Einstein Telescope Bibliography

In the following table the main papers produced thanks to the ET research activity or of interest for the ET project are listed

Author	Title	Year	Journal/Proceedings	Reftype	DOI/URL
Acernese, F. & others	Measurements of Superattenuator seismic isolation by Virgo interferometer [Abstract] [BibTeX]	2010	Astroparticle Physics Vol. 33(3), pp. 182 - 189	article	DOI URL
Abstract: Each mirror of the interferometric gravitational wave antenna Virgo is attached to a Superattenuator, a chain of mechanical filters designed to suppress seismic vibrations, starting from a few Hz. The filter chain attenuation has been measured by exciting its suspension point with sinuisodal forces and using the interferometer as sensor. The attenuation, measured at different frequencies, is compliant with the requirements of the next generation antenna Advanced Virgo. In the third generation detector Einstein Telescope, the attenuation is sufficient above 3?Hz, independently of the underground site choice.
BibTeX: @article{Acernese2010, author = {F. Acernese and others}, title = {Measurements of Superattenuator seismic isolation by Virgo interferometer}, journal = {Astroparticle Physics}, year = {2010}, volume = {33}, number = {3}, pages = {182 - 189}, url = {http://www.sciencedirect.com/science/article/B6TJ1-4Y8G5TJ-1/2/36f5cd85cb5f9260c680fe904db69f4e}, doi = {DOI: 10.1016/j.astropartphys.2010.01.006} }
Andersson, N., Ferrari, V., Jones, D., Kokkotas, K., Krishnan, B., Read, J., Rezzolla, L. & Zink, B.	Gravitational waves from neutron stars: promises and challenges [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-28	article	URL
Abstract: We discuss different ways that neutron stars can generate gravitational waves, describe recent improvements in modelling the relevant scenarios in the context of improving detector sensitivity, and show how observations are beginning to test our understanding of fundamental physics. The main purpose of the discussion is to establish promising science goals for third-generation ground-based detectors, like the Einstein Telescope, and identify the various challenges that need to be met if we want to use gravitational-wave data to probe neutron star physics.
BibTeX: @article{springerlink:10.1007/s10714-010-1059-4, author = {Andersson, N. and Ferrari, V. and Jones, D. and Kokkotas, K. and Krishnan, B. and Read, J. and Rezzolla, L. and Zink, B.}, title = {Gravitational waves from neutron stars: promises and challenges}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-28}, note = {10.1007/s10714-010-1059-4}, url = {http://dx.doi.org/10.1007/s10714-010-1059-4} }
Arun, K.G. & Will, C.M.	Bounding the mass of the graviton with gravitational waves: effect of higher harmonics in gravitational waveform templates [Abstract] [BibTeX]	2009	Classical and Quantum Gravity Vol. 26(15), pp. 155002	article	URL
Abstract: Observations by laser interferometric detectors of gravitational waves from inspiraling compact binary systems can be used to search for a dependence of the waves' propagation speed on wavelength, and thereby to bound the mass or Compton wavelength of a putative graviton. We study the effect of including higher harmonics, as well as their post-Newtonian amplitude corrections, in the template gravitational waveforms employed in the process of parameter estimation using matched filtering. We consider the bounds that could be achieved using advanced LIGO, a proposed third generation instrument called an Einstein telescope and the proposed space interferometer LISA. We find that in all cases, the bounds on the graviton Compton wavelength are improved by almost an order of magnitude for higher masses when amplitude corrections are included.
BibTeX: @article{Arun2009, author = {K G Arun and Clifford M Will}, title = {Bounding the mass of the graviton with gravitational waves: effect of higher harmonics in gravitational waveform templates}, journal = {Classical and Quantum Gravity}, year = {2009}, volume = {26}, number = {15}, pages = {155002}, url = {http://stacks.iop.org/0264-9381/26/i=15/a=155002} }
Beker, M., Cella, G., DeSalvo, R., Doets, M., Grote, H., Harms, J., Hennes, E., Mandic, V., Rabeling, D., van den Brand, J. & van Leeuwen, C.	Improving the sensitivity of future GW observatories in the 1–10 Hz band: Newtonian and seismic noise [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-34	article	URL
Abstract: The next generation gravitational wave interferometric detectors will likely be underground detectors to extend the GW detection frequency band to frequencies below the Newtonian noise limit. Newtonian noise originates from the continuous motion of the Earth’s crust driven by human activity, tidal stresses and seismic motion, and from mass density fluctuations in the atmosphere. It is calculated that on Earth’s surface, on a typical day, it will exceed the expected GW signals at frequencies below 10 Hz. The noise will decrease underground by an unknown amount. It is important to investigate and to quantify this expected reduction and its effect on the sensitivity of future detectors, to plan for further improvement strategies. We report about some of these aspects. Analytical models can be used in the simplest scenarios to get a better qualitative and semi-quantitative understanding. As more complete modeling can be done numerically, we will discuss also some results obtained with a finite-element-based modeling tool. The method is verified by comparing its results with the results of analytic calculations for surface detectors. A key point about noise models is their initial parameters and conditions, which require detailed information about seismic motion in a real scenario. We will describe an effort to characterize the seismic activity at the Homestake mine which is currently in progress. This activity is specifically aimed to provide informations and to explore the site as a possible candidate for an underground observatory. Although the only compelling reason to put the interferometer underground is to reduce the Newtonian noise, we expect that the more stable underground environment will have a more general positive impact on the sensitivity. We will end this report with some considerations about seismic and suspension noise.
BibTeX: @article{springerlink:10.1007/s10714-010-1011-7, author = {Beker, M. and Cella, G. and DeSalvo, R. and Doets, M. and Grote, H. and Harms, J. and Hennes, E. and Mandic, V. and Rabeling, D. and van den Brand, J. and van Leeuwen, C.}, title = {Improving the sensitivity of future GW observatories in the 1–10 Hz band: Newtonian and seismic noise}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-34}, note = {10.1007/s10714-010-1011-7}, url = {http://dx.doi.org/10.1007/s10714-010-1011-7} }
Beker, M.G., van den Brand, J.F.J., Hennes, E. & Rabeling, D.S.	Towards time domain finite element analysis of gravity gradient noise [Abstract] [BibTeX]	2010	Journal of Physics: Conference Series Vol. 228(1), pp. 012034	article	URL
Abstract: Gravity gradient noise generated by seismic displacements constitute a limiting factor for the sensitivity of ground based gravitational wave detectors at frequencies below 10 Hz. We present a finite element framework to calculate the soil response to various excitations. The accompanying gravity gradients as a result of the seismic displacement field can then be evaluated. The framework is first shown to accurately model seismic waves in homogenous media. Calculations of the gravity gradient noise are then shown to be in agreement with previous analytical results. Finally results of gravity gradient noise from a single pulse excitation of a homogenous medium are discussed.
BibTeX: @article{1742-6596-228-1-012034, author = {M G Beker and J F J van den Brand and E Hennes and D S Rabeling}, title = {Towards time domain finite element analysis of gravity gradient noise}, journal = {Journal of Physics: Conference Series}, year = {2010}, volume = {228}, number = {1}, pages = {012034}, url = {http://stacks.iop.org/1742-6596/228/i=1/a=012034} }
Bosi, L. & Porter, E.	Data analysis challenges for the Einstein Telescope [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-17	article	URL
Abstract: The Einstein Telescope is a proposed third generation gravitational wave detector that will operate in the region of 1 Hz to a few kHz. As well as the inspiral of compact binaries composed of neutron stars or black holes, the lower frequency cut-off of the detector will open the window to a number of new sources. These will include the end stage of inspirals, plus merger and ringdown of intermediate mass black holes, where the masses of the component bodies are on the order of a few hundred solar masses. There is also the possibility of observing intermediate mass ratio inspirals, where a stellar mass compact object inspirals into a black hole which is a few hundred to a few thousand times more massive. In this article, we investigate some of the data analysis challenges for the Einstein Telescope such as the effects of increased source number, the need for more accurate waveform models and the some of the computational issues that a data analysis strategy might face.
BibTeX: @article{springerlink:10.1007/s10714-010-1084-3, author = {Bosi, Leone and Porter, Edward}, title = {Data analysis challenges for the Einstein Telescope}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-17}, note = {10.1007/s10714-010-1084-3}, url = {http://dx.doi.org/10.1007/s10714-010-1084-3} }
van den Brand, J.F.J., Beker, M.G., Doets, M., Hennes, E. & Rabeling, D.S.	Einstein telescope site selection: Seismic and gravity gradient noise [Abstract] [BibTeX]	2010	Journal of Physics: Conference Series Vol. 203(1), pp. 012076	article	URL
Abstract: Gravity gradient noise generated by seismic displacements may be the limiting factor for the sensitivity of third-generation gravitational wave detectors at frequencies below 10 Hz. A finite element framework has been developed to calculate the soil response to various excitations. The accompanying gravity gradients as a result of the seismic displacement field can then be evaluated. The results of the gravity gradient noise are in good agreement with previous analytical results. Finally results of gravity gradient noise from a single pulse excitation of a homogenous medium are discussed for an underground detector.
