4. Results and follow-up observations
Twenty-five of the most promising pulsar candidates were re-observed in April 1996 and the detection of three pulsars was confirmed, B1952+29 and two that were previously unknown: PSRs J0215+6218 and J1957+2831. No further previously known pulsars were expected to be above our detection threshold. The new pulsars lie within the boundaries but towards the outer regions of the target supernova remnants G132.7+1.3 and G65.1+0.6 respectively. No further pulsars were discovered during these observations.
In order to accurately determine the astrometric and spin parameters of the two newly discovered pulsars, regular follow-up observations at 606 and 1400 MHz have been made ever since their discovery as part of the Jodrell Bank pulsar timing programme (see for example Shemar & Lyne 1996). We have been able to model the pulse arrival times for both pulsars using standard pulsar timing techniques (Manchester & Taylor 1977). Timing solutions obtained from these data are given in Table 2.
Table 2. Observed and derived parameters of the two newly discovered pulsars. Quoted errors refer to the last significant digit.
Total intensity pulse profiles of the newly discovered pulsars at 606 and 1412/1418 MHz are shown in Fig. 2. Mean flux densities at both frequencies were determined in an identical fashion to that described by Lorimer et al. (1995). We also list the characteristic age and the surface magnetic field Gauss which assume a constant dipolar magnetic field and short initial period (Manchester & Taylor 1977).
© European Southern Observatory (ESO) 1998
Online publication: March 3, 1998