Confusion noise level due to galactic and extragalactic binaries

Bender, P. L.; Hils, D.

doi:10.1088/0264-9381/14/6/008

Cited by 175 publications

(248 citation statements)

References 12 publications

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“…For close white dwarf binaries (CWDBs) [60,61], this value lies within a factor 2 of [62]. The GCWDBs [58,60,61,62,63,64,65,66,67] include He-He, He-CO and CO-CO white dwarf binaries, as well as a few binaries containing the rarer O/Ne/Mg white dwarfs.…”

Section: Current and Future Detectabilitymentioning

confidence: 99%

“…It is possible that confusion backgrounds are small enough to allow detection for Gµ < 10 −20 if a suitable detector could be built at 0.1 to 1 Hz , with sensitivity enough to resolve all the extragalactic binary sources and reach an instrument noise limit on the order of Ω G h 2 ≈ 10 −15 , the level required to search for inflationary graviton perturbations at zero spectral tilt (see e.g., [53,54] (UB+WUMa+GCWDB+CV) is taken from levels estimated in [60] for the total binary backgrounds, with estimates from [58] for the reduction of confusion noise at higher frequencies by fitting out Galactic binaries. For close white dwarf binaries (CWDBs) [60,61], this value lies within a factor 2 of [62].…”

Section: Current and Future Detectabilitymentioning

confidence: 99%

“…Figure 1 shows the effective confusion noise from both galactic and extragalactic binaries remaining after the resolved binaries have been fitted out of the data record (see e.g. [58,59]). Essentially none of the extragalactic stellar-mass binaries can be resolved with LISA's sensitivity [59] (in contrast to intense signals from an expected small number involving massive black hole binaries).…”

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confidence: 99%

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Gravitational waves from light cosmic strings: Backgrounds and bursts with large loops

Hogan

2006

Phys. Rev. D

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The mean spectrum and burst statistics of gravitational waves produced by a cosmological population of cosmic string loops are estimated using analytic approximations, calibrated with earlier simulations. Formulas are derived showing the dependence of observables on the string tension Gµ, in the regime where newly-formed loops are relatively large, not very much smaller than the horizon. Large loops form earlier, are more abundant, and generate a more intense stochastic background and more frequent bursts than assumed in earlier background estimates, enabling experiments to probe lighter cosmic strings of interest to string theory. Predictions are compared with instrument noise from current and future experiments, and with confusion noise from known astrophysical gravitational wave sources such as stellar and massive black hole binaries.In these large-loop models, current data from millisecond pulsar timing already suggests that Gµ is less than about 10 −10 , close to the minimum value where bursts might be detected by Advanced LIGO, and a typical value expected in strings from brane inflation. Because of confusion noise expected from massive black hole binaries, pulsar techniques will not be able to go below about Gµ ≈ 10 −11 . LISA will be sensitive to stochastic backgrounds created by strings as light as Gµ ≈ 10 −15 , at frequencies where it is limited by confusion noise of Galactic stellar populations; however, for those lightest detectable strings, bursts are rarely detectable. For Gµ > 10 −11 , the stochastic background from strings dominates the LISA noise by a large factor, and burst events may also be detectable by LISA, allowing detailed study of loop behavior. Astrophysical confusion might be low enough at 0.1 to 1 Hz to eventually reach Gµ ≈ 10 −20 with future interferometer technology.

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Section: Current and Future Detectabilitymentioning

confidence: 99%

Section: Current and Future Detectabilitymentioning

confidence: 99%

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confidence: 99%

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Gravitational waves from light cosmic strings: Backgrounds and bursts with large loops

Hogan

2006

Phys. Rev. D

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“…For details on this simulation we refer the reader to [18], and for earlier work to [2,3,4,19,20,21]. The basic ingredient for these simulations is an approximate binary evolution code.…”

Section: White Dwarf Binary Population Distributionmentioning

confidence: 99%

White-dwarf–white-dwarf galactic background in the LISA data

et al. 2005

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LISA (Laser Interferometer Space Antenna) is a proposed space mission, which will use coherent laser beams exchanged between three remote spacecraft to detect and study low-frequency cosmic gravitational radiation. In the low-part of its frequency band, the LISA strain sensitivity will be dominated by the incoherent superposition of hundreds of millions of gravitational wave signals radiated by inspiraling white-dwarf binaries present in our own galaxy. In order to estimate the magnitude of the LISA response to this background, we have simulated a synthesized population that recently appeared in the literature. Our approach relies on entirely analytic expressions of the LISA Time-Delay Interferometric responses to the gravitational radiation emitted by such systems, which allows us to implement a computationally efficient and accurate simulation of the background in the LISA data. We find the amplitude of the galactic white-dwarf binary background in the LISA data to be modulated in time, reaching a minimum equal to about twice that of the LISA noise for a period of about two months around the time when the Sun-LISA direction is roughly oriented towards the Autumn equinox. This suggests that, during this time period, LISA could search for other gravitational wave signals incoming from directions that are away from the galactic plane. Since the galactic white-dwarfs background will be observed by LISA not as a stationary but rather as a cyclostationary random process with a period of one year, we summarize the theory of cyclostationary random processes, present the corresponding generalized spectral method needed to characterize such process, and make a comparison between our analytic results and those obtained by applying our method to the simulated data. We find that, by measuring the generalized spectral components of the white-dwarf background, LISA will be able to infer properties of the distribution of the white-dwarfs binary systems present in our Galaxy.

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“…One of the major challenges that will face GW astronomers is the successful discrimination between instrumental noise, stochastic GW backgrounds, and individual, resolvable GW sources. For example, the population of galactic white dwarf binaries in close orbits will provide a major contribution to the LISA noise curve in the 0.1 − 1 mHz band [2]. At the same time, this confusion "noise" can also be treated as a signal, and its shape and amplitude will provide important information about the distribution and properties of white dwarf binaries in the galaxy (e.g.…”

Section: Introductionmentioning

confidence: 99%

Gravitational-wave background from compact objects embedded in active galactic nuclei accretion disks

2007

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We consider a model in which massive stars form in a self-gravitating accretion disk around an active galactic nucleus (AGN). These stars may evolve and collapse to form compact objects on a time scale shorter than the accretion time, thus producing an important family of sources for LISA. Assuming the compact object formation/inspiral rate is proportional to the steady-state gas accretion rate, we use the intrinsic hard X-ray AGN luminosity function to estimate expected event rates and signal strengths. We find that these sources will produce a continuous low-frequency ( < ∼ 1 mHz) background detectable by LISA if more than ∼ 1% of the accreted matter is in the form of compact objects. For compact objects with masses > ∼ 10M⊙, the last stages of the inspiral events should be resolvable above a few mHz, with rates as high as a few hundred per year.

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Confusion noise level due to galactic and extragalactic binaries

Cited by 175 publications

References 12 publications

Gravitational waves from light cosmic strings: Backgrounds and bursts with large loops

Gravitational waves from light cosmic strings: Backgrounds and bursts with large loops

White-dwarf–white-dwarf galactic background in the LISA data

Gravitational-wave background from compact objects embedded in active galactic nuclei accretion disks

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