BibTeX: @article{Brand2010, author = {J F J van den Brand and M G Beker and M Doets and E Hennes and D S Rabeling}, title = {Einstein telescope site selection: Seismic and gravity gradient noise}, journal = {Journal of Physics: Conference Series}, year = {2010}, volume = {203}, number = {1}, pages = {012076}, url = {http://stacks.iop.org/1742-6596/203/i=1/a=012076} }
Broeck, C.V.D.	Compact binary coalescence and the science case for Einstein Telescope [Abstract] [BibTeX]	2010	arXiv:1003.1386v1 [gr-qc]	article	URL
Abstract: Einstein Telescope (ET) is a possible third generation ground-based gravitational wave observatory for which a design study is currently being carried out. A brief (and non-exhaustive) overview is given of ET's projected capabilities regarding astrophysics and cosmology through observations of inspiraling and coalescing compact binaries. In particular, ET would give us unprecedented insight into the mass function of neutron stars and black holes, the internal structure of neutron stars, the evolution of coalescence rates over cosmological timescales, and the geometry and dynamics of the Universe as a whole
BibTeX: @article{Broeck2010, author = {Chris Van Den Broeck}, title = {Compact binary coalescence and the science case for Einstein Telescope}, journal = {arXiv:1003.1386v1 [gr-qc]}, year = {2010}, note = {(Very) brief summary of a talk given at the 12th Marcel Grossmann meeting; to appear in the Proceedings}, url = {http://arxiv.org/abs/1003.1386v1} }
Broeck, C.V.D. & Sengupta, A.S.	Phenomenology of amplitude-corrected post-Newtonian gravitational waveforms for compact binary inspiral: I. Signal-to-noise ratios [Abstract] [BibTeX]	2007	Classical and Quantum Gravity Vol. 24, pp. 155-176	article	DOI URL
Abstract: We study the phenomenological consequences of amplitude-corrected post-Newtonian (PN) gravitational waveforms, as opposed to the more commonly used restricted PN waveforms, for the quasi-circular, adiabatic inspiral of compact binary objects. In the case of initial detectors it has been shown that the use of amplitude-corrected waveforms for detection templates would lead to significantly lower signal-to-noise ratios (SNRs) than those suggested by simulations based exclusively on restricted waveforms. We further elucidate the origin of the effect by an in-depth analytic treatment. The discussion is extended to advanced detectors, where new features emerge. Non-restricted waveforms are linear combinations of harmonics in the orbital phase, and in the frequency domain the kth harmonic is cut off at kfLSO, with fLSO the orbital frequency at the last stable orbit. As a result, with non-restricted templates it is possible to achieve sizeable signal-to-noise ratios in cases where the dominant harmonic (which is the one at twice the orbital phase) does not enter the detector's bandwidth. This will have important repercussions on the detection of binary inspirals involving intermediate-mass black holes. For sources at a distance of 100 Mpc, taking into account the higher harmonics will double the mass reach of Advanced LIGO, and that of EGO gets tripled. Conservative estimates indicate that the restricted waveforms underestimate detection rates for intermediate mass binary inspirals by at least a factor of 20.
BibTeX: @article{Broeck2007, author = {Chris Van Den Broeck and Anand S Sengupta}, title = {Phenomenology of amplitude-corrected post-Newtonian gravitational waveforms for compact binary inspiral: I. Signal-to-noise ratios}, journal = {Classical and Quantum Gravity}, year = {2007}, volume = {24}, pages = {155-176}, url = {http://www.iop.org/EJ/abstract/0264-9381/24/1/009/}, doi = {http://dx.doi.org/ 10.1088/0264-9381/24/1/009} }
Chandra Kant Mishra, K.G. Arun, B.R.I.B.S.S.	Parametrized tests of post-Newtonian theory using Advanced LIGO and Einstein Telescope [Abstract] [BibTeX]	2010	arXiv:1005.0304v1 [gr-qc]	article	URL
Abstract: General relativity has very specific predictions for the gravitational waveforms from inspiralling compact binaries obtained using the post-Newtonian (PN) approximation. We investigate the extent to which the measurement of the PN coefficients, possible with the second generation gravitational wave detectors such as the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) and the third generation gravitational-wave detectors such as the Einstein Telescope (ET), could be used to test post-Newtonian theory and to put bounds on a class of theories which differ from general relativity in a parametrized sense. We demonstrate this possibility by employing the best inspiralling waveform models for nonspinning compact binaries which is 3.5PN accurate in phase and 3PN in amplitude. Advanced LIGO can test the theory at 1.5PN and thus the leading tail term. Future observations of stellar mass black hole binaries by ET can test the consistency between the various PN coefficients in the GW phasing over the mass range of $11$-$44 M_. The choice of the lower frequency cutoff is important for testing post-Newtonian theory using the ET.
BibTeX: @article{ChandraKantMishra2010, author = {Chandra Kant Mishra, K. G. Arun, Bala R. Iyer, B. S. Sathyaprakash}, title = {Parametrized tests of post-Newtonian theory using Advanced LIGO and Einstein Telescope}, journal = {arXiv:1005.0304v1 [gr-qc]}, year = {2010}, url = {http://arxiv.org/abs/1005.0304v1} }
Chassande-Mottin, E., Hendry, M., Sutton, P. & Márka, S.	Multimessenger astronomy with the Einstein Telescope [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-28	article	URL
Abstract: Gravitational waves (GWs) are expected to play a crucial role in the development of multimessenger astrophysics. The combination of GW observations with other astrophysical triggers, such as from gamma-ray and X-ray satellites, optical/radio telescopes, and neutrino detectors allows us to decipher science that would otherwise be inaccessible. In this paper, we provide a broad review from the multimessenger perspective of the science reach offered by the third generation interferometric GW detectors and by the Einstein Telescope (ET) in particular. We focus on cosmic transients, and base our estimates on the results obtained by ET’s predecessors GEO, LIGO, and Virgo.
BibTeX: @article{springerlink:10.1007/s10714-010-1019-z, author = {Chassande-Mottin, Eric and Hendry, Martin and Sutton, Patrick and Márka, Szabolcs}, title = {Multimessenger astronomy with the Einstein Telescope}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-28}, note = {10.1007/s10714-010-1019-z}, url = {http://dx.doi.org/10.1007/s10714-010-1019-z} }
Chen, Y., Danilishin, S., Khalili, F. & Müller-Ebhardt, H.	QND measurements for future gravitational-wave detectors [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-24	article	URL
Abstract: Second-generation interferometric gravitational-wave detectors will be operating at the Standard Quantum Limit (SQL), a sensitivity limitation set by the trade off between measurement accuracy and quantum back action, which is governed by the Heisenberg Uncertainty Principle. We review several schemes that allows the quantum noise of interferometers to surpass the SQL significantly over a broad frequency band. Such schemes may be an important component of the design of third-generation detectors.
BibTeX: @article{springerlink:10.1007/s10714-010-1060-y, author = {Chen, Yanbei and Danilishin, Stefan and Khalili, Farid and Müller-Ebhardt, Helge}, title = {QND measurements for future gravitational-wave detectors}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-24}, note = {10.1007/s10714-010-1060-y}, url = {http://dx.doi.org/10.1007/s10714-010-1060-y} }
Chen, Y., Danilishin, S.L., Khalili, F.Y. & Müller-Ebhardt, H.	QND measurements for future gravitational-wave detectors [Abstract] [BibTeX]	2009	arXiv:0910.0319v2 [gr-qc]	article	URL
Abstract: Second-generation interferometric gravitational-wave detectors will be operating at the Standard Quantum Limit, a sensitivity limitation set by the trade off between measurement accuracy and quantum back action, which is governed by the Heisenberg Uncertainty Principle. We review several schemes that allows the quantum noise of interferometers to surpass the Standard Quantum Limit significantly over a broad frequency band. Such schemes may be an important component of the design of third-generation detectors.
BibTeX: @article{Chen2009, author = {Yanbei Chen and Stefan L. Danilishin and Farid Ya. Khalili and Helge Müller--Ebhardt}, title = {QND measurements for future gravitational-wave detectors}, journal = {arXiv:0910.0319v2 [gr-qc]}, year = {2009}, url = {http://arxiv.org/pdf/0910.0319v2} }
Cokelaer, T. & Pathak, D.	Searching for gravitational-wave signals emitted by eccentric compact binaries using a non-eccentric template bank: implications for ground-based detectors [Abstract] [BibTeX]	2009	Classical and Quantum Gravity Vol. 26(4), pp. 045013	article	URL
Abstract: Most of the inspiralling compact binaries are expected to be circularized by the time their gravitational-wave signals enter the frequency band of ground-based detectors such as LIGO or VIRGO. However, it is not excluded that some of these binaries might still possess a significant eccentricity at a few tens of hertz. Despite this possibility, current search pipelinesâ€”based on matched filtering techniquesâ€”consider only non-eccentric templates. The effect of such an approximation on the loss of signal-to-noise ratio (SNR) has been investigated by Martel and Poisson (1999 Phys. Rev. D 60 124008) in the context of initial LIGO detector. They ascertained that non-eccentric templates will be successful at detecting eccentric signals. We revisit their work by incorporating current and future ground-based detectors and precisely quantify the exact loss of SNR. In order to be more faithful to an actual search, we maximized the SNR over a template bank, whose minimal match is set to 95%. For initial LIGO detector, we claim that the initial eccentricity does not need to be taken into account in our searches for any system with total mass M ##IMG## [http://ej.iop.org/icons/Entities/in.gif] in [2â€“45] M ##IMG## [http://ej.iop.org/icons/Entities/odot.gif] odot if e 0 ##IMG## [http://ej.iop.org/icons/Entities/lsim.gif] lsim 0.05 because the loss of SNR (about 5%) is consistent with the discreteness of the template bank. Similarly, this statement is also true for systems with M ##IMG## [http://ej.iop.org/icons/Entities/in.gif] in [6â€“35] M ##IMG## [http://ej.iop.org/icons/Entities/odot.gif] odot and e 0 ##IMG## [http://ej.iop.org/icons/Entities/lsim.gif] lsim 0.10. However, by neglecting the eccentricity in our searches, significant loss of detection (larger than 10%) may arise as soon as e 0 â‰¥ 0.05 for neutron-star binaries. We also provide exhaustive results for VIRGO, Advanced LIGO and Einstein Telescope detectors. It is worth noting that for Einstein Telescope, neutron star binaries with e 0 â‰¥ 0.02 lead to a 10% loss of detection.
