Relevant bibliographies by topics / Pulsar Search

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Academic literature on the topic 'Pulsar Search'

Author: Grafiati
Published: 4 June 2021
Last updated: 13 February 2022

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Journal articles on the topic "Pulsar Search"

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Levin, L., W. Armour, C. Baffa, E. Barr, S. Cooper, R. Eatough, A. Ensor, et al. "Pulsar Searches with the SKA." Proceedings of the International Astronomical Union 13, S337 (September 2017): 171–74. http://dx.doi.org/10.1017/s1743921317009528.

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AbstractThe Square Kilometre Array will be an amazing instrument for pulsar astronomy. While the full SKA will be sensitive enough to detect all pulsars in the Galaxy visible from Earth, already with SKA1, pulsar searches will discover enough pulsars to increase the currently known population by a factor of four, no doubt including a range of amazing unknown sources. Real time processing is needed to deal with the 60 PB of pulsar search data collected per day, using a signal processing pipeline required to perform more than 10 POps. Here we present the suggested design of the pulsar search engine for the SKA and discuss challenges and solutions to the pulsar search venture.
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Michel, F. Curtis. "Statistical Search for Magnetic Field Decay." International Astronomical Union Colloquium 128 (1992): 35–38. http://dx.doi.org/10.1017/s000273160015471x.

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AbstractThe claims made in many statistical analyses for magnetic field decay follow from the assumption that radio luminosity declines slower than spin-down luminosity which is suggested by least-squares fits to the data. However, such fits are very sensitive to the behaviors of the fastest and slowest pulsars. If pulsar luminosities are plotted in distance-selected groups, the (radio inefficient) Crab and Vela pulsars are clearly exceptional members and the remaining pulsars are consistent with a mean fixed conversion efficiency of 10–5. Numerical simulations (and theoretical analysis) strongly suggest that the pulsar period distribution peak is caused by luminosity selection and searches limited in distance by dispersion measure, and not by some mechanism that removes old pulsars. We cannot exclude magnetic field decay with some large time constant, ≥107 years say, but only because it would make such a small difference to the expected pulsar statistics, not because it is required by the data.
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Octau, Franck, Grégory Desvignes, Ismaël Cognard, David Champion, Patrick Lazarus, David Smith, and Gilles Theureau. "Search for and study of pulsars with the Nançay Radio Telescope." Proceedings of the International Astronomical Union 13, S337 (September 2017): 386–87. http://dx.doi.org/10.1017/s1743921317009516.

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AbstractSince the discovery of the first pulsar in 1967, over 2500 pulsars have been discovered. Pulsars enable a broad range of studies: from the study of the properties of the interstellar medium and of pulsar magnetospheres to tests of gravity in the strong-field regime and the characterisation of the cosmological gravitation wave background. These reasons are the main drive for searching for more pulsars. A blind pulsar survey, named SPAN512, was initiated with the Nançay Radio Telescope in 2012. Conducted at 1.4 GHz with a sampling time of 64μs and 500-kHz frequency channels, SPAN512 was designed to search for fast and distant pulsars in the Galactic plane. Here we describe the current status of the survey and present the latest discovery, PSR J2055+3829, a 2.08-ms pulsar in a black widow system.
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Dai, Shi, Simon Johnston, and George Hobbs. "Searching for pulsars in future radio continuum surveys." Proceedings of the International Astronomical Union 13, S337 (September 2017): 328–29. http://dx.doi.org/10.1017/s1743921317008833.

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AbstractRadio continuum surveys are equally sensitive to all pulsars, not affected by dispersion measure smearing, scattering or orbital modulation of spin periods, and therefore allow us to search for extreme pulsars, such as sub-millisecond pulsars, pulsar-black hole systems and pulsars in the Galactic Centre. As we move towards the Square Kilometre Array (SKA) era, searching for pulsars in continuum images will complement conventional pulsar searches, and make it possible to find extreme objects.
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Sett, S., R. P. Breton, C. J. Clark, M. H. Kerkwijk, and D. L. Kaplan. "A search for radio pulsars in five nearby supernova remnants." Astronomy & Astrophysics 647 (March 2021): A183. http://dx.doi.org/10.1051/0004-6361/201936108.

