Gravitational wave astronomy with the SKA

Janssen, G. H.; Hobbs, G.; McLaughlin, Maura; Bassa, C. G.; Deller, Adam T.; Krämer, M.; Lee, K.J.; Mingarelli, Chiara M. F.; Rosado, P. A.; Sanidas, S.; Sesana, Alberto; Shao, Lijing; Stairs, I. H.; Stappers, B. W.; Verbiest, J. P. W.

doi:10.48550/arxiv.1501.00127

Cited by 53 publications

(75 citation statements)

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“…The PTA will start to 'hit the signal' at much higher frequencies (f > 10 −8 Hz), where it is also likely to see individual sources and not only an unresolved GWB. We notice, nonetheless, that these numbers are quite less optimistic that those quoted in Janssen et al (2015). This is because, in that paper, both the GWB and single sources are said to be detectable if the produced S/N is larger than 4.…”

Section: Detection Probability As a Function Of Timementioning

confidence: 68%

“…However, it turns out that this is not sufficiently stringent for claiming a confident detection of a single source. One should consider the results of this work as an update to those claimed in Janssen et al (2015), keeping in mind some important caveats related to the possible resolution of multiple sources that we will discuss in Section 4.…”

Section: Detection Probability As a Function Of Timementioning

confidence: 85%

“…By inspecting the upper plot in Figure 4, one could claim that the detection of a single binary is currently (by ≈ 10 yr of observing time span for the IPTA) more likely than that of a background, since the average S/NS is larger than S/NB. Moreover, if one assumes that a detection is achieved as soon as the S/N surpasses a certain threshold (for example 4, as in Janssen et al 2015), one would also claim that detecting a single SBHB is more likely than detecting a GWB for the two SKA configurations considered. However, both claims would be wrong; as we mentioned in Section 2, the detectability should be evaluated in terms of the DP, and, as shown in Figure 2, the probability of detecting a GWB is in all cases (for all PTAs and observing times considered) larger than that of detecting a single SBHB.…”

Section: S/nmentioning

confidence: 99%

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Expected properties of the first gravitational wave signal detected with pulsar timing arrays

Rosado

Sesana

Gair

2015

Monthly Notices of the Royal Astronomical Society

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In this paper we attempt to investigate the nature of the first gravitational wave (GW) signal to be detected by pulsar timing arrays (PTAs): will it be an individual, resolved supermassive black hole binary (SBHB), or a stochastic background made by the superposition of GWs produced by an ensemble of SBHBs? To address this issue, we analyse a broad set of simulations of the cosmological population of SBHBs, that cover the entire parameter space allowed by current electromagnetic observations in an unbiased way. For each simulation, we construct the expected GW signal and identify the loudest individual sources. We then employ appropriate detection statistics to evaluate the relative probability of detecting each type of source as a function of time for a variety of PTAs; we consider the current International PTA, and speculate into the era of the Square Kilometre Array. The main properties of the first detectable individual SBHBs are also investigated. Contrary to previous work, we cast our results in terms of the detection probability (DP), since the commonly adopted criterion based on a signal-to-noise ratio threshold is statistic-dependent and may result in misleading conclusions for the statistics adopted here. Our results confirm quantitatively that a stochastic signal is more likely to be detected first (with between 75 to 93 per cent probability, depending on the array), but the DP of single-sources is not negligible. Our framework is very flexible and can be easily extended to more realistic arrays and to signal models including environmental coupling and SBHB eccentricity.

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Section: Detection Probability As a Function Of Timementioning

confidence: 68%

Section: Detection Probability As a Function Of Timementioning

confidence: 85%

Section: S/nmentioning

confidence: 99%

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Expected properties of the first gravitational wave signal detected with pulsar timing arrays

Rosado

Sesana

Gair

2015

Monthly Notices of the Royal Astronomical Society

Self Cite

194

235

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show abstract

“…The gravitational wave signal of Set 1 is within the reach of future experiments such as LISA [64,65], DECIGO [66,67], and BBO [68][69][70]. For Set 2, the signal crosses the sensitivity bound of SKA [136][137][138] in addition to that of LISA, DECIGO, and BBO. FIG.…”

Section: Detectability Of Induced Gravitational Wavesmentioning

confidence: 91%

Primordial blackholes from Gauss-Bonnet-corrected single field inflation

Kawai,

Kim

2021

Preprint

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Primordial blackholes formed in the early Universe via gravitational collapse of over-dense regions may contribute a significant amount to the present dark matter relic density. Inflation provides a natural framework for the production mechanism of primordial blackholes. For example, single field inflation models with a fine-tuned scalar potential may exhibit a period of ultra-slow-roll, during which the curvature perturbation may be enhanced to become seeds of the primordial blackholes formed as the corresponding scales reenter the horizon. In this work we propose an alternative mechanism for the primordial blackhole formation. We consider a model in which a scalar field is coupled to the Gauss-Bonnet term, and show that primordial blackholes may be seeded when a scalar potential term and the Gauss-Bonnet coupling term are nearly balanced. Large curvature perturbation in this model not only leads to the production of primordial blackholes but it also sources gravitational waves at the second order. We calculate the present density parameter of the gravitational waves and discuss the detectability of the signals by comparing them with sensitivity bounds of future gravitational wave experiments.

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“…1, we show the spectrum of GWs in terms of Ω gw • h 2 0 , where h 0 ≈ 0.7 is the dimensionless Hubble constant, for different Gµ l and f peak . We compare it with the sensitivity of current and future detectors: LIGO [24,25], Einstein Telescope (ET) [26], Cosmic Explorer (CE) [27], DECIGO [28], LISA [29,30], and PTAs [6,31,32]. For the peak frequency lying in the ranges 10 −9 Hz f peak 10 −7 Hz and 10 −5 Hz f peak 100 Hz, one will be able to probe melting strings with an initial tension as large as Gµ l 10 −6 .…”

Section: Prospects For Observationsmentioning

confidence: 99%

Gravitational waves from melting cosmic strings

Emond,

Ramazanov,

Samanta

2021

Preprint

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Appearance of cosmic strings in the early Universe is a common manifestation of new physics typically linked to some high energy scale. In this paper, we discuss a different situation, where a model underlying cosmic string formation is approximately scale free. String tension is naturally related to the square of the temperature of the hot primordial plasma in such a setting, and hence decreases with (cosmic) time. With gravitational backreaction neglected, the dynamics of these melting strings in an expanding Universe is equivalent to the dynamics of constant tension strings in a Minkowski spacetime. We provide an estimate for the emission of gravitational waves from string loops. Contrary to the standard case, the resulting spectrum is markedly non-flat and has a characteristic falloff at frequencies below the peak one. The peak frequency is defined by the underlying model and lies in the range accessible by the future detectors for very weak couplings involved.

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Gravitational wave astronomy with the SKA

Cited by 53 publications

References 0 publications

Expected properties of the first gravitational wave signal detected with pulsar timing arrays

Expected properties of the first gravitational wave signal detected with pulsar timing arrays

Primordial blackholes from Gauss-Bonnet-corrected single field inflation

Gravitational waves from melting cosmic strings

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