The Spectrum of Singly Ionized Sulphur, S II

et al. 2003

A&A

Abstract. We present a spectroscopic atlas of Deneb (A2 Iae) obtained with the long camera of the 1.22-m telescope of the Dominion Astrophysical Observatory using Reticon and CCD detectors. For λλ3826-5212 the inverse dispersion is 2.4 Å mm −1 with a resolution of 0.072 Å. At the continuum the mean signal-to-noise ratio is 1030. The wavelengths in the laboratory frame, the equivalent widths, and the identifications of the various spectral features are given. This atlas should provide useful guidance for studies of other stars with similar spectral types. The stellar and synthetic spectra with their corresponding line identifications can be examined at

Section: Line Identificationsmentioning

confidence: 99%

A spectroscopic atlas of Deneb (A2 Iae) $\lambda\lambda$3826–5212

Albayrak

Gulliver

et al. 2003

A&A

“…The stellar lines were identified with the general references A Multiplet Table of Astrophysical Interest (Moore 1945) and Wavelengths and Transition Probabilities for Atoms and Atomic Ions, Part 1 (Reader & Corliss 1980) as well as Svendenius et al (1983) for P II, Pettersson (1983) for S II, Huldt et al (1982) for Ti II, Catalan et al (1964) for Mn I, Iglesias & Velasco (1964) for Mn II, Nave et al (1994) for Fe I, and Dworetsky (1971), Johansson (1978), Guthrie (1985), and Adelman (1987) for Fe II, and Isberg & Litzen (1985) for Ga II.…”

Section: The Spectramentioning

confidence: 99%

Elemental abundance analyses with DAO spectrograms

Gulliver

Rayle

2001

A&A

Abstract. Elemental abundances analyses are performed for the Mercury-Manganese stars υ Her, φ Her, and HR 7018 consistent with previous studies of this series using spectrograms obtained with Reticon and CCD detectors. Comparisons of the first two analyses with those performed using coadded photographic plates show the general consistency of the derived elemental abundances. For υ Her and for φ Her, abundances were newly found for O, and for Al, V, Zn, and Ce, respectively. HR 7018 is discovered to be a single-lined spectroscopic binary. Its Sc abundance is the smallest of any class member with derived abundances and its Sr abundance the largest of any known HgMn star. A correlation analysis of the most complete abundance sets for 20 HgMn stars shows that the abundances of some elements are correlated with one another and some are functions of the stellar effective temperature.

“…The stellar lines were identified with the general references A Multiplet Table of Astrophysical Interest (Moore 1945) and Wavelengths and Transition Probabilities for Atoms and Atomic Ions, Part 1 (Reader & Corliss 1980) as well as the more specialized references for P II (Svendenius et al 1983), S II (Pettersson 1983), Ti II (Huldt et al 1982), Mn II (Iglesias & Velasco 1964), and Fe II (Johansson 1978). Baschek (1973) discussed the analyses of α Scl independently carried out by Schmitt (1972Schmitt ( , 1973 and Vilhu (1972).…”

Section: Observational Materials and Line Identificationsmentioning

confidence: 99%

Elemental abundance studies of CP stars

López-García

Pintado

2001

A&A

Abstract. Fine analyses of the magnetic CP stars α Scl and HD 170973 are presented using ATLAS9 model atmospheres which have same bulk metallicity as the deduced abundances. The light elements are mostly solar except for silicon, and all the heavier elements except nickel in HD 170973, which is solar, are greatly overabundant. The iron peak elements are typically 10 times overabundant, Sr is of order of 1000 times solar, Y and Zr are of order of 100 times solar. The rare earths are 1000 or more times overabundant.