This specifies that an antenna gain of just over 14 dBi at 1000 kHz bandwidth is sufficient to detect B0329+54 at 400 MHz - but again remember, the equation gives the theoretical best result. In practice an antenna with a gain of 17 dBi to 19 dBi would be required. Once again the required antenna gains for smaller bandwidths is shown to the left of the 'Dispersion Bandwidth Limit'.
Examining the result for J0835-4510 shows that if the same bandwidth is used for B0329+54 - say 120 kHz (the maximum allowable un-de-dispersed bandwidth for J0835-4510 at 400 MHz) - a higher antenna gain is needed for B0329+54 compared to J0835-4510. This is to be expected as J0835-4510 is stronger than B0329+54. Given that J0835-4510 is not visible for many Northern Hemisphere observers (while B0329+54 is) this might be seen as a disadvantage for those northern observers, however, the antenna gain increase is a modest one - from about 16 dBi for J0835-4510 to about 19 dBi for B0329+54. But that result is at the bandwidth which is the maximum for J0835-4510. When observing B0329+54 the 'Dispersion Bandwidth Limit' is 1000 kHz - not 120 kHz. From the above graph it can be seen that widening the bandwidth up to the 'Dispersion Bandwidth Limit' of 1000 kHz for B0329+54 brings the required antenna gain back down to around 14 dBi.
The upshot of this is that for an un-de-dispersed system using the full allowable 'Dispersion Bandwidth Limit' bandwidths for both pulsars at 400 MHz, the required antenna gain for B0329+54 (the second strongest pulsar) is actually a little lower (by about 2 dB) than for J0835-4510 (the strongest pulsar).
The above analysis has been verified in practice by Andrea Dell'Imaggine (IW5BHY) who used a 4 metre diameter dish (~ 22 dBi gain @ 422 Mhz) to detect B0329+54 at a S/N which, by visual examination of the graphical results provided, seems to be > 10. (see here). Those results and the S/N obtained are in line with the pulsar radiometer equation.
B0031-07 (0.052 Jy @ 400 MHz, DM=11)
For this very weak pulsar the maximum un-de-dispersed bandwidth for an observational frequency of 400 MHz is 20000 kHz because of the low dispersion measure of about 11. The required antenna gain varies with bandwidth up to this limit.
The results are compared to the claimed detection of B0031-07 with 3 metre diameter dish at 408 MHz (~ 19 dBi gain).
Solving the ΔSmin equation above and plotting the required antenna gain (calculated from required aperture) against bandwidth...