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Table 5.

The results from the spectral analysis and parameters derived from the timing model in Table 2.

PSR S129 S166 S334 S1484 S1532 α Offset τc B Ė
(mJy) (mJy) (mJy) (mJy) (mJy) (arcmin) (yr) (G) (erg s−1)
J0039+3546 7(3) 3.3(1.7) 0.34(12) < 1.4 0.14(3) −1.5(3) 1.12 1.3 × 108 1.9 × 1011 1.6 × 1031
J0059+6956 1.9(1.0) 1.3(6) < 2.5 −2(3) 1.61 × 10−3 1.3 × 108 4.1 × 1011 3.7 × 1030
J0139+5621 3.8(1.9) 2.3(1.1) 1.8(5) 0.17(3) −1.2(2) 7.7 × 10−1 3.6 × 105 1.2 × 1013 5.6 × 1032
J0305+1123 3.9(2.0) 2.0(1.0) < 0.06 < 0.006 −4.8(1.8) 5.7 × 10−1 4.5 × 107 5.2 × 1011 1.9 × 1031
J0317+1328 2.0(1.0) 1.1(5) 0.9(3) < 2.7 < 0.21 1.84 1.8 × 108 5.9 × 1011 8.7 × 1029
J0613+3731 24(12) 12(6) 1.9(5) 1.4(3) −1.0(2) 4.3 × 10−2 3.0 × 106 1.4 × 1012 5.4 × 1032
J0811+3729 6(3) 2.4(1.2) < 0.86 0.41(15) < 0.13 −4.4(1.9) 1.16 2.7 × 107 9.8 × 1011 1.5 × 1031
J0813+2202 2.9(1.5) 1.2(6) < 2.1 < 0.3 −4(2) 2.2 × 10−1 1.1 × 108 2.1 × 1011 2.0 × 1031
J0828+5304 3.1(1.5) 1.7(8) < 1.4 < 0.099 −4.0(1.9) 2.4 × 10−4 8.3 × 109 6.0 × 108 4.1 × 1032
J0928+3039 8(4) 3.4(1.7) < 1.1 < 1.6 < 0.15 −4.3(1.9) 8.5 × 10−1 4.6 × 107 6.2 × 1011 1.3 × 1031
J0935+3312 4(2) 1.8(9) < 0.77 < 2.2 < 0.22 −4.2(2.0) 1.01 4.0 × 107 6.1 × 1011 1.7 × 1031
J1303+3815 2.8(1.4) 1.5(7) < 0.12 −3.9(1.9) 1.25 1.8 × 107 3.8 × 1011 2.2 × 1032
J1334+1005 2.0(1.0) 0.9(5) 0.21(5) −0.9(6) 5.8 × 10−1 1.9 × 107 8.3 × 1011 3.9 × 1031
J1427+5211 3.0(1.5) 1.2(6) 0.24(6) 0.10(2) −1.1(3) 4.8 × 10−3 3.3 × 107 7.0 × 1011 1.9 × 1031
J1529+4050 13(6) 10(5) 1.7(5) 0.62(16) 0.56(11) −1.3(2) 1.29 2.8 × 109 3.6 × 1010 9.7 × 1029
J1707+3556 8(4) 5(2) < 2.7 −2(3) 5.3 × 10−1 3.0 × 109 1.2 × 1010 8.3 × 1030
J1715+4603 1.2(6) 0.7(4) < 0.069 < 1.6 0.0010(2) −2.9(3) 9.7 × 10−1 1.8 × 108 1.6 × 1011 1.2 × 1031
J1722+3519 21(11) 11(5) 1.4(5) 0.7(2) < 1.5 −4(2) 5.5 × 10−1 2.4 × 107 6.8 × 1011 3.9 × 1031
J1740+2715 5(2) 3.4(1.7) 1.2(4) 0.8(2) 0.41(9) −0.99(20) 1.57 7.8 × 107 4.8 × 1011 7.1 × 1030
J1745+4254 2.2(1.1) 1.6(8) 0.8(3) 0.23(7) 0.24(5) −0.9(2) 1.5 4.9 × 108 5.5 × 1010 1.4 × 1031
J1809+1705 1.5(7) 1.2(6) < 3.3 0.59(17) < 0.081 −3.5(1.9) 1.74 1.1 × 107 2.6 × 1012 1.4 × 1031
J1814+2224 1.1(5) 1.3(7) 0.8(3) 0.28(10) 0.20(4) 2.4 1.1 × 107 3.0 × 1011 8.6 × 1032
J1910+5655 10(5) 5(2) < 3.7 < 0.14 −4.3(1.8) 1.22 2.6 × 107 2.7 × 1011 2.0 × 1032
J1953+3014 5(3) 2.2(1.1) 0.37(13) 0.16(3) −1.3(3) 1.92 × 10−3 5.2 × 107 7.1 × 1011 7.4 × 1030
J1958+2214 0.6(3) 0.8(4) 1.63 × 101 3.6 × 106 2.2 × 1012 1.6 × 1032
J1958+5650 1.1(6) 0.6(3) 0.063(13) −1.1(2) 3.0 × 10−3 2.9 × 107 2.3 × 1011 2.2 × 1032
J2006+2205 3.7(1.9) 3.0(1.5) < 2.3 0.19(7) < 0.12 2.0 4.8 × 106 3.2 × 1012 4.3 × 1031
J2022+2112 5(2) 2.7(1.4) < 2.8 < 0.009 −4.6(1.7) 8.8 × 10−1 1.4 × 107 8.6 × 1011 6.9 × 1031
J2053+1718 4(2) 2.5(1.3) < 1.4 < 0.015 −4.4(1.7) 7.4 × 10−1 6.3 × 109 6.1 × 109 7.0 × 1030
J2057+2128 1.6(8) 0.8(4) < 3.0 2.3 3.5 × 107 7.9 × 1011 1.3 × 1031
J2123+3624 6(3) 4(2) < 1.4 < 1.6 −3(2) 8.2 × 10−3 9.8 × 106 1.7 × 1012 3.8 × 1031
J2209+2117 5(3) 3.7(1.9) 0.18(5) 0.29(6) −1.17(19) 6.8 × 10−1 5.5 × 106 3.0 × 1012 3.6 × 1031
J2306+3124 6(3) 3.3(1.7) 0.18(7) 0.18(4) 2.0 2.4 × 107 2.8 × 1011 2.2 × 1032
J2336−0151 9(5) 2.8(1.4) 1.2(4) < 1.4 < 0.44 −5(2) 1.54 4.7 × 107 6.0 × 1011 1.2 × 1031
J2350+3140 5(3) 1.9(1.0) < 1.2 < 1.2 < 0.2 −4.2(2.0) 1.01 2.3 × 107 4.3 × 1011 1.1 × 1032

Notes. Mean flux densities and upper limits on the mean flux densities Sν are shown with observing frequencies in MHz indicated in subscript. The inferred spectral indices α were fitted with a single power law of the form Sν ∝ να. Flux densities for which less than five observations were available are indicated in italics and were not used in the spectral fit. The offset in arcminutes refers to the difference between the centre of the telescope beam and the position reported in Table 2. For six pulsars, the spectral index was not calculated due to the large position offset. We determined the characteristic age τc, the surface magnetic field strength B, and the intrinsic spin-down energy Ė assuming a canonical neutron star with a radius of 10 km and a moment of inertia of 1045 g cm2. Furthermore, we assumed that the initial spin is negligible and that the spin-down is due to magnetic dipole radiation throughout the pulsar’s lifetime. See Lorimer & Kramer (2012) for further details.

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