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  • Searches for Continuous Gravitational Waves from Fifteen Supernova Remnants and Fomalhaut b with Advanced LIGO
    Ananyeva, A; Areeda, J S; Arnaud, N; Ballmer, S W; Bhandare, R; Bilgili, S A; Bloemen, S; Bossilkov, V; Brady, P R; Brau, J E; Brighenti, F; Brisson, V; Cadonati, L; Cerretani, G; Chao, S; Chia, H Y; Cho, M; Cleva, F; Cocchieri, C; Costa, C A; Daw, E J; Degallaix, J; Deléglise, S; Dent, T; Díaz, M C; Dietrich, T; Estelles, H; Fairhurst, S; Favata, M; Fidecaro, F; Fyffe, M; Gair, J R; Giazotto, A; Goncharov, B; Gruning, P; Hall, B R; Haughian, K; Heidmann, A; Hennig, J; Hild, S; Idzkowski, B; Ingram, C; Irwin, B; Jiang, J; Katsanevas, S; King, E J; Koekoek, G; Kumar, R; Lanza, R K; Lo, R K L; Lockerbie, N A; London, L T; Lorenzini, M; Magaña-Sandoval, F; L Magaña Zertuche; Magee, R M; Malik, A; Mansell, G L; Marsat, S; Matas, A; Mazumder, N; McClelland, D E; Miller, A; Millhouse, M; Minazzoli, O; Mitra, S; Nagar, A; Palashov, O; Pant, B C; Passuello, D; Pearlstone, B L; Prasanna, R; Rajbhandari, B; Raymond, V; Razzano, M; Roma, V J; Romel, C L; Rose, K; Schnabel, R; Shao, L; Smith, R J E; Sorazu, B; Standke, M; Steinmeyer, D; Sunil, S; Torres-Forné, A; Trozzo, L; Urban, A L; Vajente, G; van der Schaaf, L; van Veggel, A A; Vasúth, M; Walker, M; Wang, W H; Wellmann, F; Wysocki, D M; Yamamoto, H; Zevin, M; Zhang, L; Zhang, T

    arXiv.org, 08/2021
    Paper, Journal Article

    We describe directed searches for continuous gravitational waves from sixteen well localized candidate neutron stars assuming none of the stars has a binary companion. The searches were directed toward fifteen supernova remnants and Fomalhaut~b, an extrasolar planet candidate which has been suggested to be a nearby old neutron star. Each search covered a broad band of frequencies and first and second time derivatives. After coherently integrating spans of data from the first Advanced LIGO observing run of 3.5--53.7 days per search, applying data-based vetoes and discounting known instrumental artifacts, we found no astrophysical signals. We set upper limits on intrinsic gravitational wave strain as strict as \(1\times10^{-25}\), on fiducial neutron star ellipticity as strict as \(2\times10^{-9}\), and on fiducial \(r\)-mode amplitude as strict as \(3\times10^{-8}\).

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