 &   22.51 \\ 
 11772.838 & K~I  & 0.011 & 15.74 &  -6.48 &   19.44 \\ 
 11882.847 & Fe~I & 0.094 & 6.08  &  -2.99 &   19.55 \\ 
 11884.085 & Fe~I & 0.139 & 4.96  &  -3.02 &   22.66 \\ 
 11973.050 & Fe~I & 0.078 & 6.43  &  -3.21 &   17.74 \\ 
 11973.848 & Fe~I & 0.462 & 0.02  &  -3.98 &   -2.38 \\ 
 12432.273 & K~I  & 0.032 &  9.18 & -10.13 &   29.43 \\ 
 12522.134 & K~I  & 0.025 & 10.08 &  -9.68 &   25.00 \\ 
 12899.764 & Mn~I & 0.219 &  3.10 &  -4.05 &   24.90 \\ 
 13123.410 & Al~I & 0.319 & -4.76 &  -5.51 &   16.89 \\ 
 13150.753 & Al~I & 0.370 & -2.73 &  -6.24 &   19.58 \\ 
 13318.944 & Mn~I & 0.299 &  2.17 &  -4.71 &   26.03 \\ 
 15163.067 & K~I  & 0.449 & -1.32 & -12.69 &   39.75 \\ 
 15163.067 & K~I  & 0.188 & -0.05 &  -7.47 &   29.71 \\ 
 15168.376 & K~I  & 0.208 & -0.58 &  -8.22 &   31.19 \\ 
 18465.312 & Na~I & 0.575 & -2.66 & -11.25 &   22.02 \\ 
 18465.312 & Na~I & 0.353 & -2.69 &  -7.12 &   20.91 \\ 
 18465.484 & Na~I & 0.376 & -2.68 &  -8.02 &   20.94 \\ 
 19309.223 & Ca~I & 0.091 &  2.76 &   ---  &    4.85 \\ 
 19452.982 & Ca~I & 0.078 &  3.08 &  -7.82 &    3.85 \\ 
 19505.738 & Ca~I & 0.100 &  2.60 &  -7.69 &    5.39 \\ 
 19776.771 & Ca~I & 0.073 &  3.03 &  -7.71 &    3.44 \\ 
 19853.092 & Ca~I & 0.506 & -3.16 &  -5.64 &   13.11 \\ 
 19862.191 & Ca~I & 0.107 &  2.54 &  -7.51 &    5.54 \\ 
 19917.195 & Ca~I & 0.196 &  1.43 &  -7.56 &   12.57 \\ 
 19933.729 & Ca~I & 0.537 & -1.81 &  -6.34 &   14.41 \\ 
 21782.926 & Ti~I & 0.479 & -1.46 &  -4.14 &    0.17 \\ 
 22052.141 & Sc~I & 0.374 &  2.22 &  -8.95 &   29.38 \\ 
 22056.426 & Na~I & 0.311 & -0.77 &  -5.17 &   17.47 \\ 
 22065.232 & Sc~I & 0.424 &  1.91 &  -9.68 &   30.26 \\ 
 22083.662 & Na~I & 0.356 & -2.50 &  -5.42 &   17.85 \\ 
 22211.229 & Ti~I & 0.589 & -0.93 &  -6.59 &    6.50 \\
 22232.838 & Ti~I & 0.569 & -0.88 &  -6.01 &    5.41 \\
 22274.012 & Ti~I & 0.594 & -0.91 &  -6.65 &    6.64 \\
 23348.424 & Na~I & 0.564 & -2.73 &  -7.47 &   16.79 \\ 
 23379.137 & Na~I & 0.526 & -3.71 &  -7.71 &   16.45 \\ 
\end{supertabular}

\clearpage

{\bf Atomic lines in infrared spectra for ultracool dwarfs}

{\sl Yuri Lyubchik, Hugh R.A. Jones, Yakiv V. Pavlenko, et al.}\\


{\bf Description for tables.} 

Our results are shown in two tables.
Table~1 contains all identified lines with central intensities 
deeper than 0.8 of residual flux using ``ultracool dwarf model''
identifications. Table~2 investigates the sensitivity of priority 1 lines
identified in Table~1 to tempereture, gravity and metallicity.

In the first column of Table~1 we estimate the priority of 
lines for measurement of atomic data. \\ 
a) Priority 1 indicates that atomic line is deeper than 0.6 
in the 2000/5.0/0.0 synthetic spectrum. Also we include as first priority 
three lines of Ti (22211.229, 22232.838, 22274.012\AA) which are
shallower than 0.6. They are located far from strong atomic and 
molecular lines and thus are good for identification purposes in the 
spectra of ultracool dwarfs. \\ 
b) Priority 2 indicates that the residual flux of an atomic line is between 
0.8 -- 0.6.\\ 
c) Priority 3 indicates that the atomic line is located in the wing of a
nearby stronger line or in a wavelength region with strong telluric 
absorption. 

