The results obtained for the T Tauri stars' Pa Beta and Br Gamma line parameters using the method just described, are presented in Tables 5.3 and 5.4 respectively, in the next pages. Before proceeding, a point should be made about the impact of the wavelength calibration uncertainties in some of the parameters presented in Tables 5.3 and 5.4. Those uncertainties, presented in column 3 of those tables, affect mostly the values presented for vpeak and for Af. The uncertainties quoted in Tables 5.3 and 5.4 for vpeak are often similar to or smaller than the wavelength calibration uncertainty. The uncertainty quoted for Af in Tables 5.3 and 5.4 results only from the noise in the spectrum. There is, however, an uncertainty in the zero velocity that results from the wavelength calibration. Such an uncertainty is propagated into Af via EWblue and EWred. Given the fact that, as will be seen in Section 5.3.3, most lines peak near the zero velocity, the final relative uncertainty in Af can be of the order of a few tenths. These two points should be kept in mind in the remainder of this chapter.
Table 5.4: Br Gamma (T Tauri Stars) - Star name;
Heliocentric radial velocity of the star (Vsys ); Velocity
Calibration uncertainty (Vcal ); Full width at half maximum
(FWHM) and Half width at zero intensity (HWZI). The HWZI is measured at
the 2% level of the peak. Velocity of the line peak relative to
Vsys; Maximum velocities of the blue and red wings
(vblue and vred respectively); Equivalent width
(EW); Ratio of the blue wing to the red wing equivalent widths
(EWb/EWr ) and Line to Continuum ratio at the
peak (uncertainties in L/C are typically 1 to 5%). Stars that were
observed more than once have the code (0) or (3) appended to their
names. (0)=UT9410 and (3)=UT951217. All the other stars
were observed at (3) (see text).For stars for which the
line profiles are classified as Type IV R the EW is the sum of the EW of
the emission and absorption components. Each of these equivalent widths
are shown separately in Table 5.6.