BibTeX: @article{Cokelaer2009, author = {T Cokelaer and D Pathak}, title = {Searching for gravitational-wave signals emitted by eccentric compact binaries using a non-eccentric template bank: implications for ground-based detectors}, journal = {Classical and Quantum Gravity}, year = {2009}, volume = {26}, number = {4}, pages = {045013}, url = {http://stacks.iop.org/0264-9381/26/i=4/a=045013} }
Eberle, T., Steinlechner, S., Bauchrowitz, J., Händchen, V., Vahlbruch, H., Mehmet, M., Müller-Ebhardt, H. & Schnabel, R.	Quantum Enhancement of the Zero-Area Sagnac Interferometer Topology for Gravitational Wave Detection [Abstract] [BibTeX]	2010	Phys. Rev. Lett. Vol. 104(25), pp. 251102	article	DOI URL
Abstract: Only a few years ago, it was realized that the zero-area Sagnac interferometer topology is able to perform quantum nondemolition measurements of position changes of a mechanical oscillator. Here, we experimentally show that such an interferometer can also be efficiently enhanced by squeezed light. We achieved a nonclassical sensitivity improvement of up to 8.2 dB, limited by optical loss inside our interferometer. Measurements performed directly on our squeezed-light laser output revealed squeezing of 12.7 dB. We show that the sensitivity of a squeezed-light enhanced Sagnac interferometer can surpass the standard quantum limit for a broad spectrum of signal frequencies without the need for filter cavities as required for Michelson interferometers. The Sagnac topology is therefore a powerful option for future gravitational-wave detectors, such as the Einstein Telescope, whose design is currently being studied
BibTeX: @article{PhysRevLett.104.251102, author = {Eberle, Tobias and Steinlechner, Sebastian and Bauchrowitz, Jöran and Händchen, Vitus and Vahlbruch, Henning and Mehmet, Moritz and Müller-Ebhardt, Helge and Schnabel, Roman}, title = {Quantum Enhancement of the Zero-Area Sagnac Interferometer Topology for Gravitational Wave Detection}, journal = {Phys. Rev. Lett.}, publisher = {American Physical Society}, year = {2010}, volume = {104}, number = {25}, pages = {251102}, url = {http://link.aps.org/doi/10.1103/PhysRevLett.104.251102}, doi = {http://dx.doi.org/10.1103/PhysRevLett.104.251102} }
Falferi, P.	Testing the intrinsic noise of a coilâ€“magnet actuator for cryogenic gravitational wave interferometers [Abstract] [BibTeX]	2011	Classical and Quantum Gravity Vol. 28(14), pp. 145005	article	URL
Abstract: The third generation gravitational wave interferometers that will operate underground and at cryogenic temperatures will need a complex and sophisticated control system to satisfy the requirements on the alignment and position of its optics and keep the detector at its working point. The force actuators of the control systems of the present interferometers are for the most part coilâ€“magnet actuators. To check the possibility of using these actuators also at low temperature we have tested the magnetization and the magnetization noise of an SmCo magnet at 4.2 K. The magnetization loss, measured with a fluxgate magnetometer, is 7%. The magnetization noise has been measured with a superconducting quantum interference device magnetometer. The application of dc and ac (0.1 Hz) magnetic fields of an amplitude comparable to that needed to produce on the magnet a force large enough for the control system does not change the measured noise. The equivalent maximum force noise produced by the actuator as a result of the magnetization noise of the magnet has been evaluated. Its effect on the sensitivity of a third generation interferometer (Einstein Telescope) is negligible with respect to the most relevant fundamental noise contributions.
BibTeX: @article{0264-9381-28-14-145005, author = {Paolo Falferi}, title = {Testing the intrinsic noise of a coilâ€“magnet actuator for cryogenic gravitational wave interferometers}, journal = {Classical and Quantum Gravity}, year = {2011}, volume = {28}, number = {14}, pages = {145005}, url = {http://stacks.iop.org/0264-9381/28/i=14/a=145005} }
Falta, D., Fisher, R. & Khanna, G.	Gravitational Wave Emission from the Single-Degenerate Channel of Type Ia Supernovae [Abstract] [BibTeX]	2011	arXiv:1011.6387v1 [astro-ph.HE]	article	URL
Abstract: The thermonuclear explosion of a C/O white dwarf as a Type Ia supernova (SN Ia) generates a kinetic energy comparable to that released by a massive star during a SN II event. Current observations and theoretical models have established that SNe Ia are asymmetric, and therefore -- like SNe II -- potential sources of gravitational wave (GW) radiation. We establish an upper-bound GW amplitude and expected frequency range based upon the energetics and nucleosynthetic yields of SNe Ia. We perform the first detailed calculations of the gravitationally-confined detonation (GCD) mechanism within the single-degenerate channel of SNe Ia. The GCD mechanism predicts a strongly-polarized GW burst from the SD channel of SNe Ia in the frequency band around 1 Hz. Third-generation spaceborne GW observatories currently in planning, including the Big Bang Observer (BBO), and the Deci-Hertz Interferometer Gravitational Wave Observatory (DECIGO), as well as earthbound instruments, including the Einstein Telescope (ET), may be able to detect the signal predicted by the GCD mechanism from galactic SNe Ia and nearby extragalactic SNe Ia at distances up to 1 Mpc. If observable, GWs may offer a direct probe into the first few seconds of SNe Ia, and yield insights into its underlying detonation mechanism not possible in the optical portion of the spectrum.
BibTeX: @article{Falta2011, author = {Falta, David and Fisher, Robert and Khanna, Gaurav}, title = {Gravitational Wave Emission from the Single-Degenerate Channel of Type Ia Supernovae}, journal = {arXiv:1011.6387v1 [astro-ph.HE]}, year = {2011}, url = {http://arxiv.org/pdf/1011.6387v1} }
Freise, A., Chelkowski, S., Hild, S., Pozzo, W.D., Perreca, A. & Vecchio, A.	Triple Michelson interferometer for a third-generation gravitational wave detector [Abstract] [BibTeX]	2009	Classical and Quantum Gravity Vol. 26(8), pp. 085012 (14pp)	article	URL
Abstract: The upcoming European design study 'Einstein gravitational-wave Telescope' represents the first step towards a substantial, international effort for the design of a third-generation interferometric gravitational wave detector. It is generally believed that third-generation instruments might not be installed into existing infrastructures but will provoke a new search for optimal detector sites. Consequently, the detector design could be subject to fewer constraints than the on-going design of the second-generation instruments. In particular, it will be prudent to investigate alternatives to the traditional L-shaped Michelson interferometer. In this paper, we review an old proposal to use three Michelson interferometers in a triangular configuration. We use this example of a triple Michelson interferometer to clarify the terminology and will put this idea into the context of more recent research on interferometer technologies. Furthermore, the benefits of a triangular detector will be used to motivate this design as a good starting point for a more detailed research effort towards a third-generation gravitational-wave detector.
BibTeX: @article{Freise2009, author = {A Freise and S Chelkowski and S Hild and W Del Pozzo and A Perreca and A Vecchio}, title = {Triple Michelson interferometer for a third-generation gravitational wave detector}, journal = {Classical and Quantum Gravity}, year = {2009}, volume = {26}, number = {8}, pages = {085012 (14pp)}, url = {http://stacks.iop.org/0264-9381/26/085012} }
Freise, A., Hild, S., Somiya, K., Strain, K., Viceré, A., Barsuglia, M. & Chelkowski, S.	Optical detector topology for third-generation gravitational wave observatories [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-31	article	URL
Abstract: The third generation of gravitational wave observatories, with the aim of providing 100 times better sensitivity than currently operating interferometers, is expected to establish the evolving field of gravitational wave astronomy. A key element, required to achieve this ambitious sensitivity goal, is the exploration of new interferometer geometries, topologies and configurations. In this article we review the current status of the ongoing design work for third-generation gravitational wave observatories. The main focus is the evaluation of the detector geometry and detector topology. In addition we discuss some promising detector configurations and potential noise reduction schemes.
BibTeX: @article{springerlink:10.1007/s10714-010-1018-0, author = {Freise, Andreas and Hild, Stefan and Somiya, Kentaro and Strain, Ken and Viceré, Andrea and Barsuglia, Matteo and Chelkowski, Simon}, title = {Optical detector topology for third-generation gravitational wave observatories}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-31}, note = {10.1007/s10714-010-1018-0}, url = {http://dx.doi.org/10.1007/s10714-010-1018-0} }
Gair, J., Mandel, I., Miller, M. & Volonteri, M.	Exploring intermediate and massive black-hole binaries with the Einstein Telescope [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-34	article	URL
Abstract: We discuss the capability of a third-generation ground-based detector such as the Einstein Telescope (ET) to enhance our astrophysical knowledge through detections of gravitational waves emitted by binaries including intermediate-mass and massive black holes. The design target for such instruments calls for improved sensitivity at low frequencies, specifically in the $$sim 1-10$$ Hz range. This will allow the detection of gravitational waves generated in binary systems containing black holes of intermediate mass, $$00-10000M_odot$$ . We primarily discuss two different source types—mergers between two intermediate mass black holes (IMBHs) of comparable mass, and intermediate-mass-ratio inspirals (IMRIs) of smaller compact objects with mass $$-10M_odot$$ into IMBHs. IMBHs may form via two channels: (i) in dark matter halos at high redshift through direct collapse or the collapse of very massive metal-poor Population III stars, or (ii) via runaway stellar collisions in globular clusters. In this paper, we will discuss both formation channels, and both classes of merger in each case. We review existing rate estimates where these exist in the literature, and provide some new calculations for the approximate numbers of events that will be seen by a detector like the Einstein Telescope. These results indicate that the ET may see a few to a few thousand comparable-mass IMBH mergers and as many as several hundred IMRI events per year. These observations will significantly enhance our understanding of galactic black-hole growth, of the existence and properties of IMBHs and of the astrophysics of globular clusters. We finish our review with a discussion of some more speculative sources of gravitational waves for the ET, including hypermassive white dwarfs and eccentric stellar-mass compact-object binaries.
