D. Stinebring

Publications (8)6.02 Total impact

• Source

  Available from: A. Brazier

  Article: Limits on the Stochastic Gravitational Wave Background from the North American Nanohertz Observatory for Gravitational Waves

  P. B. Demorest, R. D. Ferdman, M. E. Gonzalez, D. Nice, S. Ransom, I. H. Stairs, Z. Arzoumanian, A. Brazier, S. Burke-Spolaor, S. J. Chamberlin, [......], J. Lazio, A. N. Lommen, M. McLaughlin, N. Palliyaguru, D. Perrodin, R. M. Shannon, X. Siemens, D. Stinebring, J. Swiggum, W. W. Zhu
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  ABSTRACT: We present an analysis of high-precision pulsar timing data taken as part of the North American Nanohertz Observatory for Gravitational waves (NANOGrav) project. We have observed 17 pulsars for a span of roughly five years using the Green Bank and Arecibo radio telescopes. We analyze these data using standard pulsar timing models, with the addition of time-variable dispersion measure and frequency-variable pulse shape terms. Sub-microsecond timing residuals are obtained in nearly all cases, and the best root-mean-square timing residuals in this set are ~30-50 ns. We present methods for analyzing post-fit timing residuals for the presence of a gravitational wave signal with a specified spectral shape. These optimally take into account the timing fluctuation power removed by the model fit, and can be applied to either data from a single pulsar, or to a set of pulsars to detect a correlated signal. We apply these methods to our dataset to set an upper limit on the strength of the nHz-frequency stochastic supermassive black hole gravitational wave background of h_c (1 yr^-1) < 7x10^-15 (95%). This result is dominated by the timing of the two best pulsars in the set, PSRs J1713+0747 and J1909-3744.
  01/2012;
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  Available from: Daniel Roger Billing Yardley

  Article: The international pulsar timing array project: using pulsars as a gravitational wave detector

  G. Hobbs, A. Archibald, Z. Arzoumanian, D. Backer, M. Bailes, N. D. R. Bhat, M. Burgay, S. Burke-Spolaor, D. Champion, I. Cognard, [......], X. Siemens, I. Stairs, B. Stappers, D. Stinebring, G. Theureau, R. van Haasteren, W. van Straten, J. P. W. Verbiest, D. R. B. Yardley, X. P. You
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  ABSTRACT: The International Pulsar Timing Array project combines observations of pulsars from both Northern and Southern hemisphere observatories with the main aim of detecting ultra-low frequency (~10^-9 to 10^-8 Hz) gravitational waves. Here we introduce the project, review the methods used to search for gravitational waves emitted from coalescing supermassive binary black-hole systems in the centres of merging galaxies and discuss the status of the project. Comment: accepted by Classical and Quantum Gravity. Review talk for the Amaldi8 conference series
  11/2009;
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  Available from: Lee Samuel Finn

  Article: The North American Nanohertz Observatory for Gravitational Waves

  F. Jenet, L. S. Finn, J. Lazio, A. Lommen, M. McLaughlin, I. Stairs, D. Stinebring, J. Verbiest, A. Archibald, Z. Arzoumanian, [......], P. Freire, M. Gonzalez, V. Kaspi, V. Kondratiev, D. Lorimer, R. Lynch, D. Nice, S. Ransom, R. Shannon, X. Siemens
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  ABSTRACT: The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) is a consortium of astronomers whose goal is the creation of a galactic scale gravitational wave observatory sensitive to gravitational waves in the nHz-microHz band. It is just one component of an international collaboration involving similar organizations of European and Australian astronomers who share the same goal. Gravitational waves, a prediction of Einstein's general theory of relativity, are a phenomenon of dynamical space-time generated by the bulk motion of matter, and the dynamics of space-time itself. They are detectable by the small disturbance they cause in the light travel time between some light source and an observer. NANOGrav exploits radio pulsars as both the light (radio) source and the clock against which the light travel time is measured. In an array of radio pulsars gravitational waves manifest themselves as correlated disturbances in the pulse arrival times. The timing precision of today's best measured pulsars is less than 100 ns. With improved instrumentation and signal-to-noise it is widely believed that the next decade could see a pulsar timing network of 100 pulsars each with better than 100 ns timing precision. Such a pulsar timing array (PTA), observed with a regular cadence of days to weeks, would be capable of observing supermassive black hole binaries following galactic mergers, relic radiation from early universe phenomena such as cosmic strings, cosmic superstrings, or inflation, and more generally providing a vantage on the universe whose revolutionary potential has not been seen in the 400 years since Galileo first turned a telescope to the heavens. Comment: This document is the NANOGrav consortium's submission to Astro2010's Program Prioritization Panel on Particle Astrophysics and Gravitation
  09/2009;
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  Available from: arxiv.org

