2004A&A...425..263C

We present a high resolution spectral atlas of the HgMn star HD 175640 covering the 3040-10000Å region. UVES spectra observed with 90000-110000 resolving power and signal to noise ratio ranging from 200 to 400 are compared with a synthetic spectrum computed with the SYNTHE code (Kurucz, 1993, CD-ROM, No. 18). The model atmosphere is an ATLAS12 model (Kurucz, 1997, in The 3rd Conf. on Faint Blue Stars, ed. Philip, Liebert & Saffer (Schenectady: L. Davis Press), 33) with parameters T_eff=12000K, logg=3.95, ξ=0km/s. The stellar individual abundances in ATLAS12 were derived from an iterative procedure. The starting atomic line lists downloaded from the Kurucz website have been improved and extended by examining different sources in the literature and by comparing the computed profiles with the observed spectrum. The high quality of the data allowed us to study the isotopic and hyperfine structure for several lines of MnII, GaII, BaII, PtII, HgI, and HgII. Numerous weak emission lines from CrII and TiII have been identified in the red part of the spectrum, starting at ≃λ 5847Å. Two emission lines of CI (mult. 10, mult. 9) have been observed for the first time. All CrII and TiII emission lines originate from the high excitation states (χ_low>89000cm^–1 for CrII and χ_low>62000cm^–1 for TiII) with large transition probabilities (loggf>-1.00). The synthetic spectrum superimposed on the observed spectrum as well as the adopted improved atomic line lists are available at the CDS and http://wwwuser.oat.ts.astro.it/castelli/stars.html . An extended discussion on each identified ion and related atomic data is available both on the quoted website and in an electronic Appendix to the paper.