Science with the space-based interferometer eLISA: Supermassive black hole binaries

Klein, Antoine; Barausse, Enrico; Sesana, Alberto; Petiteau, Antoine; Berti, Emanuele; Babak, S.; Gair, J. R.; Aoudia, S.; Hinder, Ian; Ohme, F.; Wardell, Barry

doi:10.1103/physrevd.93.024003

Cited by 466 publications

(552 citation statements)

References 136 publications

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“…The shape of this spectrum is quite complicated because different periods of a binary system's evolution dominate at different frequencies and have different frequency dependences [70]. For the design of LISA we consider we expect the impact of such a foreground to be small compared to the acceleration noise [72]. The BBO design we consider peaks at 0.3 Hz, which is expected to be relatively free of such sources of noise [73,74].…”

Section: IVmentioning

confidence: 99%

Finding the chiral gravitational wave background of an axion- SU(2) inflationary model using CMB observations and laser interferometers

et al. 2018

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A detection of B-mode polarization of the Cosmic Microwave Background (CMB) anisotropies would confirm the presence of a primordial gravitational wave background (GWB). In the inflation paradigm this would be an unprecedented probe of the energy scale of inflation as it is directly proportional to the power spectrum of the GWB. However, similar tensor perturbations can be produced by the matter fields present during inflation, breaking the simple relationship between energy scale and the tensor-to-scalar ratio r. It is therefore important to find ways of distinguishing between the generation mechanisms of the GWB. Without doing a full model selection, we analyse the detectability of a new axion-SU(2) gauge field model by calculating the signal-to-noise of future CMB and interferometer observations sensitive to the chirality of the tensor spectrum. We forecast the detectability of the resulting CMB temperature and B-mode (TB) or E-mode and B-mode (EB) cross-correlation by the LiteBIRD satellite, considering the effects of residual foregrounds, gravitational lensing, and assess the ability of such an experiment to jointly detect primordial TB and EB spectra and self-calibrate its polarimeter. We find that LiteBIRD will be able to detect the chiral signal for r * > 0.03 with r * denoting the tensor-to-scalar ratio at the peak scale, and that the maximum signal-to-noise for r * < 0.07 is ∼ 2. We go on to consider an advanced stage of a LISA-like mission, which is designed to be sensitive to the intensity and polarization of the GWB. We find that such experiments would complement CMB observations as they would be able to detect the chirality of the GWB with high significance on scales inaccessible to the CMB. We conclude that CMB two-point statistics are limited in their ability to distinguish this model from a conventional vacuum fluctuation model of GWB generation, due to the fundamental limits on their sensitivity to parity-violation. In order to test the predictions of such a model as compared to vacuum fluctuations it will be necessary to test deviations from the self-consistency relation, or use higher order statistics to leverage the non-Gaussianity of the model. On the other hand, in the case of a spectrum peaked at very small scales inaccessible to the CMB, a highly significant detection could be made using space-based laser interferometers.

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Section: IVmentioning

confidence: 99%

Finding the chiral gravitational wave background of an axion- SU(2) inflationary model using CMB observations and laser interferometers

et al. 2018

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“…During the study, different baselines for a spaceborne interferometer were considered. Full details can be found in [19]. In the following, six baselines featuring one, two or five million km arm-length (A1, A2, A5) and two possible low frequency noises -namely the LISA Pathfinder goal (N1) and the original LISA requirement (N2) -are considered.…”

Section: Lisa Sensitivitymentioning

confidence: 99%

Multi-band gravitational wave astronomy: science with joint space- and ground-based observations of black hole binaries

Sesana¹

2017

J. Phys.: Conf. Ser.

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Soon after the observation of the first black hole binary (BHB) by advanced LIGO (aLIGO), GW150914, it was realised that such a massive system would have been observable in the milli-Hz (mHz) band few years prior to coalescence. Operating in the frequency range 0.1-100 mHz, the Laser Interferometer Space Antenna (LISA) can potentially detect up to thousands inspiralling BHBs, based on the coalescence rates inferred from the aLIGO first observing run (O1). The vast majority of them (those emitting at f < 10 mHz) will experience only a minor frequency drift during LISA lifetime, resulting in signals similar to those emitted by galactic white dwarf binaries. At f > 10 mHz however, several of them will sweep through the LISA band, eventually producing loud coalescences in the audio-band probed by aLIGO. This contribution reviews the scientific potential of these new class of LISA sources which, in the past few months, has been investigated in several contexts, including multi-messenger and multi-band gravitational wave astronomy, BHB astrophysics, tests of alternative theories of gravity and cosmography.

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“…In addition to high-frequency GWs, Pulsar Timing Arrays (PTAs, [22]) and LISA [23] should also be detecting GWs by the late-2020's. Potential source classes for PTAs with electromagnetic counterparts including binary supermassive black holes with periods of order ∼ 1 year [24], for which AMEGO's monitoring of blazars could find sources.…”

Section: Gravitational Wave (Gw) Counterpartsmentioning

confidence: 99%

AMEGO: Transients and Multi-Messenger Sources

Racusin¹,

Lien²,

Hartmann³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The AMEGO Teamhttps://asd.gsfc.nasa.gov/amego/ The All-Sky Medium Energy Gamma-ray Observatory (AMEGO) will survey the entire sky every 3 hours with its wide field of view and excellent continuum sensitivity between 200 keV and 10 GeV, discovering new sources and automatically providing follow-up observation for multiwavelength and multi-messenger transient sources. Many of these sources have the energy spectral peaks in the AMEGO band, and/or spectral behavior that is not well understood at these energies. AMEGO will discover new gamma-ray bursts, magnetar flares, active galaxy flares, novae, and monitor the long-term light curves of variable sources including Galactic binaries. Thanks to its wide FoV and survey strategy, AMEGO is also well placed to search for electromagnetic counterparts to gravitational wave and neutrino sources.

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Science with the space-based interferometer eLISA: Supermassive black hole binaries

Cited by 466 publications

References 136 publications

Finding the chiral gravitational wave background of an axion- SU(2) inflationary model using CMB observations and laser interferometers

Finding the chiral gravitational wave background of an axion- SU(2) inflationary model using CMB observations and laser interferometers

Multi-band gravitational wave astronomy: science with joint space- and ground-based observations of black hole binaries

AMEGO: Transients and Multi-Messenger Sources

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