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Pulsar radio emission undergoes dispersion due to the presence of freeelectrons in the interstellar medium (ISM). The dispersive delay in the arrivaltime of pulsar signal changes over time due to the varying ISM electron columndensity along the line of sight. Correcting for this delay accurately iscrucial for the detection of nanohertz gravitational waves using Pulsar TimingArrays. In this work, we present in-band and inter-band DM estimates of fourpulsars observed with uGMRT over the timescale of a year using two differenttemplate alignment methods. The DMs obtained using both these methods show onlysubtle differences for PSR 1713+0747 and J1909$-$3744. A considerable offset isseen in the DM of PSR J1939+2134 and J2145$-$0750 between the two methods. Thiscould be due to the presence of scattering in the former and profile evolutionin the latter. We find that both methods are useful but could have a systematicoffset between the DMs obtained. Irrespective of the template alignment methodsfollowed, the precision on the DMs obtained is about $10^{-3}$ pc cm$^{-3}$using only BAND3 and $10^{-4}$ pc cm$^{-3}$ after combining data from BAND3 andBAND5 of the uGMRT. In a particular result, we have detected a DM excess ofabout $5\times10^{-3}$ pc cm$^{-3}$ on 24 February 2019 for PSR J2145$-$0750.This excess appears to be due to the interaction region created by fast solarwind from a coronal hole and a coronal mass ejection (CME) observed from theSun on that epoch. A detailed analysis of this interesting event is presented.

High Precision Measurements of Interstellar Dispersion Measure with the upgraded GMRT