4. Results

An elaborate procedure was developed to ensure high quality pulsar polarimetry at wide bandwidths. This scheme has served reasonably well for detecting instrumental errors on-line and for monitoring of the polarization characteristics of our instrumental set-up for a period of 2 years at the Effelsberg radio telescope. This procedure was applied to 64 polarization profiles of 28 pulsars at cm-wavelengths. The calibrated polarization profiles are shown in Figs. 5-24 at the end of this section. Whenever possible, a fit of the Rotating-Vector-Model (RVM; e.g. Manchester & Taylor 1977) to the PPA curve of each source was made which enabled a determination of the viewing geometry of each system. The viewing geometry of each system is presented in Table 3 (click here) while the fits are superimposed on the polarization plots of Figs. 5-24. The magnetic inclination angle and the the impact parameter (the closest approach of the magnetic axis to the line-of-sight trajectory) are listed in Cols. 3 and 4 of Table 3 (click here) respectively, together with their estimated errors. The values of have a certain ambiguity, because the parameters and are highly correlated. This accounts for the large errors associated with these parameters. Thus, it is doubtful whether always represents the "true'' value of the magnetic inclination. However, the BCW method that we have used to determine emission heights at cm-wavelengths is insensitive to the magnetic inclination. Therefore, our results for the emission altitudes are not effected by this ambiguity. The derived heights are presented in the last column of Table 3 (click here). A detailed description of the fitting procedure and its associated complications as well as a discussion of our findings is presented in von Hoensbroech & Xilouris (1997).

In Table 3 (click here), quantitative polarization parameters are summarized. The cut-level given in Col. 3 represents the height above the noise (relative to the peak of the respective outer component) where the outer edges of a profile were found. The resulting width of the profile is then listed in the next column. The linear and circular intensities are the relative polarized power integrated over this width. Low polarization levels which become progressively less with frequency are found for most of our sources. Additionally, the flux density was determined and listed in Table 3 (click here), together with the integration time of the particular observation.

  

PSR B Freq.

[GHz] [km]

