Abstract
NGC 4460 is an isolated lenticular galaxy, in which galactic wind has been earlier discovered as a gas outflow associated with circumnuclear regions of star formation. Using the results of observations in the Hα line with the scanning Fabry–Perot interferometer on the SAO RAS 6-m telescope, we studied the kinematics of the ionized gas in this galaxy. The parameters of gas outflow from the plane of the galactic disk were refined within a simple geometric model. We show that it is impossible to characterize the wind by a fixed velocity value. Characteristic outflow velocities are within 30–80 km s−1, and they are insufficient to make the swept-out matter ultimately leave the galaxy.
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Original Russian Text © D.V. Oparin, A.V. Moiseev, 2015, published in Astrofizicheskii Byulleten, 2015, Vol. 70, No. 4, pp. 416–424.
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Oparin, D.V., Moiseev, A.V. Galactic wind in NGC 4460: New observations. Astrophys. Bull. 70, 392–399 (2015). https://doi.org/10.1134/S1990341315040021
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DOI: https://doi.org/10.1134/S1990341315040021