The High Time Resolution Universe Pulsar Survey - I. System configuration and initial discoveries

Keith, Michael; Jameson, A.; Straten, W. van; Bailes, M.; Johnston, S.; Krämer, M.; Possenti, A.; Bates, S. D.; Bhat, N. D. R.; Burgay, M.; Burke-Spolaor, S.; D’Amico, N.; Levin, Lina; McMahon, Peter L.; Milia, S.; Stappers, B. W.

doi:10.1111/j.1365-2966.2010.17325.x

Cited by 348 publications

(326 citation statements)

References 32 publications

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“…The expected sensitivity limit for the SKA1-MID survey can be compared with, for example, the HTRU survey (Keith et al 2010) ongoing at the Parkes Radio Telescope and the Arecibo PALFA survey (Cordes et al 2006). Whereas the sensitivity for SKA1 50% would only be about half the sensitivity of the Arecibo PALFA survey (which, on the other hand, has a very limited sky coverage), it would still be significantly better than the HTRU survey by a factor of 2-6, depending on the Galactic latitude.…”

Section: A Brief Summary Of the Impact Of Early Phase Ska1 (50% Ska1)mentioning

confidence: 99%

Understanding the Neutron Star Population with the SKA

Tauris¹,

Kaspi²,

Breton³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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Since their discovery in the late 1960's the population of known neutron stars has grown to ∼2500. This sample has yielded many surprises and demonstrated that the observational properties of neutron stars are remarkably diverse. The surveys that will be performed with the SKA will produce a further tenfold increase in the number of Galactic neutron stars known. Moreover, the SKA's broad spectral coverage, sub-arraying and multi-beaming capabilities will allow us to characterise these sources with unprecedented efficiency, in turn enabling a giant leap in the understanding of their properties. We review the neutron star population and outline strategies for studying each of the growing number of diverse classes that are populating the "neutron star zoo". Questions that will be addressed by the much larger statistical samples and vastly improved timing efficiency provided by SKA include: (i) the spin period and spin-down rate distributions (and thus magnetic fields) at birth, and the associated information about the supernovae wherein they are formed; (ii) the radio pulsar-magnetar connection; (iii) the link between normal radio pulsars, intermittent pulsars and rotating radio transients; (iv) the slowest possible spin period for a radio pulsar (revealing the conditions at the pulsar death-line); (v) proper motions of pulsars (revealing supernova kick physics); (vi) the mass distribution of neutron stars; (vii) the fastest possible spin period for a recycled pulsar (constraining magnetosphere-accretion disc interactions, gravitational wave radiation and the equation-of-state); (viii) the origin of high eccentricity millisecond pulsars; (ix) the formation channels for recently identified triple systems; and finally (x) how isolated millisecond pulsars are formed. We can also expect that the first phase of the SKA (SKA1), and in particular the full SKA (SKA2), will break new ground unveiling exotic and heretofore unknown systems that will challenge our current knowledge and theories, thus fostering the development of new research areas. Some possibilities for future landmark discoveries representing significant milestones in the astrophysics of compact objects include: (i) sub-millisecond pulsars; (ii) neutron stars born as millisecond pulsars; (iii) neutron stars with masses below 1.1 or above 2.5 M ; (iv) neutron star-black hole binaries; and (v) a triple system containing a pair of neutron stars.Advancing Astrophysics with the Square Kilometre Array

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Section: A Brief Summary Of the Impact Of Early Phase Ska1 (50% Ska1)mentioning

confidence: 99%

Understanding the Neutron Star Population with the SKA

Tauris¹,

Kaspi²,

Breton³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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“…Other major surveys are the HTRU-S (Keith et al 2010), HTRU-N (Barr et al 2013), and SPAN512 (Desvignes et al 2013) surveys at ∼1.4 GHz, the GBNCC (Stovall et al 2014) and AO327 drift (Deneva et al 2013) surveys at ∼350 MHz, and the LOFAR surveys (Coenen et al 2014) at ∼150 MHz.…”

