Issue |
A&A
Volume 567, July 2014
|
|
---|---|---|
Article Number | A117 | |
Number of page(s) | 20 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/201423765 | |
Published online | 24 July 2014 |
Online material
Appendix A: CN images and profiles
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Fig. A.1
Results for DM Tau. Top: integrated line flux for CN N = 2−1 hyperfine components (histogram) with the best fit profile superimposed (red curve). The spectral resolution for the strongest group of hyperfine components is 0.103 km s-1. Bottom: S/N maps for the two groups of components, and for all observed components (rightmost panel). Contours are in steps of 2σ. |
Open with DEXTER |
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Fig. A.2
As Fig. A.1 for LkCa 15. |
Open with DEXTER |
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Fig. A.3
As Fig. A.1 for MWC 480. |
Open with DEXTER |
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Fig. A.4
Results for DN Tau. Top: integrated line flux for CN N = 2−1 hyperfine components (histogram) with the best fit profile superimposed (red curve). Bottom: S/N maps for each group of components, and for all observed components (rightmost panel). Contours are in steps of 2σ. |
Open with DEXTER |
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Fig. A.5
As Fig. A.4 for DL Tau. |
Open with DEXTER |
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Fig. A.6
As Fig. A.4 for IQ Tau. |
Open with DEXTER |
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Fig. A.7
As Fig. A.4 for IRAS 04302+2247. |
Open with DEXTER |
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Fig. A.8
As Fig. A.4 for HV Tau. |
Open with DEXTER |
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Fig. A.9
As Fig. A.4 for CI Tau. |
Open with DEXTER |
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Fig. A.10
As Fig. A.4 for CY Tau. |
Open with DEXTER |
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Fig. A.11
As Fig. A.4 for GO Tau. |
Open with DEXTER |
Appendix B: Fit residuals
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Fig. B.1
Line channels for GO Tau. For each panel, observations are displayed in the top row, the best fit model in the middle row and the residuals in the bottom row. Channels are ordered by increasing velocities (see upper left corner of each panel) from left to right and top to bottom. Contour spacing is 40 mJy/beam, or 2σ. The unusual spatial distribution is due to the three hyperfine components. The emission is essentially that of 3 Keplerian disks with systemic velocities 3.37, 4.87, and 5.66 km s-1 and relative intensities 1, 2.67 and 1.68 respectively. |
Open with DEXTER |
Appendix C: Evolutionary tracks
To compare the masses we have measured to different evolutionary models, we show in Figs. C.1−C.3 the position of the stars with accurate masses on modified HR diagram for the Baraffe et al. (1998, BCAH), the Siess et al. (2000) and the Tognelli et al. (2011, PISA) tracks; see also Fig. 7 for the Dartmouth (Dotter et al. 2008) tracks. Taken together, the four different models differ the most with respect to each other at masses less than 0.5 M⊙ and have different evolutionary time scales for all masses at ages less than 5 Myr.
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Fig. C.1
Stars on the modified, distance-independent, HR diagram L/M2 vs. Teff for the Baraffe et al. (1998) tracks. Stars with dynamical mass precisions measured to better than 5% appear in the left panel and stars with lower precions appear in the right panel. |
Open with DEXTER |
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Fig. C.2
As for Fig. C.1, but for the Siess et al. (2000) tracks. |
Open with DEXTER |
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Fig. C.3
As for Fig. C.1, but for the Tognelli et al. (2011) tracks. |
Open with DEXTER |
© ESO, 2014
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