Browsing by Author "Craig, J."

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    Detection and flux density measurements of the millisecond pulsar j2145-0750 below 100 mhz
    Dowell, J.; Ray, P. S.; Taylor, G. B.; Blythe, J. N.; Clarke, Tracy E.; Craig, J.; Ellingson, Steven W.; Helmboldt, J. F.; Henning, P. A.; Lazio, T. J. W.; Schinzel, F.; Stovall, K.; Wolfe, C. N. (IOP Publishing, 2013-09-01)
    We present flux density measurements and pulse profiles for the millisecond pulsar PSR J2145-0750 spanning 37 to 81 MHz using data obtained from the first station of the Long Wavelength Array. These measurements represent the lowest frequency detection of pulsed emission from a millisecond pulsar to date. We find that the pulse profile is similar to that observed at 102 MHz. We also find that the flux density spectrum between approximate to 40 MHz to 5 GHz is suggestive of a break and may be better fit by a model that includes spectral curvature with a rollover around 730 MHz rather than a single power law.
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    Observations of crab giant pulses in 20-84 MHz using LWA1
    Ellingson, Steven W.; Clarke, Tracy E.; Craig, J.; Hicks, B. C.; Lazio, T. J. W.; Taylor, G. B.; Wilson, T. L.; Wolfe, C. N. (IOP Publishing, 2013-05-01)
    We report the detection and observed characteristics of giant pulses from the Crab Nebula pulsar (B0531+21) in four frequency bands covering 20-84 MHz using the recently completed Long Wavelength Array Station 1 (LWA1) radio telescope. In 10 hr of observations distributed over a 72 day period in fall of 2012, 33 giant pulses having peak flux densities between 400 Jy and 2000 Jy were detected. Twenty-two of these pulses were detected simultaneously in channels of 16 MHz bandwidth centered at 44 MHz, 60 MHz, and 76 MHz, including one pulse which was also detected in a channel centered at 28 MHz. We quantify statistics of pulse amplitude and pulse shape characteristics, including pulse broadening. Amplitude statistics are consistent with expectations based on extrapolations from previous work at higher and lower frequencies. Pulse broadening is found to be relatively high, but not significantly greater than expected. We present procedures that have been found to be effective for observing giant pulses in this frequency range.