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Seismic noise measures for underground gravitational wave detectors

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Abstract

The site characterisation of future underground gravitational wave detectors is based on spectral properties of the low frequency seismic noise. The evaluation of the collected long term seismological data in the Mátra Gravitational and Geophysical Laboratory revealed some aspects that are not apparent in short term spectral noise characterisation. In this paper we survey the methodology. In particular, we argue that the spectral properties are best represented by percentiles of the data instead of the mode, because it is noisy, sensitive to the discretization and intrinsic averaging, therefore it is less suitable for a robust characterisation. The suitable cumulative measures are also scrutinized.

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Notes

  1. Global strategies for gravitational wave astronomy. Report from the Dawn IV workshop; Amsterdam August 30, 31 2018. https://dcc.ligo.org/public/0158/P1900028/004. April 22, 2019.

  2. Black Forest line is originally approximates from below the 10th percentiles of the acceleration PSD of the Black Forest site (ET Science Team 2011).

  3. See the manual of the instrument. http://www.guralp.com/documents/DAS-030-0120.pdf.

  4. Other instruments, the Trillium seismometer in Beker et al. (2015), work with 128 Hz sampling rate. Then the 128 s interval is convenient for fast Fourier calculation, but hourly or daily spectra require truncations.

  5. Beker originally defined \(sigma\_{ET}\) also to distinguish the distributions of PSDs. In this paper we do not want to explore this quantity but focus only to the rms.

  6. The planned detection length of GW signals could reach 1–10000 s. It could be reasonable to use a more suitable—less than the order of expected detection length—than the \(14\times 128\,\mathrm{{s}}\) averaging of Beker et al. (2015). Furthermore the STA makes the overlapping much easier to handle.

References

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Acknowledgements

The work was supported by the Grants National Research, Development and Innovation Office—NKFIH 116197(116375) NKFIH 124366(124508) and NKFIH 123815. The support of the PHAROS (CA16214) and G2net (CA17137) COST Actions is also acknowledged. The authors thank Géza Huba for the constant support and help, for Zoltán Zimborás and Jan Harms for important remarks. Also the help and support of the Nitrokémia Zrt and GEO-FABER Zrt. is greatly acknowledged.

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Authors and Affiliations

  1. Institute for Particle and Nuclear Physics, MTA Wigner Research Centre for Physics, Konkoly-Thege Miklós út 29-33, Budapest, 1121, Hungary

    L. Ábel Somlai, P. Lévai, M. Vasúth & P. Ván

  2. Faculty of Sciences, University of Pécs, Ifjúság út 6, Pecs, 7624, Hungary

    L. Ábel Somlai

  3. MTA Research Centre for Astronomy and Earth Sciences, Geodetic and Geophysical Institute, Csatkai E. u. 6-8, Sopron, 9400, Hungary

    Zoltán Gráczer & Z. Wéber

  4. Department of Energy Engineering, Budapest University of Technology and Economics, Bertalan Lajos u. 4-6, Budapest, 1111, Hungary

    P. Ván

  5. Montavid Thermodynamic Research Group, Budapest, Hungary

    P. Ván

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  1. L. Ábel Somlai
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  2. Zoltán Gráczer
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  3. P. Lévai
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  4. M. Vasúth
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  5. Z. Wéber
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  6. P. Ván
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Correspondence to L. Ábel Somlai.

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Somlai, L.Á., Gráczer, Z., Lévai, P. et al. Seismic noise measures for underground gravitational wave detectors. Acta Geod Geophys 54, 301–313 (2019). https://doi.org/10.1007/s40328-019-00257-5

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  • DOI: https://doi.org/10.1007/s40328-019-00257-5

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