**Table 5:** Parameters of the power law spectral fits ( $F_{\nu }=F_{\nu _0}(\nu /\nu _0)^{-\alpha _{\nu }}$ ) of the pulsar data shown in Fig. 4.
Observations	$\alpha_{\nu}$	Log $F_{\nu_0}$ ,
		$\nu_0=5.47\times10^{14}$ Hz
		[ $\mu$ Jy]
VLT spectrum	$1.88\pm0.01$	1.469(2)
(this work)
HST/FOS spectrum^a	$1.6\pm0.4$	1.228(115)
(Hill et al. 1997)
HST photometry	$\rm 1.07^{+0.20}_{-0.19}$	0.879(25)
(this work)
10 pixel measurements	$\rm 1.24^{+0.19}_{-0.18}$	1.241(22)
(this work)
Time-resolved photometry	$\rm0.26^{+0.45}_{-0.43}$	0.880(54)
(Middleditch et al. 1987)

^a Log $F_{\nu_0}$ from Hill et al. (1997).

Source LaTeX | All tables | In the text