B0329+54

Introduction

The strongest Pulsar in the northern hemisphere already detected in the past with self made software.

From the output of presto the trace of the pulsar signal is present in the entire frequency window while in the time window there is a deep scintillation (signal variation).

The presence of several RFI does not preclude to identify a well defined pulsar profile but deteriorates the pulsar definition.

A new observation, in a better noise condition, gives a much more gratifying result, the demonstration is in the chi-squared (X^2) parameter difference (33 1st observation, 240 the second),

Such a difference would be detrimental observing a weaker signal.

Below the 2 results:

Pulsar Data

Date of Observation

Thursday, ‎May ‎25, ‎2017 / Monday, ‎August ‎14, ‎2017

Length of Observation

2 Hours / 3 Hours

Center Frequency

1290 MHz

Bandwidth

10 MHz

Pulsar Flux at 1400MHz

203 mJy

Distance

3.460 light years

Pulsar Period

714 msec

Age

5.000.000 Years

Pulsar Profile 1st




Presto Output 1st


Pulsar Profile 2nd




Presto Output 2nd