Table 2: Slopes of the linear fits to the logarithm of the mean weighted PWTs with a linear correction for the magnitude of the stars before averaging.
Spectral Slope from $1.0 \times 10^{-4}$ Slope from $0.7 \times 10^{-3}$

type to $0.6 \times 10^{-3}$ Hz to $2.5 \times 10^{-3}$ Hz

F $-0.599 \pm 0.019$ $-0.506 \pm 0.006$

G $-0.537 \pm 0.016$ $-0.372 \pm 0.016$

K $-0.658 \pm 0.018$ $-0.581 \pm 0.011$

M $-0.725 \pm 0.016$ $-0.567\pm 0.013$

**Table 2:** Slopes of the linear fits to the logarithm of the mean weighted PWTs with a linear correction for the magnitude of the stars before averaging.
Spectral	Slope from $1.0 \times 10^{-4}$	Slope from $0.7 \times 10^{-3}$
type	to $0.6 \times 10^{-3}$ Hz	to $2.5 \times 10^{-3}$ Hz
F	$-0.599 \pm 0.019$	$-0.506 \pm 0.006$
G	$-0.537 \pm 0.016$	$-0.372 \pm 0.016$
K	$-0.658 \pm 0.018$	$-0.581 \pm 0.011$
M	$-0.725 \pm 0.016$	$-0.567\pm 0.013$

Source LaTeX | All tables | In the text

	1 Introduction
	2 Stellar data analysis
	3 Stellar acoustic Power Wavelet Transforms
	4 Analysis of a G type star: the Sun
	5 Discussion and conclusions
	References