Direct observational upper limit to gravitational radiation from millisecond pulsar PSR1937 + 214

Hough, J.; Drever, R. W. P.; Ward, H.; Munley, A. J.; Newton, G.; Meers, B. J.; Hoggan, S.; Kerr, G. A.

doi:10.1038/303216a0

Cited by 11 publications

(4 citation statements)

References 6 publications

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“…A specific attempt to search for gravitational waves from the Crab pulsar at a frequency of 60 Hz was, however, made with a specially designed aluminum quadrupole antenna [9,10] giving a 1 upper limit of h 0 2 10 ÿ22 . A search for gravitational waves from what was then the fastest millisecond pulsar, PSR J1939 2134, was conducted by Hough et al [11] using a split bar detector, producing an upper limit of h 0 < 10 ÿ20 .…”

Section: B Previous Resultsmentioning

confidence: 99%

Upper limits on gravitational wave emission from 78 radio pulsars

Abbott¹,

Abbott²,

Adhikari³

et al. 2007

Phys. Rev. D

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134

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We present upper limits on the gravitational wave emission from 78 radio pulsars based on data from the third and fourth science runs of the LIGO and GEO 600 gravitational wave detectors. The data from both runs have been combined coherently to maximize sensitivity. For the first time, pulsars within binary (or multiple) systems have been included in the search by taking into account the signal modulation due to their orbits. Our upper limits are therefore the first measured for 56 of these pulsars. For the remaining 22, our results improve on previous upper limits by up to a factor of 10. For example, our tightest upper limit on the gravitational strain is 2:6 10 ÿ25 for PSR J1603 ÿ 7202, and the equatorial ellipticity of PSR J2124-3358 is less than 10 ÿ6 . Furthermore, our strain upper limit for the Crab pulsar is only 2.2 times greater than the fiducial spin-down limit.

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Section: B Previous Resultsmentioning

confidence: 99%

Upper limits on gravitational wave emission from 78 radio pulsars

Abbott¹,

Abbott²,

Adhikari³

et al. 2007

Phys. Rev. D

Self Cite

134

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“…Searches for neutron stars emitting quasi-monochromatic, continuous gravitational waves using the LIGO, Virgo, GEO600 or TAMA interferometers' data have been carried out for over a decade [1][2][3][4][5][6][7][8][9][10][11][12][13]. Other searches have been performed using prototype interferometers [14][15][16] and by so-called bar detectors [17][18][19]. The different search strategies for detecting this type of gravitational radiation can be classified into three general categories: a targeted search for a known neutron star, a directed search at a particular sky location, or a search for unknown neutron stars over the entire sky.…”

Section: Introductionmentioning

confidence: 99%

“…For the first type of search, a known neutron star (typically observed as a radio-pulsar), either isolated or in a binary system, with a well-known ephemeris describing the rotation of the source, can be targeted using methods searching over a very narrow range of parameters [1,2,5,11,13,17]. The second strategy is the one in which a search for continuous gravitational waves from a particular sky location that contains a potential source-or many sources-of gravitational wave signals (e.g., Sco X-1, the supernova remnant Cassiopeia A, the galactic center, or globular clusters) are targeted by algorithms that search over a wider range of parameters [10,19].…”

Section: Introductionmentioning

confidence: 99%

An all-sky search algorithm for continuous gravitational waves from spinning neutron stars in binary systems

Goetz¹,

Riles²

2011

Class. Quantum Grav.

134

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Rapidly spinning neutron stars with non-axisymmetric mass distributions are expected to generate quasi-monochromatic continuous gravitational waves. While many searches for unknown, isolated spinning neutron stars have been carried out, there have been no previous searches for unknown sources in binary systems. Since current search methods for unknown, isolated neutron stars are already computationally limited, expanding the parameter space searched to include binary systems is a formidable challenge. We present a new hierarchical binary search method called TwoSpect, which exploits the periodic orbital modulations of the continuous waves by searching for patterns in doubly Fourier-transformed data. We will describe the TwoSpect search pipeline, including its mitigation of detector noise variations and corrections for Doppler frequency modulation caused by changing detector velocity. Tests on Gaussian noise and on a set of simulated signals will be presented.PACS numbers: 95.30. Sf, 95.75.Pq, 95.85.Sz, 04.30.Tv, 04.40.Dg ‡ The Australian National Telescope Facility maintains a database of all known radio pulsars at

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“…Bar detectors: an earlier attempt to specifically target the Crab pulsar (at f = 2ν ∼ 60 Hz) was made with a specially-designed bar detector [74], setting an upper limit of h 0 ∼ 2 × 10 −22 . A search targeting the millisecond pulsar PSR B1937+21 (at f = 2ν ∼ 1284 Hz) was performed by [46] using a split bar detector, producing an upper limit of h 0 ∼ 10 −20 . A search for unknown isolated neutron stars in a small frequency-band f = (921.35 ± 0.03) Hz and a small sky-region in the galactic center was performed using 95 days of data from the EXPLORER bar detector, and an upper limit of h 0 ∼ 3 × 10 −24 was obtained [17].…”

Section: Previous Upper Limits From Other Detectorsmentioning

confidence: 99%

Gravitational Waves from Spinning Neutron Stars

Prix

Neutron Stars and Pulsars

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This paper gives an introductory overview of the search for continuous gravitational waves from spinning neutron stars. We review the current theoretical understanding of possible emission mechanisms and the expected strength of signals received on Earth. Given the substantial uncertainties involved in neutron star physics, these searches-if sufficiently sensitive-can provide important new information and constraints about neutron star physics even in the absence of detection. We describe the challenging detection problem of such extremely weak signals and introduce some of the basic data analysis concepts and methods used. We conclude by summarizing the current status of the sensitivities and upper limits achieved so far. These results suggest that the search for spinning neutron stars using LIGO-I is already entering a regime of "astrophysical relevance". Developments in the near future make a detection of this type of source increasingly plausible.

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Direct observational upper limit to gravitational radiation from millisecond pulsar PSR1937 + 214

Cited by 11 publications

References 6 publications

Upper limits on gravitational wave emission from 78 radio pulsars

Upper limits on gravitational wave emission from 78 radio pulsars

An all-sky search algorithm for continuous gravitational waves from spinning neutron stars in binary systems

Gravitational Waves from Spinning Neutron Stars

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