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Volumn 69, Issue 8, 2004, Pages 15-

Cross-correlation of the cosmic microwave background with the 2MASS galaxy survey: Signatures of dark energy, hot gas, and point sources

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EID: 2442638930     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.69.083524     Document Type: Article
Times cited : (235)

References (58)
  • 1
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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.
    • (2003) Astrophys. J., Suppl. Ser. , vol.148 , pp. 1
    • Bennett, C.L.1
  • 22
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    • S. P. Boughn (private communication)
    • S. P. Boughn (private communication).
  • 28
    • 85038984342 scopus 로고    scopus 로고
    • We thank Doug Finkbeiner for extracting the fluxes of Andromeda in WMAP temperature maps
    • We thank Doug Finkbeiner for extracting the fluxes of Andromeda in WMAP temperature maps.
  • 33
    • 85038997978 scopus 로고    scopus 로고
    • 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/
    • 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/.
  • 35
    • 85039014296 scopus 로고    scopus 로고
    • We thank Eiichiro Komatsu for pointing out this identity
    • We thank Eiichiro Komatsu for pointing out this identity.
  • 38
    • 85039017857 scopus 로고    scopus 로고
    • 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
    • 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.
  • 40
    • 85038987944 scopus 로고    scopus 로고
    • 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)
    • 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)
  • 41
    • 85038979646 scopus 로고    scopus 로고
    • J. Huchra and J. Mader, http://cfa-www.harvard.edu/(Formula presented)huchra/2mass/verify.htm
    • J. Huchra and J. Mader, http://cfa-www.harvard.edu/(Formula presented)huchra/2mass/verify.htm.
  • 43
    • 85038979217 scopus 로고    scopus 로고
    • 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)
    • 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).
  • 44
    • 85039009829 scopus 로고    scopus 로고
    • This is also the level chosen by 46 for their autocorrelation analysis of the XSC
    • This is also the level chosen by 46 for their autocorrelation analysis of the XSC.
  • 48
    • 85039030559 scopus 로고    scopus 로고
    • 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
    • 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.
  • 49
    • 85039011030 scopus 로고    scopus 로고
    • 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
    • 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.
  • 58
    • 85038973056 scopus 로고    scopus 로고
    • E. Komatsu, N. Afshordi, and U. Seljak (unpublished)
    • E. Komatsu, N. Afshordi, and U. Seljak (unpublished).


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.