Observation of a Rapidly Pulsating Radio Source (Reprinted from Nature, February 24, 1968)

Hewish, A.; Bell, S.; Pilkington, J. D. H.; Scott, P. F.; Collins, R. A.

doi:10.1038/224472b0

Cited by 20 publications

(14 citation statements)

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“…Since the first pulsar detection (Hewish et al 1969), their radio emission process is still in debate (Beskin et al 2015). In our work we assume a simple model of pair creation.…”

Section: The Phenomenological Radio Luminositiesmentioning

confidence: 99%

Markov Chain Monte Carlo population synthesis of single radio pulsars in the Galaxy

Cieślar

Bulik

Osłowski

2020

Monthly Notices of the Royal Astronomical Society

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We present a model of evolution of solitary neutron stars, including spin parameters, magnetic field decay, motion in the Galactic potential and birth inside spiral arms. We use two parametrizations of the radio-luminosity law and model the radio selection effects. Dispersion measure is estimated from the recent model of free electron distribution in the Galaxy (YMW16). Model parameters are optimized using the Markov Chain Monte Carlo technique. The preferred model has a short decay scale of the magnetic field of 4.27 +0.4 −0.38 Myr. However, it has non-negligible correlation with parameters describing the pulsar radio luminosity. Based on the best-fit model, we predict that the Square Kilometre Array surveys will increase the population of known single radio pulsars by between 23 and 137 per cent. The Indri code used for simulations is publicly available to facilitate future population synthesis efforts.1 The code can be obtained from the GitHub repository http: //github.com/cieslar/Indri 2 At the time of writing we define such machine as an approximately 200-cores cluster.

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“…Since the first pulsar detection (Hewish et al 1969), their radio emission process is still in debate (Beskin et al 2015). In our work we assume a simple model of pair creation.…”

Section: The Phenomenological Radio Luminositiesmentioning

confidence: 99%

Markov Chain Monte Carlo population synthesis of single radio pulsars in the Galaxy

Cieślar

Bulik

Osłowski

2020

Monthly Notices of the Royal Astronomical Society

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“…Much of what is known results from follow-up of events discovered at optical, X-ray, or γ-ray wavelengths such as supernovae, gamma-ray burst, and X-ray binaries. An important exception is the sub-second domain, which has been systematically, if incompletely, explored, leading to the discovery of pulsars (Hewish et al 1969), rotating radio transients (McLaughlin et al 2006), and other unexplained phenomena (Lorimer et al 2007;Ruf et al 2009;Burke-Spolaor & Bailes 2010;Keane et al 2011). Longer-time scale searches, which tend to be sensitive to synchrotron sources, are rarer and the sky coverage is less complete.…”

Section: Introductionmentioning

confidence: 99%

THE ALLEN TELESCOPE ARRAY Pi GHz SKY SURVEY II. DAILY AND MONTHLY MONITORING FOR TRANSIENTS AND VARIABILITY IN THE BOÖTES FIELD

Bower¹,

Whysong²,

Blair³

et al. 2011

ApJ

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We present results from daily radio continuum observations of the Boötes field as part of the Pi GHz Sky Survey (PiGSS). These results are part of a systematic and unbiased campaign to characterize variable and transient sources in the radio sky. The observations include 78 individual epochs distributed over 5 months at a radio frequency of 3.1 GHz with a median RMS image noise in each epoch of 2.8 mJy. We produce 5 monthly images with a median RMS of 0.6 mJy. No transient radio sources are detected in the daily or monthly images. At 15 mJy, we set an upper limit (2σ) to the surface density of 1-day radio transients at 0.025 deg −2 . At 5 mJy, we set an upper limit (2σ) to the surface density of 1-month radio transients at 0.18 deg −2 . We also produce light curves for 425 sources and explore the variability properties of these sources. Approximately 20% of the sources exhibit some variability on daily and monthly time scales. The maximum RMS fractional modulations on the 1 day and 1 month time scales for sources brighter than 10 mJy are 2 and 0.5, respectively. The probability of a daily fluctuation for all sources and all epochs by a factor of 10 is less than 10 −4 . We compare the radio to mid-infrared variability for sources in the field and find no correlation. Finally, we apply the statistics of transient and variable populations to constrain models for a variety of source classes.

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“…Some of the most exciting advances in time-domain astronomy have only been made possible by pushing the capabilities of latest generation telescopes to be sensitive to signals of shorter and shorter duration. The serendipitous discovery of pulsars in the late 1960s is perhaps the prototypical example (Hewish et al 1968). In more recent times, the ongoing effort to detect nanohertz gravitational waves by means of pulsar timing arrays (PTAs) requires the continual monitoring of the times of arrival of millisecond pulsars (MSPs) with microsecond accuracy (e.g.…”

Section: Introductionmentioning

confidence: 99%

MWA tied-array processing III: Microsecond time resolution via a polyphase synthesis filter

McSweeney¹,

Ord²,

Meyers³

et al. 2020

Publ. Astron. Soc. Aust.

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A new high time resolution observing mode for the Murchison Widefield Array (MWA) is described, enabling full polarimetric observations with up to $30.72\,$ MHz of bandwidth and a time resolution of ${\sim}$ $0.8\,\upmu$ s. This mode makes use of a polyphase synthesis filter to ‘undo’ the polyphase analysis filter stage of the standard MWA’s Voltage Capture System observing mode. Sources of potential error in the reconstruction of the high time resolution data are identified and quantified, with the $S/N$ loss induced by the back-to-back system not exceeding $-0.65\,$ dB for typical noise-dominated samples. The system is further verified by observing three pulsars with known structure on microsecond timescales.

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Observation of a Rapidly Pulsating Radio Source (Reprinted from Nature, February 24, 1968)

Cited by 20 publications

References 0 publications

Markov Chain Monte Carlo population synthesis of single radio pulsars in the Galaxy

Markov Chain Monte Carlo population synthesis of single radio pulsars in the Galaxy

THE ALLEN TELESCOPE ARRAY Pi GHz SKY SURVEY II. DAILY AND MONTHLY MONITORING FOR TRANSIENTS AND VARIABILITY IN THE BOÖTES FIELD

MWA tied-array processing III: Microsecond time resolution via a polyphase synthesis filter

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