Section: Introductionmentioning

confidence: 99%

Arecibo Pulsar Survey Using Alfa. Iv. Mock Spectrometer Data Analysis, Survey Sensitivity, and the Discovery of 40 Pulsars

Lazarus

Brazier

Hessels

et al. 2015

ApJ

130

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The on-going Arecibo Pulsar-ALFA (PALFA) survey began in 2004 and is searching for radio pulsars in the Galactic plane at 1.4 GHz. Here we present a comprehensive description of one of its main data reduction pipelines that is based on the PRESTO software and includes new interference-excision algorithms and candidate selection heuristics. This pipeline has been used to discover 40 pulsars, bringing the survey's discovery total to 144 pulsars. Of the new discoveries, eight are millisecond pulsars (MSPs; P 10 < ms) and one is a Fast Radio Burst (FRB). This pipeline has also re-detected 188 previously known pulsars, 60 of them previously discovered by the other PALFA pipelines. We present a novel method for determining the survey sensitivity that accurately takes into account the effects of interference and red noise: we inject synthetic pulsar signals with various parameters into real survey observations and then attempt to recover them with our pipeline. We find that the PALFA survey achieves the sensitivity to MSPs predicted by theoretical models but suffers a degradation for P 100  ms that gradually becomes up to ∼10 times worse for P 4 s > at DM 150 < pc cm −3 . We estimate 33 ± 3% of the slower pulsars are missed, largely due to red noise. A population synthesis analysis using the sensitivity limits we measured suggests the PALFA survey should have found 224 ± 16 un-recycled pulsars in the data set analyzed, in agreement with the 241 actually detected. The reduced sensitivity could have implications on estimates of the number of longperiod pulsars in the Galaxy.

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“…The lone exception is the on-going High Time Resolution Universe (HTRU) survey of the southern sky with the Parkes multi-beam receiver at 1.4 GHz, which has covered the significant parts of the Fermi excess area. In particular, the low latitude component of the southern HTRU survey is making hourlong integrations with the goal of searching the galactic plane in latitude |b| < 3.5 • and longitude 30 • < l < 280 • (Keith et al 2010). HTRU has searched the direction toward PSR J1751−2737 but the pulsar does not appear in recent lists of detections (Ng et al 2015).…”

Section: Discussionmentioning

confidence: 99%

Searching for pulsars associated with the Fermi GeV excess

Bhakta

Deneva

Frail

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The Fermi Large Area Telescope has detected an extended region of GeV emission toward the Galactic Center that is currently thought to be powered by dark matter annihilation or a population of young and/or millisecond pulsars. In a test of the pulsar hypothesis, we have carried out an initial search of a 20 deg 2 area centered on the peak of the galactic center GeV excess. Candidate pulsars were identified as a compact, steep spectrum continuum radio source on interferometric images and followed with targeted single-dish pulsation searches. We report the discovery of the recycled pulsar PSR 1751−2737 with a spin period of 2.23 ms. PSR 1751−2737 appears to be an isolated recycled pulsar located within the disk of our Galaxy, and it is not part of the putative bulge population of pulsars that are thought to be responsible for the excess GeV emission. However, our initial success in this small pilot survey suggests that this hybrid method (i.e. wide-field interferometric imaging followed up with single dish pulsation searches) may be an efficient alternative strategy for testing whether a putative bulge population of pulsars is responsible for the GeV excess.

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The High Time Resolution Universe Pulsar Survey - I. System configuration and initial discoveries

Cited by 348 publications

References 32 publications

Understanding the Neutron Star Population with the SKA

Understanding the Neutron Star Population with the SKA

Arecibo Pulsar Survey Using Alfa. Iv. Mock Spectrometer Data Analysis, Survey Sensitivity, and the Discovery of 40 Pulsars

Searching for pulsars associated with the Fermi GeV excess

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