  Article: LOFAR: A powerful tool for pulsar studies

  B. W. Stappers, A. G. J. van Leeuwen, M Kramer, D. Stinebring, J. Hessels
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  ABSTRACT: The LOw Frequency ARray, LOFAR, will have the sensitivity, bandwidth, frequency range and processing power to revolutionise low-frequency pulsar studies. We present results of simulations that indicate that a LOFAR survey will find approximately 1500 new pulsars. These new pulsars will give us a much better understanding of the low end of the luminosity function and thus allow for a much more precise estimate of the true total local pulsar population. The survey will also be very sensitive to the ultra-steep spectrum pulsars, RRATs, and the pulsed radio emission from objects like Geminga and AXPs. We will also show that by enabling us to observe single pulses from hundreds of pulsars, including many millisecond pulsars, LOFAR opens up new possibilities for the study of emission physics.
  02/2007;
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  Available from: Richard A. Fallows

  Article: International Colloquium "Scattering and Scintillation in Radio Astronomy" was held on June 19-23, 2006 in Pushchino, Moscow region, Russia

  V. I. Shishov, W. A. Coles, B. J. Rickett, M. K. Bird, A. I. Efimov, L. N. Samoznaev, V. K. Rudash, I. V. Chashei, D. Plettemeier, S. R. Spangler, [......], H. E. Bignall, J. -P. Macquart, L. Kedziora-Chudczer, T. V. Smirnova, V. M. Malofeev, O. I. Malov, S. A. Tyulbashev, A. Jessner, W. Sieber, R. Wielebinski
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  ABSTRACT: Topics of the Colloquium: a) Interplanetary scintillation b) Interstellar scintillation c) Modeling and physical origin of the interplanetary and the interstellar plasma turbulence d) Scintillation as a tool for investigation of radio sources e) Seeing through interplanetary and interstellar turbulent media Ppt-presentations are available on the Web-site: http://www.prao.ru/conf/Colloquium/main.html
  10/2006;
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  Available from: arxiv.org

  Article: Nanoarcsecond single-dish imaging of the Vela pulsar

  J. -P. Macquart, S. Johnston, M Walker, D. Stinebring
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  ABSTRACT: We have measured the properties of the diffractive scintillation toward the Vela pulsar under the extremely strong scattering conditions encountered at 660 MHz. We obtain a decorrelation bandwidth of $\nu_d = 244 \pm 4$ Hz and diffractive decorrelation timescale of $t_{\rm diff} = 3.3\pm 0.3$ s. Our measurement of the modulation indices $m=0.87\pm 0.003\pm 0.05$ and $m=0.93\pm 0.03 \pm 0.05$ (one for each polarization stream), are at variance with the modulation index of the Vela pulsar obtained at 2.3 GHz by Gwinn et al. (1997) {\it if} the deviation from a modulation index of unity is ascribed to a source size effect.
  02/2000;
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  Available from: articles.adsabs.harvard.edu

  Article: Time asymmetries in pulsar signals

  D. Stinebring, J. M. Cordes
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  ABSTRACT: The paper presents a technique for analyzing time asymmetries of stochastic processes and applies it to high time resolution data from pulsars PSR 0950+08 and PSR 2016+28. Subpulses and average waveforms show similar time asymmetries. This is consistent with subpulses arising from beams of radiation rather than temporal modulations. Micropulses are, on average, time symmetric. It is possible that individual micropulses are asymmetric, but over a data set of several hundred pulses, there is no preferred sense of asymmetry.
  The Astrophysical Journal 09/1981; 249:704-719. · 6.02 Impact Factor
• Article: Measurements of the interstellar turbulent plasma spectrum of PSR B0329+54 using multi-frequency observations of interstellar scintillation

  V. I. Shishov, T. V. Smirnova, W. Sieber, V. M. Malofeev, V. A. Potapov, D. Stinebring, M Kramer, A. Jessner, R. Wielebinski
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  ABSTRACT: Interstellar scintillation multi-frequency observations of PSR 0329+54 in the frequency range from 102 MHz to 5 GHz were analysed to estimate the spectrum of interstellar plasma inhomogeneities in the direction of this pulsar. Based on the theory of diffractive scintillation, the composite structure function of phase fluctuations covering a large range of turbulence scales was constructed. We found that the spectrum is well described by a power law with $n = 3.5$ for scales from $10^6$ to $10^9$ m, which differs from the value known for a Kolmogorov spectrum. We can, however, within the accuracy of our data not exclude a Kolmogorov spectrum. It became also clear that angular refraction of emission must be taken into account to fit the data points at all observing frequencies. The size of the irregularities responsible for the angular refraction is estimated to be about $3\times 10^{13}$ m. They can be identified with clouds of neutral hydrogen that can be considered as holes of electron density.
  http://dx.doi.org/10.1051/0004-6361:20030480.