285 research outputs found
Long-term Observations of Three Nulling Pulsars
We present an analysis of approximately 200 hours of observations of the
pulsars J16345107, J17174054 and J18530505, taken over the course of
14.7 yr. We show that all of these objects exhibit long term nulls and
radio-emitting phases (i.e. minutes to many hours), as well as considerable
nulling fractions (NFs) in the range . PSR J17174054 is
also found to exhibit short timescale nulls () and burst phases
() during its radio-emitting phases. This behaviour acts to
modulate the NF, and therefore the detection rate of the source, over
timescales of minutes. Furthermore, PSR J18530505 is shown to exhibit a weak
emission state, in addition to its strong and null states, after sufficient
pulse integration. This further indicates that nulls may often only represent
transitions to weaker emission states which are below the sensitivity
thresholds of particular observing systems. In addition, we detected a
peak-to-peak variation of in the spin-down rate of PSR
J17174054, over timescales of hundreds of days. However, no long-term
correlation with emission variation was found.Comment: 10 pages, 8 figures, accepted for publication in MNRA
On the Apparent Nulls and Extreme Variability of PSR J1107-5907
We present an analysis of the emission behaviour of PSR J1107-5907, a source
known to exhibit separate modes of emission, using observations obtained over
approximately 10 yr. We find that the object exhibits two distinct modes of
emission; a strong mode with a broad profile and a weak mode with a narrow
profile. During the strong mode of emission, the pulsar typically radiates very
energetic emission over sequences of ~200-6000 pulses (~60 s-24 min), with
apparent nulls over time-scales of up to a few pulses at a time. Emission
during the weak mode is observed outside of these strong-mode sequences and
manifests as occasional bursts of up to a few clearly detectable pulses at a
time, as well as low-level underlying emission which is only detected through
profile integration. This implies that the previously described null mode may
in fact be representative of the bottom-end of the pulse intensity distribution
for the source. This is supported by the dramatic pulse-to-pulse intensity
modulation and rarity of exceptionally bright pulses observed during both modes
of emission. Coupled with the fact that the source could be interpreted as a
rotating radio transient (RRAT)-like object for the vast majority of the time,
if placed at a further distance, we advance that this object likely represents
a bridge between RRATs and extreme moding pulsars. Further to these emission
properties, we also show that the source is consistent with being a
near-aligned rotator and that it does not exhibit any measurable spin-down rate
variation. These results suggest that nulls observed in other intermittent
objects may in fact be representative of very weak emission without the need
for complete cessation. As such, we argue that longer (> 1 h) observations of
pulsars are required to discern their true modulation properties.Comment: 15 pages, 10 figures, accepted for publication in MNRA
The Millisecond Radio Sky: Transients from a Blind Single Pulse Search
We present the results of a search for transient radio bursts of between
0.125 and 32 millisecond duration in two archival pulsar surveys of
intermediate galactic latitudes with the Parkes multibeam receiver. Fourteen
new neutron stars have been discovered, seven of which belong to the recently
identified "rotating radio transients" (RRATs) class. Here we describe our
search methodology, and discuss the new detections in terms of how the RRAT
population relates to the general population of pulsars. The new detections
indicate (1) that the galactic z-distribution of RRATs in the surveys closely
resembles the distribution of pulsars, with objects up to 0.86 kpc from the
galactic plane; (2) where measurable, the RRAT pulse widths are similar to that
of individual pulses from pulsars of similar period, implying a similar beaming
fraction; and (3) our new detections span a variety of nulling fractions, and
thus we postulate that the RRATs may simply be nulling pulsars that are only
"on" for less than a pulse period. Finally, the newly discovered object PSR
J0941-39 may represent a link between pulsars and RRATs. This bizarre object
was discovered as an RRAT, but in follow-up observations often appeared as a
bright (~10 mJy) pulsar with a low nulling fraction. It is obvious therefore
that a neutron star can oscillate between being an RRAT and a pulsar.
Crucially, the sites of the RRAT pulses are coincident with the pulsar's
emission, implying that the two emission mechanisms are linked, and that RRATs
are not just pulsars observed from different orientations.Comment: 13 pages, 9 figures, accepted by MNRA
Long-term Radio Observations of the Intermittent Pulsar B1931+24
We present an analysis of approximately 13-yr of observations of the
intermittent pulsar B1931+24 to further elucidate its behaviour. We find that
while the source exhibits a wide range of nulling (~4-39 d) and radio-emitting
(~1-19 d) timescales, it cycles between its different emission phases over an
average timescale of approximately 38 d, which is remarkably stable over many
years. On average, the neutron star is found to be radio emitting for 26 +- 6 %
of the time. No evidence is obtained to suggest that the pulsar undergoes any
systematic, intrinsic variations in pulse intensity during the radio-emitting
phases. In addition, we find no evidence for any correlation between the length
of consecutive emission phases. An analysis of the rotational behaviour of the
source shows that it consistently assumes the same spin-down rates, i.e. nudot
= -16 +- 1 x 10^-15 s^-2 when emitting and nudot = -10.8 +- 0.4 x 10^-15 s^-2
when not emitting, over the entire observation span. Coupled with the stable
switching timescale, this implies that the pulsar retains a high degree of
magnetospheric memory, and stability, in spite of comparatively rapid (~ms)
dynamical plasma timescales. While this provides further evidence to suggest
that the behaviour of the neutron star is governed by magnetospheric-state
switching, the underlying trigger mechanism remains illusive. This should be
elucidated by future surveys with next generation telescopes such as LOFAR,
MeerKAT and the SKA, which should detect similar sources and provide more clues
to how their radio emission is regulated.Comment: 12 pages, 12 figures, accepted for publication in MNRA
A transient component in the pulse profile of PSR J0738-4042
One of the tenets of the radio pulsar observational picture is that the
integrated pulse profiles are constant with time. This assumption underpins
much of the fantastic science made possible via pulsar timing. Over the past
few years, however, this assumption has come under question with a number of
pulsars showing pulse shape changes on a range of timescales. Here, we show the
dramatic appearance of a bright component in the pulse profile of PSR
J0738-4042 (B0736-40). The component arises on the leading edge of the profile.
It was not present in 2004 but strongly present in 2006 and all observations
thereafter. A subsequent search through the literature shows the additional
component varies in flux density over timescales of decades. We show that the
polarization properties of the transient component are consistent with the
picture of competing orthogonal polarization modes. Faced with the general
problem of identifying and characterising average profile changes, we outline
and apply a statistical technique based on a Hidden Markov Model. The value of
this technique is established through simulations, and is shown to work
successfully in the case of low signal-to-noise profiles.Comment: Accepted for publication in MNRA
Pulsar Timing with the Parkes Radio Telescope for the Fermi Mission
We report here on two years of timing of 168 pulsars using the Parkes radio
telescope. The vast majority of these pulsars have spin-down luminosities in
excess of 10^34 erg/s and are prime target candidates to be detected in
gamma-rays by the Fermi Gamma-Ray Space Telescope. We provide the ephemerides
for the ten pulsars being timed at Parkes which have been detected by Fermi in
its first year of operation. These ephemerides, in conjunction with the
publicly available photon list, can be used to generate gamma-ray profiles from
the Fermi archive. We will make the ephemerides of any pulsars of interest
available to the community upon request. In addition to the timing ephemerides,
we present the parameters for 14 glitches which have occurred in 13 pulsars,
seven of which have no previously known glitch history. The Parkes timing
programme, in conjunction with Fermi observations, is expected to continue for
at least the next four years.Comment: Accepted for publication in PASA.12 page
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