BibTeX: @article{springerlink:10.1007/s10714-010-1104-3, author = {Gair, Jonathan and Mandel, Ilya and Miller, M. and Volonteri, Marta}, title = {Exploring intermediate and massive black-hole binaries with the Einstein Telescope}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-34}, note = {10.1007/s10714-010-1104-3}, url = {http://dx.doi.org/10.1007/s10714-010-1104-3} }
Gair, J.R., Mandel, I., Sesana, A. & Vecchio, A.	Probing seed black holes using future gravitational-wave detectors [Abstract] [BibTeX]	2009	Classical and Quantum Gravity Vol. 26, pp. 204009	article	DOI
Abstract: Identifying the properties of the first generation of seeds of massive black holes is key to understanding the merger history and growth of galaxies. Mergers between ~100 solar mass seed black holes generate gravitational waves in the 0.1-10Hz band that lies between the sensitivity bands of existing ground-based detectors and the planned space-based gravitational wave detector, the Laser Interferometer Space Antenna (LISA). However, there are proposals for more advanced detectors that will bridge this gap, including the third generation ground-based Einstein Telescope and the space-based detector DECIGO. In this paper we demonstrate that such future detectors should be able to detect gravitational waves produced by the coalescence of the first generation of light seed black-hole binaries and provide information on the evolution of structure in that era. These observations will be complementary to those that LISA will make of subsequent mergers between more massive black holes. We compute the sensitivity of various future detectors to seed black-hole mergers, and use this to explore the number and properties of the events that each detector might see in three years of observation. For this calculation, we make use of galaxy merger trees and two different seed black hole mass distributions in order to construct the astrophysical population of events. We also consider the accuracy with which networks of future ground-based detectors will be able to measure the parameters of seed black hole mergers, in particular the luminosity distance to the source. We show that distance precisions of ~30% are achievable, which should be sufficient for us to say with confidence that the sources are at high redshift.
BibTeX: @article{Gair2009a, author = {Jonathan R Gair and Ilya Mandel and Alberto Sesana and Alberto Vecchio}, title = {Probing seed black holes using future gravitational-wave detectors}, journal = {Classical and Quantum Gravity}, year = {2009}, volume = {26}, pages = {204009}, doi = {http://dx.doi.org/10.1088/0264-9381/26/20/204009} }
Giacomazzo, B., Rezzolla, L. & Baiotti, L.	Accurate evolutions of inspiralling and magnetized neutron stars: Equal-mass binaries [BibTeX]	2011	Phys. Rev. D Vol. 83(4), pp. 044014	article	DOI
BibTeX: @article{PhysRevD.83.044014, author = {Giacomazzo, Bruno and Rezzolla, Luciano and Baiotti, Luca }, title = {Accurate evolutions of inspiralling and magnetized neutron stars: Equal-mass binaries}, journal = {Phys. Rev. D}, publisher = {American Physical Society}, year = {2011}, volume = {83}, number = {4}, pages = {044014}, doi = {http://dx.doi.org/10.1103/PhysRevD.83.044014} }
Hannam, M. & Hawke, I.	Numerical relativity simulations in the era of the Einstein Telescope [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-19	article	URL
Abstract: Numerical-relativity (NR) simulations of compact binaries are expected to be an invaluable tool in gravitational-wave astronomy. The sensitivity of future detectors such as the Einstein Telescope (ET) will place much higher demands on NR simulations than first- and second-generation ground-based detectors. We discuss the issues facing compact-object simulations over the next decade, with an emphasis on estimating where the accuracy and parameter space coverage will be sufficient for ET and where significant work is needed.
BibTeX: @article{springerlink:10.1007/s10714-010-1008-2, author = {Hannam, Mark and Hawke, Ian}, title = {Numerical relativity simulations in the era of the Einstein Telescope}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-19}, note = {10.1007/s10714-010-1008-2}, url = {http://dx.doi.org/10.1007/s10714-010-1008-2} }
Hannam, M. & Hawke, I.	Numerical relativity simulations in the era of the Einstein Telescope [Abstract] [BibTeX]	2009	arXiv:0908.3139v1 [gr-qc]	article	URL
Abstract: Numerical-relativity (NR) simulations of compact binaries are expected to be an invaluable tool in gravitational-wave (GW) astronomy. The sensitivity of future detectors such as the Einstein Telescope (ET) will place much higher demands on NR simulations than first- and second-generation ground-based detectors. We discuss the issues facing compact-object simulations over the next decade, with an emphasis on estimating where the accuracy and parameter space coverage will be sufficient for ET and where significant work is needed.
BibTeX: @article{Hannam2009, author = {Mark Hannam and Ian Hawke}, title = {Numerical relativity simulations in the era of the Einstein Telescope}, journal = {arXiv:0908.3139v1 [gr-qc]}, year = {2009}, url = {http://arxiv.org/abs/0908.3139} }
Harms, J., Acernese, F., Barone, F., Bartos, I., Beker, M., van den Brand, J.F.J., Christensen, N., Coughlin, M., DeSalvo, R., Dorsher, S., Heise, J., Kandhasamy, S., Mandic, V., MÃ¡rka, S., Mueller, G., Naticchioni, L., O'Keefe, T., Rabeling, D.S., Sajeva, A., Trancynger, T. & Wand, V.	Characterization of the seismic environment at the Sanford Underground Laboratory, South Dakota [Abstract] [BibTeX]	2010	Classical and Quantum Gravity Vol. 27(22), pp. 225011	article	URL
Abstract: An array of seismometers is being developed at the Sanford Underground Laboratory, the former Homestake mine, in South Dakota to study the properties of underground seismic fields and Newtonian noise, and to investigate the possible advantages of constructing a third-generation gravitational-wave detector underground. Seismic data were analyzed to characterize seismic noise and disturbances. External databases were used to identify sources of seismic waves: ocean-wave data to identify sources of oceanic microseisms and surface wind-speed data to investigate correlations with seismic motion as a function of depth. In addition, sources of events contributing to the spectrum at higher frequencies are characterized by studying the variation of event rates over the course of a day. Long-term observations of spectral variations provide further insight into the nature of seismic sources. Seismic spectra at three different depths are compared, establishing the 4100 ft level as a world-class low seismic-noise environment.
BibTeX: @article{0264-9381-27-22-225011, author = {J Harms and F Acernese and F Barone and I Bartos and M Beker and J F J van den Brand and N Christensen and M Coughlin and R DeSalvo and S Dorsher and J Heise and S Kandhasamy and V Mandic and S MÃ¡rka and G Mueller and L Naticchioni and T O'Keefe and D S Rabeling and A Sajeva and T Trancynger and V Wand}, title = {Characterization of the seismic environment at the Sanford Underground Laboratory, South Dakota}, journal = {Classical and Quantum Gravity}, year = {2010}, volume = {27}, number = {22}, pages = {225011}, url = {http://stacks.iop.org/0264-9381/27/i=22/a=225011} }
Harms, J., DeSalvo, R., Dorsher, S. & Mandic, V.	Simulation of underground gravity gradients from stochastic seismic fields [BibTeX]	2009	Phys. Rev. D Vol. 80(12), pp. 122001	article	DOI
BibTeX: @article{PhysRevD.80.122001, author = {Harms, Jan and DeSalvo, Riccardo and Dorsher, Steven and Mandic, Vuk }, title = {Simulation of underground gravity gradients from stochastic seismic fields}, journal = {Phys. Rev. D}, publisher = {American Physical Society}, year = {2009}, volume = {80}, number = {12}, pages = {122001}, doi = {http://dx.doi.org/10.1103/PhysRevD.80.122001} }
Hild, S., Chelkowski, S. & Freise, A.	Pushing towards the ET sensitivity using 'conventional' technology [Abstract] [BibTeX]	2008	arXiv:0810.0604v2 [gr-qc]	article	URL
Abstract: Recently, the design study `Einstein gravitational wave Telescope' (ET) has been funded within the European FP7 framework. The ambitious goal of this project is to provide a conceptual design of a detector with a hundred times better sensitivity than currently operating instruments. It is expected that this will require the development and implementation of new technologies, which go beyond the concepts employed for the first and second detector generations. However, it is a very interesting and educational exercise to imagine a Michelson interferometer in which conventional technologies have been pushed to - or maybe beyond - their limits to reach the envisaged sensitivity for the Einstein Telescope. In this document we present a first sketchy analysis of what modifications and improvements are necessary to go, step-by-step, from second generation gravitational wave detectors to the Einstein Telescope.
BibTeX: @article{HildETconventional, author = {Stefan Hild and Simon Chelkowski and Andreas Freise}, title = {Pushing towards the ET sensitivity using 'conventional' technology}, journal = {arXiv:0810.0604v2 [gr-qc]}, year = {2008}, url = {http://www.citebase.org/abstract?id=oai:arXiv.org:0810.0604} }
Hild, S., Chelkowski, S., Freise, A., Franc, J., Morgado, N., Flaminio, R. & DeSalvo, R.	A xylophone configuration for a third-generation gravitational wave detector [Abstract] [BibTeX]	2010	Classical and Quantum Gravity Vol. 27(1), pp. 015003 (8pp)	article	URL
Abstract: 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 38 000 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.
BibTeX: @article{Hild2010, author = {S Hild and S Chelkowski and A Freise and J Franc and N Morgado and R Flaminio and R DeSalvo}, title = {A xylophone configuration for a third-generation gravitational wave detector}, journal = {Classical and Quantum Gravity}, year = {2010}, volume = {27}, number = {1}, pages = {015003 (8pp)}, url = {http://stacks.iop.org/0264-9381/27/015003} }
Hild, S. & others	Sensitivity studies for third-generation gravitational wave observatories [Abstract] [BibTeX]	2011	Classical and Quantum Gravity Vol. 28(9), pp. 094013	article	URL
Abstract: Advanced gravitational wave detectors, currently under construction, are expected to directly observe gravitational wave signals of astrophysical origin. The Einstein Telescope (ET), a third-generation gravitational wave detector, has been proposed in order to fully open up the emerging field of gravitational wave astronomy. In this paper we describe sensitivity models for ET and investigate potential limits imposed by fundamental noise sources. A special focus is set on evaluating the frequency band below 10 Hz where a complex mixture of seismic, gravity gradient, suspension thermal and radiation pressure noise dominates. We develop the most accurate sensitivity model, referred to as ET-D, for a third-generation detector so far, including the most relevant fundamental noise contributions.