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Context. Most neutron stars are expected to be born in supernovae, but only about half of supernova remnants (SNRs) are associated with a compact object. In many cases, a supernova progenitor may have resulted in a black hole. However, there are several possible reasons why true pulsar-SNR associations may have been missed in previous surveys: The pulsar’s radio beam may not be oriented towards us; the pulsar may be too faint to be detectable; or there may be an offset in the pulsar position caused by a kick. Aims. Our goal is to find new pulsars in SNRs and explore their possible association with the remnant. The search and selection of the remnants presented in this paper was inspired by the non-detection of any X-ray bright compact objects in these remnants when previously studied. Methods. Five SNRs were searched for radio pulsars with the Green Bank Telescope at 820 MHz with multiple pointings to cover the full spatial extent of the remnants. A periodicity search plus an acceleration search up to 500 m s−2 and a single pulse search were performed for each pointing in order to detect potential isolated binary pulsars and single pulses, respectively. Results. No new pulsars were detected in the survey. However, we were able to re-detect a known pulsar, PSR J2047+5029, near SNR G89.0+4.7. We were unable to detect the radio-quiet gamma-ray pulsar PSR J2021+4026, but we do find a flux density limit of 0.08 mJy. Our flux density limits make our survey two to 16 times more sensitive than previous surveys, while also covering the whole spatial extent of the same remnants. Conclusions. We discuss potential explanations for the non-detection of a pulsar in the studied SNRs and conclude that sensitivity is still the most likely factor responsible for the lack of pulsars in some remnants.
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Somer, A. "New Pulsars from Arecibo Drift Scan Search." International Astronomical Union Colloquium 177 (2000): 17–20. http://dx.doi.org/10.1017/s0252921100058875.

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AbstractWe report the discovery of 3 pulsars, PSR J0030+0451, PSR J0711+09, and PSR J1313+09 that were found in a three dimensional (DM, period, position) search at 430 MHz using the 305m Arecibo telescope. PSR J0030+0451 is a nearby 4.8-millisecond solitary pulsar. Spin and astrometric parameters are presented for the three new pulsars. We have measured significant polarization in the millisecond pulsar, PSR J0030+0451, over more than 50% of the period and use these data and also a morphological decomposition of the profile to briefly discuss magnetospheric models.
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van Leeuwen, Joeri, Klim Mikhailov, Evan Keane, Thijs Coenen, Liam Connor, Vlad Kondratiev, Daniele Michilli, and Sotiris Sanidas. "LOFAR radio search for single and periodic pulses from M 31." Astronomy & Astrophysics 634 (January 28, 2020): A3. http://dx.doi.org/10.1051/0004-6361/201937065.

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Bright short radio bursts are emitted by sources at a wide range of distances: from the nearby Crab pulsar to remote fast radio bursts (FRBs). FRBs are likely to originate from distant neutron stars, but our knowledge of the radio pulsar population has been limited to the Galaxy and the Magellanic Clouds. In an attempt to increase our understanding of extragalactic pulsar populations and their giant-pulse emission, we employed the low-frequency radio telescope LOFAR to search the Andromeda galaxy (M 31) for radio bursts emitted by young Crab-like pulsars. For direct comparison we also present a LOFAR study on the low-frequency giant pulses from the Crab pulsar; their fluence distribution follows a power law with slope 3.04 ± 0.03. A number of candidate signals were detected from M 31, but none proved persistent. FRBs are sometimes thought of as Crab-like pulsars with exceedingly bright giant pulses; based on our sensitivity, we can rule out that M 31 hosts pulsars that are more than an order of magnitude brighter than the Crab pulsar if their pulse scattering follows that of the known FRBs.
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Siemion, Andrew, Matthew Bailes, Geoff Bower, Jayanth Chennamangalam, Jim Cordes, Paul Demorest, Julia Deneva, et al. "A search for pulsars in the central parsecs of the Galactic center." Proceedings of the International Astronomical Union 8, S291 (August 2012): 57. http://dx.doi.org/10.1017/s1743921312023149.

