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. 2017 Jan 25;4(1):160652. doi: 10.1098/rsos.160652

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© 2017 The Authors.

Published by the Royal Society under the terms of the Creative Commons Attribution License http://creativecommons.org/licenses/by/4.0/, which permits unrestricted use, provided the original author and source are credited.

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Figure 4. — WISE epoch photometry at 3.4, 4.6, 12 and 22 μm (W1, W2, W3 and W4, in magnitudes). Panel (a) shows the time variation in W1 over 5.5 years. Panels (b–d) show how W1 correlates with W2, W3 and W4, which do not have observations at all W1 epochs. The dashed lines show the slope expected for constant disc flux variation with wavelength (the variation is smaller in W1/2, because the total flux is not dominated by the disc).