English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT

Released

Journal Article

Subtraction of temperature induced phase noise in the LISA frequency band

MPS-Authors
/persons/resource/persons40483

Nofrarias,  M.
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons40525

Hewitson,  M.
Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons40460

Heinzel,  G.
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

/persons/resource/persons40437

Danzmann,  K.
Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society;

External Ressource
No external resources are shared
Fulltext (public)

1302.5628.pdf
(Preprint), 844KB

PRD87_102003.pdf
(Any fulltext), 696KB

Supplementary Material (public)
There is no public supplementary material available
Citation

Nofrarias, M., Gibert, F., Karnesis, N., Garcia, A. F., Hewitson, M., Heinzel, G., et al. (2013). Subtraction of temperature induced phase noise in the LISA frequency band. Physical Review D, 87: 102003. doi:10.1103/PhysRevD.87.102003.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0013-AA44-E
Abstract
Temperature fluctuations are expected to be one of the limiting factors for gravitational wave detectors in the very low frequency range. Here we report the characterisation of this noise source in the LISA Pathfinder optical bench and propose a method to remove its contribution from the data. Our results show that temperature fluctuations are indeed limiting our measurement below one millihertz, and that their subtraction leads to a factor 5.6 (15 dB) reduction in the noise level at the lower end of the LISA measurement band 10^{-4} Hz, which increases to 20.2 (26 dB) at even lower frequencies, i.e., 1.5x10^{-5} Hz. The method presented here can be applied to the subtraction of other noise sources in gravitational wave detectors in the general situation where multiple sensors are used to characterise the noise source.