A detailed study of giant pulses from PSR B1937+21 using the Large European Array for Pulsars. (arXiv:1811.02856v1 [astro-ph.HE])

A detailed study of giant pulses from PSR B1937+21 using the Large European Array for Pulsars. (arXiv:1811.02856v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+McKee_J/0/1/0/all/0/1">J. W. McKee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stappers_B/0/1/0/all/0/1">B. W. Stappers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bassa_C/0/1/0/all/0/1">C. G. Bassa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_S/0/1/0/all/0/1">S. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cognard_I/0/1/0/all/0/1">I. Cognard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaikwad_M/0/1/0/all/0/1">M. Gaikwad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janssen_G/0/1/0/all/0/1">G. H. Janssen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karuppusamy_R/0/1/0/all/0/1">R. Karuppusamy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kramer_M/0/1/0/all/0/1">M. Kramer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_K/0/1/0/all/0/1">K. J. Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_K/0/1/0/all/0/1">K. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perrodin_D/0/1/0/all/0/1">D. Perrodin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanidas_S/0/1/0/all/0/1">S. A. Sanidas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smits_R/0/1/0/all/0/1">R. Smits</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_L/0/1/0/all/0/1">L. Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_W/0/1/0/all/0/1">W. W. Zhu</a>

We have studied 4265 giant pulses (GPs) from the millisecond pulsar B1937+21;
the largest-ever sample gathered for this pulsar, in observations made with the
Large European Array for Pulsars. The pulse energy distribution of GPs
associated with the interpulse are well-described by a power law, with index
$alpha = -3.99 pm 0.04$, while those associated with the main pulse are
best-described by a broken power law, with the break occurring at $sim7$ Jy
$mu$s, with power law indices $alpha_{text{low}} = -3.48 pm 0.04$ and
$alpha_{text{high}} = -2.10 pm 0.09$. The modulation indices of the GP
emission are measured, which are found to vary by $sim0.5$ at pulse phases
close to the centre of the GP phase distributions. We find the
frequency-resolved structure of GPs to vary significantly, and in a manner that
cannot be attributed to the interstellar medium influence on the observed
pulses. We examine the distribution of polarisation fractions of the GPs and
find no correlation between GP emission phase and fractional polarisation. We
use the GPs to time PSR B1937+21 and although the achievable time of arrival
precision of the GPs is approximately a factor of two greater than that of the
average pulse profile, there is a negligible difference in the precision of the
overall timing solution when using the GPs.

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