new results in the geometry of random fields, with applications to cmb and galaxy density keith...

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New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics and Statistics, McConnell Brain Imaging Centre, Montreal Neurological Institute, McGill University

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Page 1: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

New results in the geometry of random fields, with applications

to CMB and galaxy density

Keith Worsley, Hugo Drouin, Pauline Klein

Department of Mathematics and Statistics, McConnell Brain Imaging Centre, Montreal Neurological Institute,

McGill University

Page 2: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

Milky way

Page 3: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

-5 -4 -3 -2 -1 0 1 2 3 4 5-100

-80

-60

-40

-20

0

20

40

60

80

100CfA red shift survey, FWHM=13.3

Gaussian threshold

Eul

er C

hara

cter

istic

(E

C)

"Bubble"topology

"Sponge"topology

"Meat ball" topology

CfARandomExpected

Page 4: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

The 2dF Galaxy Redshift Survey: spectra and redshiftsMon. Not. R. Astron. Soc. 328, 1039–1063 (2001)

Milky way

Page 5: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics
Page 6: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

0

500

1000First scan of fMRI data

-5

0

5

T statistic for hot - warm effect

0 100 200 300

870880890 hot

restwarm

Highly significant effect, T=6.59

0 100 200 300

800

820hotrestwarm

No significant effect, T=-0.74

0 100 200 300

790800810

Drift

Time, seconds

fMRI data: 120 scans, 3 scans each of hot, rest, warm, rest, hot, rest, …

T = (hot – warm effect) / S.d. ~ t110 if no effect

Page 7: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

Gaussianized χ2 field?

-5 -4 -3 -2 -1 0 1 2 3 4 5-30

-20

-10

0

10

20

30

CfAGaussianChisq, 5 dfChisq, 4 dfChisq, 3 df

Gaussian threshold

EC

Page 8: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

-5 -4 -3 -2 -1 0 1 2 3 4 5-30

-20

-10

0

10

20

30

CfAGaussianT, 10 dfT, 6 dfT, 4 df

Gaussianized T field?

Gaussian threshold

EC

Page 9: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

EC for WMAP, unsmoothed, FWHM = 1.6o

-5 -4 -3 -2 -1 0 1 2 3 4 5-2500

-2000

-1500

-1000

-500

0

500

1000

1500

2000

2500

Gaussian threshold

EC

ObservedExpected

-8 -7 -6 -5 -4-10

0

10

4 5 6 7 80

10

20

Page 10: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

-5 -4 -3 -2 -1 0 1 2 3 4 5-200

-150

-100

-50

0

50

100

150

Observed - Expected+1 sd (~ \sqrt Expected)-1 sd (~ \sqrt Expected)

Observed – Expected EC, with Poisson sd in tails

EC

Gaussian threshold

Page 11: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

EC for WMAP smoothed to FWHMo (expected)no smoothing

scale space

-5 0 5

-2000

0

2000 1.6o

EC

-5 0 5-1000

0

10002.7o

-5 0 5-500

0

500

4.1o

-5 0 5-200

0

200

6.2o

EC

-5 0 5-100

0

1008.7o

-5 0 5-50

0

5012.1o

-5 0 5-50

0

50

16.1o

EC

threshold-5 0 5

-20

0

20

20.5o

threshold-5 0 5

-1000

0

1000

20001.6o 20.5o

threshold

Page 12: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

Simulation (expected)no smoothing

scale space

-5 0 5

-2000

0

20001.7o

EC

-5 0 5-2000

0

2000

2o

-5 0 5-1000

0

1000

2.7o

-5 0 5-500

0

5003.5o

EC

-5 0 5

-200

0

200 4.8o

-5 0 5

-100

0

100 6.6o

-5 0 5-100

0

100

9.1o

EC

threshold-5 0 5

-50

0

50

12.7o

threshold-5 0 5

-1000

0

1000

2000

1.7o 12.7o

threshold

Page 13: New results in the geometry of random fields, with applications to CMB and galaxy density Keith Worsley, Hugo Drouin, Pauline Klein Department of Mathematics

Scale space WMAP data

-5 -4 -3 -2 -1 0 1 2 3 4 5-1000

-500

0

500

1000

1500

2000

1.6o 20.5o

Gaussian threshold

EC

Observed

Expected

-4.5 -4 -3.5-10

0

10

3.5 4 4.5 50

10

20