\begin{table}%t1
%\centering
\par
\caption{\label{tab:solution}Timing solutions for the pulsars.}
\par
\begin{tabular}{lcccc}
\hline\hline \noalign{\smallskip}
Pulsar name\dotfill &  J1721$-$2457 & J1745$-$0952 & J1810$-$2005 & J1918$-$0642\\ 
\hline  
\multicolumn{2}{c}{Fit and data-set} \\
MJD range\dotfill &  52~076--54~799 & 52~076--54~776 & 50~757--54~796 & 52~094--54~814\\ 
Number of TOAs\dotfill & 120 & 113 & 491 & 152 \\
Rms timing residual ($\mu$s)\dotfill & 31.9 & 20.8 & 270.7 & 2.6\\
Weighted fit\dotfill &  Y & Y & Y & Y \\ 
Reduced $\chi^2$ value\tablefootmark{a}\dotfill & 1.05 & 1.02 & 1.01 & 1.04 \\
\hline  
\multicolumn{2}{c}{Measured quantities} \\ 
Right ascension, $\alpha$ (J2000)\dotfill & 17$^{\rm h}$21$^{\rm m}$05\fs4963(3) & 17$^{\rm h}$45$^{\rm m}$09\fs1348(2) & 18$^{\rm h}$10$^{\rm m}$58\fs9919(6) & 19$^{\rm h}$18$^{\rm m}$48\fs035270(13)\\ 
Declination, $\delta$ (J2000)\dotfill & $-$24\degr57\arcmin06\farcs36(6) & $-$09\degr52\arcmin39\farcs682(15) &  $-$20\degr05\arcmin08\farcs27(14)& $-$06\degr42\arcmin34\farcs8636(6)\\ 
Pulse frequency, $\nu$~(s$^{-1}$)\dotfill & 285.989343507338(15) & 51.609431233273(5) & 30.467142155106(7)& 130.7895141841235(6) \\ 
First derivative of pulse frequency, $\dot{\nu}$ (s$^{-2}$)\dotfill & $-$$4.533(5) \times 10^{-16}$ & $-$$2.4627(13)\times 10^{-16}$ & $-$$1.3684(11) \times 10^{-16}$& $-$$4.39525(17) \times 10^{-16}$ \\ 
Dispersion measure, DM (cm$^{-3}$pc)\dotfill & 48.34(3) & 64.27(9) & 241.0(3) & 26.554(10) \\
Proper motion in RA, $\mu_{\rm \alpha}$ (mas~yr$^{-1}$)\dotfill & 1.8(1.8) & $-$21.2(1.1) & 0(2) & $-$7.20(10)\\
Proper motion in Dec, $\mu_{\rm \delta}$ (mas~yr$^{-1}$)\dotfill & $-$14(25) & 11(5) & 17(37)& $-$5.7(3) \\
Binary\dotfill & $-$ & ELL1 & ELL1 & ELL1 \\
Orbital period, $P_{\rm b}$ (d)\dotfill & & 4.943453386(12) & 15.01201911(4) & 10.9131777486(12) \\
Projected semi-major axis of orbit, $x$ (lt-s)\dotfill & & 2.378599(5) & 11.977880(18) & 8.3504716(4) \\
TASC~(MJD)\dotfill & & 53198.621445(3) & 53195.528458(4) &  53402.53135510(8)\\
EPS1 ($\epsilon_1$)\dotfill & & \phantom{$-$}0.000009(3) & \phantom{$-$}0.000009(3) & $-$0.00001244(9) \\
EPS2 ($\epsilon_2$)\dotfill & & $-$0.000004(4) & $-$0.000017(3) &  $-$0.00001555(9)\\
\hline  
\multicolumn{2}{c}{Set quantities} \\ 
Epoch of frequency determination (MJD)\dotfill & 53400.0 & 53200.0 & 53200.0 & 53400.0 \\
Epoch of position determination (MJD)\dotfill & 53400.0 & 53200.0 & 53200.0 & 53400.0 \\
Epoch of DM determination (MJD)\dotfill &  53400.0 & 53200.0 & 53200.0 & 53400.0 \\ 
\hline  
\multicolumn{2}{c}{Derived quantities} \\
Orbital eccentricity, $e = \sqrt{\epsilon_1^{2}+\epsilon_2^{2}}$\dotfill & -- & $1.0(0.4) \times 10^{-5}$ & $1.9(4) \times 10^{-5}$ & $1.991(13) \times 10^{-5}$\\
Omega, $\omega$ = arctan ($\epsilon_1/\epsilon_2)$~($\degr$)\dotfill & -- & 114(28) & 152(12) & 218.6(4)\\
Characteristic age, (Gyr)\dotfill & 10.0 & 3.3 & 3.5 & 4.7\\
Surface magnetic field strength, ($10^{8}$G) \dotfill & 1.4 & 13.5 & 22.4 & 4.4\\
Distance\tablefootmark{b}, (kpc)\dotfill &  $1.3(2)$ & $1.8(3)$ & $4.0(4)$ & $1.23(13)$\\
Spin period (ms)\dotfill & 3.49663 & 19.3763 & 32.8222 & 7.64587\\
Spin period derivative\dotfill & $5.55 \times 10^{-21}$ & $9.23 \times 10^{-20}$ & $1.47 \times 10^{-19}$  & $2.57 \times 10^{-20}$\\
Mass function, (\msun)\dotfill & $-$ & 0.000591270(4) & 0.00818737(4) & 0.0052494438(8) \\
Minimum companion mass, (\msun)\dotfill & $-$ & 0.11 & 0.28 & 0.24 \\
Total proper motion, $\mu_{\rm T}$ (mas~yr$^{-1}$)\dotfill & 15(25) & 24(2) & 17(37) & 9.2(2)\\
Transverse velocity, $V_{\rm T}$ (km~s$^{-1}$)\dotfill & $<$140\tablefootmark{c} & 200(50) & $<$400\tablefootmark{c} & 54(7)\\
\hline  
\multicolumn{2}{c}{Assumptions} \\
Clock correction procedure \dotfill & \multicolumn{2}{c}{TT(TAI)}\\
Solar system ephemeris model \dotfill & \multicolumn{2}{c}{DE405}\\
Model version number \dotfill & \multicolumn{2}{c}{5.00}\\
\hline \noalign{\smallskip}
\end{tabular}
\tablefoot{Figures in parentheses are the nominal 1$\sigma$ \textsc{tempo}2
uncertainties in the least-significant digits quoted.
\tablefoottext{a}{Before combining the data sets from the different observatories, the errors on the TOAs were scaled with a constant factor to have each individual data set return a reduced $\chi^2\approx 1$.}  
\tablefoottext{b}{The DM distances are estimated from the \cite{cl02} model.} \tablefoottext{c}{Velocity limits from Eq.~(\ref{eq:pdot}).}}
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\end{table}