Timing observations of three Galactic millisecond pulsars. (arXiv:2108.03946v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Lorimer_D/0/1/0/all/0/1">D.R. Lorimer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawash_A/0/1/0/all/0/1">A.M. Kawash</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Freire_P/0/1/0/all/0/1">P.C.C. Freire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_D/0/1/0/all/0/1">D.A. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kerr_M/0/1/0/all/0/1">M. Kerr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McLaughlin_M/0/1/0/all/0/1">M.A. McLaughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mickaliger_M/0/1/0/all/0/1">M.B. Mickaliger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spiewak_R/0/1/0/all/0/1">R. Spiewak</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:+Barr_E/0/1/0/all/0/1">E. Barr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burgay_M/0/1/0/all/0/1">M. Burgay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cameron_A/0/1/0/all/0/1">A.D. Cameron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Camilo_F/0/1/0/all/0/1">F. Camilo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnston_S/0/1/0/all/0/1">S. Johnston</a>, <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:+Keane_E/0/1/0/all/0/1">E.F. Keane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Keith_M/0/1/0/all/0/1">M. Keith</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:+Possenti_A/0/1/0/all/0/1">A. Possenti</a>
We report observed and derived timing parameters for three millisecond
pulsars (MSPs) from observations collected with the Parkes 64-m telescope,
Murriyang. The pulsars were found during re-processing of archival survey data
by Mickaliger et al. One of the new pulsars (PSR J1546-5925) has a spin period
$P=7.8$ ms and is isolated. The other two (PSR J0921-5202 with $P=9.7$ ms and
PSR J1146-6610 with $P=3.7$ ms) are in binary systems around low-mass ($>0.2
M_{odot}$) companions. Their respective orbital periods are $38$.2 d and
$62.8$ d. While PSR J0921-5202 has a low orbital eccentricity $e=1.3 times
10^{-5}$, in keeping with many other Galactic MSPs, PSR J1146-6610 has a
significantly larger eccentricity, $e = 7.4 times 10^{-3}$. This makes it a
likely member of a group of eccentric MSP-He white dwarf binary systems in the
Galactic disk whose formation is poorly understood. Two of the pulsars are
co-located with previously unidentified point sources discovered with the Fermi
satellite’s Large Area Telescope, but no $gamma$-ray pulsations have been
detected, likely due to their low spin-down powers. We also show that,
particularly in terms of orbital diversity, the current sample of MSPs is far
from complete and is subject to a number of selection biases.
We report observed and derived timing parameters for three millisecond
pulsars (MSPs) from observations collected with the Parkes 64-m telescope,
Murriyang. The pulsars were found during re-processing of archival survey data
by Mickaliger et al. One of the new pulsars (PSR J1546-5925) has a spin period
$P=7.8$ ms and is isolated. The other two (PSR J0921-5202 with $P=9.7$ ms and
PSR J1146-6610 with $P=3.7$ ms) are in binary systems around low-mass ($>0.2
M_{odot}$) companions. Their respective orbital periods are $38$.2 d and
$62.8$ d. While PSR J0921-5202 has a low orbital eccentricity $e=1.3 times
10^{-5}$, in keeping with many other Galactic MSPs, PSR J1146-6610 has a
significantly larger eccentricity, $e = 7.4 times 10^{-3}$. This makes it a
likely member of a group of eccentric MSP-He white dwarf binary systems in the
Galactic disk whose formation is poorly understood. Two of the pulsars are
co-located with previously unidentified point sources discovered with the Fermi
satellite’s Large Area Telescope, but no $gamma$-ray pulsations have been
detected, likely due to their low spin-down powers. We also show that,
particularly in terms of orbital diversity, the current sample of MSPs is far
from complete and is subject to a number of selection biases.
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