Volume 542, June 2012
|Number of page(s)||16|
|Published online||30 May 2012|
Line identification in high-resolution, near-infrared CRIRES spectra of chemically peculiar and Herbig Ae stars⋆,⋆⋆
1 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
2 Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste, Italy
3 Instituto de Ciencias Astronomicas, de la Tierra, y del Espacio (ICATE), 5400 San Juan, Argentina
4 Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK
5 European Southern Observatory, Casilla 19001, Santiago, Chile
6 Department of Astronomy, University of Michigan, Ann Arbor, MI 48109-1042, USA
7 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
Received: 6 February 2012
Accepted: 22 March 2012
Context. Contrary to the late-type stars, our knowledge of atomic transitions in intermediate-mass stars is still very poor. The recent availability of ESO’s high-resolution spectrograph CRIRES offers now the opportunity to study numerous spectral features in the near-IR in intermediate-mass main-sequence and pre-main-sequence stars.
Aims. The aim of the study is to explore the diagnostic potential of near-IR spectral regions. We carry out the first line identification in a few spectral regions for the two strongly magnetic Ap stars γ Equ and HD 154708, and their potential precursors two pre-main sequence Herbig Ae/Be stars HD 101412 and 51 Oph.
Methods. High-resolution CRIRES spectra were obtained in three spectral regions, two regions around 1 μm and one region around 1.57 μm containing magnetically sensitive Fe i lines. To study the spectral line variability in the Herbig Ae star HD 101412, the observations were collected on six different rotation phases. All currently available atomic line lists were involved to properly identify the detected spectral features.
Results. The largest number of near-IR spectral features was detected and identified in the well-studied magnetic Ap star γ Equ. Nearly 30% of the spectral lines in the Ap star HD 154708 with one of the strongest magnetic fields known among the Ap stars of the order of 25 kG, remain unidentified due to a lack of atomic data. Only very few lines belonging to the rare earth element group have been identified in both Ap stars. A number of spectral lines including the Ce iii and Dy ii lines appear magnetically split due to the presence of a strong magnetic field in their atmospheres. The content of the spectra of the Herbig Ae/Be stars HD 101412 and 51 Oph is rather unexciting. Variable behaviour of lines of the elements He, N, Mg, Si, and Fe over the rotation period in the spectra of HD 101412 confirm our previous finding of variability in the optical region. Due to the very fast rotation of 51 Oph, only a few spectral lines have been identified with certainty.
Key words: atomic data / stars: atmospheres / stars: chemically peculiar / stars: magnetic field / stars: pre-main sequence
Based on observations obtained at the European Southern Observatory (ESO programme 087.C-0124(A)).
Appendix A is available in electronic form at http://www.aanda.org
© ESO, 2012
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