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| Format: | Preprint |
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2025
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| Online-Zugang: | https://arxiv.org/abs/2505.10189 |
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| _version_ | 1866908410378715136 |
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| author | Bednarek, W. Sitarek, J. Ulatowski, M. |
| author_facet | Bednarek, W. Sitarek, J. Ulatowski, M. |
| contents | The GeV-TeV γ-ray emission is observed from the direction of the source Sgr A^*, which is identified with the SMBH in the centre of our Galaxy. According to some models this γ-ray emission might originate in the very compact, central region identified with the direct surrounding of the SMBH. Sgr A^* is surrounded by a massive nuclear star cluster. Occasionally these stars might pass close to the line of sight of the observer, resulting in partial absorption of the sub-TeV γ-ray emission. We investigate the conditions at which an absorption feature appears in the γ-ray light curves from the Galactic Centre or nuclei of other galaxies containing SMBHs. The detection of such features would allow to obtain constraints on the emission site of γ rays in active galaxies. We calculate the optical depths for γ rays in the radiation of individual massive stars, or from the whole population of stars for different parameters of the star cluster. We show that the observer with a line of sight close to the orbital plane of the star can register a γ-ray absorption dip lasting from a fraction of a day up to a few tens of days. The combined effect of the bulk absorption on the whole population of stars instead can produce a flickering of the observed emission of a red-noise type in the power spectrum of the emission. Predicted absorption features in the sub-TeV γ-ray light curves from galaxies with SMBHs should be easily detectable by the Large-Sized Telescopes of the Cherenkov Telescope Array Observatory. The discovery of such absorption features provides a unique indication that the γ-ray production is occurring in a compact region, close to the horizon of the SMBH. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_10189 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Dips in the sub-TeV gamma-ray light curves from central parts of galaxies due to transiting luminous stars Bednarek, W. Sitarek, J. Ulatowski, M. High Energy Astrophysical Phenomena The GeV-TeV γ-ray emission is observed from the direction of the source Sgr A^*, which is identified with the SMBH in the centre of our Galaxy. According to some models this γ-ray emission might originate in the very compact, central region identified with the direct surrounding of the SMBH. Sgr A^* is surrounded by a massive nuclear star cluster. Occasionally these stars might pass close to the line of sight of the observer, resulting in partial absorption of the sub-TeV γ-ray emission. We investigate the conditions at which an absorption feature appears in the γ-ray light curves from the Galactic Centre or nuclei of other galaxies containing SMBHs. The detection of such features would allow to obtain constraints on the emission site of γ rays in active galaxies. We calculate the optical depths for γ rays in the radiation of individual massive stars, or from the whole population of stars for different parameters of the star cluster. We show that the observer with a line of sight close to the orbital plane of the star can register a γ-ray absorption dip lasting from a fraction of a day up to a few tens of days. The combined effect of the bulk absorption on the whole population of stars instead can produce a flickering of the observed emission of a red-noise type in the power spectrum of the emission. Predicted absorption features in the sub-TeV γ-ray light curves from galaxies with SMBHs should be easily detectable by the Large-Sized Telescopes of the Cherenkov Telescope Array Observatory. The discovery of such absorption features provides a unique indication that the γ-ray production is occurring in a compact region, close to the horizon of the SMBH. |
| title | Dips in the sub-TeV gamma-ray light curves from central parts of galaxies due to transiting luminous stars |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2505.10189 |