0136+57 4.85 96.0 15.0 -3.6 15.0 530 74

0301+19 4.85 94.3 15.0 -13.9 15.0 1416 888

0329+54 10.45 94.0 15.0 -12.4 15.0 -23 192

0355+54 1.71 53.1 80.0 -8.6 4.0 303 76

4.85 155.8 80.0 -2.7 4.0 214 120

10.45 111.9 80.0 -10.2 6.0 128 211

0525+21 1.41 135.8 60.0 1.3 .2 224 31

1.71 66.3 80.0 2.0 1.0 736 467

4.85 17.8 70.0 0.6 2.0 378 174

0535+28 1.41 108.5 30.0 -11.5 6.0 619 96

4.85 79.5 15.0 -18.5 15.0 240 267

0540+23 1.41 162.5 80.0 -3.5 6.0 612 81

4.85 80.3 20.0 10.0 10.0 730 155

10.45 101.1 90.0 -8.3 6.0 297 167

0740-28 1.41 96.2 20.0 -16.0 15.0 210 29

4.85 78.2 15.0 14.8 15.0 268 38

10.45 47.3 90.0 -6.9 5.0 225 218

0809+74 1.71 93.4 10.0 -9.8 15.0 1267 438

4.85 174.3 90.0 -0.7 7.5 447 725

0823+26 1.41 89.8 25.0 1.0 0.2 37 53

1.71 82.3 80.0 1.7 1.5 107 67

4.85 97.5 15.0 -12.1 15.0 80 21

0919+06 1.71 90.4 80.0 2.9 2.0 314 87

4.85 48.0 80.0 2.9 2.5 247 68

0950+08 1.41 -0.7 15.0 1.0 15.0 432 249

4.85 -26.9 90.0 4.1 5.0 159 348

1133+16 1.41 26.9 90.0 2.8 4.4 452 102

1.71 103.6 80.0 4.1 2.5 505 146

4.85 33.0 80.0 3.1 4.0 426 165

1915+13 4.85 90.7 12.5 -9.3 15.0 346 75

1946+35 4.85 52.9 80.0 4.2 3.0 133 168

2016+28 4.85 89.8 15.0 4.2 15.0 159 181

2021+51 1.41 22.5 90.0 1.2 2.5 787 42

1.71 21.0 80.0 3.1 5.0 450 91

4.85 22.4 90.0 4.0 5.0 389 137

10.45 87.9 80.0 5.8 3.0 590 182

2045-16 4.85 89.5 15.0 -1.5 15.0 443 232

2154+40 4.85 101.1 15.0 -16.0 15.0 904 470

2319+40 1.41 102.3 80.0 -8.1 4.0 -418 223

4.85 89.9 15.0 -6.5 15.0 -1242 540

2351+61 1.41 61.2 80.0 -2.9 2.0 379 241

   

Pulsar Freq. Cut-level Width Linear Circular Time Flux

[GHz] [%] [%] [%] [min] [mJy]

PSR B0136+57 4.85 10 12.5 2.6 54.0 1.0 12.1 1.5 20 0.17

PSR B0301+19 4.85 10 14.0 1.6 10.3 3.0 5.5 5.0 45 3.09

PSR B0329+54 1.41 2 30.7 1.1 24.1 0.1 36.3 0.1 10 90.9

1.71 7 28.8 1.2 21.0 0.0 9.3 0.0 10 39.4

4.85 7.6 27.4 0.9 12.3 0.2 7.4 0.2 10 20.5

10.45 33 22.2 1.7 12.9 2.3 7.3 3.3 15 1.75

PSR B0355+54 1.71 10 35.2 4.8 53.9 2.1 4.7 0.4 1 33.4

4.85 5 33.5 6.0 69.3 1.3 8.2 1.0 10 3.36

10.45 5 31.4 21.7 41.9 5.5 0.9 5.7 15 3.37

PSR B0450+55 1.41 5 33.5 3.0 35.2 0.9 11.0 1.4 5 21.9

4.85 10 29.3 6.1 44.8 1.5 6.0 1.6 15 1.78

PSR B0525+21 1.41 1 21.1 0.3 40.4 0.2 3.9 0.3 3 85.7

1.71 10 17.9 0.7 30.9 1.5 3.4 1.1 10 8.8

4.85 3 17.2 0.4 20.6 0.6 1.0 0.9 90 0.10

PSR B0535+28 1.41 15.9 29.7 4.5 82.9 1.7 1.0 0.9 13 3.1

4.85 16.9 31.9 11.3 51.1 2.8 1.0 0.9 15 0.94

PSR B0540+23 1.41 3 33.7 4.9 46.9 0.9 3.8 0.4 3 22.2

4.85 7 28.4 4.9 29.7 1.2 13.4 1.3 20 2.19

10.45 10 22.5 4.2 6.2 7.1 3.6 7.6 35 1.16

PSR B0740-28 1.41 4 19.6 2.1 77.0 0.5 10.7 0.5 5 20.7

4.85 7 20.3 2.0 63.4 1.7 8.5 1.9 60 2.47

10.45 10 14.2 8.8 39.9 12.2 4.3 12.9 30 0.65

PSR B0809+74 1.71 8 29.0 3.4 23.4 2.5 9.1 2.6 8 10.7

4.85 10 26.7 3.6 14.1 1.0 3.1 1.6 15 2.54

PSR B0823+26 1.41 5 9.3 1.1 20.0 3.1 3.4 2.7 3 12.8

1.71 5 8.0 1.4 22.8 5.9 2.8 6.9 10 4.1

4.85 1 13.8 1.6 17.3 0.9 0.7 1.4 30 2.63

PSR B0919+06 1.71 8 10.5 2.0 38.5 10.6 27.5 13.5 5 3.2

4.85 7 7.9 1.4 47.3 2.6 4.6 3.0 45 0.63

PSR B0950+08 1.41 1 72.4 4.7 14.8 0.1 3.7 0.1 5 80.4

4.85 4 45.3 8.6 8 0.8 0.3 1.3 10 41.3

10.45 15 23.8 11.9 5.3 6.4 3.2 9.2 50 8.61

PSR B1133+16 1.41 8 10.9 0.6 15.8 0.4 1.8 0.7 5 19.5

1.71 4 11.6 0.3 12.1 0.2 5.4 0.3 10 24.5

4.85 8 9.4 0.5 10.4 0.3 2.4 0.4 20 4.38

10.45 8 9.8 6.9 7.8 23.9 10.4 31.2 20 0.45

   

