Pulsar Timing Arrays Current and Future Instrumentation - DCC

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$Numerical simulation of diffraction grating alignment and ... - DCC$

Pulsar TimingHistorical Context• 1974: Hulse-Taylor binary pulsar– Arecibo telescope @ 430 MHz– ≤ 8 MHz bandwidth– 175 K system temperatureT sky = 25 K @ 430 MHz• 1982: first millisecond pulsar (B1937+21)– Arecibo telescope @ 1400 MHz– 16 MHz bandwidth– 40 K system temperatureT sky ~ 7 K @ 1400 MHz
Pulsar Timing ArraysCurrent InstrumentationTypical Parameters• A eff ~ 100 m• ∆ν ~ 100 MHz• T sys ~ 30 K• ∆t ~ 15 min.Current Publications• Yardley et al. 2011, “On detection of thestochastic gravitational-wave background usingthe Parkes pulsar timing array,” Mon. Not. R.Astron. Soc., 414, 1777• van Haasteren et al. 2011, “Placing limits on thestochastic gravitational-wave background usingEuropean Pulsar Timing Array data,” Mon. Not.R. Astron. Soc., 414, 3117• Demorest et al. 2012, “Limits on the StochasticGravitational Wave Background from the NorthAmerican Nanohertz Observatory forGravitational Waves,” ApJ, in press• Hobbs et al. 2010, “The International PulsarTiming Array project: using pulsars as agravitational wave detector,” Class. Quant.Grav., 27, 084013
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Pulsar Timing Arrays Current and Future Instrumentation - DCC

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