Measuring the integrated Sachs-Wolfe effect | Astronomy & Astrophysics (A&A)

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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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