BibTeX: @article{0264-9381-28-9-094013, author = {Hild, S and others}, title = {Sensitivity studies for third-generation gravitational wave observatories}, journal = {Classical and Quantum Gravity}, year = {2011}, volume = {28}, number = {9}, pages = {094013}, url = {http://stacks.iop.org/0264-9381/28/i=9/a=094013} }
Howell, E., Regimbau, T., Corsi, A., Coward, D. & Burman, R.	Gravitational wave background from sub-luminous GRBs: prospects for second and third generation detectors [Abstract] [BibTeX]	2010	arXiv:1008.3941v1 [astro-ph.HE]	article	URL
Abstract: We assess the detection prospects of a gravitational wave background associated with sub-luminous gamma-ray bursts (SL-GRBs). We assume that the central engines of a significant proportion of these bursts are provided by newly born magnetars and consider two plausible GW emission mechanisms. Firstly, the deformation-induced triaxial GW emission from a newly born magnetar. Secondly, the onset of a secular bar-mode instability, associated with the long lived plateau observed in the X-ray afterglows of many gamma-ray bursts (Corsi & Meszaros 2009a). With regards to detectability, we find that the onset of a secular instability is the most optimistic scenario: under the hypothesis that SL-GRBs associated with secularly unstable magnetars occur at a rate of (48; 80)Gpc^-3yr^-1 or greater, cross-correlation of data from two Einstein Telescopes (ETs) could detect the GW background associated to this signal with a signal-to-noise ratio of 3 or greater after 1 year of observation. Assuming neutron star spindown results purely from triaxial GW emissions, we find that rates of around (130;350)Gpc^-3yr^-1 will be required by ET to detect the resulting GW background. We show that a background signal from secular instabilities could potentially mask a primordial GW background signal in the frequency range where ET is most sen- sitive. Finally, we show how accounting for cosmic metallicity evolution can increase the predicted signal-to-noise ratio for background signals associated with SL-GRBs.
BibTeX: @article{Howell2010, author = {Howell, E. and Regimbau, T. and Corsi, A. and Coward, D. and Burman, R.}, title = {Gravitational wave background from sub-luminous GRBs: prospects for second and third generation detectors}, journal = {arXiv:1008.3941v1 [astro-ph.HE]}, year = {2010}, url = {http://arxiv.org/abs/1008.3941v1} }
Huerta, E.A. & Gair, J.R.	Intermediate-mass-ratio inspirals in the Einstein Telescope. I. Signal-to-noise ratio calculations [BibTeX]	2011	Phys. Rev. D Vol. 83(4), pp. 044020	article	DOI
BibTeX: @article{PhysRevD.83.044020, author = {Huerta, E. A. and Gair, Jonathan R.}, title = {Intermediate-mass-ratio inspirals in the Einstein Telescope. I. Signal-to-noise ratio calculations}, journal = {Phys. Rev. D}, publisher = {American Physical Society}, year = {2011}, volume = {83}, number = {4}, pages = {044020}, doi = {http://dx.doi.org/10.1103/PhysRevD.83.044020} }
Huerta, E.A. & Gair, J.R.	Intermediate-mass-ratio inspirals in the Einstein Telescope. II. Parameter estimation errors [BibTeX]	2011	Phys. Rev. D Vol. 83(4), pp. 044021	article	DOI
BibTeX: @article{PhysRevD.83.044021, author = {Huerta, E. A. and Gair, Jonathan R.}, title = {Intermediate-mass-ratio inspirals in the Einstein Telescope. II. Parameter estimation errors}, journal = {Phys. Rev. D}, publisher = {American Physical Society}, year = {2011}, volume = {83}, number = {4}, pages = {044021}, doi = {http://dx.doi.org/10.1103/PhysRevD.83.044021} }
Ilya Mandel, Jonathan R. Gair, M.C.M.	Detecting coalescences of intermediate-mass black holes in globular clusters with the Einstein Telescope [Abstract] [BibTeX]	2010	arXiv:0912.4925v2 [astro-ph.CO]	article	URL
Abstract: We discuss the capability of a third-generation ground-based detector such as the Einstein Telescope to detect mergers of intermediate-mass black holes that may have formed through runaway stellar collisions in globular clusters. We find that detection rates of 500 events per year are plausible
BibTeX: @article{IlyaMandel2010, author = {Ilya Mandel, Jonathan R. Gair, M. Coleman Miller}, title = {Detecting coalescences of intermediate-mass black holes in globular clusters with the Einstein Telescope}, journal = {arXiv:0912.4925v2 [astro-ph.CO]}, year = {2010}, url = {http://arxiv.org/abs/0912.4925v2} }
Jonathan R. Gair, Ilya Mandel, M.C.M.M.V.	Exploring intermediate and massive black-hole binaries with the Einstein Telescope [Abstract] [BibTeX]	2010	arXiv:0907.5450v2 [astro-ph.CO]	article	URL
Abstract: We discuss the capability of a third-generation ground-based detector such as the Einstein Telescope (ET) to enhance our astrophysical knowledge through detections of gravitational waves emitted by binaries including intermediate-mass and massive black holes. The design target for such instruments calls for improved sensitivity at low frequencies, specifically in the ~ 1-10 Hz range. This will allow the detection of gravitational waves generated in binary systems containing black holes of intermediate mass, ~ 100-1000 solar masses. We primarily discuss two different source types -- mergers between two intermediate mass black holes (IMBHs) of comparable mass, and intermediate-mass-ratio inspirals (IMRIs) of smaller compact objects with mass ~ 1-10 solar masses into IMBHs. IMBHs may form via two channels: (i) in dark matter halos at high redshift through direct collapse or the collapse of very massive metal-poor Population III stars, or (ii) via runaway stellar collisions in globular clusters. In this paper, we will discuss both formation channels, and both classes of merger in each case. We review existing rate estimates where these exist in the literature, and provide some new calculations for the approximate numbers of events that will be seen by a detector like the Einstein Telescope. These results indicate that the ET may see a few to a few thousand comparable-mass IMBH mergers and as many as several hundred IMRI events per year. These observations will significantly enhance our understanding of galactic black-hole growth, of the existence and properties of IMBHs and of the astrophysics of globular clusters. We finish our review with a discussion of some more speculative sources of gravitational waves for the ET, including hypermassive white dwarfs and eccentric stellar-mass compact-object binaries.
BibTeX: @article{JonathanR.Gair2010, author = {Jonathan R. Gair, Ilya Mandel, M. Coleman Miller, Marta Volonteri}, title = {Exploring intermediate and massive black-hole binaries with the Einstein Telescope}, journal = {arXiv:0907.5450v2 [astro-ph.CO]}, year = {2010}, url = {http://arxiv.org/abs/0907.5450v2} }
I, K., Bulik, T., Belczynski, K., Dominik, M. & Gondek-Rosinska, D.	The eccentricity distribution of compact binaries [Abstract] [BibTeX]	2011	arXiv:1010.0511v3 [astro-ph.CO]	article	URL
Abstract: The current gravitational wave detectors have reached their operational sensitivity and are nearing detection of compact object binaries. In the coming years, we expect that the Advanced LIGO/VIRGO will start taking data. At the same time, there are plans for third generation ground-based detectors such as the Einstein Telescope, and space detectors such as DECIGO. We discuss the eccentricity distribution of inspiral compact object binaries during they inspiral phase. We analyze the expected distributions of eccentricities at three frequencies that are characteristic of three future detectors: Advanced LIGO/VIRGO (30 Hz), Einstein Telescope (3 Hz), and DECIGO (0.3 Hz). We use the StarTrack binary population code to investigate the properties of the population of compact binaries in formation. We evolve their orbits until the point that they enter a given detector sensitivity window and analyze the eccentricity distribution at that time. We find that the eccentricities of BH-BH and BH-NS binaries are quite small when entering the Advanced LIGO/VIRGO detector window for all considered models of binary evolution. Even in the case of the DECIGO detector, the typical eccentricities of BH-BH binaries are below 10^-4, and the BH-NS eccentricities are smaller than 10^-3. Some fraction of NS-NS binaries may have significant eccentricities. Within the range of considered models, we found that a fraction of between 0.2% and 2% NS-NS binaries will have an eccentricity above 0.01 for the Advanced LIGO/VIRGO detectors. For the ET detector, this fraction is between 0.4% and 4%, and for the DECIGO detector it lies between 2% and 27%.
