Peremennye Zvezdy

"Peremennye Zvezdy",
vol. 12, N 13 (2012)

New Cepheid in Cygnus and Four New Eclipsing Variables

S. V. Antipin#1,2, A. M. Zubareva#2,1
#1. Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow, Russia;
#2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

Received:   11.07.2012;   accepted:   7.11.2012
(E-mail for contact:

#NameOtherCoord (J2000)TypeMaxMinSystemPeriodEpoch (JD)typeSpCommentL.CurveFind.ChartData
1 USNO-B1.0 1394-040622821 33 42.72, +49 28 14.8EW16.5816.80R0.4833772455409.3025min Comm. 11.jpgch1.jpgdata1.txt
2 USNO-B1.0 1394-040626821 33 45.07, +49 29 22.0DCEP12.4312.75R2.130832455415.55max Comm. 22.jpgch2.jpgdata2.txt
3 USNO-B1.0 1394-040632221 33 49.25, +49 29 20.5EW16.0816.61R0.3361402455410.5710min Comm. 33.jpgch3.jpgdata3.txt
4 USNO-B1.0 1394-040633021 33 49.61, +49 29 35.2EW17.5317.92R0.3519432455409.8629min Comm. 44.jpgch4.jpgdata4.txt
5 USNO-B1.0 1272-043400919 51 45.07, +37 16 28.7EA16.0416.17R1.5302455424.327min Comm. 55.jpgch5.jpgdata5.txt


1. MinII = 16.78.

2. The brightness changes from 15.35 to 15.85 in Bpg.

3. Minima:
2455765.3665 ± 0.0005 (II);
2455777.4668 ± 0.0005 (II).
MinII = 16.58.

4. MinII = 17.87.

5. Minima:
2455424.3274 ± 0.0011 (I);
2455430.4469 ± 0.0015 (I).
MinII = 16.08.

Several years ago, one of us (S.V.A.) discovered a new Cepheid on the plates of Moscow archive taken with the 40-cm astrograph of the Crimean laboratory of Sternberg Astronomical Institute. To confirm the discovery of variability and classification, we carried out CCD photometry of the star with the 60-cm reflector of the Crimean laboratory equipped with an Apogee AP-47p CCD camera for thirty-five nights on July 30 – August 23, 2010 (JD 2455408–2455432) and July 22 – August 8, 2011 (JD 2455765–2455782). The CCD images were taken with 60-s and 80-s exposure times in the Johnson R filter and then reduced with the MaxIM DL aperture photometry package in the standard way involving flat-field and dark-frame corrections. USNO-B1.0 1394-0406224 (α = 21h33m42s.48, δ = +49°29′05″.9, J2000, 2MASS; R = 12m.83) was used for comparison. Stability of the comparison star was verified by brightness measurements with respect to several check stars. In addition to the new Cepheid, we discovered three more eclipsing variable stars on the same frames using VaST software (Sokolovsky & Lebedev 2005). The coordinates of variable stars were drawn from the 2MASS catalogue (Skrutskie et al. 2006).

In the last line of the Table, we report on the discovery of one more variable star of Algol type in the field of the cataclysmic variable RX J1951.7+3716 (the field was earlier studied by Virnina et al. 2011, but this particular star was not noticed). Detailed information on the data and the comparison star can be found in the cited paper.

Acknowledgements: The study was partially supported by the Russian Foundation for Basic Research through grant No. 11-02-00495. The authors wish to thank Dr. V.P. Goranskij for providing his software.

Skrutskie, M.F., Cutri, R.M., Stiening, R., et al., 2006, Astron. J, 131, 1163
Sokolovsky, K., Lebedev, A., 2005, in 12th Young Scientists' Conference on Astronomy and Space Physics, Kyiv, Ukraine, April 19-23, 2005, eds.: Simon, A.; Golovin, A., p.79
Virnina, N., Antipin, S.V., Zubareva, A.M., 2011, Perem. Zvezdy Prilozh., 11, No. 9

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