The Clipped Power Spectrum Fergus Simpson University of Edinburgh FS, James, Heavens, Heymans (2011 PRL) FS, Heavens, Heymans (arXiv:1306.6349)

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Presentation transcript:

The Clipped Power Spectrum Fergus Simpson University of Edinburgh FS, James, Heavens, Heymans (2011 PRL) FS, Heavens, Heymans (arXiv: )

Outline  Introduction to Clipping  Part I: The Clipped Bispectrum  Part II: The Clipped Power Spectrum

Outline  Introduction to Clipping  Part I: The Clipped Bispectrum  Part II: The Clipped Power Spectrum

Ripples Waves (hard) (easy)

…but also spatial dependence: Accuracy of Perturbation Theory Not only time dependence…

Local Density Transformations Reduce nonlinear contributions by suppressing high density regions Neyrinck et al (2009)

Clipping Typically only 1% of the field is subject to clipping

Outline  Introduction to Clipping  Part I: The Clipped Bispectrum  Part II: The Clipped Power Spectrum

The Bispectrum

The Clipped Bispectrum

FS, James, Heavens, Heymans PRL (2011)

Part I Summary  >10 4 times more triangles available after clipping  Enables precise determination of galaxy bias BUT  Why does it work to such high k?  What about P(k)?

Outline  Introduction to Clipping  Part I: The Clipped Bispectrum  Part II: The Clipped Power Spectrum

The Power Spectrum

The Clipped Power Spectrum

Clipped Perturbation Theory Reduce contributions from by suppressing regions with large

Clipping Part II: The Power Spectrum  Exact solution for a Gaussian Random Field δ G :  Exact solution for δ 2 :

The Clipped Power Spectrum

The Clipped Galaxy Power Spectrum

Parameter Constraints FS, Heavens, Heymans arXiv:

Part II: Summary  Clipped power spectrum is analytically tractable  Higher order PT terms are suppressed  Nonlinear galaxy bias terms are suppressed  Well approximated by  Applying δ max allows k max to be increased  ~ 300 times more Fourier modes available  BUT what happens in redshift space?