Pulsar Freq. Cut-level Width Linear Circular Time Flux

[GHz] [%] [%] [%] [min] [mJy]

PSR B1237+25 1.41 2 15.4 0.5 51.0 0.2 16.0 0.2 8 28.3

4.85 5 13.6 1.4 13.5 1.7 5.2 2.1 20 0.79

PSR B1642-03 1.41 1.6 17.9 3.1 11.2 1.9 9.2 2.4 3 15.2

4.85 10 18.6 3.3 8.6 3.5 1.2 3.5 25 1.10

PSR B1822-09 1.41 18 22.8 2.2 32.9 1.1 11.6 1.2 5 6.3

4.85 10 23.5 1.7 32.1 1.7 2.3 0.5 15 4.76

10.45 30 19.3 5.5 86.7 76.5 36.3 71.6 25 0.26

PSR B1915+13 4.85 8 20.4 2.6 31.6 2.5 1.4 3.6 60 0.50

PSR B1929+10 1.41 1 53.8 4.1 71.9 0.1 12.5 0.1 3 233.3

1.71 1 52.1 4.8 71.5 0.2 13.8 0.2 2 160.6

4.85 1 41.8 6.0 65.7 0.5 0.6 0.5 5 6.80

10.45 10 14.8 3.0 43.1 4.1 2.9 5.0 20 2.23

PSR B1946+35 4.85 10 18.7 1.4 12.6 2.7 0.3 4.3 20 0.50

PSR B2016+28 4.85 10 15.1 1.9 0.8 1.7 3.0 2.1 20 0.85

PSR B2020+28 4.85 2 18.3 0.9 14.3 0.3 5.7 0.3 20 1.64

10.45 8 13.7 0.5 5.4 6.4 8.4 10.7 45 0.77

PSR B2021+51 1.41 2 23.8 1.1 28.6 0.1 3.6 0.1 5 52.3

1.71 3 22.2 2.2 38.8 0.3 11.0 0.5 5 30.8

4.85 3 19.3 2.0 22.7 0.3 0.7 0.3 25 9.73

10.45 10 12.7 2.6 29.6 6.3 0.7 8.3 10 1.22

PSR B2045-16 4.85 10 14.2 0.4 9.2 1.6 2.2 2.1 20 1.06

PSR B2154+40 4.85 10 23.9 3.0 25.1 4.8 0.7 6.2 20 0.64

PSR B2310+42 1.41 5 17.3 1.6 28.4 2.0 4.4 1.6 30 12.4

4.85 10 14.3 0.9 6.9 0.4 2.7 1.0 30 0.20

PSR B2319+60 1.41 4 23.3 0.9 40.1 0.3 9.5 0.1 8 27.1

4.85 5 20.9 1.6 21.3 0.9 9.4 1.5 20 0.24

PSR B2351+61 1.41 7 12.0 1.4 64.6 10.0 22.8 11.3 20 1.1

4.85 10 9.5 3.1 6.8 3.8 1.8 4.9 20 0.08

Polarization plots for all the pulsars in our sample at many frequencies are presented in Figs. 5-24. For each polarization plot, the upper panel contains the total intensity I (solid line), the linearly polarized L (dashed line), and the circularly polarized V (dotted line) intensities. The lower panel contains the derived PPA curve with associated errors at each point. The points were chosen so that the linear polarization was 3 above the noise level. In certain cases where significant off-pulse emission was detected, this criterion was relaxed. When a fit of the RVM to the data was applied, the fitted function was overplotted to the data as a solid line. The points which were considered for these fits are marked with circles.