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J/A+A/339/165       The red spectrum of HD 101065         (Cowley+ 1998)

Line identifications and preliminary abundances from the red spectrum of HD 101065 (Przybylski's star) Cowley C.R., Mathys G. <Astron. Astrophys. 339, 165 (1998)> =1998A&A...339..165C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, peculiar ; Spectra, red ; Abundances, peculiar Keywords: stars: individual: HD 101065 - stars: abundances - stars: chemically peculiar - stars: magnetic fields Description: Wavelength list for Przybylski's star (a rapidly rotation Ap star) including a measurement of the line depths. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 11 37 37.2 -46 42 37 HD 101065 = Przybylski's star ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 114 1066 Wavelength list for Przybylski's star
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 7 F7.2 0.1nm Lambda Measured wavelength 9- 12 F4.2 --- Int Measured central intensity (1) 14- 15 I2 --- Strength Line strength (2) 16 A1 --- n_Strength [:] : when eye estimates 19- 42 A24 --- Id1 First identification (3) 43- 66 A24 --- Id2 Second identification (3) 67- 90 A24 --- Id3 Third identification (3) 91-114 A24 --- Id4 Fourth identification (3)
Note (1): Central depth of the line, as measured from a convolved and Fourier filtered spectrum (1.00 corresponds to the continuum level). Note (2): Estimate of the line strength on an arbitrary scale, derived from the measured line depth. Intensities of lines in the wing of Hα are eye estimates, and not computed from the line depths. They are given with colons Note (3): Up to 4 possible contributing transitions are identified for the measured lines. The fractional part of the laboratory wavelength of the transition is given, followed by spectrum (e.g. Nd II). For most of the lanthanide spectra, the parenthesized number following the spectrum is the intensity from Meggers, Corliss, and Scribner (NBS Monog. 145, 1975). Iron-group spectra are typically followed by Multiplet numbers (e.g. Fe I-15 is a line from Multiplet 15). Energy levels are sometimes given for third spectra of the lanthanides. These are from Martin, Zalubas, and Hagan (NSRDS-NBS 60, 1978), or unpublished material provided to CRC by Hannah Crosswhite. Lines lacking energy-level classifications are designated "uncl."-------------------------------------------------------------------------------- Acknowledgements: Gautier Mathys
Acknowledgements: Gautier Mathys
(End) G. Mathys (ESO, Santiago, Chile), Patricia Bauer [CDS] 28-Sep-1998
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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