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Gravitational wave detection in space

Wei-Tou Ni

School of Optical-Electrical and Computer Engineering, University of Shanghai for Science and Technology, 516, Jun Gong Rd., Shanghai 200093, P. R. China

Kavli Institute for Theoretical Physics China, CAS, Beijing 100190, P. R. China

E-mail Address: weitouni@163.com

E-mail Address: weitou@gmail.com

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https://doi.org/10.1142/S0218271816300019Cited by:41 (Source: Crossref)

Abstract

Gravitational Wave (GW) detection in space is aimed at low frequency band (100nHz–100mHz) and middle frequency band (100mHz–10Hz). The science goals are the detection of GWs from (i) Supermassive Black Holes; (ii) Extreme-Mass-Ratio Black Hole Inspirals; (iii) Intermediate-Mass Black Holes; (iv) Galactic Compact Binaries and (v) Relic GW Background. In this paper, we present an overview on the sensitivity, orbit design, basic orbit configuration, angular resolution, orbit optimization, deployment, time-delay interferometry (TDI) and payload concept of the current proposed GW detectors in space under study. The detector proposals under study have arm length ranging from 1000km to $1.3 \times 1 0^{9}$ km (8.6AU) including (a) Solar orbiting detectors — (ASTROD Astrodynamical Space Test of Relativity using Optical Devices (ASTROD-GW) optimized for GW detection), Big Bang Observer (BBO), DECi-hertz Interferometer GW Observatory (DECIGO), evolved LISA (e-LISA), Laser Interferometer Space Antenna (LISA), other LISA-type detectors such as ALIA, TAIJI etc. (in Earthlike solar orbits), and Super-ASTROD (in Jupiterlike solar orbits); and (b) Earth orbiting detectors — ASTROD-EM/LAGRANGE, GADFLI/GEOGRAWI/g-LISA, OMEGA and TIANQIN.

This paper is to be published also as Chapter 12 of the book “One Hundred Years of General Relativity: From Genesis and Empirical Foundations to Gravitational Waves, Cosmology and Quantum Gravity”, ed. by W.-T. Ni (World Scientific, Singapore, 2016).

Keywords:

PACS: 04.80.Nn, 04.80.-y, 95.30.Sf, 95.55.Ym, 98.62.Ai, 98.80.Es

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