| Abstract
| - The known β Cephei star HD 180 642 was observed by the CoRoT satellite in 2007. From the very high-precision light curve, its pulsation frequency spectrum could be derived for the first time (Degroote and collaborators). In this paper, we obtain additional constraints for forthcoming asteroseismic modeling of the target. Our results are based on both extensive ground-based multicolour photometry and high-resolution spectroscopy. We determine $T_{\rm eff} = 24\,500\pm 1000$ K and $\log g = 3.45\pm 0.15$ dex from spectroscopy. The derived chemical abundances are consistent with those for B stars in the solar neighbourhood, except for a mild nitrogen excess. A metallicity $Z =$$0.0099\pm 0.0016$ is obtained. Three modes are detected in photometry. The degree $ell$ is unambiguously identified for two of them: $ell = 0$ and $ell = 3$ for the frequencies 5.48694 d -1 and 0.30818 d -1, respectively. The radial mode is non-linear and highly dominant with an amplitude in the U-filter about 15 times larger than the strongest of the other modes. For the third frequency of 7.36673 d -1 found in photometry, two possibilities remain: $ell = 0$ or 3. In the radial velocities, the dominant radial mode presents a so-called stillstand but no clear evidence of the existence of shocks is observed. Four low-amplitude modes are found in spectroscopy and one of them, with frequency 8.4079 d -1, is identified as $(ell,m)=(3,2)$. Based on this mode identification, we finally deduce an equatorial rotational velocity of $38\pm 15$ km s -1.
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