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Comprehensive analysis of HD 105, a young solar system analog

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Table 1Photometry used in disc modelling.
Figure 1. Segments of the FEROS spectrum covering the Hα (top) and CaIIH&K (bottom). The median stellar spectrum from X FEROS observationsis presented in black, whilst the best-fitting model is presented in red
Table 3Architecture of HD 105’s disc determined from the ALMA image.
Figure 2. ALMA 1.3 mm (Band 6) naturally weighted, dirty image of HD 105, the best fit annular model for the disc, and the residuals in the observed imageafter subtraction of a model convolved with the dirty beam (from left to right)
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