BibTeX: @article{KowalskaI2011, author = {Kowalska I, and Bulik, T and Belczynski, K and Dominik, M and Gondek-Rosinska, D}, title = {The eccentricity distribution of compact binaries}, journal = {arXiv:1010.0511v3 [astro-ph.CO]}, year = {2011}, url = {http://arxiv.org/pdf/1010.0511v3} }
Kowalska, I., Bulik, T., Belczynski, K., Dominik, M. & Gondek-Rosinska, D.	The eccentricity of binaries detectable in gravitational waves [Abstract] [BibTeX]	2010	arXiv:1010.0511v1 [astro-ph.CO]	article	URL
Abstract: The current gravitational wave detectors have reached their operational sensitivity and are nearing detection of compact object binaries. In the coming years we expect that the Advanced LIGO/VIRGO will start taking data. At the same time there are plans for third generation ground based detectors like the Einstein Telescope, and space detectors like DECIGO. We discuss the detectability of eccentricity of inspiral compact object binaries with the use of their gravitational wave signal. We analyze the expected distributions of eccentricities and calculate the fraction of binaries with detectable eccentricity. We use the StarTrack binary population code to investigate the properties of the population of compact binaries at formation. We evolved their orbits until the point they enter a given detector sensitivity window and analyze the distribution of eccentricity at that time. We find that in the case of NS-NS binaries a small fraction (0.53%) should have eccentricities detectable with the Advanced LIGO/VIRGO. This fraction increases for the planned Einstein Telescope (ET) and reaches 2.98%, while for the DECIGO type detectors the majority (68.11%) of NS-NS binaries shall have detectable eccentricities. In the case of BH-NS fraction of detectable binaries with non-zero eccentricities for Advanced LIGO/VIRGO, ET and DECIGO are equal to 0.15%, 1.16% and 15.99%, respectively. For BH-BH binaries the fraction of objects with detectable eccentricities is very small - in Advanced LIGO/VIRGO it's dropping to zero, while for ET and DECIGO it's equal to 0.62% and 2.49%, respectively
BibTeX: @article{Kowalska2010, author = {I. Kowalska and T. Bulik and K. Belczynski and M. Dominik and D. Gondek-Rosinska}, title = {The eccentricity of binaries detectable in gravitational waves}, journal = {arXiv:1010.0511v1 [astro-ph.CO]}, year = {2010}, url = {http://arxiv.org/abs/1010.0511v1} }
Leone Bosi, E.K.P.	Data Analysis Challenges for the Einstein Telescope [Abstract] [BibTeX]	2009	arXiv:0910.0380v1 [gr-qc]	article	URL
Abstract: The Einstein Telescope is a proposed third generation gravitational wave detector that will operate in the region of 1 Hz to a few kHz. As well as the inspiral of compact binaries composed of neutron stars or black holes, the lower frequency cut-off of the detector will open the window to a number of new sources. These will include the end stage of inspirals, plus merger and ringdown of intermediate mass black holes, where the masses of the component bodies are on the order of a few hundred solar masses. There is also the possibility of observing intermediate mass ratio inspirals, where a stellar mass compact object inspirals into a black hole which is a few hundred to a few thousand times more massive. In this article, we investigate some of the data analysis challenges for the Einstein Telescope such as the effects of increased source number, the need for more accurate waveform models and the some of the computational issues that a data analysis strategy might face.
BibTeX: @article{LeoneBosi2009, author = {Leone Bosi, Edward K. Porter}, title = {Data Analysis Challenges for the Einstein Telescope}, journal = {arXiv:0910.0380v1 [gr-qc]}, year = {2009}, url = {http://arxiv.org/abs/0910.0380v1} }
Mapelli, M., Huwyler, C., Mayer, L., Jetzer, P. & Vecchio, A.	Gravitational waves from intermediate-mass black holes in young clusters [Abstract] [BibTeX]	2010	arXiv:1006.1664v1 [astro-ph]	article	URL
Abstract: Massive young clusters (YCs) are expected to host intermediate-mass black holes (IMBHs) born via runaway collapse. These IMBHs are likely in binaries and can undergo mergers with other compact objects, such as stellar mass black holes (BHs) and neutron stars (NSs). We derive the frequency of such mergers starting from information available in the Local Universe. Mergers of IMBH-NS and IMBH-BH binaries are sources of gravitational waves (GWs), which might allow us to reveal the presence of IMBHs. We thus examine their detectability by current and future GW observatories, both ground- and space-based. In particular, as representative of different classes of instruments we consider Initial and Advanced LIGO, the Einstein gravitational-wave Telescope (ET) and the Laser Interferometer Space Antenna (LISA). We find that IMBH mergers are unlikely to be detected with instruments operating at the current sensitivity (Initial LIGO). LISA detections are disfavored by the mass range of IMBH-NS and IMBH-BH binaries: less than one event per year is expected to be observed by such instrument. Advanced LIGO is expected to observe a few merger events involving IMBH binaries in a 1-year long observation. Advanced LIGO is particularly suited for mergers of relatively light IMBHs (~100 Msun) with stellar mass BHs. The number of mergers detectable with ET is much larger: tens (hundreds) of IMBH-NS (IMBH-BH) mergers might be observed per year, according to the runaway collapse scenario for the formation of IMBHs. We note that our results are affected by large uncertainties, produced by poor observational constraints on many of the physical processes involved in this study, such as the evolution of the YC density with redshift
BibTeX: @article{2010arXiv1006.1664M, author = {Mapelli, M. and Huwyler, C. and Mayer, L. and Jetzer, P. and Vecchio, A.}, title = {Gravitational waves from intermediate-mass black holes in young clusters}, journal = {arXiv:1006.1664v1 [astro-ph]}, year = {2010}, url = {http://arxiv.org/abs/1006.1664v1} }
Marassi, S., Ciolfi, R., Schneider, R., Stella, L. & Ferrari, V.	Stochastic background of gravitational waves emitted by magnetars [Abstract] [BibTeX]	2010	arXiv:1009.1240v2 [astro-ph.CO]	article	URL
Abstract: Two classes of high energy sources in our galaxy are believed to host magnetars, neutron stars whose emission results from the dissipation of their magnetic field. The extremely high magnetic field of magnetars distorts their shape, and causes the emission of a conspicuous gravitational waves signal if rotation is fast and takes place around a different axis than the symmetry axis of the magnetic distortion. Based on a numerical model of the cosmic star formation history, we derive the cosmological background of gravitational waves produced by magnetars, when they are very young and fast spinning. We adopt different models for the configuration and strength of the internal magnetic field (which determines the distortion) as well as different values of the external dipole field strength (which governs the spin evolution of magnetars over a wide range of parameters). We find that the expected gravitational wave background differs considerably from one model to another. The strongest signals are generated for magnetars with very intense toroidal internal fields ($sim 10^16$ G range) and external dipole fields of $sim 10^14$, as envisaged in models aimed at explaining the properties of the Dec 2004 giant flare from SGR 1806-20. Such signals should be easily detectable with third generation ground based interferometers such as the Einstein Telescope.
BibTeX: @article{Marassi2010, author = {Stefania Marassi and Riccardo Ciolfi and Raffaella Schneider and Luigi Stella and Valeria Ferrari}, title = {Stochastic background of gravitational waves emitted by magnetars}, journal = {arXiv:1009.1240v2 [astro-ph.CO]}, year = {2010}, url = {http://arxiv.org/abs/1009.1240v2} }
Mavalvala, N., McClelland, D., Mueller, G., Reitze, D., Schnabel, R. & Willke, B.	Lasers and optics: looking towards third generation gravitational wave detectors [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-24	article	URL
Abstract: Third generation terrestrial interferometric gravitational wave detectors will likely require significant advances in laser and optical technologies to reduce two of the main limiting noise sources: thermal noise due to mirror coatings and quantum noise arising from a combination of shot noise and radiation pressure noise. Increases in laser power and possible changes of the operational wavelength require new high power laser sources and new electro-optic modulators and Faraday isolators. Squeezed light can be used to further reduce the quantum noise while nano-structured optical components can be used to reduce or eliminate mirror coating thermal noise as well as to implement all-reflective interferometer configurations to avoid thermal effects in mirror substrates. This paper is intended to give an overview on the current state-of-the-art and future trends in these areas of ongoing research and development.
BibTeX: @article{springerlink:10.1007/s10714-010-1023-3, author = {Mavalvala, Nergis and McClelland, David and Mueller, Guido and Reitze, D. and Schnabel, Roman and Willke, Benno}, title = {Lasers and optics: looking towards third generation gravitational wave detectors}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-24}, note = {10.1007/s10714-010-1023-3}, url = {http://dx.doi.org/10.1007/s10714-010-1023-3} }
N. Andersson, V. Ferrari, D.J.K.K.B.K.J.R.L.R.B.Z.	Gravitational waves from neutron stars: Promises and challenges [Abstract] [BibTeX]	2009	arXiv:0912.0384v1 [astro-ph.SR]	article	URL
Abstract: We discuss different ways that neutron stars can generate gravitational waves, describe recent improvements in modelling the relevant scenarios in the context of improving detector sensitivity, and show how observations are beginning to test our understanding of fundamental physics. The main purpose of the discussion is to establish promising science goals for third-generation ground-based detectors, like the Einstein Telescope, and identify the various challenges that need to be met if we want to use gravitational-wave data to probe neutron star physics.
BibTeX: @article{N.Andersson2009, author = {N. Andersson, V. Ferrari, D.I. Jones, K.D. Kokkotas, B. Krishnan, J. Read, L. Rezzolla, B. Zink}, title = {Gravitational waves from neutron stars: Promises and challenges}, journal = {arXiv:0912.0384v1 [astro-ph.SR]}, year = {2009}, url = {http://arxiv.org/abs/0912.0384v1} }
Nawrodt, R., Rowan, S., Hough, J., Punturo, M., Ricci, F. & Vinet, J.-Y.	Challenges in thermal noise for 3rd generation of gravitational wave detectors [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-30	article	URL
Abstract: Various noise sources limit the sensitivity of current interferometric gravitational wave detectors, including seismic noise, thermal noise of the optical components and suspension elements and photon shot noise. Plans are in place for a suite of hardware upgrades which should increase the sensitivity of these detectors by reducing the various noise sources. With these designs for 2nd generation detectors mature, techniques for further improvement of detector sensitivity by a factor of approximately 10 are under study. A particular challenge is the reduction of the thermal noise associated with the interferometer mirrors and their suspensions. We review the current status of research on thermal noise in interferometric gravitational wave detectors. Aspects of possible techniques for use in future ‘3rd generation detectors’ such as cryogenics and diffractive optics are discussed.
