Table 3: Slopes of the linear fits to the logarithm of the mean weighted PWTs leveling up all the stars of each spectral type to have the same level of noise above 3 mHz.
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 $-0.604 \pm 0.019$ $-0.510\pm 0.006$

G $-0.582 \pm 0.016$ $-0.431\pm 0.007$

K $-0.644 \pm 0.019$ $-0.558\pm 0.010$

M $-0.695 \pm 0.014$ $-0.563\pm 0.011$

**Table 3:** Slopes of the linear fits to the logarithm of the mean weighted PWTs leveling up all the stars of each spectral type to have the same level of noise above 3 mHz.
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	$-0.604 \pm 0.019$	$-0.510\pm 0.006$
G	$-0.582 \pm 0.016$	$-0.431\pm 0.007$
K	$-0.644 \pm 0.019$	$-0.558\pm 0.010$
M	$-0.695 \pm 0.014$	$-0.563\pm 0.011$

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