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AbstractThe discovery of a pulsar or pulsars orbiting near the Galactic Center (GC) could offer an unprecedented probe of strong-field gravity, the properties of our galaxy's supermassive black hole and insights into the paradoxical star formation history of the region. However, searching for pulsars near the GC is severely hampered by the large electron densities along our line of sight and the scattering-induced pulse broadening of the pulsar emission observed through it. As the broadened pulse length approaches the pulsar period, the periodicity in pulsar emission becomes nearly undetectable. Searches extended to higher frequencies, in an effort to reduce scattering, suffer from reduced intrinsic flux, higher system temperatures and increased atmospheric opacity. We are currently attempting to mitigate the challenges associated with searching for pulsars near the GC by employing new wide bandwidth receivers, upgraded IF distribution systems and novel digital spectrometers in a GC pulsar search campaign at the Green Bank Telescope in West Virginia, USA.Our search will cover two frequency bands, from 12-15 GHz (Ku Band) and 18-26 GHz (K Band), during a total of approximately 30 hours of observations, with expected characteristic 10-sigma sensitivities between 5-10 micro-Jy. Our first observations are scheduled for mid-March 2012. Here we will present the status of our observations and initial results.
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D’Amico, N., R. N. Manchester, R. N. Manchester, J. M. Durdin, and W. C. Erickson. "A Search of Steep-Spectrum Radio Sources for Millisecond Pulsars." Publications of the Astronomical Society of Australia 6, no. 2 (1985): 174–76. http://dx.doi.org/10.1017/s1323358000018026.

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AbstractA total of 18 radio sources selected on the basis of steep low-frequency radio spectra have been searched for the presence of millisecond pulsars using the Molonglo Observatory synthesis telescope. The search covered pulsar periods down to 2 ms with a limiting sensitivity of approximately 10 mJy. No pulsars were detected.
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Kramer, M., A. Jessner, P. Müller, and R. Wielebinski. "A high frequency search for highly dispersed pulsars." International Astronomical Union Colloquium 160 (1996): 13–14. http://dx.doi.org/10.1017/s0252921100040884.

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The majority of known pulsars have been discovered by pulsar searches at low radio frequencies (v< 1 GHz). However, such searches are subject to various deleterious effects, viz the Galactic background radiation (∝v−2.8), dispersion smearing (∝v−3) and also scatter broadening (∝v−4.4). Dispersion smearing and, in particular, scatter broadening prohibit the detection of pulsars with high dispersion measures at low frequencies (cf. Fig. 1a). This is highlighted by the fact that all 11 known pulsars with DM>600 cm−3pc have been discovered during the only two surveys performed to date above 1 GHz, i.e. at 1.4 GHz by Clifton et al. (1992) and at 1.5 GHz by Johnston et al. (1992). However, scattering is still a limiting factor at even 1.4/1.5 GHz. For example B1750—24 is observed with a double component profile at 4.85 GHz (Kijak et al. 1996), whereas at 1.4 GHz the components are completely smeared out due to scatter broadening (cf. Clifton et al. 1992). Therefore, the galactic population of highly dispersed pulsars is still not known. In order to reveal this hidden sample, we have recently started a search in Effelsberg at 4.85 GHz where limitations due to scattering are essentially not existent (see Fig. 1a). The use of this extraordinary high frequency for pulsar searches enables us to observe with a large bandwidth but a small number of filterbank channels, so that the necessary computer power is radically reduced. However, the general steepness of pulsar spectra demands a highly sensitive observing system, otherwise, only the most luminous sources can be detected. A serious disadvantage of a high frequency search is the small telescope beam requiring a lot of observing time to search even a small area of the sky. A restriction of the search area is therefore highly recommended.
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Dissertations / Theses on the topic "Pulsar Search"

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Ford, John M. "Pulsar Search Using Supervised Machine Learning." NSUWorks, 2017. http://nsuworks.nova.edu/gscis_etd/1001.

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Pulsars are rapidly rotating neutron stars which emit a strong beam of energy through mechanisms that are not entirely clear to physicists. These very dense stars are used by astrophysicists to study many basic physical phenomena, such as the behavior of plasmas in extremely dense environments, behavior of pulsar-black hole pairs, and tests of general relativity. Many of these tasks require information to answer the scientific questions posed by physicists. In order to provide more pulsars to study, there are several large-scale pulsar surveys underway, which are generating a huge backlog of unprocessed data. Searching for pulsars is a very labor-intensive process, currently requiring skilled people to examine and interpret plots of data output by analysis programs. An automated system for screening the plots will speed up the search for pulsars by a very large factor. Research to date on using machine learning and pattern recognition has not yielded a completely satisfactory system, as systems with the desired near 100% recall have false positive rates that are higher than desired, causing more manual labor in the classification of pulsars. This work proposed to research, identify, propose and develop methods to overcome the barriers to building an improved classification system with a false positive rate of less than 1% and a recall of near 100% that will be useful for the current and next generation of large pulsar surveys. The results show that it is possible to generate classifiers that perform as needed from the available training data. While a false positive rate of 1% was not reached, recall of over 99% was achieved with a false positive rate of less than 2%. Methods of mitigating the imbalanced training and test data were explored and found to be highly effective in enhancing classification accuracy.
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Antonucci, Federica <1976&gt. "Search for gravitational waves from known pulsar." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2009. http://amsdottorato.unibo.it/2061/.

