Table 1
Polarisation properties of the 20 pulsars presented in this paper, as measured from LOFAR observations, between 105 and 197 MHz.
| PSR | Duration [min] | RMpub [rad m-2] | RMLOFAR [rad m-2] | RMiono [rad m-2] | L [%] | |V| [%] | L+|V| [%] |
|
|
|||||||
| B0031−07 | 10 | 9.8(2)1 | 10.977(4) | 1.09(7) | 41.1(1) | 9.8(2) | 50.0(3) |
| J0034−0534 | 20 | – | – | 1.10(7) | <15.7(2)* | 12.0(2) | <27.7(3)* |
| B0136+57 | 10 | −90(4)1 | −93.689(6) | 0.44(8) | 47.3(3) | 8.7(5) | 56.0(6) |
| B0809+74 | 10 | −11.7(13)2 | −13.566(1) | 0.43(7) | 18.43(1) | 4.18(3) | 22.61(3) |
| B0823+26 | 10 | 5.9(3)3 | 5.942(3) | 0.56(6) | 25.18(4) | 6.21(7) | 31.4(1) |
| B0834+06 | 10 | 23.6(7)1 | 26.095(1) | 0.77(7) | 25.45(2) | 2.59(4) | 28.05(5) |
| B0950+08 | 10 | −0.66(4)4 | 2.151(1) | 0.67(6) | 73.9(1) | 11.54(5) | 85.4(1) |
| J1012+5307 | 20 | – | 3.38(1) | 0.40(6) | 92(1) | 9(1) | 100(2) |
| J1022+1001 | 20 | −0.6(5)5 | 2.18(2) | 0.79(5) | 82(2) | 14(2) | 96(2) |
| B1133+16 | 10 | 1.1(2)4 | 4.770(1) | 0.80(7) | 33.92(1) | 17.00(4) | 50.93(4) |
| B1237+25 | 10 | – 0.33(6)6 | 0.864(2) | 1.06(6) | 46.3(1) | 7.5(1) | 53.8(2) |
| B1257+12 | 30 | – | 9.24(3) | 1.33(6) | 24.2(4) | 18(1) | 42(1) |
| B1508+55 | 10 | 0.8(7)2 | 2.449(2) | 1.17(6) | 10.21(1) | 6.57(3) | 16.78(4) |
| B1911−04 | 10 | 4.4(9)4 | 6.23(2) | 2.25(5) | 16.1(2) | 7.0(4) | 23.1(5) |
| B1919+21 | 10 | −16.5(5)1 | −16.104(2) | 0.89(5) | 18.74(3) | 6.82(7) | 25.6(1) |
| B1929+10 | 10 | −6.87(2)4 | −5.841(2) | 1.11(4) | 87.0(3) | 22.8(3) | 109.9(4) |
| B1953+50 | 10 | −22(2)1 | −23.07(1) | 0.77(5) | 19.6(2) | 6.0(5) | 25.6(5) |
| B2111+46 | 10 | −224(2)2 | – | 0.53(6) | 1.423(4)** | 5.6(2) | 7.1(2)** |
| B2217+47 | 10 | −35.3(18)2 | −35.407(2) | 0.52(6) | 19.33(2) | 9.17(5) | 28.5(1) |
| B2224+65 | 10 | −21(3)1 | −22.486(8) | 0.50(7) | 48.1(4) | 8.7(8) | 56.7(9) |
Notes. The duration of each observation is shown in Col. 2. The 1σ statistical uncertainties, shown in parentheses, refer to the last significant digit of the tabulated values. Column 3 shows the published value of the RM, from the ATNF pulsar catalogue. Column 4 shows the value of the RM obtained from LOFAR data, using RM Synthesis. The quoted uncertainties are purely statistical and do not incorporate systematics due to e.g. the ionospheric and solar-wind contributions. Column 5 shows the contribution of the ionosphere to the measured RM values from LOFAR, calculated for each observation, from the model of Sotomayor-Beltran et al. (2013). The last three columns show the linear, circular and total polarisation fraction in the average profiles from LOFAR. The quoted uncertainties are purely statistical and do not incorporate a systematic uncertainty of 5–10%, attributable to the calibration model (see Sect. 3.2.2). We note that because of the lack of significant linear polarisation, it was not possible to meaure an RM for PSRs J0034−0534 and B2111+46. The corresponding linear-polarisation fraction for PSR J0034−0534 was calculated assuming the RM = 0 rad m-2, which only yields an upper limit due to significant instrumental polarisation (see Sect. 8.3.1); the linear-polarisation fraction for PSR B2111+46 was calculated assuming the published RM.
Reference.
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