The UTMOST pulsar timing programme I: overview and first results. (arXiv:1812.04038v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Jankowski_F/0/1/0/all/0/1">F. Jankowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailes_M/0/1/0/all/0/1">M. Bailes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Straten_W/0/1/0/all/0/1">W. van Straten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keane_E/0/1/0/all/0/1">E. F. Keane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flynn_C/0/1/0/all/0/1">C. Flynn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barr_E/0/1/0/all/0/1">E. D. Barr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bateman_T/0/1/0/all/0/1">T. Bateman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhandari_S/0/1/0/all/0/1">S. Bhandari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caleb_M/0/1/0/all/0/1">M. Caleb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Campbell_Wilson_D/0/1/0/all/0/1">D. Campbell-Wilson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Farah_W/0/1/0/all/0/1">W. Farah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Green_A/0/1/0/all/0/1">A. J. Green</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hunstead_R/0/1/0/all/0/1">R. W. Hunstead</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jameson_A/0/1/0/all/0/1">A. Jameson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oslowski_S/0/1/0/all/0/1">S. Oslowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parthasarathy_A/0/1/0/all/0/1">A. Parthasarathy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosado_P/0/1/0/all/0/1">P. A. Rosado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krishnan_V/0/1/0/all/0/1">V. Venkatraman Krishnan</a>
We present an overview and the first results from a large-scale pulsar timing
programme that is part of the UTMOST project at the refurbished Molonglo
Observatory Synthesis Radio Telescope (MOST) near Canberra, Australia. We
currently observe more than 400 mainly bright southern radio pulsars with up to
daily cadences. For 205 (8 in binaries, 4 millisecond pulsars) we publish
updated timing models, together with their flux densities, flux density
variability, and pulse widths at 843 MHz, derived from observations spanning
between 1.4 and 3 yr. In comparison with the ATNF pulsar catalogue, we improve
the precision of the rotational and astrometric parameters for 123 pulsars, for
47 by at least an order of magnitude. The time spans between our measurements
and those in the literature are up to 48 yr, which allows us to investigate
their long-term spin-down history and to estimate proper motions for 60
pulsars, of which 24 are newly determined and most are major improvements. The
results are consistent with interferometric measurements from the literature. A
model with two Gaussian components centred at 139 and $463~text{km} :
text{s}^{-1}$ fits the transverse velocity distribution best. The pulse duty
cycle distributions at 50 and 10 per cent maximum are best described by
log-normal distributions with medians of 2.3 and 4.4 per cent, respectively. We
discuss two pulsars that exhibit spin-down rate changes and drifting subpulses.
Finally, we describe the autonomous observing system and the dynamic scheduler
that has increased the observing efficiency by a factor of 2-3 in comparison
with static scheduling.
We present an overview and the first results from a large-scale pulsar timing
programme that is part of the UTMOST project at the refurbished Molonglo
Observatory Synthesis Radio Telescope (MOST) near Canberra, Australia. We
currently observe more than 400 mainly bright southern radio pulsars with up to
daily cadences. For 205 (8 in binaries, 4 millisecond pulsars) we publish
updated timing models, together with their flux densities, flux density
variability, and pulse widths at 843 MHz, derived from observations spanning
between 1.4 and 3 yr. In comparison with the ATNF pulsar catalogue, we improve
the precision of the rotational and astrometric parameters for 123 pulsars, for
47 by at least an order of magnitude. The time spans between our measurements
and those in the literature are up to 48 yr, which allows us to investigate
their long-term spin-down history and to estimate proper motions for 60
pulsars, of which 24 are newly determined and most are major improvements. The
results are consistent with interferometric measurements from the literature. A
model with two Gaussian components centred at 139 and $463~text{km} :
text{s}^{-1}$ fits the transverse velocity distribution best. The pulse duty
cycle distributions at 50 and 10 per cent maximum are best described by
log-normal distributions with medians of 2.3 and 4.4 per cent, respectively. We
discuss two pulsars that exhibit spin-down rate changes and drifting subpulses.
Finally, we describe the autonomous observing system and the dynamic scheduler
that has increased the observing efficiency by a factor of 2-3 in comparison
with static scheduling.
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