Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data

By R. V. Haasteren, Y. Levin, G. Janssen, K. Lazaridis, Michael Kramer, B. W. Stappers, G. Desvignes, M. Purver, Andrew G. Lyne, R. Ferdman and 10 more. 2011

215 citations recorded by the source corpus.

The paper ‘Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data’ was published in Mon. Not. R. Astron. Soc. 414, 3117–3128 (2011).

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/eaa933a289d685b71b056fb088715cf89a58ab60

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Citations in the corpus

European Pulsar Timing Array Limits On An Isotropic Stochastic Gravitational-Wave Background (2015, methodology): “…11, 2016 http://m nras.oxfordjournals.org/ D ow nloaded from The most recent limit placed when allowing the intrinsic noise parameters of the pulsars to vary is given by van Haasteren et al. (2011), in which a 95 per cent upper limit of A = 6 × 10−15 was obtained at a spectral index of 13/3.”
The International Pulsar Timing Array: First Data Release (2016, background): “Such a test was already performed on a smaller scale by van Haasteren et al. (2011), who found that for the few pulsars and telescopes they compared, lowfrequency noise models were consistent.”
The NANOGrav 11 Year Data Set: Pulsar-timing Constraints on the Stochastic Gravitational-wave Background (2018, background): “The increasing sensitivity of PTAs is apparent in the evertightening upper limits (van Haasteren et al. 2011; Demorest et al. 2013; Shannon et al. 2013; Lentati et al. 2015; Shannon et al. 2015; Arzoumanian et al. 2016) on the stochastic GWB from the unresolved superposition of SMBHB signals out to…”
The Parkes Pulsar Timing Array Project (2006, background): “…detections will be possible even if the GW background is relatively weak, enabling accurate measurement of properties such as spectral index and possible origin of the background (e.g., van Haasteren et al. 2011) and investigation of non-GR effects in the received signals (e.g., Lee et al. 2008).”
Gravitational-wave sensitivity curves (2014, background): “There are published limits on the amplitude of the stochastic background from all three detectors: the most recent from EPTA is van Haasteren et al (2011), from PPTA 5 http://www.epta.eu.org/ 6 http://www.atnf.csiro.au/research/pulsar/ppta/ 7 http://nanograv.org/ is Shannon et al (2013) and from…”
On the maximal strength of a first-order electroweak phase transition and its gravitational wave signal (2018, background): “In the Figure we show explicitly the current and future sensitivities (see also [88]) of the European Pulsar Timing Array (EPTA) [89] and LIGO [90–92], as well as the projected sensitivities of LISA [93], the Einstein Telescope (ET) [94, 95], the Cosmic Explorer (CE) [96], and the Square Kilometre A”
Searching for the Nano-Hertz Stochastic Gravitational Wave Background with the Chinese Pulsar Timing Array Data Release I (2023, methodology): “…to account for inaccuracies in the process of TOA extraction using the template-matching method (Taylor 1992), EQUAD adds white noise in quadrature (van Haasteren et al. 2011), and ECORR (NANOGrav Collaboration et al. 2015) models the correlated white noise (phase jitter) among different…”
The European Pulsar Timing Array and the Large European Array for Pulsars (2013, methodology): “Finally, the first limits on the stochastic GWB using EPTA data were published by van Haasteren et al (2011).”
Measurement and correction of variations in interstellar dispersion in high-precision pulsar timing (2012, methodology): “…Timing Array (PPTA; Manchester et al. 2012), aim to use MSPs to detect red signals such as errors in the atomic time standard (Hobbs et al. 2012); errors in the Solar system ephemeris (Champion et al. 2010) or the effect of gravitational waves (Yardley et al. 2010, 2011; van Haasteren et al. 2011).”
Systematic investigation of the expected gravitational wave signal from supermassive black hole binaries in the pulsar timing band (2012, methodology): “Note that this latter upper bound is only a factor 1.5 below the best limit placed by van Haasteren et al. (2011).”