The galaxy SBS1001+555 is studied as an object from the base sample in our program for study of evolutionary processes of star formation in galaxies. The work is based on the results of panoramic spectroscopy of the central part, which is the activity zone of the galaxy with its main star formation region, which we denote by A. The observations employ an MPFS (multipupil fiber spectrograph) on the 6-m telescope of the Special Astrophysical Observatory (SAO) of the Russian Academy of Sciences (RAS) to yield a 635-725 nm spectral band with a dispersion of 0.76 Å/pixel. Besides the most intense Balmer Hα emission line, the resulting integrated spectrum includes the HeI 6678 and HeI 7065 lines, forbidden lines of nitrogen, sulfur, and argon, [NII] 6548, 6583, [SII] 6716, 6731, and [ArIII] 7136 Å, and more than ten faint lines of neutral and singly ionized iron and neon, FeI 6824, 6837, 7447, 7453, and 7544, NeI 7245 and 7544, FeII 7682 and 7687, and NeII 7213 Å. A detailed analysis is made of the twodimensional distributions of the intensities, radial velocities, and other parameters over the field of view in Hα. Besides A, the largest and brightest HII region, three small regions A1, A2, and A3 have been identified, which form a common structure with A. One of the secondary regions, A1, is revealed with a condensation that stands out in an IRAC 4.5 μm image. The values of the main parameters in their peaks are taken to be the numerical characteristics of the HII regions, and those of the integral formations are taken to be the equivalent radius, luminosity, and star-formation rate, Req, L(Hα), and SFR(Hα). The data shown here, in particular, are indicative of active processes immediately associated with the brightest source of visible radiation in SBS1001+555 and the development of a star-formation structure around it.
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Translated from Astrofizika, Vol. 65, No. 3, pp. 301-313 (August 2022)
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Hakopian, S.A., Dodonov, S.N., Moiseev, A.V. et al. Study of Galaxies with Star-Formation Regions. Panoramic Spectroscopy of SBS1001+555. Astrophysics 65, 297–307 (2022). https://doi.org/10.1007/s10511-022-09742-2
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DOI: https://doi.org/10.1007/s10511-022-09742-2