  In time-domain radio astronomy with arrays, voltages from individual antennas
are added together with proper delay and fringe correction to form the beam in
real-time. In order to achieve the correct phased addition of antenna voltages
one has to also correct for the ionospheric and instrumental gains.
Conventionally this is done using observations of a calibrator source located
near to the target field. This scheme is sub-optimal since it does not correct
for the variation of the gains with time and position in the sky. Further,
since the ionospheric phase variation is typically most rapid at the longest
baselines, the most distant antennas are often excluded while forming the beam.
We present here a different methodology ("in-field phasing"), in which the
gains are obtained in real-time using a model of the intensity distribution in
the target field, which overcomes all of these drawbacks. We present
observations with the upgraded Giant Metrewave Radio Telescope (uGMRT) which
demonstrates that in-field phasing does lead to a significant improvement in
sensitivity. We also show, using observations of the millisecond pulsar
J1120$-$3618 that this in turn leads to a significant improvement of
measurements of the Dispersion Measure and Time of Arrival. Finally, we present
test observations of the GMRT discovered eclipsing black widow pulsar
J1544+4937 showing that in-field phasing leads to improvement in the
measurement of the cut-off frequency of the eclipse.
