A&A 478, 795 (2008)
DOI: 10.1051/0004-6361:20078536e

Erratum

A search for near-infrared molecular hydrogen emission in the CTTS LkH$\alpha$ 264 and the debris disk 49 Ceti

A. Carmona^1,2 - M. E. van den Ancker² - Th. Henning¹ - M. Goto¹ - D. Fedele^2,3 - B. Stecklum⁴

1 - Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
2 - European Southern Observatory, Karl Schwarzschild Strasse 2, 85748 Garching bei München, Germany
3 - Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio 2, 35122 Padova, Italy
4 - Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany

A&A 476, 853-862 (2007), DOI: 10.1051/0004-6361:20078536

Key words: stars: emission-line, Be - stars: pre-main sequence - planetary systems: protoplanetary disks - errata, addenda

Figure 3: Physical properties of classical T Tauri stars in which a search for the H2 $\upsilon =1{-}0$ S(1) line was performed. Filled stars represent detections, non-filled stars represent non-detections. a) H$\alpha$ EW versus $(U-V)_{\rm excess}$. b) log$L_{\rm X}$ [erg s-1] versus H$\alpha$ EW. c) log$L_{\rm X}$ [erg s-1] versus $(U-V)_{\rm excess}$. d) $M_{\rm disk}$ versus $(U-V)_{\rm excess}$.

Open with DEXTER

In the text (end of Sect. 4.1) and in Table 4 of the original paper, the U-V colour of LkH$\alpha$ 264 was mistakenly taken as -0.46. The U-V colour of LkH$\alpha$ 264 should be 0.37 (Bastian & Mundt 1979). Therefore, in Table 4 of the original paper, in the fields corresponding to LkH$\alpha$ 264, $(U-V)_{\rm obs}$ should be 0.37 instead of -0.46, $(U-V)_{\rm dered}$ should be 0.08 instead of -0.74, and $(U-V)_{\rm ex}$ should be -2.10 instead of -2.92. In Table 4 we present the correct input of LkH$\alpha$ 264 for Table 4 of the original paper. In Fig. 3 we present the corrected version of Fig. 3 of the original paper, here taking into account the correct value of the U-V excess for LkH$\alpha$ 264. This correction on the U-V excess of LkH$\alpha$ 264 affects no conclusion in the original paper, therefore, the conclusions presented in the original paper remain unchanged.

Table 4: Physical properties of LkH$\alpha$ 264.

Acknowledgements

We thank G. Meeus for bringing the error on the U-V colour of LkH$\alpha$ 264 to our attention.

References

• Bastian, U., & Mundt, R. 1979, A&AS, 36, 57 [NASA ADS] (In the text)
• Carmona, A., van den Ancker, M. E., Henning, T., et al. 2007, A&A, 476, 853 [NASA ADS] [CrossRef] [EDP Sciences]
• Itoh, Y., Sugitani, K., Ogura, K., & Tamura, M. 2003, PASJ, 55, L77 [NASA ADS]