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Keogh, Dominic Robert. "The search for pulsar wind nebulae in the very high energy gamma-ray regime." Thesis, Durham University, 2010. http://etheses.dur.ac.uk/776/.

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The aim of this Thesis is to study the development of pulsar wind nebulae in the TeV regime and in doing so uncover more sources which have as yet not been observed at these wavelengths. It is found that the extent of pulsar wind nebula in the TeV gamma-ray increases with its age while no developmental relationship is seen concerning the luminosity or spectral index of the nebulae when observed in the TeV gamma-ray regime due to uncertainties in the measurements available. TeV gamma-ray upper limits are calculated for several nebulae observed in the X-ray regime allowing the strength of their magnetic fields to be constrained but only one new source, which was previously confused with its companion, was discovered, the Eel Nebula. Predictions of the fluxes of many of the sources for which upper limits are derived in this work have been calculated from observations of their emission in X-rays and some of these sources should be uncovered with the next generation CTA instrument.
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Lyon, Robert James. "Why are pulsars hard to find?" Thesis, University of Manchester, 2016. https://www.research.manchester.ac.uk/portal/en/theses/why-are-pulsars-hard-to-find(f15226ec-355d-4794-b2b8-e0a8e793948e).html.

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Searches for pulsars during the past fifty years, have been characterised by two problems making their discovery difficult: i) an increasing volume of data to be searched, and ii) an increasing number of `candidate' pulsar detections arising from that data, requiring analysis. Whilst almost all are caused by noise or interference, these are often indistinguishable from real pulsar detections. Deciding which candidates should be studied is therefore difficult. Indeed it has become known as the `candidate selection problem'. This thesis presents an interdisciplinary study of the selection problem, with the aim of developing a new method able to mitigate it. Specifically for future pulsar surveys undertaken with the Square kilometre Array (SKA). Through a combination of critical literature evaluations, theoretical modelling exercises, and empirical investigations, the selection problem is described in-depth here for the first time. It is shown to be characterised by the dominance of Gaussian distributed noise signals, a factor that no existing selection method accounts for. It also reveals the presence of a significant trend in survey data rates, which suggest that candidate selection is transitioning from an off-line processing procedure, to an on-line, and real-time, decision making process. In response, a new real-time machine learning based method, the GH-VFDT, is introduced in this thesis. The results presented here show that a significant improvement in selection performance can be achieved using the GH-VFDT, which utilises a learning procedure optimised for data characterised by skewed class distributions. Whilst the principled development of new numerical features that maximise the separation between pulsars and Gaussian noise, have also greatly improved GH-VFDT pulsar recall. It is therefore concluded that the sub-optimal performance of existing selection systems, is due to a combination of poor feature design, insensitivity to noise, and an inability to deal with skewed class distributions.
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Betzwieser, Joseph (Joseph Charles). "Analysis of spatial mode sensitivity of gravitational wave interferometer and targeted search for gravitational radiation from the Crab pulsar." Thesis, Massachusetts Institute of Technology, 2007. http://hdl.handle.net/1721.1/45422.

