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Home All issues Volume 517 (July 2010) A&A, 517 (2010) A67 Full HTML
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Table 4:

Equivalent widths of H$\alpha $, He I, Ca II, and forbidden emission lines observed in the spectra.
Star H$\alpha $ P(17) He I [O I] [S II] [N II] Ca II
  (6563 Å) (8467 Å) (6548 Å) (6301 Å, 6365 Å, 8446 Å) (6716 Å, 6731 Å) (6549 Å, 6585 Å) (8498 Å, 8662 Å)
Confirmed Herbig Ae/Be and T Tauri stars
Hen 3-1121S EIA $^{\rm +2.8}_{-0.1}$ (0.1) +0.8 -0.02 (0.01) (0.05) (0.01) (0.01) +0.01 (0.01) (0.01) (0.0)
Hen 3-1121N EIA $^{\rm +2.0}_{-0.4}$ (0.1) +0.8 -0.03 (0.02) (0.08) (0.01) (0.01) -0.04 -0.13 (0.1) (0.0)
MWC 878 -54 -2.0 -3.5 -0.12 (0.01) -8.3 (0.01) (0.01) -0.5 -1.6 -7.1 -8.1
WRAY 15-1435 -20 -1.7 +0.6 -0.02 (0.02) -4.1 -0.01 (0.01) (0.01) (0.02) -0.3 -0.5
MWC 953 -32 -3.5 +0.3 -0.01 (0.02) -2.2 (0.01) (0.01) +0.03 +0.1 -0.4 -0.7
HD 313571 -34 -2.1 -0.3 -0.01 (0.02) -4.8 (0.02) (0.01) +0.01 (0.01) -1.3 -0.1
Hen 3-823 -25 -1.4 +0.6 (0.01) (0.03) -1.4 (0.01) (0.01) (0.01) (0.01) (0.1) (0.1)
MWC 593 -35 -1.3 -0.2 -0.01 (0.03) -3.7 (0.01) (0.01) (0.01) (0.02) -0.6 (0.1)
Hen 2-80 -150 -1.8 +0.6 -9.9 -3.4 -16 -0.1 -0.2 -0.06 -0.2 -0.2 -0.2
WRAY 15-1372 -15 (0.2) (0.02) (0.1) (0.1) (0.6) (0.01) (0.03) (0.01) (0.1) (0.3) (0.6)
Th 17-35 -90 (0.6) +0.2 -0.3 -0.4 -5.3 -0.1 -0.1 -0.07 -0.2 -0.1 -0.2
HD 145718 PC $^{\rm +2.4}_{-0.2}$ (0.6) (0.1) (0.2) (0.1) +0.5 (0.01) (0.01) (0.3) (0.0) +0.6 +1.4
CD-38 4380 EIA $^{\rm +1.0}_{-3.0}$ (0.6) (0.03) (0.1) (0.2) +0.5 (0.1) (0.02) (0.01) (0.3) +0.7 +1.4
Hen 3-1145 -30 (0.1) -0.5 -0.5 (0.3) (0.02) +0.2 (0.04) (0.02) (0.05) -0.5 -0.5
Giant stars with emission lines that may be Herbig Ae/Be stars  
HD 152291 -3.4 -0.8 +0.2 (0.01) (0.02) (0.05) (0.01) (0.01) (0.01) (0.01) -0.5 (0.1)
Hen 3-416 PC $^{\rm +0.5}_{-27}$ (1.0) +0.2 -0.4 -0.2 (0.0) (0.1) (0.02) (0.01) (1) -5.3 -9
WRAY 15-488 PC $^{\rm +7.2}_{-0.8}$ +1.0 (0.06) (0.1) (0.1) +0.6 +0.1 (0.1) (0.01) (0.3) +1.2 +2.0
Giants and Supergiants with emission lines
HD 323154 -26 -0.9 -2.0 (0.01) (0.01) (0.02) (0.05) (0.01) (0.01) -0.07 -0.8 -0.9
WRAY 15-1104 PC $^{\rm +0.2}_{-10}$ +0.5 PC $^{\rm +0.4}_{-0.4}$ (0.2) -0.02 -0.7 (0.01) (0.01) (0.01) (0.3) (0.5) (0.5)
Hen 3-1428 -18 PC $^{\rm +0.25}_{-0.04}$ -1.4 -0.8 -0.3 -4.0 (0.02) -0.05 -0.15 PC $^{\rm +0.2}_{-0.9}$ (0.1) (0.1)
MWC 314 -118 -2.4 -6.1 -0.01 (0.01) -4.7 -0.06 (0.03) -0.04 -0.17 -13 -19
HD 320156 -7.8 -0.7 0.3 (0.02) (0.03) PC $^{\rm +0.2}_{-0.05}$ (0.02) (0.02) +0.1 PC -0.15+0.03 -8 -14
Hen 3-1347 PC $^{\rm +0.8}_{-12}$ +0.1 0.2 -0.3 -0.1 -0.7 (0.05) (0.04) (0.01) +0.2 +0.5 EIA $^{\rm +0.7}_{-0.2}$

