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BVRI CCD-Photometry of comparison stars in the fields of galaxies with active nuclei. V

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Observations of 79 comparison stars in the fields of seven Seyfert galaxies (Akn 79, Mrk 374, Mrk 382, Mrk 478, Mrk 493, Mrk 618, and Mrk 1513) and a single quasar (CTA 102) are reported. The observations were made with CCD photometry in the B, V, R, and I bands. The stellar magnitudes of these stars in the V band range from 12m.9 to 18m.4. The typical photometric uncertainties for magnitude 15 stars are 0m.008, 0m.011, 0m.009 and 0m.015 in the BVRI bands, respectively. For most of these stars the B, V, R, and I magnitudes have not been known previously. A variable star with brightness variations over a period of P = 0.1705 d was found in the field of the galaxy Mrk 478 and the sampled stars in the field of the galaxy Mrk 1513 include a variable with a period of P = 0.2211 d. These stars may be type W UMa contact binary systems with orbital periods of 0.341 and 0.4422 d, respectively. Finding charts for the comparison stars are included. These results can be used for differential photometry of the AGNs.

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Authors and Affiliations

  1. Southern Station, M. V. Lomonosov Moscow State University, Moscow, Russia

    V. T. Doroshenko

  2. Scientific-research Institute Crimean Astrophysical Observatory, T. G. Shevchenko Kiev National University, Kiev, Ukraine

    S. G. Sergeev, Yu. S. Efimov, G. A. Borman, D. N. Okhmat, N. G. Pulatova & S. V. Nazarov

  3. National Astronomical Research Institute of Thailand, Bangkok, Thailand

    N. G. Pulatova

Authors
  1. V. T. Doroshenko
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  2. S. G. Sergeev
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  3. Yu. S. Efimov
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  4. G. A. Borman
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  5. D. N. Okhmat
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  6. N. G. Pulatova
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  7. S. V. Nazarov
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Corresponding author

Correspondence to V. T. Doroshenko.

Additional information

Translated from Astrofizika, Vol. 56, No. 3, pp. 373-388 (August 2013).

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Doroshenko, V.T., Sergeev, S.G., Efimov, Y.S. et al. BVRI CCD-Photometry of comparison stars in the fields of galaxies with active nuclei. V. Astrophysics 56, 343–358 (2013). https://doi.org/10.1007/s10511-013-9290-9

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  • DOI: https://doi.org/10.1007/s10511-013-9290-9

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