Detector configuration of DECIGO/BBO and identification of cosmological neutron-star binaries

By Kent Yagi, N. Seto. 2011

377 citations recorded by the source corpus.

The primary target for the planned space-borne gravitational wave interferometers DECIGO/BBO (Decihertz Interferometer Gravitational Wave Observatory/Big Bang Observer) is a primordial gravitational wave background. However there exist astrophysical foregrounds, and among them, gravitational waves from neutron-star (NS) binaries are the solid and strong component that must be identified and subtracted. In this paper, we discuss the geometry of detector configurations preferable for identifying the NS/NS binary signals. As a first step, we analytically estimate the minimum signal-to-noise ratios of the binaries for several static detector configurations that are characterized by adjustable geometrical parameters, and determine the optimal values for these parameters. Next we perform numerical simulations to take into account the effect of detector motions, and find reasonable agreements with the analytical results. We show that, with the standard network formed by 4 units of triangle detectors, the proposed BBO sensitivity would be sufficient in receiving gravitational waves from all the NS/NS binaries at z{<=}5 with signal-to-noise ratios higher than 25. We also discuss the minimum sensitivity of DECIGO required for the foreground identification.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/bf36ce495c716774e34dfbc8730671f5ce1526ec

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Citations in the corpus

• Beyond the Standard Models with cosmic strings (2019, methodology): “3 Results For the purpose of our study, we computed the power-law integrated sensitivity curve ΩPI(f), starting from the noise spectral density in [108] for ET, [110] for CE and [106] for BBO/DECIGO.”
• Gravitational-wave sensitivity curves (2014, methodology): “We use a simple analytic fit to the sensitivity curve for ALIA (Bender et al 2013), while for DECIGO and BBO, fits to the sensitivity curves given by Yagi and Seto (2011) are used.”
• Phase transitions in an expanding universe: stochastic gravitational waves in standard and non-standard histories (2020, neutral): “(DECIGO) [10], Taiji [11], and Tianqin [12].”
• Probing the pre-BBN universe with gravitational waves from cosmic strings (2018, background): “Indeed, GWs emitted as far back as inflation could potentially be detected by LIGO/Virgo [24] or proposed future detectors such as LISA [25], BBO/DECIGO [26], the Einstein Telescope (ET) [27, 28], and Cosmic Explorer (CE) [29].”
• Generating PBHs and small-scale GWs in two-field models of inflation (2020, background): “Moving to higher frequencies ΩGW h 2 peaks well inside the range of detectability of LISA [102, 103] and its tail can also be detected by DECIGO/BBO [104] for certain values of b1.”
• Detecting high-frequency gravitational waves with microwave cavities (2021, background): “[7] Kent Yagi and Naoki Seto, “Detector configuration of DECIGO/BBO and identification of cosmological neutron-star binaries,” Phys.”
• Induced gravitational waves as a probe of thermal history of the universe (2020, background): “V. DISCUSSION AND CONCLUSIONS The possible detection of stochastic gravitational wave backgrounds with cosmic origin by future space based detectors, e.g. LISA [5], Tiaji [6], Tianqin [7], DECIGO [8, 9], AION/MAGIS [10], ET [11] or PTA [12–15], may yield crucial information about the physics of the ”
• Gravitational wave constraints on the primordial black hole dominated early universe (2020, methodology): “With newly derived analytical formulas [35–38], the so-called induced GW are also drawing a lot of interest since they could lie within the future observational window of LISA [39], Taiji [40], Tianqin [41], DECIGO [42, 43], AION/MAGIS [44], ET [45] and PTA [46, 47].”
• Gravitational wave, collider and dark matter signals from a scalar singlet electroweak baryogenesis (2017, background): “3 and 4, we illustrate this effect and show the regions of the parameter space accessible to the most promising future GW detectors, specifically LISA (with the most promising configuration A5M5) [68] and BBO [69].”
• Gravitational wave energy budget in strongly supercooled phase transitions (2019, methodology): “We also show the envisioned sensitivities of the proposed future missions DECIGO [80] and Big Bang Observer (BBO) [81, 82].”
• On the maximal strength of a first-order electroweak phase transition and its gravitational wave signal (2018, background): “Finally, we also show the prospective sensitivities of the DECIGO [98] and Big Bang Observer (BBO) [99, 100] projects in the frequency range between LISA and LIGO (another project aimed at probing a similar frequency range is MAGIS-100 [101]).”