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Table 1:

Polarization data for four groups of peculiar O-type stars observed during the AAT and WHT runs described in the body text.
Name Spec.Tp Date $P_{\rm cont}^{\rm R}$ (%) $\theta_{\rm cont}^{\rm R}$ ($^{\rm o}$) $P^{\rm lit}$ (%) $\theta^{\rm lit}$ $P^{\rm IS}$ (%) $\theta^{\rm IS}$ ISP map
(I)   OVz and weak wind dwarfs
$\Theta ^1$ Ori C O7 Vp 31-12-95 $0.31 \pm 0.01$ $139.9 \pm 0.3$          
    01-01-96 $0.29 \pm 0.01$ $148.2 \pm 0.8$          
    31-12-96 $0.29 \pm 0.01$ $144.0 \pm 0.6$          
    14-02-03 $0.284 \pm 0.005$ $136.3 \pm 0.5$ 0.35 151.8 0.240 88.5 No
$\Theta^2$ Ori A O9.5 Vpe 14-02-03 $1.051 \pm 0.005$ $99.7 \pm 0.1$ 0.702 93.1 0.221 88.5 No
HD 42088 O6.5 V 14-02-03 $2.431 \pm 0.008$ $177.0 \pm 0.1$ 2.53 178 2.126 168.8 OK
HD 54662 O6.5 V 14-02-03 $0.881 \pm 0.098$ $145.5 \pm 3.8$ 0.83 145 0.481 154.4 No
HD 93128 O3.5 V((f+)) 12-02-03 $2.265 \pm 0.014$ $89.0 \pm 0.2$          
HD 93129B O3.5 V((f+)) 12-02-03 $1.889 \pm 0.063$ $117.5 \pm 1.0$          
HD 152590 O7.5 V 14-02-03 $0.998 \pm 0.009$ $29.1 \pm 0.3$ 0.96 19.2 0.737 27.9 No
CPD-58$^{\rm o}$2611 O6 V((f)) 13-02-03 $2.222 \pm 0.010$ $84.7 \pm 0.1$          
CPD-58$^{\rm o}$2620 O6.5 V((f)) 14-02-03 $1.717 \pm 0.009$ $90.6 \pm 0.1$          
(II)   Of?p
HD 148937 O6.5 f?p 12-02-03 $1.580 \pm 0.020$ $46.9 \pm 0.4$ 1.63 50.6 1.727 36.1 OK
    15-08-03 $1.803 \pm 0.014$ $49.3 \pm 0.2$          
(III)   Oe stars
HD 45314 O9:pe 14-02-03 $1.316 \pm 0.091$ $167.4 \pm 2.0$ 1.38 171 1.369 171.6 OK
HD 46485 O7 Vn(e) WHT 03 $1.887 \pm 0.013$ $26.1 \pm 0.2$ 1.89 159.0 0.808 165.8 OK
HD 60848 O8 V:pev WHT 03 $0.431 \pm 0.007$ $35.7 \pm 0.4$ 0.78 56 0.372 27.0 No
HD 120678 O8 III:nep 13-02-03 $1.637 \pm 0.015$ $77.8 \pm 0.3$ 1.7 76 1.781 71.7 OK
Zeta Oph O9.5 Vnn 14-02-03 $1.572 \pm 0.004$ $127.3 \pm 0.1$ 1.42 127 0.411 76.4 No
HD 155806 O7.5 V[n]e 14-08-03 $0.821 \pm 0.013$ $156.4 \pm 0.5$ 0.86 147 0.742 159.0 OK
(IV)   Onfp
HD 152248 O7 Ib:(n)(f)p 15-08-03 $0.477 \pm 0.016$ $114.9 \pm 1.0$ 0.66 112 0.812 27.9 OK
The spectral types are taken from the O-star catalogue of Maiz-Apellaniz et al. (2004) and listed in Col. 2, with the dates of the observations provided in the third column. The errors in the polarization data (Col. 4) are of the order of 0.01% based on photon-statistics only. Yet, systematic (external) errors in the polarization are estimated to be 0.1%. The errors in the PA $\theta $ (Col. 5) are of order a degree. The literature values of the polarization and PA are taken from the catalogue of Mathewson et al. (1978) and so are the values for the ISP (Cols. 8 and 9). The last Col. 10 indicates whether an ISP map is well ordered and well populated (see body text in Sect. 3 for more detailed explanation).

Source LaTeX | All tables | In the text

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