EDP Sciences
Free Access
Volume 555, July 2013
Article Number A3
Number of page(s) 13
Section Planets and planetary systems
DOI https://doi.org/10.1051/0004-6361/201321147
Published online 18 June 2013

Online material

Appendix A: Astrometry and photometry data of the visual range measurements

Table A.1

Astrometry of 2012 DR30 from Faulkes South 2 m r′-band imaging over four nights in 2012.

Table A.2

Comparison stars selected in photometric reduction of Faulkes South 2 m r′-band imagery of 2012 DR30.

Appendix B: Input fluxes for thermal modelling

We calculate the colour corrected flux from the measured flux using the Cλ colour correction factors and the rcorr flux correction factors. The colour correction factors of the Herschel data are calculated using the actual spectral energy distribution of the target according to Müller et al. (2011), while in the case of WISE data the correction factors are taken from Cutri et al. (2012). Then the corrected flux is: (B.1)and the uncertainty of the corrected flux is: (B.2)

where δCλ is the uncertainty of the colour correction factor. The final “input flux”, used for the modelling of the thermal emission is the colour corrected flux, Fλ,i = Fλ,cc. However, the uncertainties of the absolute calibration have to be considered in the final “input” uncertainties: (B.3)where rcal is the calibration uncertainty factor that is given as a certain fraction of the measured point source flux for all bands of the WISE and Herschel/PACS instruments. The actual values of all the factors mentioned above are summarized in Table 3, also listing the final input fluxes used in the thermal emission modelling.

© ESO, 2013

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