AGILE detection of transient γ-ray emission from the region of the supergiant fast X-ray transient source IGR J17354-3255
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| Format: | Preprint |
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2026
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| author | Bulgarelli, Andrea Panebianco, Gabriele Sguera, Vito Tavani, Marco Fioretti, Valentina di Piano, Ambra Parmiggiani, Nicolò Romano, Patrizia Vercellone, Stefano Aboudan, Alessio Longo, Francesco Principe, Giacomo De Palma, Francesco Dolera, Emanuele Pittori, Carlotta Lucarelli, Fabrizio Verrecchia, Francesco Chen, Andrew W. Bazzano, Angela |
| author_facet | Bulgarelli, Andrea Panebianco, Gabriele Sguera, Vito Tavani, Marco Fioretti, Valentina di Piano, Ambra Parmiggiani, Nicolò Romano, Patrizia Vercellone, Stefano Aboudan, Alessio Longo, Francesco Principe, Giacomo De Palma, Francesco Dolera, Emanuele Pittori, Carlotta Lucarelli, Fabrizio Verrecchia, Francesco Chen, Andrew W. Bazzano, Angela |
| contents | Context. On April 14, 2009, the AGILE satellite detected a γ-ray flare from an unknown transient source. Subsequent X-ray follow-up observations with Swift and INTEGRAL identified the supergiant fast X-ray transient (SFXT) IGR J17354-3255 as the best candidate counterpart, based on positional coincidence and a similar temporal behaviour. Aside from this hint, no SFXT has been firmly detected at high energies to date. Overall, SFXTs comprise a subclass of high-mass X-ray binaries (HMXBs) that host a massive OB supergiant star as a companion donor. They tend to display the most extreme X-ray variability among HMXBs. These systems might be able to emit photons at MeV-TeV energies in the form of fast flares lasting from hours to a few days, with a low-duty cycle.
Aims. In this work, we analyse archival AGILE data to search for γ-ray flares consistent with IGR J17354-3255 and evaluate their possible physical origin.
Methods. We identified a transient source, AGL J1736-3250, which emitted 19 γ-ray flares and was seen to be positionally consistent with IGR J17354-3255. Most flares, detected on a 1 d timescale, concentrate most of their emission on two, four, and six hour timescales, resembling those observed in the X-ray band from IGR J17354-3255.
Results. An orbital phase analysis revealed that approximately half of the γ-ray activity occurs around the apastron passage of the compact object hosted in the binary system. We also incorporated archival Swift and INTEGRAL observations to provide phase-folded light curves at lower energies. Our collected results strongly support a physical association between IGR J17354-3255 and AGL J1736-3250, offering evidence that SFXTs could constitute a new class of Galactic high-energy transient emitters. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2605_04818 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | AGILE detection of transient γ-ray emission from the region of the supergiant fast X-ray transient source IGR J17354-3255 Bulgarelli, Andrea Panebianco, Gabriele Sguera, Vito Tavani, Marco Fioretti, Valentina di Piano, Ambra Parmiggiani, Nicolò Romano, Patrizia Vercellone, Stefano Aboudan, Alessio Longo, Francesco Principe, Giacomo De Palma, Francesco Dolera, Emanuele Pittori, Carlotta Lucarelli, Fabrizio Verrecchia, Francesco Chen, Andrew W. Bazzano, Angela High Energy Astrophysical Phenomena Context. On April 14, 2009, the AGILE satellite detected a γ-ray flare from an unknown transient source. Subsequent X-ray follow-up observations with Swift and INTEGRAL identified the supergiant fast X-ray transient (SFXT) IGR J17354-3255 as the best candidate counterpart, based on positional coincidence and a similar temporal behaviour. Aside from this hint, no SFXT has been firmly detected at high energies to date. Overall, SFXTs comprise a subclass of high-mass X-ray binaries (HMXBs) that host a massive OB supergiant star as a companion donor. They tend to display the most extreme X-ray variability among HMXBs. These systems might be able to emit photons at MeV-TeV energies in the form of fast flares lasting from hours to a few days, with a low-duty cycle. Aims. In this work, we analyse archival AGILE data to search for γ-ray flares consistent with IGR J17354-3255 and evaluate their possible physical origin. Methods. We identified a transient source, AGL J1736-3250, which emitted 19 γ-ray flares and was seen to be positionally consistent with IGR J17354-3255. Most flares, detected on a 1 d timescale, concentrate most of their emission on two, four, and six hour timescales, resembling those observed in the X-ray band from IGR J17354-3255. Results. An orbital phase analysis revealed that approximately half of the γ-ray activity occurs around the apastron passage of the compact object hosted in the binary system. We also incorporated archival Swift and INTEGRAL observations to provide phase-folded light curves at lower energies. Our collected results strongly support a physical association between IGR J17354-3255 and AGL J1736-3250, offering evidence that SFXTs could constitute a new class of Galactic high-energy transient emitters. |
| title | AGILE detection of transient γ-ray emission from the region of the supergiant fast X-ray transient source IGR J17354-3255 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2605.04818 |