Although originally discovered as a radio-quiet gamma-ray pulsar , J1732 - 3131 has exhibited intriguing detections at decameter wavelengths .
We report an extensive follow-up of the pulsar at 327 MHz with the Ooty radio telescope .
Using the previously observed radio characteristics , and with an effective integration time of 60 hrs , we present a detection of the pulsar at a confidence level of 99.82 \% .
The 327 MHz mean flux density is estimated to be 0.5 - 0.8 mJy , which establishes the pulsar to be a steep spectrum source and one of the least luminous pulsars known to date .
We also phase-aligned the radio and gamma-ray profiles of the pulsar , and measured the phase-offset between the main peaks in the two profiles to be 0.24 \pm 0.06 .
We discuss the observed phase-offset in the context of various trends exhibited by the radio-loud gamma-ray pulsar population , and suggest that the gamma-ray emission from J1732 - 3131 is best explained by outer magnetosphere models .
Details of our analysis leading to the pulsar detection , and measurements of various parameters and their implications relevant to the pulsar ’ s emission mechanism are presented .