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Keywords
(13)
Data Analysis
Data Analysis Methods
Data Management
Followup Study
Gravitational Radiation
Gravitational Wave Detector
Gravitational Wave
Mass Spectrometer
Matched Filter
Parameter Space
Confidence Level
Low Mass X Ray Binary
Neutron Star
Related Publications
(3)
Data analysis of gravitationalwave signals from spinning neutron stars: The signal and its detection
First allsky upper limits from LIGO on the strength of periodic gravitational waves using the Hough transform
Pulsars ellipticity revised
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Searches for periodic gravitational waves from unknown isolated sources and Scorpius X1: Results from the second LIGO science run
Searches for periodic gravitational waves from unknown isolated sources and Scorpius X1: Results from the second LIGO science run,10.1103/PhysRevD.76
Edit
Searches for periodic gravitational waves from unknown isolated sources and Scorpius X1: Results from the second LIGO science run
(
Citations: 24
)
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B. Abbott
,
R. Abbott
,
R. Adhikari
,
J. Agresti
,
P. Ajith
,
B. Allen
,
R. Amin
,
S. B. Anderson
,
W. G. Anderson
,
M. Arain
,
M. Araya
,
H. Armandula
http://academic.research.microsoft.com/io.ashx?type=5&id=6799242&selfId1=0&selfId2=0&maxNumber=12&query=
We carry out two searches for periodic gravitational waves using the most sensitive few hours of data from the second {LIGO} science run. Both searches exploit fully coherent matched filtering and cover wide areas of parameter space, an innovation over previous analyses which requires considerable algorithm development and computational power. The first search is targeted at isolated, previously unknown neutron stars, covers the entire sky in the frequency band 160728.8 Hz, and assumes a frequency derivative of less than 4 x 10(10) Hz/s. The second search targets the accreting
neutron star
in the lowmass xray binary Scorpius X1 and covers the frequency bands 464484 Hz and 604624 Hz as well as the two relevant binary orbit parameters. Because of the high computational cost of these searches we limit the analyses to the most sensitive 10 hours and 6 hours of data, respectively. Given the limited sensitivity and duration of the analyzed data set, we do not attempt deep followup studies. Rather we concentrate on demonstrating the
data analysis
method on a real data set and present our results as upper limits over large volumes of the parameter space. In order to achieve this, we look for coincidences in
parameter space
between the Livingston and Hanford 4km interferometers. For isolated neutron stars our 95\%
confidence level
upper limits on the
gravitational wave
strain amplitude range from 6.6 x 10(23) to 1 x 10(21) across the frequency band; for Scorpius X1 they range from 1.7 x 10(22) to 1.3 x 10(21) across the two 20Hz frequency bands. The upper limits presented in this paper are the first broadband wide
parameter space
upper limits on periodic gravitational waves from coherent search techniques. The methods developed here lay the foundations for upcoming hierarchical searches of more sensitive data which may detect astrophysical signals.
Journal:
Physical Review D  PHYS REV D
, vol. 76, no. 8, 2007
DOI:
10.1103/PhysRevD.76.082001
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Citation Context
(3)
...where α ∼ 0.6 and h160 ∼ 10 −22 , see [
34
]...
...Note that reducing the observation time has 2 effects: the first one is to drop the GW strength relative to the detector sensitivity since h160 is proportional to T −1/2 obs [
34
]...
Florian Dubath
,
et al.
Periodic gravitational waves from small cosmic string loops
...The LIGO Scientific Collaboration (LSC) has so far published three types of searches for periodic gravitational waves (GWs): searches for known nonaccreting pulsars [1–4], for the nonpulsing lowmass xray binary Sco X1 [
5
, 6] and allsky searches for as yet unknown neutron stars [5, 7–9]...
...The first and last types of searches are approaching the indirect upper limits on gravitational wave emission inferred from the observed spindowns (spin frequency derivatives) of pulsars and supernovabased estimates of the neutron star population of the galaxy [
5
]...
