uvby – β photoelectric photometry of Cepheid stars¹

 

J. H. Peña,² A. Arellano Ferro,² R. Peña–Miller,³ M. Álvarez,⁴ Y. Rosas,⁵ H. García,⁶ G. Muñoz,⁷ B. Vargas,⁸ J. P. Sareyan,⁹ C. A. Guerrero,² and A. Rentería²

 

² Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70–264, México D. F. CP 04510, México (jhpena@astroscu.unam.mx).

³ Department of Mathematics, Imperial College London, South Kensington Campus, London SW7 2AZ, UK.

⁴ Instituto de Astronomía, Observatorio Astronómico, Universidad Nacional Autónoma de México, Ensenada.

⁵ Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, México.

⁶ Facultad de Ciencia, UNAN–Managua, Nicaragua.

⁷ ESIME, Instituto Politécnico Nacional, México.

⁸ Instituto de Geofísica, Universidad Nacional Autónoma de México, México.

⁹ OCA, Department Gemini, Boulevard de l'Observatoire BP 4229, 06304 Nice Cedex 4, France.

 

Received 2010 May 4
Accepted 2010 June 10

 

RESUMEN

Presentamos fotometría fotoeléctrica uvby—β de 41 estrellas Cefeidas clásicas. Se llevó a cabo una breve discusión de los datos comparados con observaciones análogas.

 

ABSTRACT

We present time–series uvby —β photometry of 41 classical Cepheid stars. A brief discussion of a comparison between the present data and previous photometric observations is included.

Key Words: stars: variables: Cepheids — techniques: photometric.

 

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ACKNOWLEDGMENTS

We thank the staff of the OAN for their assistance in securing the observations, and acknowledge the help of several colleagues who participated in the observations: R. Peniche, L. Parrao, V. H. Alvarado and P. Zasche. This work was partially supported by PAPIIT IN110102 and IN108106–3. RPM, GM, BV, VHA and HG thank the IA–Universidad Nacional Autónoma de México for the opportunity to carry out the observations. Typing was partially done by J. Orta, and proofreading by J. Miller. C. Guzmán, F. Ruiz and A. Díaz assisted us in the computer reductions. We are indebted to an anonymous referee for a series of comments and suggestions that led to improvement of the present paper. This research has made use of the Simbad databases operated at CDS, Strasbourg, France, and the NASA ADS Astronomy Query Form.

 

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NOTE

¹Based on observations collected at the San Pedro Mártir Observatory, México.