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Kinematics and Origin of Gas in the Disk Galaxy NGC 2655

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Abstract—The new observational data concerning distribution, excitation, and kinematics of the ionized gas in the giant early-type galaxy NGC 2655 obtained at the 6m telescope of the Special Astrophysical Observatory (SAO RAS) and at the 2.5 m telescope of the Caucasian Mountain Observatory (CMO SAI MSU) are presented in this work. The joint analysis of these and earlier spectral observations has allowed us to make a conclusion about multiple nature of the gas in NGC 2655. Together with a proper large gaseous disk experiencing regular circular rotation in the equatorial plane of the stellar potential of the galaxy for billions years, we observe also remnants of a merged small satellite having striked the central part of NGC 2655 almost vertically for some 10 million years ago.

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Notes

  1. The data are provided by the DESI Legacy Imaging Surveys website legacysurvey.org.

  2. Let us note that although the FPI instrumental profile differs from the Gaussian one and is described by the Voigt profile and, in the case of the given FPI with a relatively low resolution, the observed line profiles differ little from the Gaussian one which can be clearly seen in Fig. 5.2.

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ACKNOWLEDGMENTS

We obtained the observed data partially with the unique scientific installation—the Big Telescope Alt-azimuth of SAO RAS. Observations with the SAO RAS telescopes are supported by the Ministry of Science and Higher Education of the Russian Federation. Upgrading of the instruments is carried out within the framework of the “Science and Universities” national project. In our paper, we used the data from the NED Extragalactic Database (NASA/IPAC) operated by the Jet Propulsion Laboratory and the California Institute of Technology under the contract to NASA. We used the public data from the Hubble Space Telescope taken from the Hubble Legacy Archive (the collaboration of the Telescope Science Institute, the Space Telescope European Coordinating Facility, and the Canadian Astronomy Data Centre), the data from the GALEX space telescope (NASA Galaxy Evolution Explorer) operated by the California Institute of Technology under the NASA contract No. NAS5-98034. The GALEX data comes from the MAST (Mikulski Archive for Space Telescopes) public archive maintained by the NASA Space Office under grant NNX13AC07G and other grants. The optical photometry data were provided by the Legacy Survey service based on the BASS survey data. BASS is a key project of the Chinese Telescope Access Program (TAP) funded by the National Astronomical Observatories of China, the Chinese Academy of Sciences (the Strategic Priority Research Program “Emergence of Cosmological Structures”, grant No. XDB09000000), and the Special Fund for Astronomy from the Ministry of Finance. BASS is also supported by the External Cooperation Program of the Chinese Academy of Sciences (grant no. 114A11KYSB20160057) and the National Natural Science Foundation of China (grants no. 12120101003 and no. 11433005).

Funding

Spectroscopic observations and data analysis were supported by the grant from the Russian Science Foundation no. 22-12-00080. Photometric observations in narrow filters were supported by the RFBR grant no. 20-02-00080.

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Authors and Affiliations

  1. Sternberg Astronomical Institute, Lomonosov Moscow State University, 119234, Moscow, Russia

    O. K. Sil’chenko, A. V. Moiseev & A. S. Gusev

  2. Special Astrophysical Observatory, Russian Academy of Sciences, 369167, Nizhnii Arkhyz, Russia

    A. V. Moiseev

  3. Leibniz-Institut für Astrophysik (AIP), Ander Sternwarte 16, 14482, Potsdam, Germany

    D. V. Kozlova

Authors
  1. O. K. Sil’chenko
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  2. A. V. Moiseev
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  3. A. S. Gusev
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  4. D. V. Kozlova
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Corresponding authors

Correspondence to O. K. Sil’chenko, A. V. Moiseev or A. S. Gusev.

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Translated by N. Oborina

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Sil’chenko, O.K., Moiseev, A.V., Gusev, A.S. et al. Kinematics and Origin of Gas in the Disk Galaxy NGC 2655. Astrophys. Bull. 77, 397–406 (2022). https://doi.org/10.1134/S1990341322040137

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  • DOI: https://doi.org/10.1134/S1990341322040137

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