Atomic lines without an assigned priority might be relevant in the 
analysis of ultracool dwarf 
spectra, but they are predicted to be weak in the synthetic spectrum. 

The second column shows the wavelength of the line in \AA~ in air . These 
values were taken from VALD. We check that wavelengths from Arcturus and 
Sunspot umbra 
atlases identification files are in a good agreement with VALD.
The wavelengths of a few lines differ from VALD values by less 
than 0.1\AA~ in the region 10000 -- 20000 \AA~ and by less than 
0.3\AA~ beyond 20000 \AA.  

The third column shows the atomic identifications of the line.

Columns 4 -- 7 show the linedepths of identified lines. Column 4 -- 
the residual flux in the line obtained from the ``ultracool dwarf'' 
synthetic spectrum; 
column 5 -- from the "Arcturus-like" synthetic spectrum; column 6 -- measured 
from the hard copy of Arcturus 
atlas depth of identified atomic lines; column 7 -- the same as column 6 for 
the hard copy of the Sunspot umbra atlas. 
As was mentioned above we used the hard copy versions 
of the Arcturus and Sunspot umbra atlases to measure linedepths. 
The accuracy of our line depth measurements from the hardcopy atlases is 
$\sim$0.01 -- 0.02 for the Arcturus atlas (column 6) and $\sim$0.02 -- 0.03 
for the Sunspot umbra atlas (column 7). 
We note that linedepth information given in columns 6 and 7 
is only used to check the presence of a line in the observed spectra.
Thus we do not need  high accuracy linedepth measurements for the  
observable spectra of the Sunspot umbra and Arcturus. 

We note that the data in the Sunspot umbra atlas provide a spectrum from 
11600\AA, rather than 10000\AA~ where our figures and tables start from. 
Some lines are labelled (see column 7) by the symbol "$\sim$" 
which means that part of the line in the hard copy of the atlas is obscured by 
a gap in the data and the value given in the table is for the visible part of 
the line. In columns 6 and 7 there are also some lines with "bl" suffices. 
This means that these lines are blended with stronger nearby lines.

There are two regions with strong telluric absorption ( marked in columns 6 and 
7 by $\bigoplus$): 13600--14770\AA~ and 18260--19450\AA~, regions between 
the J and H, and H and K photometric bands. Lines 
identified from VALD in these regions are difficult to
observe in ground based observations but can be used in probable 
future space observations of ultracool dwarfs. 

Finally we note, that in Table~1 we italicise atomic lines of 
Rb, Y, Ba and Lu, identified only 
using theoretical computations. Although these lines are not seen in the 
observations of Arcturus and Sunspot umbra, they are strong in synthetic 
spectrum computed for the 2000/5.0/0.0 model atmosphere, 
and therefore also likely to be strong below 2000~K.

In Table~2 we show only lines which were marked in Table~1 as first 
priority lines. 
The first column are wavelengths in \AA; the second column are names of elements.
In the third column we give the central line intensity for the ``ultracool 
dwarf'' (2000/5.0/0.0) spectrum.
We compute some synthetic spectra for ultracool objects varying parameters 
of \Teff, log~g and metallicity to show the sensitivity of the central 
intensities of identified lines to these parameters. 
For our computations we chose the minimal step in model atmospheres grid:
$\Delta$\Teff = 100~K, $\Delta$log~g = 0.5, $\Delta$[M/H]=-0.5.
In columns 4 -- 6 we 
show the difference of central intensity ( in \% ) computations with ``new''
models from central intensity computations for our ``ultracool dwarf model''. 
Negative values in columns 4 -- 6 indicate that a line is stronger in the 
new model relative to the reference model 2000/5.0/0.0.

Column 4 shows the dependence of residual fluxes on effective temperature. 
For comparison 
a 2100/5.0/0.0 synthetic spectrum was used. One can see that only a few 
lines show strong temperature dependence for $\Delta$\Teff=100~K. 
The NextGen 2000/4.5/0.0 model was used with 2000/5.0/0.0 to test gravity 
sensitivity. The dependence for $\Delta$(log~g)=0.5 is also relatively 
weak for most lines and is shown in column 5. 
$\Delta$[M/H]=0.5 from computations using NextGen model atmospheres 
2000/5.0/-0.5 and 2000/5.0/0.0 is shown in column 6.
The metallicity dependence is relatively high for all lines. 
Thus Table~2 indicates that relatively small variations of model 
atmosphere parameters will
not seriously affect our line selection and prioritisation.

\end{document}

\end{document}

