The very faint X-ray transient Swift J174610-290018 at the Galactic center
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2025
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| author | Stel, Giovanni Ponti, Gabriele Degenaar, Nathalie Sidoli, Lara Mereghetti, Sandro Mori, Kaya Bao, Tong Illiano, Giulia Mondal, Samaresh Reynolds, Mark Jin, Chichuan Lian, Tianying Mandel, Shifra Scaringi, Simone Zhang, Shuo Sanger-Johnson, Grace Wijnands, Rudy Miller, Jon M. Kennea, Jamie Zhu, Zhenlin |
| author_facet | Stel, Giovanni Ponti, Gabriele Degenaar, Nathalie Sidoli, Lara Mereghetti, Sandro Mori, Kaya Bao, Tong Illiano, Giulia Mondal, Samaresh Reynolds, Mark Jin, Chichuan Lian, Tianying Mandel, Shifra Scaringi, Simone Zhang, Shuo Sanger-Johnson, Grace Wijnands, Rudy Miller, Jon M. Kennea, Jamie Zhu, Zhenlin |
| contents | Very Faint X-ray Transients (VFXTs) are a class of X-ray binary systems that exhibit occasional outbursts with peak X-ray luminosities (L_X< 1e36 erg s^-1) much lower than typical X-ray transients. On 22nd February 2024, during its daily Galactic center monitoring, Swift-XRT detected a VFXT, 7 arcmin from Sgr A* dubbing it Swift J174610--290018. We aim to characterize the outburst that occurred in 2024, and a second, distinct outburst in 2025, to understand the nature and accretion flow properties of this new VFXT. Swift-XRT light curves are used to constrain the duration of the two events. We carried out X-ray spectral analysis exploiting XMM and NuSTAR data. We used Chandra and XMM observations of the last 25 years to constrain the quiescent luminosity of the source. During the 2024 outburst, which lasted about 50 days, the source reached a luminosity in the 2-10 keV band of L_X = 1.2e35 erg s^-1 (assuming it is located at the Galactic center). The 2025 outburst is shorter (about 5 days), and reached L_X = 9e34 erg s^-1. The spectral features of the source include an excess at 6.5-7 keV, which can be associated either with a single reflection line or with the ionized Fe XXV and XXVI lines. The same source was identified in both the XMM and Chandra catalogs of point sources (known as 4XMM J174610.7--290020). During previous detections, the source displayed luminosity levels ranging from L_X= 2e32 to L_X = 3e34 erg s^-1 between 2000 and 2010. Moreover, it exhibited a potential type I X-ray burst in 2004. The analysis of the outbursts and the potential type I burst strongly suggests the neutron star low mass X-ray binary (NS-LMXB) nature of the VFXT. The source can be described by an accretion disk corona (as has been recently proposed by the XRISM/Xtend analysis). This scenario explains the overall low luminosity of this transient and the peculiar iron lines in the spectrum. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_02079 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The very faint X-ray transient Swift J174610-290018 at the Galactic center Stel, Giovanni Ponti, Gabriele Degenaar, Nathalie Sidoli, Lara Mereghetti, Sandro Mori, Kaya Bao, Tong Illiano, Giulia Mondal, Samaresh Reynolds, Mark Jin, Chichuan Lian, Tianying Mandel, Shifra Scaringi, Simone Zhang, Shuo Sanger-Johnson, Grace Wijnands, Rudy Miller, Jon M. Kennea, Jamie Zhu, Zhenlin High Energy Astrophysical Phenomena Very Faint X-ray Transients (VFXTs) are a class of X-ray binary systems that exhibit occasional outbursts with peak X-ray luminosities (L_X< 1e36 erg s^-1) much lower than typical X-ray transients. On 22nd February 2024, during its daily Galactic center monitoring, Swift-XRT detected a VFXT, 7 arcmin from Sgr A* dubbing it Swift J174610--290018. We aim to characterize the outburst that occurred in 2024, and a second, distinct outburst in 2025, to understand the nature and accretion flow properties of this new VFXT. Swift-XRT light curves are used to constrain the duration of the two events. We carried out X-ray spectral analysis exploiting XMM and NuSTAR data. We used Chandra and XMM observations of the last 25 years to constrain the quiescent luminosity of the source. During the 2024 outburst, which lasted about 50 days, the source reached a luminosity in the 2-10 keV band of L_X = 1.2e35 erg s^-1 (assuming it is located at the Galactic center). The 2025 outburst is shorter (about 5 days), and reached L_X = 9e34 erg s^-1. The spectral features of the source include an excess at 6.5-7 keV, which can be associated either with a single reflection line or with the ionized Fe XXV and XXVI lines. The same source was identified in both the XMM and Chandra catalogs of point sources (known as 4XMM J174610.7--290020). During previous detections, the source displayed luminosity levels ranging from L_X= 2e32 to L_X = 3e34 erg s^-1 between 2000 and 2010. Moreover, it exhibited a potential type I X-ray burst in 2004. The analysis of the outbursts and the potential type I burst strongly suggests the neutron star low mass X-ray binary (NS-LMXB) nature of the VFXT. The source can be described by an accretion disk corona (as has been recently proposed by the XRISM/Xtend analysis). This scenario explains the overall low luminosity of this transient and the peculiar iron lines in the spectrum. |
| title | The very faint X-ray transient Swift J174610-290018 at the Galactic center |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2510.02079 |