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Photometry of the δ Scuti Star DG Leo: Preliminary Results

Published online by Cambridge University Press:  22 February 2018

P. Lampens ,
R. Garrido ,
L. Parrao ,
J.H. Peña ,
T. Arentoft  and
Y. Frémat
P. Lampens
Affiliation:
Royal Astronomical Observatory, Belgium, email: patricia.lampens@oma.be
R. Garrido
Affiliation:
Instituto de Astrofísica de Andalucia, España
L. Parrao
Affiliation:
Instituto de Astronomía, UNAM, México
J.H. Peña
Affiliation:
Instituto de Astronomía, UNAM, México
T. Arentoft
Affiliation:
Royal Astronomical Observatory, Belgium, email: patricia.lampens@oma.be Aarhus University, Denmark
Y. Frémat
Affiliation:
Royal Astronomical Observatory, Belgium, email: patricia.lampens@oma.be

Abstract

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New uvby photoelectric photometry has been acquired for the triple star DG Leo at two different observatories equipped with analogous instrumentation. A preliminary period analysis indicates the presence of at least 3 close δ Scuti frequencies (10-12 c/d, 3-6 mmag) and a slow variation. This slow variation fits quite well with half the orbital period of the spectroscopic binary; the noise level in the amplitude spectrum is only 3–4 mmag (after prewhitening).

Resumen

Resumen

Se ha obtenido fotometría fotoeléctrica uvby para el sistema estelar triple DG Leo desde dos diferentes observatorios equipados con instrumentación semejante. El análisis preliminar de períodos indica la presencia de al menos 3 frecuencias próximas (10-12 c/d, 3-6 mmag) en la δ Scuti y una variación lenta. Esta variación lenta concuerda muy bien con la mitad del período orbital de la binaria espectroscópica; el nivel de ruido en el espectro de amplitudes es de 3 − 4 mmag (después del filtrado).

Keywords

BinariesVisual — BinariesSpectroscopic — StarsVariablesδ Scuti — TechniquesPhotometric
Type
Observational properties and Statistics of Binary Stars in the Field
Information
International Astronomical Union Colloquium , Volume 191: The Environment and Evolution of Double and Multiple Stars , August 2004 , pp. 73 - 74
Copyright
Copyright © Instituto de Astronomia – Mexico 2004

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