Radio emission from the high-mass X-ray binary BP Crucis - First detection

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Table 3:

Details of the detections and upper limits for the non-detections of BP Cru ordered by orbital phase.
Epoch (phase)^a	Flux [mJy]^b		$\alpha$ ^cg
	4.8 GHz	8.6 GHz
1(-7)	1.02 (0.17)	0.82 (0.18)	$\rm -0.38^{+0.28}_{-1.10}$
9(-4)^d	1.01 (0.16)	0.51 (0.13)	$\it -1.17^{-0.49}_{-1.93}$
2(-3)	0.75 (0.14)	<0.48 (0.16)	$\rm -0.88^{+0.0}$
10(+0)	0.70 (0.14)	0.72 (0.13)	$\rm +0.05^{+0.72}_{-0.61}$
3(+1)^h	(0.18)	(0.15)
7(+1)^e	0.67 (0.13)	0.91 (0.14)	$\it +0.53^{+1.14}_{-0.07}$
8(+16)^f	0.51 (0.09)	0.63 (0.09)	$\rm +0.36^{+0.92}_{-0.18}$

^a Phase indicates ``days from periastron''.
^b Numbers in parenthesis indicate the rms value in the maps.
^c Spectral index, $\alpha=\log(F_{8.6}/F_{4.8}) / \log(\nu_{8.6} / \nu_{4.8})$ .
^d Orbital phase also observed in epoch 6 with a compact configuration, and hence not considered useful for this project.
^e Orbital phase also observed in epoch 3 without detection. See text.
^f Note that for this epoch Stokes Q at 8.6 GHz is 0.38 mJy, while Stokes V and U were not detected. No polarisation signal was detected at 4.8 GHz.
^g Maximum and minimum values of the spectral index when adding/subtracting 1 $\sigma$ rms to the listed flux.
^h As mentioned in the text, we do not detect BP Cru at this epoch.

Source LaTeX | All tables | In the text

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