A Superconducting Tensor Detector for Mid-Frequency Gravitational Waves: Its Multichannel Nature and Main Astrophysical Targets

• Published in: Progress of theoretical and experimental physics Vol. 2024; no. 5
• Main Authors: Bae, Yeong-Bok, Park, Chan, Son, Edwin J, Ahn, Sang-Hyeon, Jeong, Minjoong, Kang, Gungwon, Kim, Chunglee, Kim, Dong Lak, Kim, Jaewan, Kim, Whansun, Lee, Hyung Mok, Lee, Yong-Ho, Norton, Ronald S, Oh, John J, Oh, Sang Hoon, Paik, Ho Jung
• Format: Journal Article
• Language: English
• Published: Oxford Oxford University Press 01.05.2024
• Subjects: Gravitational waves; Sensors
• ISSN: 2050-3911; 2050-3911
• DOI: 10.1093/ptep/ptae045

Mid-frequency band gravitational-wave detectors will be complementary to the existing Earth-based detectors (sensitive above 10 Hz or so) and the future space-based detectors such as the Laser Interferometer Space Antenna (LISA), which will be sensitive below around 10 mHz. A ground-based superconducting omnidirectional gravitational radiation observatory (SOGRO) has recently been proposed along with several design variations for the frequency band of 0.1–10 Hz. For two conceptual designs of SOGRO (i.e. SOGRO and advanced SOGRO [aSOGRO]), we examine their multichannel natures, sensitivities, and science cases. One of the key characteristics of the SOGRO concept is its six detection channels. The response functions of each channel are calculated for all possible gravitational wave (GW) polarizations including scalar and vector modes. Combining these response functions, we also confirm the omnidirectional nature of SOGRO. Hence, even a single SOGRO detector will be able to determine the position of a source and polarizations of GWs, if detected. Taking into account SOGRO’s sensitivity and technical requirements, two main targets are most plausible: GWs from compact binaries and stochastic backgrounds. Based on assumptions we consider in this work, detection rates for intermediate-mass binary black holes (in the mass range of hundreds up to $10^{5}\, M_\odot$) are expected to be 0.0065–8.1 yr−1. In order to detect the stochastic GW background, multiple detectors are required. Two aSOGRO detector networks may be able to put limits on the stochastic background beyond the indirect limit from cosmological observations.