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Fig. 6

image

Distribution of spectral indices for 48 pulsars without previously published spectral fits. Each of the 48 dark squares marks the mean of the posterior distribution of the spectral index α. The lighter histogram was constructed using the whole posterior distribution of α for all pulsars, and thus reflects the uncertainty in the spectral index determination. The grey line marks the distribution of spectral indices for 175 non-recycled pulsars in the similar frequency range (100–400 MHz) from Malofeev et al. (2000).

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