Determination of dark energy by the Einstein Telescope: Comparing with CMB, BAO, and SNIa observations

Zhao, Wen; Broeck, C. Van Den; Baskaran, D.; Li, T. G. F.

doi:10.1103/physrevd.83.023005

Cited by 239 publications

(495 citation statements)

References 65 publications

(79 reference statements)

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“…Its noise spectrum is given in Ref. [62]. We found that ℓ u = 5.6 × 10 3 µm with SNR=93, which is much weaker than the one from the table-top experiment.…”

Section: Conclusion and Discussionmentioning

confidence: 81%

Probing the size of extra dimensions with gravitational wave astronomy

2011

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In Randall-Sundrum II (RS-II) braneworld model, it has been conjectured according to the AdS/CFT correspondence that brane-localized black hole (BH) larger than the bulk AdS curvature scale ℓ cannot be static, and it is dual to a four dimensional BH emitting the Hawking radiation through some quantum fields. In this scenario, the number of the quantum field species is so large that this radiation changes the orbital evolution of a BH binary. We derived the correction to the gravitational waveform phase due to this effect and estimated the upper bounds on ℓ by performing Fisher analyses. We found that DECIGO/BBO can put a stronger constraint than the current table-top result by detecting gravitational waves from small mass BH/BH and BH/neutron star (NS) binaries. Furthermore, DECIGO/BBO is expected to detect 10 5 BH/NS binaries per year. Taking this advantage, we found that DECIGO/BBO can actually measure ℓ down to ℓ = 0.33µm for 5 year observation if we know that binaries are circular a priori. This is about 40 times smaller than the upper bound obtained from the table-top experiment. On the other hand, when we take eccentricities into binary parameters, the detection limit weakens to ℓ = 1.5µm due to strong degeneracies between ℓ and eccentricities. We also derived the upper bound on ℓ from the expected detection number of extreme mass ratio inspirals (EMRIs) with LISA and BH/NS binaries with DECIGO/BBO, extending the discussion made recently by McWilliams [1]. We found that these less robust constraints are weaker than the ones from phase differences.

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“…Its noise spectrum is given in Ref. [62]. We found that ℓ u = 5.6 × 10 3 µm with SNR=93, which is much weaker than the one from the table-top experiment.…”

Section: Conclusion and Discussionmentioning

confidence: 81%

Probing the size of extra dimensions with gravitational wave astronomy

2011

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“…(5). For instance, a coincident observation of a GRB and a GW [18,27,31,45] implies a priori knowledge of the sky position and redshift of the GW source. Therefore, it is equivalent to imposing p(z, α, δ|I) = δ(z − z GRB )δ(α − α GRB )δ(δ − δ GRB ) where α GRB , δ GRB and z GRB are sky position and redshift of the observed GRB.…”

Section: Methodsmentioning

confidence: 99%

“…As the GW error-box is ≈ 1 − 100 deg 2 , direct redshift measurements may be very challenging, despite optimistic assumptions made by several authors. For example, if short-lived Gamma Ray Bursts (GRB) are associated to the merger of compact objects with at least a neutron star component, this would provide such a measurement [27,31,45]. However, regardless of the still open debate on whether short GRB progenitors are indeed compact binaries, the fraction of coalescing systems producing a short GRBs might be as low as 10 −2 [5].…”

Section: Introductionmentioning

confidence: 99%

Inference of cosmological parameters from gravitational waves: Applications to second generation interferometers

2012

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The advanced world-wide network of gravitational waves (GW) observatories is scheduled to begin operations within the current decade. Thanks to their improved sensitivity, they promise to yield a number of detections and thus to open a new observational windows for astronomy and astrophysics. Among the scientific goals that should be achieved, there is the independent measurement of the value of the cosmological parameters, hence an independent test of the current cosmological paradigm. Due to the importance of such task, a number of studies have evaluated the capabilities of GW telescopes in this respect. However, since GW do not yield information about the source redshift, different groups have made different assumptions regarding the means through which the GW redshift can be obtained. These different assumptions imply also different methodologies to solve this inference problem. This work presents a formalism based on Bayesian inference developed to facilitate the inclusion of all assumptions and prior information about a GW source within a single data analysis framework. This approach guarantees the minimisation of information loss and the possibility of including naturally event-specific knowledge (such as the sky position for a Gamma Ray Burst -GW coincident observation) in the analysis. The workings of the method are applied to a specific example, loosely designed along the lines of the method proposed by Schutz in 1986, in which one uses information from wide-field galaxy surveys as prior information for the location of a GW source. I show that combining the results from few tens of observations from a network of advanced interferometers will constrain the Hubble constant H0 to an accuracy of ∼ 4 − 5% at 95% confidence.PACS numbers: 95.85. Sz,

