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Astron. Astrophys. 363, 343-348 (2000)

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Fe+ column density and line opacities of the UV2 multiple of Fe II in laboratory and peculiar stellar sources *

R.F. Viotti 1, N. Spector **  1, G.B. Baratta 2 and C. Rossi 3

1 Istituto di Astrofisica Spaziale, CNR, Area di Ricerca Tor Vergata, 00133 Roma, Italy
2 Osservatorio Astronomico di Roma, Via del Parco Mellini 84, 00136 Roma, Italy
3 Dipartimento di Fisica, Università La Sapienza, Piazza Aldo Moro, 2, 00185 Roma, Italy

Received 4 May 2000 / Accepted 4 July 2000


The Self-Absorption Curve method has been applied to the UV2 multiplet [FORMULA] of Fe  II observed in the laboratory and in emission-line stars. For the laboratory observations line opacities of this multiplet were obtained using various sets of atomic data. The best fit is obtained using data by Bergeson et al. (1996), which provide line opacities that are in remarkable agreement with results by Kastner (1999a), derived using independent methods. A value of 7.3[FORMULA] cm-2 for the Fe+ column density is derived for the laboratory source, and lower limits of 2.1[FORMULA] and [FORMULA]2[FORMULA] cm-2 are obtained for the peculiar stars KQ Pup and RR Tel, respectively.

Key words: atomic data – line: formation – methods: data analysis – stars: emission-line, Be – stars: individual: KQ Pup – stars: individual: RR Tel

* Based on observations made with the International Ultraviolet retrieved from the IUE archive.
** On leave of absence from Soreq Research Center, Yavne 81800, Israel

Send offprint requests to: R. Viotti (uvspace@ saturn.ias.rm.cnr.it)

© European Southern Observatory (ESO) 2000

Online publication: December 5, 2000