Newtonian noise studies for future generation gravitational-wave - PowerPoint PPT Presentation

Newtonian noise studies for future generation gravitational-wave detectors Pat Meyers University of Melbourne OzGrav November 14th, 2018 � 1

Outline • Gravitational waves (GWs) and LIGO • The case for low frequency sensitivity • Proposed low frequency detectors • Newtonian noise • Basic seismology • Newtonian noise studies with Homestake 3D seismometer array • Seismologically useful results 2

3 GW Polarization “Plus” Polarization time

4 GW Polarization “Plus” Polarization time “Cross” Polarization time

5 GW Amplitude GW amplitude is measured in strain : h = Δ L / L Blue arrows divided by radius of ring (from previous slide)

6 Advanced LIGO/Advanced Virgo (b) (a) Martynov, D. V., et al. (2016). Phys. Rev. D , 93 (11), 433. http://doi.org/10.1103/PhysRevD.93.112004

7 GW sources targeted by LIGO rotating neutron stars stochastic background Long Short compact binary mergers supernovae Well-modeled Poorly-modeled

8 Stochastic Gravitational-wave Background Sources SGWB Properties/Assumptions • • Unresolved astrophysical sources Gaussian • • CBCs unpolarized • • Rotating neutron stars stationary • • Early universe models Isotropic • • cosmic strings In some searches (not discussed here) we relax one or more of these assumptions

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Critical energy density to close the universe