Table B.1
Rest wavelengths (λ0) used to computed the RVs.
| Line | λ0 (Å) | Reference |
|
|
||
| He i+iiλ4026 | 4026.072a | CLL77 |
| He iiλ4200 | 4199.832 | PvH/NIST |
| He iλ4387 | 4387.929 | PvH |
| He iλ4471 | 4471.480 | NIST |
| He iiλ4541 | 4541.591 | PvH/NIST |
| He iiλ4686 | 4685.710 | PvH |
| He iλ4713 | 4713.146 | NIST |
| He iλ4922 | 4921.931 | PvH/NIST |
Notes.
Because of the strong blend between He iλ4026.1914 and He iiλ4025.602, the effective rest wavelength is function of the temperature, thus the spectral type. We use here an observed value which is representative of mid- to late- O-type stars.
References. CLL77: Conti et al. (1977); NIST atomic spectra data base: http://www.nist.gov/pml/data/asd.cfm; PvH : Peter van Hoof atomic line list (http://www.pa.uky.edu/~peter/atomic/).
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