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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.

(a)

Although these lines are partly resolved in low- resolution LAMOST spectra, we chose to probe the blend of the region from 4248 to 4262 Å.

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