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Thesis (Ph. D.)--Massachusetts Institute of Technology, Dept. of Physics, February 2008.
Includes bibliographical references (p. 167-171).
Over the last several years the Laser Interferometer Gravitational Wave Observatory (LIGO) has been making steady progress in improving the sensitivities of its three interferometers, two in Hanford, Washington, and one in Livingston, Louisiana. These interferometers have reached their target design sensitivities and have since been collecting data in their fifth science run for well over a year. On the way to increasing the sensitivities of the interferometers, difficulties with increasing the input laser power, due to unexpectedly high optical absorption, required the installation of a thermal compensation system. We describe a frequency resolving wavefront sensor, called the phase camera, which was used on the interferometer to examine the heating effects and corrections of the thermal compensation system. The phase camera was also used to help understand an output mode cleaner which was temporarily installed on the Hanford 4 km interferometer. Data from the operational detectors was used to carry out two continuous gravitational wave searches directed at isolated neutron stars. The first, targeted RX J1856.5-3754, now known to be outside the LIGO detection band, was used as a test of a new multi interferometer search code, and compared it to a well tested single interferometer search code and data analysis pipeline. The second search is a targeted search directed at the Crab pulsar, over a physically motivated parameter space, to complement existing narrow time domain searches. The parameter space was chosen based on computational constraints, expected final sensitivity, and possible frequency differences due to free precession and a simple two component model.
(cont.) An upper limit on the strain of gravitational radiation from the Crab pulsar of 1.6 x 10-24 was found with 95% confidence over a frequency band of 6 x 10-3 Hz centered on twice the Crab pulsar's electromagnetic pulse frequency of 29.78 Hz. At the edges of the parameter space, this search is approximately 105 times more sensitive than the time domain searches. This is a preliminary result, presently under review by the LIGO Scientific Collaboration.
by Joseph Betzwieser.
Ph.D.
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Keane, Evan. "The transient radio sky." Thesis, University of Manchester, 2010. https://www.research.manchester.ac.uk/portal/en/theses/the-transient-radio-sky(37c08735-cd96-4598-a8b9-2d24ef9e871d).html.

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The high time-resolution radio sky represents unexplored astronomical territory where the discovery potential is high. In this thesis I have studied the transient radio sky, focusing on millisecond scales. As such, this work is concerned primarily with neutron stars, the most populous member of the radio transient parameter space. In particular, I have studied the well known radio pulsars and the recently identified group of neutron stars which show erratic radio emission, known as RRATs, which show radio bursts every few minutes to every few hours. When RRATs burst onto the scene in 2006, it was thought that they represented a previously unknown, distinct class of sporadically emitting sources. The difficulty in their identification implies a large underlying population, perhaps larger than the radio pulsars. The first question investigated in this thesis was whether the large projected population of RRATs posed a problem, i.e. could the observed supernova rate account for so many sources. In addition to pulsars and RRATs, the various other known neutron star manifestations were considered, leading to the conclusion that distinct populations would result in a 'birthrate problem'. Evolution between the classes could solve this problem - the RRATs are not a distinct population of neutron stars. Alternatively, perhaps the large projected population of RRATs is an overestimate. To obtain an improved estimate, the best approach is to find more sources. The Parkes Multi-beam Pulsar Survey, wherein the RRATs were initially identified, offered an opportunity to do just this. About half of the RRATs showing bursts during the survey were thought to have been missed, due to the deleterious effects of impulsive terrestrial interference signals. To remove these unwanted signals, so that we could identify the previously shrouded RRATs, we developed new interference mitigation software and processing techniques. Having done this, the survey was completely re-processed, resulting in the discovery of 19 new sources. Of these, 12 have been re-detected on multiple occasions, whereas the others have not been seen to re-emit since the initial discovery observations, and may be very low burst-rate RRATs, or, isolated burst events. These discoveries suggest that the initial population estimate was not over-estimated - RRATs, though not a distinct population, are indeed numerous. In addition to finding new sources, characterisation of their properties is vital. To this end, a campaign of regular radio observations of the newly discovered sources, was mounted, at the Parkes Observatory, in Australia. In addition, some of the initially identified RRATs were observed with the Lovell Telescope at Jodrell Bank. These have revealed glitches in J1819-1458, with anomalous post-glitch recovery of the spin-down rate. If such glitches were common, it would imply that the source was once a magnetar, neutron stars with the strongest known magnetic fields of up to 10¹⁵ gauss. The observations have also been used to perform 'timing' observations of RRATs, i.e. determination of their spin-down characteristics. At the beginning of this thesis, 3 of the original sources had 'timing solutions' determined. This has since risen to 7, and furthermore, 7 of the newly discovered sources now also have timing solutions. With this knowledge, we can see where RRATs lie in period-period derivative space. The Parkes RRATs seem to be roughly classifiable into three groupings, with high observed nulling fractions - normal pulsars, high magnetic field pulsars and old, 'dying' pulsars. It seems that RRATs and pulsars are one and the same. When a pulsar is more easily detected in searches for single bright pulses, as opposed to in periodicity searches, we label it a RRAT. Such searches impart a selection effect on the parameter space of possible sources, in both nulling fraction and rotation period. In this sense, an observational setup could be designed to make any pulsar appear as a RRAT. For realistic survey parameters however, this is not the case, and the groups mentioned above seem to be the most likely to appear as RRATs. In fact, we can utilise RRAT searches to identify neutron stars, difficult to find by other means, in particular high-magnetic field pulsars, and pulsars approaching the pulsar "death valley". Some of the RRATs are well explained as being distant/weak pulsars with a high modulation index, others seem to be nulling pulsars. This highlights the incomplete knowledge of nulling behaviour in the pulsar population. It seems that there may be a continuum of nulling durations, under a number of guises, from 'nulling pulsars' to 'RRATs' to 'intermittent pulsars'. In fact this nulling may fit into the emerging picture, whereby pulsar magnetospheres switch between stable configurations.
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Begin, Steve. "A search for fast pulsars in globular clusters." Thesis, Link to full text, 2006. http://hdl.handle.net/2429/69.

