Table 2.
Absorption lines and blends identified by the modified versions of the MKCLASS code.
(1) | (2) | (3) |
---|---|---|
Blend/Line | Wavelength (Å) | SpT_range |
(Si II/Cr II/Sr II) | 4076/77 | B7−F5 |
(Si II/Eu II) | 4128/30 | B3−F2 |
Si II | 3856 | B3−F2 |
Si II | 4200 | B3−A2 |
Si II | 5041 | B3−F2 |
Si II | 5056 | B3−F2 |
Si II | 6347 | B3−F2 |
Si II | 6371 | B3−F2 |
Cr II | 3866 | B7−F2 |
Cr II | 4172 | B7−F2 |
Sr II | 4216 | B7−F2 |
Eu II | 4205 | B7−F2 |
He I | 4009 | B0−A0 |
He I | 4026 | B0−A0 |
He I | 4144 | B0−A0 |
He I | 4387 | B0−A0 |
Hg II | 3984 | O6–A3 |
Mn II | 4136 | O6–A3 |
Mn II | 4206 | O6–A3 |
Mn II | 4252/9(a) | O6–A3 |
Notes. Normal font denotes features identified by the MKCLASS_mCP code (Hümmerich et al. 2020), bold font the additional lines used for the identification of CP3 stars by the MKCLASS_HgMn code. The columns denote: (1) Blend/Line. (2) Wavelength (Å). (3) Spectral range in which the corresponding feature was probed. At the resolution of the LAMOST low-resolution spectra, all features listed in Table 2 are, to some extent, blended with other absorption lines. Nevertheless, the specified elements generally constitute the main contributors to these blends in the investigated groups of CP stars.
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