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1
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0142053792
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C.L. Bennett, Astrophys. J., Suppl. Ser. 148, 1 (2003); the public data and other WMAP papers are available at http://lambda.gsfc.nasa.gov/product/map.
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(2003)
Astrophys. J., Suppl. Ser.
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Bennett, C.L.1
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21
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Abell, G.O.1
Corwin, H.2
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22
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85038994413
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S. P. Boughn (private communication)
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S. P. Boughn (private communication).
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28
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85038984342
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We thank Doug Finkbeiner for extracting the fluxes of Andromeda in WMAP temperature maps
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We thank Doug Finkbeiner for extracting the fluxes of Andromeda in WMAP temperature maps.
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33
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85038997978
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K. M. Gorski, E. Hivon, and B. D. Wandelt, in Evolution of Large-Scale Structure: From Recombination to Garching, edited by A.J. Banday, R.S. Sheth, and L. da Costa (PrintPartners, Ipskamp, The Netherlands, 1999), p. 37; the HEALPix package is available from http://www.eso.org/science/healpix/
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K. M. Gorski, E. Hivon, and B. D. Wandelt, in Evolution of Large-Scale Structure: From Recombination to Garching, edited by A.J. Banday, R.S. Sheth, and L. da Costa (PrintPartners, Ipskamp, The Netherlands, 1999), p. 37; the HEALPix package is available from http://www.eso.org/science/healpix/.
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35
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85039014296
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We thank Eiichiro Komatsu for pointing out this identity
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We thank Eiichiro Komatsu for pointing out this identity.
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36
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0242456166
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E. Hivon, K.M. Gorski, C.B. Netterfield, B.P. Crill, S. Prunet, and F. Hansen, Astrophys. J. 567, 2 (2002).
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Hivon, E.1
Gorski, K.M.2
Netterfield, C.B.3
Crill, B.P.4
Prunet, S.5
Hansen, F.6
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38
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85039017857
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M.F. Skrutskie et al., in The Impact of Large Scale Near-IR Sky Survey, edited by F. Garzon et al. (Kluwer, Dordrecht, 1997), p. 187
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M.F. Skrutskie et al., in The Impact of Large Scale Near-IR Sky Survey, edited by F. Garzon et al. (Kluwer, Dordrecht, 1997), p. 187.
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40
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85038987944
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This is different from (Formula presented) used by 48 whose luminosity function parameters we use to estimate the redshift distribution, but the median difference of extinction derived between the two is small (Formula presented)
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This is different from (Formula presented) used by 48 whose luminosity function parameters we use to estimate the redshift distribution, but the median difference of extinction derived between the two is small (Formula presented)
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41
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85038979646
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J. Huchra and J. Mader, http://cfa-www.harvard.edu/(Formula presented)huchra/2mass/verify.htm
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J. Huchra and J. Mader, http://cfa-www.harvard.edu/(Formula presented)huchra/2mass/verify.htm.
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43
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85038979217
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Ž. Ivezić et al., in AGN Surveys, Proceedings of IAU Colloquium 184, edited by R.F. Green, E. Ye. Khachikian, and D.B. Saunders (ASP, Byurakan, Armenia, 2001)
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Ž. Ivezić et al., in AGN Surveys, Proceedings of IAU Colloquium 184, edited by R.F. Green, E. Ye. Khachikian, and D.B. Saunders (ASP, Byurakan, Armenia, 2001).
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44
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85039009829
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This is also the level chosen by 46 for their autocorrelation analysis of the XSC
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This is also the level chosen by 46 for their autocorrelation analysis of the XSC.
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48
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85039030559
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Given that the galaxy distribution is nonlinear and non-Gaussian, the (Formula presented) fit is not the optimal bias estimator. However, the fact that the biases for different bins are so close implies that the error in bias, as we see below, is much smaller than the error in our cross-correlation signal and so is negligible
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Given that the galaxy distribution is nonlinear and non-Gaussian, the (Formula presented) fit is not the optimal bias estimator. However, the fact that the biases for different bins are so close implies that the error in bias, as we see below, is much smaller than the error in our cross-correlation signal and so is negligible.
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49
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85039011030
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A low (Formula presented) is to be expected if we overestimate the noise in the ISW signal. In particular, this could be the case if the CMB power is suppressed on large angles. This would increase the significance of an ISW detection at such scales. This effect is elaborated in 52
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A low (Formula presented) is to be expected if we overestimate the noise in the ISW signal. In particular, this could be the case if the CMB power is suppressed on large angles. This would increase the significance of an ISW detection at such scales. This effect is elaborated in 52.
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56
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17144376103
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A. Refregier, E. Komatsu, D.N. Spergel, and U. Pen, Phys. Rev. D 61, 123001 (2000).
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(2000)
Phys. Rev. D
, vol.61
, pp. 123001
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Refregier, A.1
Komatsu, E.2
Spergel, D.N.3
Pen, U.4
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58
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85038973056
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E. Komatsu, N. Afshordi, and U. Seljak (unpublished)
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E. Komatsu, N. Afshordi, and U. Seljak (unpublished).
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