Lower frequency companions for the Advanced LIGO gravitational wave interferometric detectors: an observational opportunity?

DeSalvo, R.

doi:10.1088/0264-9381/21/5/113

Cited by 4 publications

(4 citation statements)

References 32 publications

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“…The design of advanced terrestrial GW detector AdLIGO and space detector LISA is well on the way. There are also plans for a new generation of low-frequency underground detectors especially sensitive for lower frequencies (DeSalvo 2004), which might be especially sensitive to PEs, which we will discuss in a separate paper in detail. Finally, there are plans for possible future improvements of space detectors: Decihertz Interferometric Gravitational-wave Observatory (DECIGO) (Seto, Kawamura, & Nakamura 2001), Advanced Laser Interferometer Antenna (ALIA) and the Big Bang Observer (BBO) .…”

Section: Overview Of Gravitational-wave Detectorsmentioning

confidence: 99%

Detection Rate Estimates of Gravity Waves Emitted during Parabolic Encounters of Stellar Black Holes in Globular Clusters

Kocsis

Gáspár

Márka

2006

ApJ

106

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The rapid advance of gravitational-wave (GW) detector facilities makes it very important to estimate the event rates of possible detection candidates. We consider an additional possibility of GW bursts produced during unbound orbits of stellar mass compact objects. We estimate the rate of successful detections for specific detectors: the initial Laser Interferometric Gravitational-Wave Observatory (InLIGO), the French-Italian gravitational-wave antenna VIRGO, the near-future Advanced-LIGO (AdLIGO), the space-based Laser Interferometric Space Antenna (LISA), and the Next Generation LISA (NGLISA). The dominant contribution among unbound orbits that have GW frequencies in the sensitive band of the detectors correspond to near-parabolic encounters (PEs) within globular clusters (GCs). Simple GC models are constructed to account for the compact object mass function, mass segregation, number density distribution, and velocity distribution. We calculate encounters both classically and account for general relativistic corrections by extrapolating the results for infinite mass ratios. We also include the cosmological redshift of waveforms and event rates. We find that typical PEs with masses m 1 = m 2 = 40M ⊙ are detectable with matched filtering over a signal to noise ratio S/N = 5 within a distance d L ∼ 200 Mpc for InLIGO and VIRGO, z = 1 for AdLIGO, 0.4 Mpc for LISA, and 1 Gpc for NGLISA. We estimate single datastream detection rates of 5.5 × 10 −5 yr −1 for InLIGO, 7.2 × 10 −5 yr −1 for VIRGO, 0.063 yr −1 for AdLIGO, 2.9 × 10 −6 yr −1 for LISA, and 1.0 yr −1 for NGLISA, for reasonably conservative assumptions. These estimates are subject to uncertainties in the GC parameters, most importantly the total number and mass-distribution of black holes (BHs) in the cluster core. In reasonably optimistic cases, we get ∼ > 1 detections for AdLIGO per year. We can expect that a coincident analysis using multiple detectors and accounting for GW recoil capture significantly increases the detection rates. We give ready-to-use formulas to recalculate the estimates when these input parameters become better-determined. In addition, we provide the partial detection rates for various masses. The regular detection of GWs during PEs would provide a unique observational probe for constraining the stellar BH mass function of dense clusters.

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Section: Overview Of Gravitational-wave Detectorsmentioning

confidence: 99%

Detection Rate Estimates of Gravity Waves Emitted during Parabolic Encounters of Stellar Black Holes in Globular Clusters

Kocsis

Gáspár

Márka

2006

ApJ

106

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“…Future interferometers could improve this type of measurement, especially if their lowfrequency sensitivity is better [28] so that the mass can be rotated at a lower frequency. In particular, a design study is currently underway for a future underground "Einstein Telescope" [29] with projected sensitivity shown by the lowest curve in figure 2.…”

Section: Discussionmentioning

confidence: 99%

Feasibility of measuring the Shapiro time delay over meter-scale distances

Ballmer

Márka

Shawhan

2010

Class. Quantum Grav.

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The time delay of light as it passes by a massive object, first calculated by Shapiro in 1964, is a hallmark of the curvature of space-time. To date, all measurements of the Shapiro time delay have been made over solar-system distance scales. We show that the new generation of kilometer-scale laser interferometers being constructed as gravitational wave detectors, in particular Advanced LIGO, will in principle be sensitive enough to measure variations in the Shapiro time delay produced by a suitably designed rotating object placed near the laser beam. We show that such an apparatus is feasible (though not easy) to construct, present an example design, and calculate the signal that would be detectable by Advanced LIGO. This offers the first opportunity to measure space-time curvature effects on a laboratory distance scale.

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“…The xylophone concept was first suggested for Advanced LIGO, proposing to complement the standard broadband interferometers with an interferometer optimized for lower frequency, thus enhancing the detection of high-mass binary systems [12][13][14]. The concept was then taken forward for underground observatories [15].…”

Section: Potential Benefits Of Xylophone Configurations For Third-gen...mentioning

confidence: 99%

A xylophone configuration for a third-generation gravitational wave detector

Hild¹,

Chelkowski²,

Freise³

et al. 2009

Class. Quantum Grav.

188

214

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Achieving the demanding sensitivity and bandwidth, envisaged for third generation gravitational wave (GW) observatories, is extremely challenging with a single broadband interferometer. Very high optical powers (Megawatts) are required to reduce the quantum noise contribution at high frequencies, while the interferometer mirrors have to be cooled to cryogenic temperatures in order to reduce thermal noise sources at low frequencies. To resolve this potential conflict of cryogenic test masses with high thermal load, we present a conceptual design for a 2-band xylophone configuration for a third generation GW observatory, composed of a high-power, high-frequency interferometer and a cryogenic low-power, low-frequency instrument. Featuring inspiral ranges of 3200 Mpc and 38000 Mpc for binary neutron stars and binary black holes coalesences, respectively, we find that the potential sensitivity of xylophone configurations can be significantly wider and better than what is possible in a single broadband interferometer.PACS numbers: 04.80. Nn, 07.60.Ly, 95.75.Kk, 95.55.Ym

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Lower frequency companions for the Advanced LIGO gravitational wave interferometric detectors: an observational opportunity?

Cited by 4 publications

References 32 publications

Detection Rate Estimates of Gravity Waves Emitted during Parabolic Encounters of Stellar Black Holes in Globular Clusters

Detection Rate Estimates of Gravity Waves Emitted during Parabolic Encounters of Stellar Black Holes in Globular Clusters

Feasibility of measuring the Shapiro time delay over meter-scale distances

A xylophone configuration for a third-generation gravitational wave detector

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