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Radial Velocity Studies of Pulsations in roAp Stars: γ Equ Revisited

Published online by Cambridge University Press:  12 April 2016

A. Kanaan ,
A. P. Hatzes  and
D. Mkrtichian
A. Kanaan
Affiliation:
Departamento de Física, Universidade Federal de Santa Catarina, Brazil
A. P. Hatzes
Affiliation:
Department of Astronomy, University of Texas at Austin, U.S.A.
D. Mkrtichian
Affiliation:
Odessa Observatory, Ukraine

Extract

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We have used the 2D-Coudé spectrograph of the 2.7-m telescope at McDonald Observatory at a resolution of 60,000. We use an iodine cell which provides us with permanent wavelength reference.

γ Equ was observed for a period of approximately 6 hours. The signal to noise ratio was variable due to the presence of clouds. A typical value for the “good” spectra is 80.

The use of a large detector provides us with complete spectral coverage from 5,000 to 6,000 Å (the region where I2 lines are most visible and useful as a wavelength reference). This allowed us to expand over our previous work analyzing the pulsations of γ Equulei through the use of spectroscopy.

Type
Part 6. Variables Close to the Main Sequence
Information
International Astronomical Union Colloquium , Volume 176: The Impact of Large-Scale Surveys on Pulsating Star Research , 2000 , pp. 489
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Kanaan, A. & Hatzes, A.P. 1998, ApJ, 503, 848 Google Scholar