AS 231

 PC $^{\rm +1.4}_{-14}$ +0.7 0.2 (0.01) (0.02) +0.8 +0.01 +0.03 (0.03) (0.01) +1.3 +2.0
Unclassified stars with strong emission line spectrum
WRAY 15-1651 -92 -1.2 (0.6) -0.90 -0.1 -7.4 -0.1 -0.12 (0.06) (0.02) -1.5 -1.7
MWC 930 PC $^{\rm +0.1}_{-42}$ PC $^{\rm +0.7}_{-1.0}$ +0.2 -0.02 (0.01) PC $^{\rm +1.5}_{-1.5}$ PC $^{\rm +0.2}_{-0.1}$ (0.04) -0.04 (0.01) PC $^{\rm +1.7}_{-5.1}$ PC $^{\rm +2.0}_{-6.6}$
Dwarf stars without H$\alpha $ in emission
AS 321 +5.7 (0.1) (0.03) -0.02 (0.01) +0.6 (0.01) (0.01) (0.01) (0.01) +0.8 +1.8
Giant and Supergiant stars without H$\alpha $ in emission
WRAY 15-522 +1.2 +0.2 (0.03) -0.2 (0.1) (0.1) +0.1 (0.2) (0.01) (0.1) +1.3 +2.1
Th 35-41 +1.2 +1.4 -0.15 (0.1) (0.1) (0.2) (0.5) (0.4) (0.01) (0.2) +2.2 +2.7
WRAY 15-566 +0.4 (0.06) -0.15 (0.3) (0.1) (0.1) (0.6) (0.1) (0.1) (0.2) +0.6 +0.6
WRAY 15-1650 +1.0 +0.6 (0.01) (0.2) (0.1) (0.2) (0.5) (0.2) (0.1) (0.3) +1.3 +2.1
WRAY 15-1702 +0.8 +0.8 (0.02) (0.1) (0.1) (0.3) (0.5) (0.5) (0.1) (0.3) +1.1 +2.0
WRAY 15-770 +0.5 (0.05) (0.04) (0.2) (0.1) (0.1) (1.0) (1.0) (0.1) (0.1) EIA $^{\rm +0.4}_{-0.1}$ PC -0.3+0.4
HD 305773 +2.0 (0.07) +0.7 (0.05) (0.01) (0.05) (0.01) (0.02) (0.01) (0.05) (0.1) (0.1)

Notes. In the cases where emission lines are observed inside a broad absorption line, we give the EW of the absorption and emission component and write EIA meaning ``Emission Inside Absorption''. In the case of P Cygni and inverse P Cygni profiles are noted by PC and the equivalent width (EW) of the absorption and emission component are given. For the stars displaying Paschen emission, the Ca II lines at 8498 and 8662 Å are blended with the Paschen(16) and Paschen(13) respectively. For these sources the EW of Ca II line at 8498 and 8662 Å, is the EW measured at the position of the Ca II line minus the EW of the Paschen(17) and Paschen(14) lines respectively. Upper limits are displayed in parenthesis.


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