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“…Indeed, space observatories such as DECIGO [4], the Big Bang Observer (BBO) [10] and AS-TROD [11], currently in the planning stage, are likely to have a directional sensitivity of a few arc seconds or better, in which case one might expect only a single galaxy to fall within the field of view for a large fraction of observing directions [13]. These space based observatories are expected to measure the equation of state of dark energy to an unprecedented accuracy [13,15]. Although BBO/DECIGO experiments are in reality at a conceptual stage, for the purpose of this paper we treat the above mentioned characteristics as a generic stand in for a future highly advanced gravitational-wave mission and use the label BBO/DECIGO as a convenient abbreviation for such a mission.…”

Section: Figmentioning

confidence: 99%

Reconstructing the properties of dark energy using standard sirens

2013

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Future space-based gravity wave experiments such as the Big Bang Observatory (BBO), with their excellent projected, one sigma angular resolution, will measure the luminosity distance to a large number of gravity wave (GW) sources to high precision, and the redshift of the single galaxies in the narrow solid angles towards the sources will provide the redshifts of the gravity wave sources. One sigma BBO beams contain the actual source only in 68 per cent cases; the beams that do not contain the source may contain a spurious single galaxy, leading to misidentification. To increase the probability of the source falling within the beam, larger beams have to be considered, decreasing the chances of finding single galaxies in the beams. Saini, Sethi and Sahni (2010) argued, largely analytically, that identifying even a small number of GW source galaxies furnishes a rough distance-redshift relation, which could be used to further resolve sources that have multiple objects in the angular beam. In this work we further develop this idea by introducing a self-calibrating iterative scheme which works in conjunction with Monte-Carlo simulations to determine the luminosity distance to GW sources with progressively greater accuracy. This iterative scheme allows one to determine the equation of state of dark energy to within an accuracy of a few percent for a gravity wave experiment possessing a beam width an order of magnitude larger than BBO (and therefore having a far poorer angular resolution). This is achieved with no prior information about the nature of dark energy from other data sets such as SN Ia, BAO, CMB etc.A remarkable property of our universe is that it is accelerating. The cause of cosmic acceleration is presently unknown and theorists have speculated that it might be due to the presence of the cosmological constant, an all pervasive scalar field called Quintessence, a Born-Infeld type scalar called the Chaplygin gas, etc. It has also been suggested that modifications to the gravity sector of the theory, such as extra dimensional 'braneworld' models or f (R) theories, might be responsible for cosmic acceleration. Establishing the nature and cause of cosmic acceleration is clearly a paramount objective of modern cosmology [1,2]. Standard candles in the form of type Ia supernovae (SNIa) and standard rulers such as baryon acoustic oscillations (BAO) observed in the clustering of galaxies, have played a key role in garnering support for the accelerating universe hypothesis. Standard candles rely on an accurate determination of the luminosity distance to infer the expansion history and to make a case for cosmic acceleration. As pointed out in [3][4][5][6][7] a complementary probe of the expansion history is available in the form of gravitational radiation emitted from compact binary objects such as neutron star -neutron star (NS-NS) binaries, neutron star -black hole (NS-BH) binaries, or black hole -black hole (BH-BH) binaries.Indeed, it appears that if the underlying physics behind gravitational radiation emitted by...

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Determination of dark energy by the Einstein Telescope: Comparing with CMB, BAO, and SNIa observations

Cited by 239 publications

References 65 publications

Probing the size of extra dimensions with gravitational wave astronomy

Probing the size of extra dimensions with gravitational wave astronomy

Inference of cosmological parameters from gravitational waves: Applications to second generation interferometers

Reconstructing the properties of dark energy using standard sirens

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