Table 2
Emission line around 1318 nm.
HD Number | Stellar velocity (km s−1) | Ref. | MJD | EmL, Abs. Wavelength (nm) at |peak| | δλ (nm) | EmL, Abs. norm. flux peak (abs. value) | Hel. RV corr (km s−1) |
---|---|---|---|---|---|---|---|
105056 | +5±6, −9.0±3.1, | (1), (4) | 56411.272 | 1317.56, 1317.95 | 0.39 | 1.020, 0.955 | +2.4 |
" | + 14.5 ±1.8 | (5) | (1317.61, 1318.05) | 0.44 | |||
112272 | −36±2, −38.0±4.4 | (1) | 56440.172 | 1317.46, 1317.89 | 0.43 | 1.025, 0.918 | −6.0 |
" | −37.1±1.8 | (5) | (1317.47, 1318.02) | 0.55 | |||
56732.333 | 1317.38, 1317.79 | 0.41 | 1.025, 0.917 | +14.7 | |||
(1317.39, 1317.92) | 0.53 | ||||||
113904 | +7±5, +4.4±1.5 | (1), (5) | 56459.143 | 1317.56, 1317.97 | 0.41 | 1.010, 0.965 | −10.5 |
" | (1317.58, 1318.07) | 0.49 | |||||
115363 | −70±2, −71.0±4.5 | (1), (4) | 56465.029 | 1317.41, 1317.92 | 0.51 | 1.023, 0.929 | −12.4 |
" | −70.4±1.4 | (5) | (1317.39, 1318.02) | 0.63 | |||
" | 56732.346 | 1317.30, 1317.80 | 0.50 | 1.021, 0.929 | +15.8 | ||
" | (1317.31, 1317.90) | 0.59 | |||||
115842 | −21±2 −3.0±4.3 | (1), (4) | 56465.058 | 1317.61, 1317.95 | 0.34 | 1.020, 0.980 | −15.7 |
" | −21.1±1.7 | (5) | (1317.57, 1318.07) | 0.50 | |||
152235 | −25±1, −35.2±2.3 | (1), (4) | 56467.098 | 1317.43, 1317.91 | 0.48 | 1.015, 0.913 | −7.2 |
" | −35.9±1.8 | (5) | (1317.50, 1318.01) | 0.51 | |||
159455 | 87.5±1.9 | (2) | 56435.263 | 1317.44, 1317.90 | 0.46 | 1.029, 0.880 | +11.5 |
" | (1317.46, 1318.00) | 0.54 | |||||
" | 56764.186 | 1317.33, 1317.78 | 0.45 | 1.032, 0.875 | +25.4 | ||
" | (1317.34, 1317.93) | 0.59 | |||||
160065 | 59.9±6.4, 10.4±2.7 | (2), (6) | 56434.396 | 1317.33, 1317.83 | 0.50 | 1.022, 0.873 | +12.0 |
" | (1317.32, 1317.94) | 0.62 | |||||
" | 56746.394 | 1317.27, 1317.75 | 0.48 | 1.022, 0.870 | +29.7 | ||
" | (1317.22, 1317.68) | 0.46 | |||||
169754 | 32.0±7.4 | (3) | 56497.240 | 1317.34, 1317.91 | 0.57 | 1.025, 0.904 | −12.4 |
" | (1317.37, 1318.04) | 0.67 |
Notes. Stellar velocities, velocity of the peak of the emission line and velocity at peak of absorption line towards stars where the 1318 nm showed strong emission. The standard of rest is heliocentric. Values in brackets are flux weighted wavelengths determined using fitting as shown in Fig. 7.
References. (1) POP, UVES pop survey (Bagnulo et al. 2003); (2) Gaia DR2; (3) Kharchenko et al. (2007); (4) Gontcharov (2006); (5) This paper with the stellar velocity measured using He I at λ = 4387 Å; (6) Gaia DR3 (Gaia Collaboration 2023). There is a large (50 km s−1) difference in the Gaia DR2 and DR3 velocities for the one star (HD 160065) for which data are available for both releases.
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