Abstract
After first reviewing the gravitational wave (GW) spectral classification. we discuss the sensitivities of GW detection in space aimed at low frequency band (100 nHz–100 mHz) and middle frequency band (100 mHz–10 Hz). The science goals are to detect GWs from (i) Supermassive Black Holes; (ii) Extreme-Mass-Ratio Black Hole Inspirals; (iii) Intermediate-Mass Black Holes; (iv) Galactic Compact Binaries; (v) Stellar-Size Black Hole Binaries; and (vi) Relic GW Background. The detector proposals have arm length ranging from 100 km to 1.35×109 km (9 AU) including (a) Solar orbiting detectors and (b) Earth orbiting detectors. We discuss especially the sensitivities in the frequency band 0.1-10 μHz and the middle frequency band (0.1 Hz–10 Hz). We propose and discuss AMIGO as an Astrodynamical Middlefrequency Interferometric GW Observatory.
Highlights
After first reviewing the gravitational wave (GW) spectral classification. we discuss the sensitivities of GW detection in space aimed at low frequency band (100 nHz 100 mHz) and middle frequency band (100 mHz 10 Hz)
We propose a first-generation middle-frequency mission concept AMIGO: Astrodynamical Middle-frequency Interferometric GW Observatory with the following specification: Arm length: 10,000 km
4 Discussion and outlook s measurement of GWs from black hole coalescence fully ushered us into the era of GW astronomy
Summary
After first reviewing the gravitational wave (GW) spectral classification. we discuss the sensitivities of GW detection in space aimed at low frequency band (100 nHz 100 mHz) and middle frequency band (100 mHz 10 Hz). To possibly increase the sensitivity in the frequency band 0.1-10 Hz, Super-ASTROD with arm length of 9 AU has been proposed [8].
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