Exploring the origin of magnetic fields in massive stars - II. New magnetic field measurements in cluster and field stars

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Table 2

Longitudinal magnetic fields measured with FORS 2 in the studied sample.

Name	MJD	S/N	⟨B_z⟩_all	⟨B_z⟩_hydr	Spectral	Phase	Comment
			[G]	[G]	Regions (Å)

CPD−28 2561	^∗55 338.969	2262	−381 ± 122	−534 ± 167	3580–4588		PD
	55 685.982	2481	99 ± 82	65 ± 108
	55 686.984	2516	−44 ± 80	6 ± 102
	55 687.980	2490	269 ± 81	281 ± 90			CD
CPD−47 2963	^∗55 337.094	2722	−190 ± 62	−154 ± 96	3696–5622		PD
	55 686.019	2691	−66 ± 57	−119 ± 82
	55 687.037	3035	−169 ± 52	−77 ± 76			CD
	55 688.013	2164	95 ± 69	148 ± 101
Vela X-1	55 686.096	3604	−15 ± 30	−11 ± 45	3562–5886
	55 687.058	2894	−80 ± 32	−114 ± 50
	55 688.048	2433	57 ± 37	88 ± 69
HD 92206c	55 686.135	2393	204 ± 46	140 ± 88	3658–5944		ND
	55 687.085	3439	−104 ± 30	−123 ± 54
	55 688.151	2528	10 ± 43	23 ± 46
HD 303225	55 688.220	1902	−59 ± 54	−81 ± 90	3447–5299
HD 93026	55 687.247	1647	−19 ± 75	−52 ± 100	3470–4900
HD 93521	55 686.042	3891	32 ± 52	45 ± 73	3689–5414
	55 687.015	3304	−202 ± 66	−293 ± 91			ND
	55 688.063	3059	−74 ± 62	−64 ± 68
HD 93632	55 687.217	2927	−152 ± 50	−120 ± 62	3318–4593		ND
	55 688.198	2443	−10 ± 32	5 ± 68
CPD−58 2611	55 687.151	2631	−58 ± 44	−80 ± 59	3580–4588
	55 688.125	2005	−25 ± 56	−9 ± 74
HD 93843	^∗55 339.099	3504	−157 ± 42	−173 ± 56	3370–5545		PD
	55 686.115	3230	−34 ± 38	−12 ± 52
	55 687.185	3385	−132 ± 39	−93 ± 56			CD
	55 688.180	2647	−63 ± 47	−130 ± 61
HD 130298	^∗55 339.159	3037	113 ± 38	193 ± 62	3573–5284		PD
	55 686.347	2264	−64 ± 66	−64 ± 85
	55 688.261	2699	59 ± 55	122 ± 72
HD 148937	^∗54 550.416	2616	−276 ± 88	−145 ± 104	3210–3599	0.631	PD
	^∗55 337.285	3364	−204 ± 71	−225 ± 103		0.529
	^∗55 339.206	2253	−290 ± 85	−389 ± 129		0.802	PD
	55 686.370	2664	−110 ± 90	−165 ± 115		0.172	CD
	55 687.265	3083	−87 ± 74	−137 ± 95		0.299	CD
	55 688.285	2941	−139 ± 33	−174 ± 121		0.444	CD
	55 689.361	2522	−241 ± 91	−229 ± 118		0.597	CD

Notes. Entries related to previous measurements are indicated by an asterisk in the second column of the Table. The wavelength region used for the magnetic field measurements is indicated in the sixth column. The seventh column provides the rotation phases for the Of?p star HD 148937, which has a known rotation period of about seven days (Nazé et al. 2010). In the last column ND stands for new detections, PD for previous detections (Hubrig et al. 2008; 2011b), and CD for confirmed detections. All quoted errors are 1σ uncertainties.

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