A New Source Detection Algorithm Using the False-Discovery Rate

Hopkins, A. M.; Miller, Christopher J.; Connolly, A. J.; Genovese, Christopher R.; Nichol, R. C.; Wasserman, Larry

doi:10.1086/338316

Cited by 123 publications

(131 citation statements)

References 7 publications

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“…This technique was described by Miller et al (2001);Hopkins et al (2002); Starck et al (2006b); Pires et al (2006) for several astrophysical applications. Instead of controlling the chance of any false positives, FDR controls the expected proportion of false positives.…”

Section: Appendix A: the Fdr Methodsmentioning

confidence: 99%

Cosmological model discrimination with weak lensing

Pires

Starck

Amara

et al. 2009

A&A

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Weak gravitational lensing provides a unique way of mapping directly the dark matter in the Universe. The majority of lensing analyses use the two-point statistics of the cosmic shear field to constrain the cosmological model, a method that is affected by degeneracies, such as that between σ 8 and Ω m which are respectively the rms of the mass fluctuations on a scale of 8 Mpc/h and the matter density parameter, both at z = 0. However, the two-point statistics only measure the Gaussian properties of the field, and the weak lensing field is non-Gaussian. It has been shown that the estimation of non-Gaussian statistics for weak lensing data can improve the constraints on cosmological parameters. In this paper, we systematically compare a wide range of non-Gaussian estimators to determine which one provides tighter constraints on the cosmological parameters. These statistical methods include skewness, kurtosis, and the higher criticism test, in several sparse representations such as wavelet and curvelet; as well as the bispectrum, peak counting, and a newly introduced statistic called wavelet peak counting (WPC). Comparisons based on sparse representations indicate that the wavelet transform is the most sensitive to non-Gaussian cosmological structures. It also appears that the most helpful statistic for non-Gaussian characterization in weak lensing mass maps is the WPC. Finally, we show that the σ 8 -Ω m degeneracy could be even better broken if the WPC estimation is performed on weak lensing mass maps filtered by the wavelet method, MRLens.

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Section: Appendix A: the Fdr Methodsmentioning

confidence: 99%

Cosmological model discrimination with weak lensing

Pires

Starck

Amara

et al. 2009

A&A

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“…Both packages allow calculation of rms and mean images and identification of sources in radio maps through the use either of a false detection rate (FDR) method (Hopkins et al 2002), or of a threshold technique that locates islands of emission above some multiple of the noise in the image. Gaussians are then fitted to each island for accurate measurement of source properties.…”

Section: Source Findingmentioning

confidence: 99%

The LOFAR Multifrequency Snapshot Sky Survey (MSSS)

Heald

Pizzo

Orrù

et al. 2015

A&A

107

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We present the Multifrequency Snapshot Sky Survey (MSSS), the first northern-sky Low Frequency Array (LOFAR) imaging survey. In this introductory paper, we first describe in detail the motivation and design of the survey. Compared to previous radio surveys, MSSS is exceptional due to its intrinsic multifrequency nature providing information about the spectral properties of the detected sources over more than two octaves (from 30 to 160 MHz). The broadband frequency coverage, together with the fast survey speed generated by LOFAR's multibeaming capabilities, make MSSS the first survey of the sort anticipated to be carried out with the forthcoming Square Kilometre Array (SKA). Two of the sixteen frequency bands included in the survey were chosen to exactly overlap the frequency coverage of large-area Very Large Array (VLA) and Giant Metrewave Radio Telescope (GMRT) surveys at 74 MHz and 151 MHz respectively. The survey performance is illustrated within the MSSS Verification Field (MVF), a region of 100 square degrees centered at (α, δ) J2000 = (15 h , 69 • ). The MSSS results from the MVF are compared with previous radio survey catalogs. We assess the flux and astrometric uncertainties in the catalog, as well as the completeness and reliability considering our source finding strategy. We determine the 90% completeness levels within the MVF to be 100 mJy at 135 MHz with 108 resolution, and 550 mJy at 50 MHz with 166 resolution. Images and catalogs for the full survey, expected to contain 150 000-200 000 sources, will be released to a public web server. We outline the plans for the ongoing production of the final survey products, and the ultimate public release of images and source catalogs.

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“…The result of this analysis shows clearly that it will be crucial to first develop and then implement an automated algorithm for establishing the appropriate scale size on which to estimate the 'local' background and rms noise values for each image, and that this may not be common to all images. This analysis also suggests that the false discovery rate approach (Hopkins et al 2002) to thresholding may be the most robust, optimising for both completeness and reliability.…”

Section: Compact Source Extractionmentioning

confidence: 91%