BibTeX: @article{springerlink:10.1007/s10714-010-1066-5, author = {Nawrodt, Ronny and Rowan, Sheila and Hough, Jim and Punturo, Michele and Ricci, Fulvio and Vinet, Jean-Yves}, title = {Challenges in thermal noise for 3rd generation of gravitational wave detectors}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-30}, note = {10.1007/s10714-010-1066-5}, url = {http://dx.doi.org/10.1007/s10714-010-1066-5} }
Pau Amaro-Seoane, L.S.	Detection of IMBHs with Ground-based Gravitational Wave Observatories: A Biography of a Binary of Black Holes, from Birth to Death [Abstract] [BibTeX]	2010	The Astrophysical Journal Vol. 722(2), pp. 1197	article	URL
Abstract: Even though the existence of intermediate-mass black holes (IMBHs; black holes with masses ranging between 10 2 M ##IMG## [http://ej.iop.org/icons/Entities/sun.gif] sun and 10 4 M ##IMG## [http://ej.iop.org/icons/Entities/sun.gif] sun ) has not yet been corroborated observationally, these objects are of high interest for astrophysics. Our understanding of the formation and evolution of supermassive black holes, as well as galaxy evolution modeling and cosmography would dramatically change if an IMBH were to be observed. From the point of view of traditional photon-based astronomy, which relies on the monitoring of innermost stellar kinematics, the direct detection of an IMBH seems to be rather far in the future. However, the prospect of the detection and characterization of an IMBH has good chances in lower frequency gravitational-wave (GW) astrophysics using ground-based detectors such as the Laser Interferometer Gravitational-Wave Observatory (LIGO), Virgo, and the future Einstein Telescope (ET). We present an analysis of the signal of a system of a binary of IMBHs based on a waveform model obtained with numerical relativity simulations coupled with post-Newtonian calculations at the highest available order. IMBH binaries with total masses between 200 and20,000Â M ##IMG## [http://ej.iop.org/icons/Entities/sun.gif] sun would produce significant signal-to-noise ratios in Advanced LIGO and Virgo and the ET. We have computed the expected event rate of IMBH binary coalescences for different configurations of the binary, finding interesting values that depend on the spin of the IMBHs. The prospects for IMBH detection and characterization with ground-based GW observatories would not only provide us with a robust test of general relativity, but would also corroborate the existence of these systems. Such detections should allow astrophysicists to probe the stellar environments of IMBHs and their formation processes.
BibTeX: @article{PauAmaro-Seoane2009, author = {Pau Amaro-Seoane, Lucia Santamaria}, title = {Detection of IMBHs with Ground-based Gravitational Wave Observatories: A Biography of a Binary of Black Holes, from Birth to Death}, journal = {The Astrophysical Journal}, year = {2010}, volume = {722}, number = {2}, pages = {1197}, url = {http://stacks.iop.org/0004-637X/722/i=2/a=1197} }
Pitkin, M.	Prospects of observing continuous gravitational waves from known pulsars [Abstract] [BibTeX]	2011	arXiv:1103.5867v1 [astro-ph.HE]	article	URL
Abstract: Several searches for gravitational waves from a selection of known pulsars have been performed with data from the science runs of the LIGO gravitational wave detectors. So far these have lead to no detection, but upper limits on the gravitational wave amplitudes have been set. Here we study our intrinsic ability to detect, and estimate the gravitational wave amplitude for non-accreting pulsars. Using spin-down limits on emission as a guide we examine amplitudes that would be required to observe known pulsars with future detectors (Advanced LIGO, Advanced Virgo and the Einstein Telescope), assuming that they are triaxial stars emitting at precisely twice the known rotation frequency. Maximum allowed amplitudes depend on the stars' equation of state (e.g. a normal neutron star, a quark star, a hybrid star) and the theoretical mass quadrupoles that they can sustain. We study what range of quadrupoles, and therefore equations of state, would be consistent with being able to detect these sources. For globular cluster pulsars, with spin-downs masked by accelerations within the cluster, we examine what spin-down values gravitational wave observations would be able to set. For all pulsars we also alternatively examine what internal magnetic fields they would need to sustain observable ellipticities.
BibTeX: @article{Pitkin2011, author = {Matthew Pitkin}, title = {Prospects of observing continuous gravitational waves from known pulsars}, journal = {arXiv:1103.5867v1 [astro-ph.HE]}, year = {2011}, url = {http://arxiv.org/pdf/1103.5867v1} }
Punturo, M. & Lück, H.	Toward a third generation of gravitational wave observatories [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-23	article	URL
Abstract: Large gravitational wave interferometric detectors, like Virgo and LIGO, demonstrated the capability to reach their design sensitivity, but to transform these machines into an effective observational instrument for gravitational wave astronomy a large improvement in sensitivity is required. Advanced detectors in the near future and third generation observatories in slightly more than one decade will open the possibility to perform gravitational wave astronomical observations from the Earth. An overview of the technological progress needed to realize a third generation observatory, like the Einstein Telescope (ET), and a possible evolution scenario are discussed in this paper.
BibTeX: @article{GRG-ET-2010, author = {Punturo, Michele and Lück, Harald}, title = {Toward a third generation of gravitational wave observatories}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-23}, note = {10.1007/s10714-010-1010-8}, url = {http://dx.doi.org/10.1007/s10714-010-1010-8} }
Punturo, M. & others	The Einstein Telescope: a third-generation gravitational wave observatory [Abstract] [BibTeX]	2010	Classical and Quantum Gravity Vol. 27(19), pp. 194002	article	URL
Abstract: Advanced gravitational wave interferometers, currently under realization, will soon permit the detection of gravitational waves from astronomical sources. To open the era of precision gravitational wave astronomy, a further substantial improvement in sensitivity is required. The future space-based Laser Interferometer Space Antenna and the third-generation ground-based observatory Einstein Telescope (ET) promise to achieve the required sensitivity improvements in frequency ranges. The vastly improved sensitivity of the third generation of gravitational wave observatories could permit detailed measurements of the sources' physical parameters and could complement, in a multi-messenger approach, the observation of signals emitted by cosmological sources obtained through other kinds of telescopes. This paper describes the progress of the ET project which is currently in its design study phase.
BibTeX: @article{0264-9381-27-19-194002, author = {M Punturo and others}, title = {The Einstein Telescope: a third-generation gravitational wave observatory}, journal = {Classical and Quantum Gravity}, year = {2010}, volume = {27}, number = {19}, pages = {194002}, url = {http://stacks.iop.org/0264-9381/27/i=19/a=194002} }
Punturo, M. & others	The third generation of gravitational wave observatories and their science reach [Abstract] [BibTeX]	2010	Classical and Quantum Gravity Vol. 27(8), pp. 084007	article	URL
Abstract: Large gravitational wave interferometric detectors, like Virgo and LIGO, demonstrated the capability to reach their design sensitivity, but to transform these machines into an effective observational instrument for gravitational wave astronomy a large improvement in sensitivity is required. Advanced detectors in the near future and third-generation observatories in more than one decade will open the possibility to perform gravitational wave astronomical observations from the Earth. An overview of the possible science reaches and the technological progress needed to realize a third-generation observatory are discussed in this paper. The status of the project Einstein Telescope (ET), a design study of a third-generation gravitational wave observatory, will be reported.
BibTeX: @article{Punturo2010, author = {M Punturo and others}, title = {The third generation of gravitational wave observatories and their science reach}, journal = {Classical and Quantum Gravity}, year = {2010}, volume = {27}, number = {8}, pages = {084007}, url = {http://stacks.iop.org/0264-9381/27/i=8/a=084007} }
Puppo, P. & Ricci, F.	Cryogenics and Einstein Telescope [Abstract] [BibTeX]	2010	General Relativity and Gravitation, pp. 1-13	article	URL
Abstract: The dominant noises which limit the present sensitivity of the gravitational wave detectors are the thermal noise of the suspended mirrors and the shot noise. For the third generation of gravitational wave detectors as the Einstein Telescope (ET), the reduction of the shot noise implies to increase the power stored in the detector at 1 MW level and, at the same time, to compensate the huge optic distortion due to induced thermal lensing. At low temperature it is possible to reduce both these effects. However, lowering the temperature of the test masses without injecting vibration noise from the cooling system is a technological challenge. We review here the thermal noise impact on the ultimate ET sensitivity limit and we discuss possible cryogenic configurations to cool the mirror.
BibTeX: @article{springerlink:10.1007/s10714-010-1037-x, author = {Puppo, Paola and Ricci, Fulvio}, title = {Cryogenics and Einstein Telescope}, journal = {General Relativity and Gravitation}, publisher = {Springer Netherlands}, year = {2010}, pages = {1-13}, note = {10.1007/s10714-010-1037-x}, url = {http://dx.doi.org/10.1007/s10714-010-1037-x} }
R. Schnabel, M. Britzger, F.B.O.B.K.D.J.D.T.E.D.F.H.L.M.M.R.N.S.S. & Willke, B.	Building blocks for future detectors: Silicon test masses and 1550 nm laser light [Abstract] [BibTeX]	2009	arXiv:0912.3164v1 [physics.ins-det]	article	URL
Abstract: Current interferometric gravitational wave detectors use the combination of quasi-monochromatic, continuous-wave laser light at 1064 nm and fused silica test masses at room temperature. Detectors of the third generation, such as the Einstein-Telescope, will involve a considerable sensitivity increase. The combination of 1550 nm laser radiation and crystalline silicon test masses at low temperatures might be important ingredients in order to achieve the sensitivity goal. Here we compare some properties of the fused silica and silicon test mass materials relevant for decreasing the thermal noise in future detectors as well as the recent technology achievements in the preparation of laser radiation at 1064 nm and 1550 nm relevant for decreasing the quantum noise. We conclude that silicon test masses and 1550 nm laser light have the potential to form the future building blocks of gravitational wave detection.
