Effective temperature determinations of late-type stars based on 3D non-LTE Balmer line formation

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Table 3

Sensitivity of the effective temperatures inferred from the 1D non-LTE Balmer lines (using MARCS model atmospheres) to changes in the atmospheric parameters log g or with respect to the adopted literature value, or to a change in the placement of the continuum with respect to the best-fitting value.

Star	_eff∕K			_eff∕K			_eff∕K
	Hα	Hβ	Hγ	Hα	Hβ	Hγ	Hα	Hβ	Hγ
Sun	− 47∕42	− 28∕19	− 3∕− 2	9∕− 10	− 46∕38	− 97∕86	− 35∕37	− 12∕24	− 19∕22
Procyon	− 25∕0	23∕− 35	29∕− 41	− 67∕64	− 82∕63	− 87∕65	− 29∕31	− 23∕26	− 14∕18
HD 103095	− 42∕51	− 24∕29	− 17∕27	82∕− 96	6∕− 11	− 35∕36	− 23∕23	− 22∕22	− 56∕57
HD 84937	− 103∕55	28∕− 32	36∕− 38	− 18∕14	− 17∕12	− 16∕12	− 43∕42	− 32∕32	− 15∕20
HD 140283	− 159∕107	25∕− 28	25∕− 26	− 9∕8	− 15∕10	− 16∕11	− 65∕73	− 41∕42	− 18∕24
HD 122563	− 93∕95	− 2∕− 2	26∕− 27	31∕− 28	− 17∕13	− 25∕15	− 73∕80	− 47∕48	− 49∕46

Notes. A positive value indicates that a higher effective temperature is inferred upon performing the stated perturbation.

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