AAS Meeting #193 - Austin, Texas, January 1999
Session 45. Spectral Observations of Stars
Display, Thursday, January 7, 1999, 9:20am-6:30pm, Exhibits Hall 1

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[45.04] HD 101065: Improved Identification Lists

C.R. Cowley (UM), W.P. Bidelman (CWR), G. Mathys (ESO)

A new, high-resolution and low-noise ESO spectrum has made it possible to improve on an earlier study of HD 101065. This spectrum was made with the 3.5m New Technology Telescope and the ESO Multi-Mode Instrument in its cross-dispersed echelle mode. The resolving power is 80000 over a wavelength range covering 2700A; the S/N ratio of the reduced spectrum is approximately 200 at the blue, faintest end.

Wavelengths lists and identifications have been made for the region 3959-6652A. The new material includes 8010 measured wavelengths, and central depths. We have been able to find plausible identifications for nearly 40% of the lines, as of 2 October 1998. The presence of Fe I is now certain. Some 150 features are identified wholely or partially as Fe I. Confidence levels from wavelength coincidence statistics range as high as 6.9 sigma for lines within 0.03A of their laboratory positions. Numerous other iron-group spectra are present, but weak {\em relative to} the second spectra of the lanthanides. Third spectra of several lanthanides (Nd III, Sm III, and Pr III) are strong, and some first spectra may be present. Ca II H is present and stronger than the other metal lines, as are the hydrogen lines.

If we order the lines from the strongest to the weakest, we find nearly 400 features due to lanthanides before we come to a feature which may be primarily Fe I. The stellar features include lines that are intrinsically fainter than the faintest lines of NBS Monograph 145. For Ce II, Nd II, Sm II, and Gd II there are no f-values for lines that are weak in this star. Some features are identified with elements heavier than than the lanthanides including W, Hg, Pt, and U; thus far only tungsten has support from wavelength coincidence statistics.

If you would like more information about this abstract, please follow the link to http://www.astro.lsa.umich.edu:80/users/cowley/przyb.html. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

The author(s) of this abstract have provided an email address for comments about the abstract: cowley@umich.edu

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