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Table 1

Meta-analysis of ISW detections to date and their reported statistical significance.

Author CMB LSS Tracer Wavelength Method Claimed
detection

Boughn & Crittenden (2002) COBE XRB X-ray D2 No
Giannantonio et al. (2008) W3 D2 2.7σ

Boughn & Crittenden (2004, 2005) W1 XRB/NVSS X-ray/radio D2 “tentative” (2–3σ)

Fosalba et al. (2003) W1 SDSS DR1 D2 2σ (low z)
3.6σ (high z)
Cabré et al. (2006) W3 SDSS DR4 Optical D2  >2σ
Giannantonio et al. (2008) W3 SDSS DR6 D2 2.2σ
Sawangwit et al. (2010) W5 SDSS DR5 D2 “marginal”
López-Corredoira et al. (2010) W5 SDSS DR7 D2 “No detection”

Giannantonio et al. (2006) W3 SDSS Quasars Optical D2 2σ
Giannantonio et al. (2008) W3 SDSS Quasars D2 2.5σ
Xia et al. (2009) W5 SDSS Quasars D2 2.7σ

Scranton et al. (2003) W1 D2  >2σ
Padmanabhan et al. (2005) W1 D1 2.5σ
Granett et al. (2009) W3 SDSS LRG Optical D1 2σ
Giannantonio et al. (2008) W3 D2 2.2σ
Sawangwit et al. (2010) W5 SDSS LRG, 2SLAQ D2 “marginal”
Sawangwit et al. (2010) W5 AAOmega LRG D2 Null

Fosalba & Gaztañaga (2004) W1 APM Optical D2 2.5σ

Afshordi et al. (2004) W1 D1 2.5σ
Rassat et al. (2007) W3 2MASS NIR D1 2σ
Giannantonio et al. (2008) W3 D2 0.5σ
Francis & Peacock (2010b) W3 D1 “weak”

Boughn & Crittenden (2002) COBE D2 No
Nolta et al. (2004) W1 D2 2.2σ
Pietrobon et al. (2006) W3 NVSS Radio D3  >4σ
Vielva et al. (2006) W3 D3 3.3σ
McEwen et al. (2007) W3 D3  >2.5σ
Raccanelli et al. (2008) W3 D2 2.7σ
McEwen et al. (2008) W3 D3  ~4σ
Giannantonio et al. (2008) W3 D2 3.3σ
Hernández-Monteagudo (2010) W3 D1  <2σ
Sawangwit et al. (2010) W5 D2 “marginal” (~2σ)

Corasaniti et al. (2005) W1 D2  >2σ
Gaztañaga et al. (2006) W1 D2 2σ
Ho et al. (2008) W3 Combination Combination D1 3.7σ
Giannantonio et al. (2008) W3 D2 4.5σ

Notes. The “Method” describes the space in which the power spectrum analysis is conducted (configuration, spherical harmonic, etc.), not the method for measuring the significance level of the detection (this is described in Sect. 3). D1 corresponds to the spherical harmonic space, D2 to the configuration space, D3 to the wavelet space. The highest detections are made in wavelet space. Regarding the survey used, the highest detections are made using NVSS (though weak and marginal detections using NVSS are also reported) or using combinations of LSS surveys as the matter tracer.

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