Peremennye Zvezdy

"Peremennye Zvezdy",
Prilozhenie
,
vol. 16, N 2 (2016)

Discovery of Three Eclipsing Binaries in the field of AW Cru

C. Quiñones#1, F. D. Mina#1,2, N. Suárez#1
#1. Grupo de Astrometria y Fotometria, Observatorio Astronomico Cordoba, Argentina;
#2. Facultad de Filosofia y Humanidades, Universidad Nacional de Cordoba, Argentina.

Received:   4.06.2015;   accepted:   15.04.2016
(E-mail for contact: fede_mina@hotmail.com)


#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 USNO B1.0 0295-039602512 11 00.60, -60 29 03.4EW16.5717.21*0.3276742456356.774min Comm. 1variable1_phase.jpgvariable1_finder.pngvariable1_data.txt
2 USNO-B1.0 0295-039607812 11 05.69, -60 29 25.5EB17.1817.87*0.7190342456356.810min Comm. 2variable2_phase.jpgvariable2_finder.pngvariable2_data.txt
3 USNO-B1.0 0295-039614512 11 10.69, -60 29 53.5EW16.8817.67*0.3173652456356.741min Comm. 3variable3_phase.jpgvariable3_finder.pngvariable3_data.txt

Comments:


1. USNO-B1.0 0295-0396025 = USNO-A2.0 0225-13488535.

2. USNO-B1.0 0295-0396078 = USNO-A2.0 0225-13492997.
Min I = JD 2456762.709 ± 0.009; Min II = JD 2457083.764 ± 0.001.

3. USNO-B1.0 0295-0396145 = USNO-A2.0 0225-13497346. MinI = JD 2457083.826 ± 0.002; MinII = JD 2456846.5966 ± 0.0003, MinI = JD 2456762.6520 ± 0.0006; MinII = JD 2456762.811 ± 0.005; MinI = JD 2456356.7409 ± 0.0002.

Remarks:
We present the light elements of three newly discovered eclipsing binaries. Their variability was detected during our observations of the variable AW Cru in 2013. All the observations were made at the Estación Astrofísica Bosque Alegre, in Argentina with a 1.54 meter reflector telescope and an unfiltered CCD camera. The reductions of the images were done using the Fotodif 3.93 software. We use two comparison stars USNO-A2.0 0225-13471141 and 0225-13461332 for the photometry; their red magnitudes from the USNO-A2.0 catalog (Monet et. al. 1998) were used.

We also calculated some times of minima, when enough data points were available, with AVE software. The period and the phase-plotted images of the stars were obtained using the Lomb–Scargle algorithm in the NASA Exoplanet Archive Periodogram Service. The names, positions and magnitudes of the stars were obtained thanks to the VizieR catalogue access tool, CDS, Strasbourg, France (Ochsenbein et. al. 2000).

References:
Monet, D.G., Bird, A., Canzian, B., et al., 1998, USNO-A2.0, A Catalogue of Astrometric Standards (U.S. Naval Observatory, Washington, DC), Centre de Données Astronomiques de Strasbourg, I/252
Ochsenbein, F., Bauer, P., Marcout, J., 2000, Astron. Astrophys. Suppl., 143, 23



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