• High DM, RM… resolution • Possible “off-pulse” emission • Increasing of flux density at low frequencies (for some pulsars) High Scattering in ISM. Big dispersion delay Bad Signal/Noise due to galactic background Interference ~ 70-80 dB more than background.
given parameters were detected in the decameter range - identification of disturbing factors for detection - ways to eliminate their influence - Fraction (Fr) of KNOWN pulsar (detected in the decameter range) for estimation: Fr * (N of PSRs)*(cone broad.-1) ≅ NEW PSRs
Big dispersion delay (?) (DM=10 pc/cm3 ~100 s in Δf=16…30MHz). But with optimum DM compensations it is NOT a problem Scattering in ISM. But in [Popov M.V. et al. Astronomy Reports. – 2006. – Vol. 50, – P. 562–568. ] shown that for Crab pulsar ("plerion“, Galaxy plane, DM≈57 pc/cm3) at 24 MHz τsc ≈ 3 s.
= 4) 25000 vs 500 K (galactic background ratio ~ 4 2…3 times) 0.5 vs 2 Jy (ratio ~ 4 1…2) Resulted ratio ~ 100…200 times. But Aeff UTR-2 =150 000 sq m Interference ~ 70-80 dB more than background. But high interference immunity and filtering let us to clean raw data.