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OPTIMus - a survey of massive star-forming regions at OPTical, Infrared, and Millimeter wavelengths

M. S. Kirsanova, A. V. Moiseev, A. M. Tatarnikov, A. S. Gusev, A. D. Yarovova, D. S. Wiebe

Abstract

This work presents a description of the scientific goals and objectives of OPTIMus (OPTical, Infrared, Millimeter survey of massive star-forming regions), a survey of massive star-forming regions in the optical, infrared, and millimeter wavelengths. The survey is aimed at constructing a comprehensive characterization of the multicomponent and structurally complex interstellar medium in the vicinity of young massive stars, combining both observational and theoretical aspects. Using multi-wavelength observational data, we will reconstruct the three-dimensional structure and determine the physical parameters of HII regions, photodissociation regions, and the surrounding molecular clouds. The paper describes the observational data obtained with the BTA 6-m and Zeiss-1000 telescopes of the Special Astrophysical Observatory of the Russian Academy of Sciences, the 2.5-m telescope of the Caucasian Mountain Observatory of the Sternberg Astronomical Institute of Moscow State University, and the 20-m telescope of the Onsala Space Observatory.

OPTIMus - a survey of massive star-forming regions at OPTical, Infrared, and Millimeter wavelengths

Abstract

This work presents a description of the scientific goals and objectives of OPTIMus (OPTical, Infrared, Millimeter survey of massive star-forming regions), a survey of massive star-forming regions in the optical, infrared, and millimeter wavelengths. The survey is aimed at constructing a comprehensive characterization of the multicomponent and structurally complex interstellar medium in the vicinity of young massive stars, combining both observational and theoretical aspects. Using multi-wavelength observational data, we will reconstruct the three-dimensional structure and determine the physical parameters of HII regions, photodissociation regions, and the surrounding molecular clouds. The paper describes the observational data obtained with the BTA 6-m and Zeiss-1000 telescopes of the Special Astrophysical Observatory of the Russian Academy of Sciences, the 2.5-m telescope of the Caucasian Mountain Observatory of the Sternberg Astronomical Institute of Moscow State University, and the 20-m telescope of the Onsala Space Observatory.
Paper Structure (18 sections, 19 equations, 4 figures, 1 table)

This paper contains 18 sections, 19 equations, 4 figures, 1 table.

Table of Contents

  1. INTRODUCTION
  2. Evolutionary stages of H II regions
  3. Structure and properties of ISM in star-forming regions
  4. Aims and Objectives of the OPTIMus Survey
  5. Spatial structure of H II regions and the role of stellar winds in their formation
  6. Molecular Hydrogen in PDRs
  7. Three-dimensional Structure of Massive Star-forming Regions and the Impact of H II Regions on Star Formation
  8. Objects
  9. Observational methods and data analysis
  10. Optical spectral range
  11. Near IR spectral range
  12. Millimeter wavelength range
  13. Archival Data Analysis
  14. Far-infrared spectral range
  15. X-ray and Ultraviolet wavelengths
  16. ...and 3 more sections

Figures (4)

  • Figure 1: Structure of massive star-forming regions and the morphology of ionized regions. In the schematic, ionized gas is shown in blue, the circumstellar disk in red, and the molecular cloud in brown. The asterisk symbolically represents either a single massive star or a stellar cluster, where multiple stars may contribute to the ionization of the surrounding material. During the hypercompact and ultracompact stages, a molecular disk with outflows (red and brown arrows) is observed around the massive star, along with a collapsing outer envelope. Ionized components of the outflows are indicated by blue arrows. At later stages, a dense molecular shell (dark brown) can be located at distances ranging from 0.1 pc up to several parsecs from the ionizing star. Jeans instability within the dense shell may lead to the formation of a subsequent generation of stars, including massive ones (orange circles oriented along the shell).
  • Figure 2: Optical images of H II regions from the OPTIMus survey. The images are taken from the MaNGaL instrument gallery on the website https://www.sao.ru/hq/lsfvo/devices/mangal/
  • Figure 3: Structure of the S 235 region. The H II region is shown in blue, with the depth of the color corresponding to higher or lower $n_{\rm e}$. Molecular gas is shown in brown. The ionizing star is marked with a yellow symbol, and young stars embedded in dense molecular gas are marked with orange symbols.
  • Figure 4: Infrared images of the survey objects in three filters (including continuum) shown in false colors: $\rm Br\gamma$ (green), [Fe II] (blue), H$_2$ (red).