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Van, Heerden Elmarie. "Data challenges in pulsar searches." Thesis, University of Oxford, 2017. https://ora.ox.ac.uk/objects/uuid:98b329d6-4dbf-4956-9277-4b52fa2971bd.

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Technological advances coupled with a decline in digital storage costs have resulted in a profusion of data being created, collected and consumed. These data give rise to new challenges and opportunities in many disciplines ranging from science and engineering to biology and finance. An example of a future project in radio astronomy that promises both Big Data and Big Discoveries is the Square Kilometre Array (SKA) radio telescope project. Astrophysicists are confident that the Big Data amassed by the SKA will not only answer fundamental questions regarding the Universe but also contain big discoveries not yet postulated. The transformational potential of the SKA and its ensuing data and algorithmic challenges, in particular for the discovery and study of pulsars, drive the research of this thesis. Discovering all pulsars beaming towards Earth is one of the key science goals of the SKA. However, in addition to low signal strengths, searching for pulsars is extremely difficult due to the intrinsic weakness of their signals, propagation effects and the presence of anthropogenic interferences. Numerous techniques have been developed to overcome some of these difficulties and to assist in the quest to find more pulsars. However, despite the success of these techniques, the number of pulsars discovered in recent surveys (Swiggum et al. 2014, Lazarus et al. 2015) has fallen well short of the number predicted by pulsar population synthesis models (Lorimer 2011). This shortfall in pulsar detections can be attributed to radio frequency interference (RFI), red noise and scintillation (Lazarus et al. 2015). For this thesis, and in order to investigate and quantify these claims, I first developed a new technique to simulate pulsar search data that contain different types of RFI and varying noise baselines (i.e. red noise). This surrogate modelling technique was then used in a framework that I developed to inexpensively explore the sensitivity of pulsar search pipelines for different noise and RFI settings. The results from this framework highlight the necessity to develop algorithms that are able to identify and remove non-stationary variations from the data before RFI excision and searching is performed in order to limit false positive detections. To address the shortcomings identified with the framework which assessed the performance of existing pulsar search pipelines, I developed a new real-time algorithm for excising RFI while simultaneously normalising the variability in time and frequency inherent to pulsar observations. Processing synthetic data with the algorithm resulted in an expansion of the noise/pulsar spin period parameter space for which we are able to successfully detect pulsars. Furthermore, the algorithm is shown to reduce the number of false positive detections. In conclusion, the insights gained from the work presented in this thesis and the improvements achieved will contribute to the development of a new realtime pulsar search pipeline adept at dealing with the challenges posed by the SKA.
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Chandler, Adam M. Prince Thomas A. "Pulsar searches : from radio to gamma-rays /." Diss., Pasadena, Calif. : California Institute of Technology, 2003. http://resolver.caltech.edu/CaltechETD:etd-01232003-213508.

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Paul, Ralph Paul. "A Search for Relativistic Binary Pulsars in the Galactic Plane." Thesis, University of Manchester, 2009. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.508555.

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Books on the topic "Pulsar Search"

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Robinson, Clive. Searches for radio pulsars in 47 Tucanae and other globular clusters. Manchester: University of Manchester, 1994.

