A lack of close binaries among hot horizontal branch stars in globular clusters - M 80 and NGC 5986

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Table 5:

Statistical analysis of RV variations for our target EHB stars.
ID	$\Delta$ (RV) $_{\max}$	$\frac{\Delta({\rm RV})_{\max}}{\sigma}$	$p\left(\frac{\Delta({\rm RV})_{\max}}{\sigma}\right)$	$p\left(\leq\Delta{\rm (RV)}_{\max}\right)$
	(km s^-1)		(%)	(%)
NGC 5986
17 691	12.2	1.51	73.6	11.9
4175	26.9	3.84	0.15	28.3
8131	9.1	1.52	73.6	8.3
11 571	20.4	2.83	4.0	21.2
12 099	14.1	2.39	13.4	14.1
M 80
14 327	8.1	1.40	60.4	11.9
14 985*	12.6	2.74	3.0	19.5
16 389	23.1	5.02	$2.4\times 10^{-6}$	35.1
16 707	11.1	1.63	44.6	35.1
17 737	11.8	1.93	26.7	18.2
19 191	11.2	2.20	14.2	17.2
19 127	18.1	2.35	10.0	28.0
12 304	17.9	2.45	3.5	51.0
12 663	16.5	2.75	1.5	48.3
12 767	4.5	0.96	65.2	17.5
14 022	4.8	0.98	65.2	18.5
12 526	12.0	1.90	14.4	38.6

Source LaTeX | All tables | In the text

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