[en] The 2CG sources 218-00, 135+01, 121+04 and 95+04 have been observed at two radio frequencies and the flux values and spectra of the radio sources observed within the gamma-ray fields are catalogued down to a sensitivity of approx 30 mJy at lambda 11 cm. Possible gamma-ray counterpart candidate objects are briefly discussed

[en] Recent results on the relationship between radio pulsars and supernova remnants are presented. No clear general picture has as jet emerged from the observations, although some interrelationships between pulsars or neutron stars and supernova remnants are now well documented and understood. The most interesting cases are presented and discussed. (orig.)

[en] The γ-ray source CG 195+04 has been searched for radio counterparts at wavelengths between 2.8 cm and 18 cm with the 100-m telescope of the Max-Planck-Institut fuer Radioastronomie, Bonn. We have detected a number of sources and measured their spectra. Our positions may form the basis for future surveys in other frequency ranges. Different physical emission models suggest compactness of the γ-ray source. (orig.)

[en] Polarization and morphology of large (old) supernova remnants beyond 1 GHz can be easily observed with the 100-m telescope at Effelsberg. The authors briefly describe the ongoing observation program. (Auth.)

[en] We report on a multifrequency, full polarization analysis of the two classical mode-switching pulsars PSR 0329+54 and PSR 1237+35 and compare properties of all known mode-switchers

[en] Using the MPIfR 100m radio-telescope, observations of mean pulse profiles have been made of a large sample of pulsars at 2.7, 4.9 and 10.7 GHz. The measurements were repeated many times during numerous observing sessions so that the data presented take account of the short-term and medium-term fluctuations of pulsar energies. The observed pulsars are compared with similar observations at lower frequencies showing that in nearly all cases the mean pulse shape changes with frequency. The changes include both variations of the 3dB-width of pulse profiles and variations of component distances. It is shown that in the majority of cases, pulse widths decrease with increasing frequency, whereas the component distances may either increase or decrease. The component separation may furthermore be characterized by a critical frequency which is correlated with the cut-off frequency in the spectra of the corresponding pulsars. (orig.)

No abstract available

[en] The rate of depolarisation of the linear polarisation of the average pulse profil is a function of pulsar period. Short period pulsar depolarise less rapidly and show a variation of depolarisation rate across their pulse profiles. The trailing edge depolarises more rapidly than the leading edge. This is paralleled by a front to back asymetry of the total intensity profile. These latter effects are presumably due to distortion of the magnetosphere near the velocity of high cylinder. The predominant depolarisation mechanism is apparently different for the long and short period pulsars. Randomisation of the position angle of polarisation during propagation in the weaker fields of the outer magnetosphere may account for the depolarisation of the long period pulsars. An increased frequency of occurence of orthogonally polarised radiation may be responsible for the depolarisation of the short period pulsars. The majority of pulsar (> 70% in this sample) show depolarisation of their circular polarization at high frequency. There are indications that this is period dependent. (orig.)

No abstract available

[en] A mode change that is, a change in the average pulse profile, has been detected in the 11 cm radiation from PSR 0355 + 54. It is distinctive in its apparently slow onset and by the quite marked changes in the degree of linear polarization which take place. (orig.) 891 WL/orig. 892 MB