BibTeX: @article{R.Schnabel, author = {R. Schnabel, M. Britzger, F. Brückner, O. Burmeister, K. Danzmann, J. Dück, T. Eberle, D. Friedrich, H. Lück, M. Mehmet, R. Nawrodt, S. Steinlechner and B. Willke}, title = {Building blocks for future detectors: Silicon test masses and 1550 nm laser light}, journal = {arXiv:0912.3164v1 [physics.ins-det]}, year = {2009}, url = {http://arxiv4.library.cornell.edu/abs/0912.3164v1} }
Regimbau, T. & Hughes, S.A.	Gravitational-wave confusion background from cosmological compact binaries: Implications for future terrestrial detectors [Abstract] [BibTeX]	2009	Phys. Rev. D Vol. 79(6), pp. 062002	article	DOI
Abstract: Increasing the sensitivity of a gravitational-wave (GW) detector improves our ability to measure the characteristics of detected sources. It also increases the number of weak signals that contribute to the data. Because GW detectors have nearly all-sky sensitivity, they can be subject to a confusion limit: Many sources which cannot be distinguished may be measured simultaneously, defining a stochastic noise floor to the sensitivity. For GW detectors operating at present and for their planned upgrades, the projected event rate is sufficiently low that we are far from the confusion-limited regime. However, some detectors currently under discussion may have large enough reach to binary inspiral that they enter the confusion-limited regime. In this paper, we examine the binary inspiral confusion limit for terrestrial detectors. We consider a broad range of inspiral rates in the literature, several planned advanced gravitational-wave detectors, and the highly advanced “Einstein telescope” design. Though most advanced detectors will not be impacted by this limit, the Einstein telescope with a very low-frequency “seismic wall” may be subject to confusion noise. At a minimum, careful data analysis will be require to separate signals which will appear confused. This result should be borne in mind when designing highly advanced future instruments.
BibTeX: @article{Regimbau2009, author = {Regimbau, T. and Hughes, Scott A.}, title = {Gravitational-wave confusion background from cosmological compact binaries: Implications for future terrestrial detectors}, journal = {Phys. Rev. D}, publisher = {American Physical Society}, year = {2009}, volume = {79}, number = {6}, pages = {062002}, doi = {http://dx.doi.org/10.1103/PhysRevD.79.062002} }
Sathyaprakash, B.S., Schutz, B. & Broeck, C.V.D.	Cosmography with the Einstein Telescope [Abstract] [BibTeX]	2009	arXiv:0906.4151v1 [astro-ph.CO]	article	URL
Abstract: Einstein Telescope (ET) is a 3rd generation gravitational-wave (GW) detector that is currently undergoing a design study. ET can detect millions of compact binary mergers up to redshifts 2-8. A small fraction of mergers might be observed in coincidence as gamma-ray bursts, helping to measure both the luminosity distance and red-shift to the source. By fitting these measured values to a cosmological model, it should be possible to accurately infer the dark energy equation-of-state, dark matter and dark energy density parameters. ET could, therefore, herald a new era in cosmology.
BibTeX: @article{Sathyaprakash2009, author = {B. S. Sathyaprakash and Bernard Schutz and Chris Van Den Broeck}, title = {Cosmography with the Einstein Telescope}, journal = {arXiv:0906.4151v1 [astro-ph.CO]}, year = {2009}, url = {http://arxiv.org/abs/0906.4151} }
Sesana, A., Gair, J., Mandel, I. & Vecchio, A.	Observing Gravitational Waves from the First Generation of Black Holes [Abstract] [BibTeX]	2009	The Astrophysical Journal Letters Vol. 698(2), pp. L129	article	URL
Abstract: The properties of the first generation of black hole seeds trace and distinguish different models of formation of cosmic structure in the high-redshift universe. The observational challenge lies in identifying black holes in the mass range ~100-1000 M ##IMG## [http://ej.iop.org/icons/Entities/sun.gif] sun at redshift z ~ 10. The typical frequencies of gravitational waves produced by the coalescence of the first generation of light seed black hole binaries fall in the gap between the spectral ranges of low-frequency space-borne detectors (e.g., LISA) and high-frequency ground-based detectors (e.g., LIGO, Virgo, and GEO 600). As such, these sources are targets for proposed third-generation ground-based instruments, such as the Einstein Telescope which is currently in design study. Using galaxy merger trees and four different models of black hole accretionâ€”which are meant to illustrate the potential of this new type of source rather than to yield precise event-rate predictionsâ€”we find that such detectors could observe a few to a few tens of seed black hole merger events in three years and provide possibly unique information on the evolution of structure in the corresponding era. We show further that a network of detectors may be able to measure the luminosity distance to sources to a precision of ~40%, allowing us to be confident of the high-redshift nature of the sources.
BibTeX: @article{Sesana2009, author = {Alberto Sesana and Jonathan Gair and Ilya Mandel and Alberto Vecchio}, title = {Observing Gravitational Waves from the First Generation of Black Holes}, journal = {The Astrophysical Journal Letters}, year = {2009}, volume = {698}, number = {2}, pages = {L129}, url = {http://stacks.iop.org/1538-4357/698/i=2/a=L129} }
Tanja Hinderer, Benjamin D. Lackey, R.N.L.J.S.R.	Tidal deformability of neutron stars with realistic equations of state and their gravitational wave signatures in binary inspiral [Abstract] [BibTeX]	2009	arXiv:0911.3535v1 [astro-ph.HE]	article	URL
Abstract: The early part of the gravitational wave signal of binary neutron star inspirals can potentially yield robust information on the nuclear equation of state. The influence of a star's internal structure on the waveform is characterized by a single parameter: the tidal deformability lambda, which measures the star's quadrupole deformation in response to the companion's perturbing tidal field. We calculate lambda for a wide range of equations of state and find that the value of lambda spans an order of magnitude for the range of equation of state models considered. An analysis of the feasibility of discriminating between neutron star equations of state with gravitational wave observations of the early part of the inspiral reveals that the measurement error in lambda increases steeply with the total mass of the binary. Comparing the errors with the expected range of lambda, we find that Advanced LIGO observations of binaries at a distance of 100 Mpc will probe only unusually stiff equations of state, while the proposed Einstein Telescope is likely to see a clean tidal signature.
BibTeX: @article{TanjaHinderer2009, author = {Tanja Hinderer, Benjamin D. Lackey, Ryan N. Lang, Jocelyn S. Read}, title = {Tidal deformability of neutron stars with realistic equations of state and their gravitational wave signatures in binary inspiral}, journal = {arXiv:0911.3535v1 [astro-ph.HE]}, year = {2009}, url = {http://arxiv.org/abs/0911.3535v1} }
Yunes, N., Arun, K.G., Berti, E. & Will, C.M.	Post-circular expansion of eccentric binary inspirals: Fourier-domain waveforms in the stationary phase approximation [BibTeX]	2009	Phys. Rev. D Vol. 80(8), pp. 084001	article	DOI
BibTeX: @article{Yunes2009, author = {Yunes, Nicolas and Arun, K. G. and Berti, Emanuele and Will, Clifford M.}, title = {Post-circular expansion of eccentric binary inspirals: Fourier-domain waveforms in the stationary phase approximation}, journal = {Phys. Rev. D}, publisher = {American Physical Society}, year = {2009}, volume = {80}, number = {8}, pages = {084001}, doi = {http://dx.doi.org/10.1103/PhysRevD.80.084001} }
Zhao, W., Van Den Broeck, C., Baskaran, D. & Li, T.G.F.	Determination of dark energy by the Einstein Telescope: Comparing with CMB, BAO, and SNIa observations [BibTeX]	2011	Phys. Rev. D Vol. 83(2), pp. 023005	article	DOI
BibTeX: @article{PhysRevD.83.023005, author = {Zhao, W. and Van Den Broeck, C. and Baskaran, D. and Li, T. G. F.}, title = {Determination of dark energy by the Einstein Telescope: Comparing with CMB, BAO, and SNIa observations}, journal = {Phys. Rev. D}, publisher = {American Physical Society}, year = {2011}, volume = {83}, number = {2}, pages = {023005}, doi = {http://dx.doi.org/10.1103/PhysRevD.83.023005} }
Zhu, X.-J., Howell, E., Regimbau, T., Blair, D. & Zhu, Z.-H.	Stochastic Gravitational Wave Background from Coalescing Binary Black Holes [Abstract] [BibTeX]	2011	arXiv:1104.3565v2 [gr-qc]	article	URL
Abstract: We estimate the stochastic gravitational wave (GW) background signal from the field population of coalescing binary stellar mass black holes (BHs) throughout the Universe. This study is motivated by recent observations of BH-Wolf-Rayet star systems and by new estimates in the metallicity abundances of star forming galaxies that imply BH-BH systems are more common than previously assumed. Using recent analytical results of the inspiral-merger-ringdown waveforms for coalescing binary BH systems, we estimate the resulting stochastic GW background signal. Assuming average quantities for the single source energy emissions, we explore the parameter space of chirp mass and local rate density required for detection by advanced and third generation interferometric GW detectors. For an average chirp mass of 8.7$M_odot$, we find that detection through 3 years of cross-correlation by two advanced detectors will require a rate density, $r_0 geq 0.5 Mpc^-3 Myr^-1$. Combining data from multiple pairs of detectors can reduce this limit by up to 40%. Investigating the full parameter space we find that detection could be achieved at rates $r_0 sim 0.1 Mpc^-3 Myr^-1$ for populations of coalescing binary BH systems with average chirp masses of $sim 15M_odot$ which are predicted by recent studies of BH-Wolf-Rayet star systems tepBulik08. While this scenario is at the high end of theoretical estimates, cross-correlation of data by two Einstein Telescopes could detect this signal under the condition $r_0 geq 10^-3 Mpc^-3 Myr^-1$. Such a signal could potentially mask a primordial GW background signal of dimensionless energy density, $GWsim 10^-10$, around the (1--500) Hz frequency range.
BibTeX: @article{Zhu2011, author = {Zhu, Xing-Jiang and Howell, Eric and Regimbau, Tania and Blair, David and Zhu, Zong-Hong}, title = {Stochastic Gravitational Wave Background from Coalescing Binary Black Holes}, journal = {arXiv:1104.3565v2 [gr-qc]}, year = {2011}, url = {http://arxiv.org/pdf/1104.3565v2} }

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