The spectroscopic binary fraction of the young stellar cluster M17

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Volume 690 (October 2024)

A&A, 690 (2024) A178

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Table B.1

Spectral lines used per star to measure the RV.

	B1ll	B150	B164	B181	B205	B213	B215	B230	B234	B243	B253	B268	B269	B272	B275	B289	B290	B293	B311	B331	B336	B337	B86	B93	CEN55
CII 4267.26																			X					X
MgII 4481.13					X												X		X				X
SiII 4128.0																							X
SiIII 4552.62																			X
OII 4661.6332																			X
Ba-12 3750.151																	X							X
Ba-11 3770.633																	X							X
Ba-10 3797.909					X																			X
Ba-9 3835.397					X				X
Hη 3889.064									X
Hϵ 3970.075				X						X								X
Hδ 4101.734					X	X			X	X
Hγ 4340.472				X	X	X			X	X		X												X
Hβ 4861.35				X	X	X						X
Hα 6562.79				X
Pa-11 8862.89				X	X	X		X	X	X		X	X	X						X		X
Pa-10 9015.3												X		X				X
Pa-9 9229.7				X	X	X			X			X										X
Pa-7 10049.8				X	X	X		X	X	X			X	X				X				X
HeI 3819.6074																					X			X
HeI 3888.648	X	X				X			X		X						X
HeI+II 4026.1914	X	X			X				X															X
HeI 4387.9296		X		X	X						X													X	X
HeI 4471.4802	X		X		X	X			X		X			X										X	X
HeI 4921.9313		X		X	X				X		X													X	X
HeI 5015.6783			X	X	X									X
HeI 5875.621	X		X	X	X	X	X				X				X	X									X
HeI 6678.151			X	X	X	X	X	X	X		X				X	X								X
HeI 7065.19			X	X	X		X									X									X
HeII 4199.6	X
HeII 4541.0																	X
HeII 4685.7	X		X

Notes. The central wavelength shown in this table is the exact central value used to calculate the RV.

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