...where � is the equatorial ellipticity, Izz is the principal moment of inertia (assumed constant) and f is the gravitational wave frequency (assumed to be twice the spin frequency) [
5
, 16]...
...where D is the distance of the source [
5
, 17]...
...spinning significantly more slowly than it was at birth, we can relate the frequency evolution to the characteristic age τ and braking index n by [
5
, 18, 19]...
...We therefore use the fully coherent Fstatistic search [
5
], as implemented by the ComputeFStatistic v2 routine in the LSC Algorithm Library [28]...
...The computation is conducted in the frequency domain using short Fourier transforms (SFTs) of segments of strain data, typically of 30 min duration so that the GW frequency will remain in one frequency bin over the length of the SFT [
5
]...
...In the event no plausible signal is found, we will set upper limits by methods similar to the frequentist analyses in [1,
5
]. These are based on Monte Carlo simulations searching the data for a multitude of softwareinjected signals with a distribution of amplitudes, inclination angles and polarization angles in each frequency bin...
Unknown.
Searching for gravitational waves from Cassiopeia A with LIGO
...Three techniques that trade off between sensitivity and computation have been implemented: (1) semicoherent, long duration allsky searches sensitive only to power and neglecting phase using the entire data set [86]; (2) coherent, shortduration allsky searches sensitive to amplitude and phase but computationally limited to ≈5000 h integration time [
87
]; (3) coherent, targeted searches for millisecond radio pulsars with accurate and ...
Unknown.
LIGO: the Laser Interferometer GravitationalWave Observatory
References
(2)
Introduction to Solid State Physics
(
Citations: 5748
)
C. Kittel
Published in 1968.
Introduction to Solid State Physics
(
Citations: 227
)
Kittel Charles
,
Mceuen Paul
Published in 2005.
Sort by:
Citations
(24)
Gravitational waves from neutron stars: promises and challenges
(
Citations: 1
)
N. Andersson
,
V. Ferrari
,
D. I. Jones
,
K. D. Kokkotas
,
B. Krishnan
,
J. S. Read
,
L. Rezzolla
,
B. Zink
Journal:
General Relativity and Gravitation  GEN RELATIV GRAVIT
, vol. 43, no. 2, pp. 409436, 2011
Current status of gravitational wave observations
(
Citations: 1
)
Stephen Fairhurst
,
Gianluca M. Guidi
,
Patrice Hello
,
John T. Whelan
,
Graham Woan
Journal:
General Relativity and Gravitation  GEN RELATIV GRAVIT
, vol. 43, no. 2, pp. 387407, 2011
Gravitational wave emission from rotating superfluid neutron stars
(
Citations: 2
)
D. I. Jones
Journal:
Monthly Notices of The Royal Astronomical Society  MON NOTIC ROY ASTRON SOC
, vol. 402, no. 4, pp. 25032519, 2010
Sinking of a magnetically confined mountain on an accreting neutron star
(
Citations: 1
)
K. Wette
,
M. Vigelius
,
A. Melatos
Journal:
Monthly Notices of The Royal Astronomical Society  MON NOTIC ROY ASTRON SOC
, vol. 402, no. 2, pp. 10991110, 2010
LIGO: the Laser Interferometer GravitationalWave Observatory
(
Citations: 36
)
B. P. Abbott
,
R. Abbott
,
R. Adhikari
,
P. Ajith
,
B. Allen
,
G. Allen
,
R. S. Amin
,
S. B. Anderson
,
W. G. Anderson
,
M. A. Arain
,
M. Araya
,
H. Armandula
http://academic.research.microsoft.com/io.ashx?type=5&id=5664483&selfId1=0&selfId2=0&maxNumber=12&query=
Journal:
Reports on Progress in Physics  REP PROGR PHYS
, vol. 72, no. 7, 2009