Research interests

The main focus of my research is how feedback from massive stars regulates the appearance of the interstellar medium (ISM), ongoing star formation and the chemical evolution of nearby galaxies (with a particular interest in the Local Volume dwarf galaxies). Besides, I am interested in how external gas inflows (gas accretion, tidal interactions, mergers) regulate the star formation activity and evolution of galaxies.
I use the multiwavelength observations (in particular, optical integral-field spectroscopy) from different telescopes and instruments to analyse the morphology, kinematics, physical conditions and chemical abundances of gas and dust at the scales from individual HII regions to giant kpc-sized star-forming complexes, superbubbles and outflows.

I am a member of the PHANGS collaboration and the Local Volume Mapper (SDSS-V/LVM) science team.

More information in my CV and publications.

Most recent first/corresponding author papers

PHANGS-JWST First Results: Destruction of the PAH Molecules in H II Regions Probed by JWST and MUSE

Egorov O.V. et al., ApJL, 944, L16 (2023)

Polycyclic aromatic hydrocarbons (PAHs) play a critical role in the reprocessing of stellar radiation and balancing the heating and cooling processes in the interstellar medium but appear to be destroyed in H II regions. However, the mechanisms driving their destruction are still not completely understood. Using PHANGS-JWST and PHANGS-MUSE observations, we investigate how the PAH fraction changes in about 1500 H II regions across four nearby star-forming galaxies ... (NGC 628, NGC 1365, NGC 7496, and IC 5332).We find a strong anticorrelation between the PAH fraction and the ionization parameter (the ratio between the ionizing photon flux and the hydrogen density) of H II regions. This relation becomes steeper for more luminous H II regions. The metallicity of H II regions has only a minor impact on these results in our galaxy sample. We find that the PAH fraction decreases with the Hα equivalent width-a proxy for the age of the H II regions-although this trend is much weaker than the one identified using the ionization parameter. Our results are consistent with a scenario where hydrogen-ionizing UV radiation is the dominant source of PAH destruction in star-forming regions.

Unveiling the nitrogen-rich massive star in the metal-poor galaxy NGC 4068

Yarovova A.D., Egorov O.V. et al. MNRAS, 518, 2256 (2023)

We report the identification of the unusual emission-line stellar-like object in the nearby low-metallicity (Z∼0.1Z⊙) dwarf galaxy NGC 4068. Our observations performed with long-slit spectrograph and Fabry-Perot interferometer demonstrate high velocity dispersion in H α line, presence of He II λ4686Å line and peculiarly low [S II]/[N II] fluxes ratio for this object. From observational data, we derived that the object represents a single star of high bolometric luminosity (L* ~1.5e6 L⊙) surrounded by an expanding nebula with kinematical age of t~0.5 Myr.... The nebula exhibits significant nitrogen overabundance [log (N/O)~-0.05, that is by ~1.4 dex higher than expected for low-metallicity galaxies]. We suggested that this is a massive blue supergiant (BSG) or Wolf-Rayet (WR) star surrounded by its ejecta interacting with the interstellar medium. We calculated the models of the nebula using CLOUDY photoionization code, applying CMFGEN-modelled BSG and WR stars as ionization sources. We found a best agreement between the modelled and observed spectra for the model assuming ionization by low-metallicity WR star of mass M∗≈80M⊙, ionizing the nebula through the strong wind and enriching the interstellar medium with nitrogen.

Stellar feedback impact on the ionized gas kinematics in the dwarf galaxy Sextans A

Gerasimov I.S., Egorov O.V. et al., MNRAS, 517, 4968 (2022)

Feedback from massive stars shapes the interstellar medium (ISM) and affects the evolution of galaxies, but its mechanisms acting at the small scales (~10 pc) are still not well constrained observationally, especially in the low-metallicity environments. We present the analysis of the ionized gas (focusing on its kinematics, which were never studied before) and its connection to the massive stars in the nearby (D ~ 1.4 Mpc) star-forming very metal poor (Z∼0.07Z⊙) galaxy Sextans A.... The analysis is based on the observations with a scanning Fabry-Perot interferometer, long-slit spectroscopy, and imaging in emission lines with narrow-band tunable filters. We found 10 expanding superbubbles of ionized gas with ages of 1-3 Myr. We argue that three of them are probable supernova remnants, while the pre-supernova feedback is an important source of energy for blowing out the remaining superbubbles. The two brightest sites of star formation exhibit signs of outflowing ionized gas, which is traced by its ionized and atomic gas kinematics and (in one case) by its emission line flux ratios. Overall, the ionized gas kinematics in Sextans A is highly affected by the feedback from several generations of massive stars and inconsistent with the mere solid-body rotation observed in atomic hydrogen.

Star formation in the nearby dwarf galaxy DDO 53: interplay between gas accretion and stellar feedback

Egorov O.V. et al., MNRAS, 508, 2650 (2021)

We present the results of a multiwavelength study of the nearby dwarf galaxy DDO 53 - a relatively isolated member of the M 81 group. We analyse the atomic and ionized gas kinematics (based on the observations with Fabry-Perot interferometer in H α line and archival data in H I 21 cm line), distribution, excitation, and oxygen abundance of the ionized gas (based on the long-slit and integral-field spectroscopy and on imaging with narrow-band filters), and their relation with the young massive stars ...(based on archival HST data). We detect a faint 2-kpc sized supershell of ionized gas surrounding the galaxy. Most probably, this structure represents a large-scale gas outflow, however, it could be also created by the ionizing quanta leaking from star-forming regions to the marginally detected atomic hydrogen surrounding the galactic disc. We analyse the properties of the anomalous H I in the north part of the galaxy and find that its peculiar kinematics is also traced by ionized gas. We argue that this H I feature is related to the accreting gas cloud captured from the intergalactic medium or remaining after the merger event occurred >1 Gyr ago. The infalling gas produces shocks in the interstellar medium and could support the star formation activity in the brightest region in DDO 53.


  • Address

    Astronomisches Rechen-Institut,
    Zentrum für Astronomie der Universität Heidelberg
    Mönchhofstraße 12-14,
    Heidelberg 69120
  • Email

    oleg.egorov (at)