Sensitivity study using machine learning algorithms on simulated<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>r</mml:mi></mml:math>-mode gravitational wave signals from newborn neutron stars

Mytidis, A.; Panagopoulos, Athanasios Aris; Panagopoulos, Orestis P.; Miller, A.

doi:10.1103/physrevd.99.024024

Cited by 19 publications

(16 citation statements)

References 48 publications

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“…This type of signal can be searched for with techniques developed to detect transient continuous waves lasting O(hours-days) that come from remnants of binary neutron star mergers or supernova [78,79]. Transient continuous waves also follow power laws, but n = 5 or n = 7 for canonical gravitational-wave emission from a deformation [62] or r-modes [80][81][82], respectively, and ḟ is negative.…”

Section: Gravitational Waves From Inspirals: the Signalmentioning

confidence: 99%

Probing planetary-mass primordial black holes with continuous gravitational waves

Miller,

Clesse,

De Lillo

et al. 2020

Preprint

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Gravitational waves can probe the existence of planetary-mass primordial black holes. Considering a mass range of [10 −7 − 10 −2 ]M , inspiraling primordial black holes could emit either continuous gravitational waves, quasi-monochromatic signals that last for many years, or transient continuous waves, signals whose frequency evolution follows a power law and last for O(hours-months). We show that primordial black hole binaries in our galaxy may produce detectable gravitational waves for different mass functions and formation mechanisms. In order to detect these inspirals, we adapt methods originally designed to search for gravitational waves from asymmetrically rotating neutron stars. The first method, the Frequency-Hough, exploits the continuous, quasi-monochromatic nature of inspiraling black holes that are sufficiently light and far apart such that their orbital frequencies can be approximated as linear with a small spin-up. The second method, the Generalized Frequency-Hough, drops the assumption of linearity and allows the signal frequency to follow a power-law evolution. We explore the parameter space to which each method is sensitive, derive a theoretical sensitivity estimate, determine optimal search parameters and calculate the computational cost of all-sky and directed searches. We forecast limits on the abundance of primordial black holes within our galaxy, showing that we can constrain the fraction of dark matter that primordial black holes compose, fPBH, to be fPBH 1 for chirp masses between [4 × 10 −5 − 10 −3 ]M for current detectors. For the Einstein Telescope, we expect the constraints to improve to fPBH 10 −2 for chirp masses between [10 −4 − 10 −3 ]M .

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Section: Gravitational Waves From Inspirals: the Signalmentioning

confidence: 99%

Probing planetary-mass primordial black holes with continuous gravitational waves

Miller,

Clesse,

De Lillo

et al. 2020

Preprint

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“…The kernel moves over subsets of the image and returns a measure of overlap between itself and the image, before this output is fed into an activation function. Convolutions are the mechanism by which the image is passed through each layer of the network, and allow deeper non-linear combinations of the information present in the map than Artificial Neural Networks (ANNs), where a simple matrix dot product is used to push the images through each layer [21,23,24,32].…”

Section: A Convolution Neural Networkmentioning

confidence: 99%

How effective is machine learning to detect long transient gravitational waves from neutron stars in a real search?

et al. 2019

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We present a comprehensive study of the effectiveness of Convolution Neural Networks (CNNs) to detect long duration transient gravitational-wave signals lasting O(hours − days) from isolated neutron stars. We determine that CNNs are robust towards signal morphologies that differ from the training set, and they do not require many training injections/data to guarantee good detection efficiency and low false alarm probability. In fact, we only need to train one CNN on signal/noise maps in a single 150 Hz band; afterwards, the CNN can distinguish signals/noise well in any band, though with different efficiencies and false alarm probabilities due to the non-stationary noise in LIGO/Virgo. We demonstrate that we can control the false alarm probability for the CNNs by selecting the optimal threshold on the outputs of the CNN, which appears to be frequency dependent. Finally we compare the detection efficiencies of the networks to a well-established algorithm, the Generalized FrequencyHough (GFH), which maps curves in the time/frequency plane to lines in a plane that relates to the initial frequency/spindown of the source. The networks have similar sensitivities to the GFH but are orders of magnitude faster to run and can detect signals to which the GFH is blind. Using the results of our analysis, we propose strategies to apply CNNs to a real search using LIGO/Virgo data to overcome the obstacles that we would encounter, such as a finite amount of training data. We then use our networks and strategies to run a real search for a remnant of GW170817, making this the first time ever that a machine learning method has been applied to search for a gravitational wave signal from an isolated neutron star.

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“…Investigations of r-mode gravitational-wave emission (n = 7) are not presented here; such searches are more technically challenging and require different methods that search over a range of frequencies (see, e.g., Mytidis et al 2015Mytidis et al , 2019Abbott et al 2019b;Fesik & Papa 2020a due to uncertainty in gravitational-wave frequency for a given rotation frequency (Andersson et al 2014;Idrisy et al 2015;Caride et al 2019). Nevertheless, we are able to reach below the spindown limit of PSR J0537−6910 for the first time, which means that the minimum amplitude we could detect in our analysis is lower than the one obtained by assuming all of the pulsar's rotational energy loss is converted to gravitational waves (see Section 2.1).…”

Section: Introductionmentioning

confidence: 99%

Diving below the Spin-down Limit: Constraints on Gravitational Waves from the Energetic Young Pulsar PSR J0537-6910

Abbott

Abraham

et al. 2021

ApJL

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We present a search for quasi-monochromatic gravitational-wave signals from the young, energetic X-ray pulsar PSR J0537−6910 using data from the second and third observing runs of LIGO and Virgo. The search is enabled by a contemporaneous timing ephemeris obtained using Neutron star Interior Composition Explorer (NICER) data. The NICER ephemeris has also been extended through 2020 October and includes three new glitches. PSR J0537 −6910 has the largest spin-down luminosity of any pulsar and exhibits fRequent and strong glitches. Analyses of its long-term and interglitch braking indices provide intriguing evidence that its spin-down energy budget may include gravitational-wave emission from a time-varying mass quadrupole moment. Its 62 Hz rotation frequency also puts its possible gravitational-wave emission in the most sensitive band of the LIGO/Virgo detectors. Motivated by these considerations, we search for gravitational-wave emission at both once and twice the rotation frequency from PSR J0537−6910. We find no signal, however, and report upper limits. Assuming a rigidly rotating triaxial star, our constraints reach below the gravitational-wave spin-down limit for this star for the first time by more than a factor of 2 and limit gravitational waves from the l = m = 2 mode to account for less than 14% of the spin-down energy budget. The fiducial equatorial ellipticity is constrained to less than about 3 ×10 −5 , which is the third best constraint for any young pulsar.

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Sensitivity study using machine learning algorithms on simulatedr-mode gravitational wave signals from newborn neutron stars

Cited by 19 publications

References 48 publications

Probing planetary-mass primordial black holes with continuous gravitational waves

Probing planetary-mass primordial black holes with continuous gravitational waves

How effective is machine learning to detect long transient gravitational waves from neutron stars in a real search?

Diving below the Spin-down Limit: Constraints on Gravitational Waves from the Energetic Young Pulsar PSR J0537-6910

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