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1938-, Trefil James, ed. Exoplanets: Diamond worlds, super earths, pulsar planets, and the new search for life beyond our solar system. Smithsonian Books, 2017.

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Trefil, James S. Exoplanets: Diamond Worlds, Super Earths, Pulsar Planets, and the New Search for Life beyond Our Solar System. Smithsonian Books, 2018.

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Maggiore, Michele. Gravitational Waves. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198570899.001.0001.

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A comprehensive and detailed account of the physics of gravitational waves and their role in astrophysics and cosmology. The part on astrophysical sources of gravitational waves includes chapters on GWs from supernovae, neutron stars (neutron star normal modes, CFS instability, r-modes), black-hole perturbation theory (Regge-Wheeler and Zerilli equations, Teukoslky equation for rotating BHs, quasi-normal modes) coalescing compact binaries (effective one-body formalism, numerical relativity), discovery of gravitational waves at the advanced LIGO interferometers (discoveries of GW150914, GW151226, tests of general relativity, astrophysical implications), supermassive black holes (supermassive black-hole binaries, EMRI, relevance for LISA and pulsar timing arrays). The part on gravitational waves and cosmology include discussions of FRW cosmology, cosmological perturbation theory (helicity decomposition, scalar and tensor perturbations, Bardeen variables, power spectra, transfer functions for scalar and tensor modes), the effects of GWs on the Cosmic Microwave Background (ISW effect, CMB polarization, E and B modes), inflation (amplification of vacuum fluctuations, quantum fields in curved space, generation of scalar and tensor perturbations, Mukhanov-Sasaki equation,reheating, preheating), stochastic backgrounds of cosmological origin (phase transitions, cosmic strings, alternatives to inflation, bounds on primordial GWs) and search of stochastic backgrounds with Pulsar Timing Arrays (PTA).
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Book chapters on the topic "Pulsar Search"

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Lyne, A. G. "Radio Pulsar Search Techniques." In Gravitational Wave Data Analysis, 95–103. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-1185-7_7.

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Carreto Fidalgo, David. "Search for the Next Very-High-Energy Pulsar." In Revealing the Most Energetic Light from Pulsars and Their Nebulae, 141–55. Cham: Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-030-24194-0_7.

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Azhari, Mourad, Altaf Alaoui, Abdallah Abarda, Badia Ettaki, and Jamal Zerouaoui. "Using Ensemble Methods to Solve the Problem of Pulsar Search." In Big Data and Networks Technologies, 183–89. Cham: Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-030-23672-4_14.

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Wang, Dayang, Qian Yin, and Hongfeng Wang. "Weighting Features Before Applying Machine Learning Methods to Pulsar Search." In IFIP Advances in Information and Communication Technology, 241–47. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-68121-4_26.

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Deelman, Ewa, James Blythe, Yolanda Gil, Carl Kesselman, Scott Koranda, Albert Lazzarini, Gaurang Mehta, Maria Alessandra Papa, and Karan Vahi. "Pegasus and the Pulsar Search: From Metadata to Execution on the Grid." In Parallel Processing and Applied Mathematics, 821–30. Berlin, Heidelberg: Springer Berlin Heidelberg, 2004. http://dx.doi.org/10.1007/978-3-540-24669-5_107.

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Azhari, Mourad, Altaf Alaoui, Abdallah Abarda, Badia Ettaki, and Jamal Zerouaoui. "A Comparison of Random Forest Methods for Solving the Problem of Pulsar Search." In Innovations in Smart Cities Applications Edition 3, 796–807. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-37629-1_57.

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Zhou, Qingyong, Hongfei Ren, Fumei Wu, Jianfeng Ji, Zhenhe Zhai, and Bohao Ban. "The Quick Search Algorithm of Pulsar Period Based on Unevenly Spaced Timing Data." In Lecture Notes in Electrical Engineering, 581–94. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-29187-6_57.

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Keane, Evan Francis. "PMSingle: A Re-Analysis of the Parkes Multi-Beam Pulsar Survey in Search of RRATs." In The Transient Radio Sky, 61–99. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-19627-0_4.

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Fegan, D. J., M. F. Cawley, K. Gibbs, P. W. Gorham, R. C. Lamb, N. A. Porter, P. T. Reynolds, V. J. Stenger, and T. C. Weekes. "Search for a 12.59 ms. Pulsar in Cygnus X-3 at E > 400 GeV." In Very High Energy Gamma Ray Astronomy, 111–14. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3831-1_13.

