Panoramic Spectroscopy of Galaxies with Star Formation Regions. A Study of SBS0750+603B

• Published in: Astrophysics Vol. 63; no. 1; pp. 45 - 55
• Main Authors: Hakopian, S. A., Dodonov, S. N., Moiseev, A. V., Smirnova, A. A.
• Format: Journal Article
• Language: English
• Published: New York Springer US 01.02.2020; Springer; Springer Nature B.V
• Subjects: Astronomical spectroscopy; Astronomy; Astrophysical observatories; Astrophysics; Astrophysics and Astroparticles; Astrophysics and Cosmology; Emission analysis; Galactic evolution; Galaxies; Hydrogen; Kinematics; Methods; Observations; Observations and Techniques; Parameters; Physics; Physics and Astronomy; Space Exploration and Astronautics; Space Sciences (including Extraterrestrial Physics; Spectroscopy; Spectrum analysis; Star & galaxy formation; Star formation; Stars; Stereoscope; Russia; α
• ISSN: 0571-7256; 1573-8191
• DOI: 10.1007/s10511-020-09612-9

Details of investigation of SBS0750+603B by providing 3D-spectroscopy are presented as part of a study of a sample of about 350 galaxies of star-formation activity. The observations were made on the 6-m telescope at the Special Astrophysical Observatory (SAO) of the Russian Academy of Sciences using the MPFS multi-pupil spectrograph. An analysis of the surface distributions of the major parameters of emission in the lines of the hydrogen Balmer Hα and the forbidden doublets of nitrogen [NII]6548,6583 and [SII]6716,6731, along with using data from astroarchives, revealed the morphological and kinematic features of this object. Two main components, A and B, are identified in the structure of SBS0750+603B that are associated with the two observed regions of ionized hydrogen. Their spatial characteristics and radiative parameters in the detected spectrum lines are shown. In particular, the star formation rates SFR(Hα) in components A and B are estimated to be 0.42 and 0.05 M ⊙ /year, respectively, which indicates that they differ substantially. The distribution of the radial velocities in Hα is indicative of an axial rotation in which two arms show up separately. Their mutual position and enhanced dust concentration are the likely causes of the existence of a brightness contrast plateau in the center of component A.