Table 1: Results of single Gaussian (top) and 7-component HFS (bottom) fits to the spectra observed toward the center of Cha-MMS1.
Line $V_{{\rm lsr}}$(1) FWHM(1) Area(1) $T^\star_{{\rm a}}$ rms $\Delta V^{(1,2)}_{{\rm NT}}$
  (km s-1) (km s-1) (K km s-1) (K) (mK) (km s-1)
H13CO+(4-3) 4.42(8) 0.53(3) 0.20(1) 0.35 41 0.53(3)
DCO+(4-3) 4.42(1) 0.51(3) 0.58(3) 1.08 90 0.49(3)
DCO+(5-4) 4.47(4) 0.46(8) 0.095(15) 0.20 71 0.44(8)
H2D+ (110-111) 4.57(4) 0.63(7) 0.20(2) 0.31 78 0.53(8)
Line $V_{{\rm lsr}}$(1) FWHM(1) $T^\star_{{\rm a}}$ $\times \tau_{{\rm tot}}$(1) $\tau_{{\rm tot}}$(1) rms $\Delta V^{(1,2)}_{{\rm NT}}$
  (km s-1) (km s-1) (K)   (mK) (km s-1)
N2H+(3-2) 4.44(1) 0.42(1) 24(2) 24(2) 50 0.40(1)
N2H+(4-3) 4.65(2) 0.50(5) 2.3(7) 3.4(14) 81 0.49(5)
N2D+(4-3) 4.44(2) 0.41(3) 0.53(3) 0.5(0) 44 0.40(3)
(1)
The statistical uncertainties in parenthesis are given in units of the last digit. 0 means the parameter was fixed. For $V_{{\rm lsr}}$, they include the contribution of the frequency uncertainties listed in Table 2.
(2)
The non-thermal linewidth was computed assuming $T_{{\rm K}}$ = 10 K and, for the Gaussian fits, optically thin emission.


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