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Buccheri, R., M. Busetta, and C. M. Carollo. "Search for Bursts of Gamma-Ray Emission from the Crab Pulsar in the Cos-B Data by Adaptive Cluster Analysis." In Data Analysis in Astronomy III, 67–74. Boston, MA: Springer US, 1989. http://dx.doi.org/10.1007/978-1-4684-5646-2_7.

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Conference papers on the topic "Pulsar Search"

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Wang, Haomiao, and Oliver Sinnen. "FPGA based acceleration of FDAS module for Pulsar Search." In 2015 International Conference on Field Programmable Technology (FPT). IEEE, 2015. http://dx.doi.org/10.1109/fpt.2015.7393158.

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Philp, Colin, Dale A. Frail, Charles R. Evans, and Peter J. T. Leonard. "A search for pulsar companions to runaway OB stars." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.45961.

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Baffa, C. "SKA pulsar search: technological challenges and best algorithms development." In SPIE Astronomical Telescopes + Instrumentation, edited by Suzanne K. Ramsay, Ian S. McLean, and Hideki Takami. SPIE, 2014. http://dx.doi.org/10.1117/12.2056561.

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Ray, P. S., J. E. Grove, J. D. Kurfess, T. A. Prince, and M. P. Ulmer. "An OSSE search for the binary radio pulsar 1259−63." In COMPTON GAMMA-RAY OBSERVATORY. AIP, 1993. http://dx.doi.org/10.1063/1.44128.

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Mori, Masaki, and Ken Ebisawa. "Search for a gamma-ray pulsar in the SNR RCW103." In The fourth compton symposium. AIP, 1997. http://dx.doi.org/10.1063/1.54020.

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Joshi, B. C., M. A. McLaughlin, M. Kramer, A. G. Lyne, D. R. Lorimer, D. A. Ludovici, M. Davies, et al. "A 610-MHz Galactic Plane Pulsar Search with the Giant Meterwave Radio Telescope." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900311.

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Alexandreas, D. E., D. Berley, S. D. Biller, R. L. Burman, D. R. Cady, C. Y. Chang, B. L. Dingus, et al. "A search for UHE cosmic ray from the Crab pulsar/nebula." In High Energy Gamma−Ray Astronomy. AIP, 1991. http://dx.doi.org/10.1063/1.40333.

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Potapov, Vladimir A., Marta Burgay, Nicolò D’Amico, Paolo Esposito, Alberto Pellizzoni, and Andrea Possenti. "Sensitivity of pulsar timing observations to low-frequency noise and search for the Gravitational Wave Background using Pulsar Timing Array." In RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE. AIP, 2011. http://dx.doi.org/10.1063/1.3615084.

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Mikami, Ryo, Toshio Terasawa, Shota Kisaka, Hideaki Miyamoto, Katsuaki Asano, Nobuyuki Kawai, Yosuke Yamakoshi, et al. "Search for a Correlation between Giant Radio Pulses and Hard X-Ray Emissions in the Crab Pulsar." In Proceedings of the 12th Asia Pacific Physics Conference (APPC12). Journal of the Physical Society of Japan, 2014. http://dx.doi.org/10.7566/jpscp.1.015106.

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Wang, Haomiao, Ben Stappers, Prabu Thiagaraj, and Oliver Sinnen. "Optimisation of Convolution of Multiple Different Sized Filters in SKA Pulsar Search Engine." In 2018 International Conference on Field-Programmable Technology (FPT). IEEE, 2018. http://dx.doi.org/10.1109/fpt.2018.00073.

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Reports on the topic "Pulsar Search"

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Sasseen, T. P. An optical and near infrared search for a pulsar in Supernova 1987A. Office of Scientific and Technical Information (OSTI), December 1990. http://dx.doi.org/10.2172/6223782.

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Lauer, E. J., G. J. Caporaso, F. W. Chambers, Y.-J. Chen, S. Falabella, G. Guethlein, J. McCarrick, R. Richardson, S. Sampayan, and J. Weir. Search for Defocusing During a Single Pulse of a 2 kA Relativistic Electron Beam Due to Ions Accelerated from a Target. Office of Scientific and Technical Information (OSTI), September 2002. http://dx.doi.org/10.2172/15002787.

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