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In Tables 6.1 and 6.2 we collect the results obtained by testing the AT, RRAT, and LBT methods: we run each method 50 times considering different noise realizations, and the average values are displayed.
So far, we can see that the AT and LBT methods seem to outperform the RRAT method both in terms of efficiency and quality of the reconstruction.
In this case we take into account all the methods previously described, i.e., the AT, RRAT, LBT, NSLT, and RRNSLT methods.
In particular, the image [x.sup.ex.sub.m] obtained by the RRAT method seems to be the most low-frequency one.
As previously remarked, the AT method is the fastest one, while the RRAT method is the slowest one; the LBT method is the most stable one.
The newfound objects, dubbed rotating radio transients (RRATs), may be cousins of the radio pulsars, the discovery team suggests.
This star and at least two other RRATs are slowing their spins, further suggesting that they might be old radio pulsars or fading magnetars, Duncan notes.
During the bursts, the RRATs are the brightest natural radio sources ever observed except for giant radio pulses detected from the Crab Nebula pulsar and another pulsar named B1937+21--another indication that RRATs are neutron stars.
Given their transient nature, RRATs are extremely difficult to study.
Two other RRATs have spin characteristics that indicate they are middle-aged neutron stars, perhaps a few tens of millions of years old.
Factoring the spatial coverage and sensitivity of the Parkes survey and the ephemeral nature of the sources, McLaughlin and her colleagues estimate that there could be roughly 400,000 RRATs in our galaxy, which means they would outnumber the familiar radio pulsars by about 4 to 1.
The 11 Rotating Radio Transients (RRATs) seem to be a unique class of pulsars which burst for short periods and when in outburst can be among the most radio-bright objects in the sky.
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