ERASSt J040515.6-745202, an X-ray burster in the Magellanic Bridge
| Autor: | F. Haberl, G. Vasilopoulos, C. Maitra, F. Valdes, D. Lang, V. Doroshenko, L. Ducci, I. Kreykenbohm, A. Rau, P. Weber, J. Wilms, P. Maggi, C. D. Bailyn, G. K. Jaisawal, P. S. Ray, H. Treiber |
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| Přispěvatelé: | HEP, INSPIRE |
| Jazyk: | angličtina |
| Rok vydání: | 2023 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
mass-loss [Stars] individuals: eRASSt J040515.6-745202 [X-rays] Space and Planetary Science bursts [X-rays] Magellanic Clouds FOS: Physical sciences Astronomy and Astrophysics neutron [Stars] binaries [X-rays] Astrophysics - High Energy Astrophysical Phenomena [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph] |
| Zdroj: | Haberl, F, Vasilopoulos, G, Maitra, C, Valdes, F, Lang, D, Doroshenko, V, Ducci, L, Kreykenbohm, I, Rau, A, Weber, P, Wilms, J, Maggi, P, Bailyn, C D, Jaisawal, G K, Ray, P S & Treiber, H 2023, ' ERASSt J040515.6-745202, an X-ray burster in the Magellanic Bridge ', Astronomy and Astrophysics, vol. 669, A66 . https://doi.org/10.1051/0004-6361/202245015 |
| Popis: | During the third all-sky survey (eRASS3), eROSITA, the soft X-ray instrument aboard Spectrum-Roentgen-Gamma, detected a new hard X-ray transient, eRASSt J040515.6-745202, in the direction of the Magellanic Bridge. We arranged follow-up observations and searched for archival data to reveal the nature of the transient. Using X-ray observations with XMM-Newton, NICER, and Swift, we investigated the temporal and spectral behaviour of the source for over about 10 days. The X-ray light curve obtained from the XMM-Newton observation with an 28 ks exposure revealed a type-I X-ray burst with a peak bolometric luminosity of at least 1.4e37 erg/s. The burst energetics are consistent with a location of the burster at the distance of the Magellanic Bridge. The relatively long exponential decay time of the burst of 70 s indicates that it ignited in a H-rich environment. The non-detection of the source during the other eROSITA surveys, twelve and six months before and six months after eRASS3, suggests that the burst was discovered during a moderate outburst which reached 2.6e36 erg/s in persistent emission. During the NICER observations, the source showed alternating flux states with the high level at a similar brightness as during the XMM-Newton observation. This behaviour is likely caused by dips as also seen during the last hour of the XMM-Newton observation. Evidence for a recurrence of the dips with a period of 21.8 hr suggests eRASSt J040515.6-745202 is a low-mass X-ray binary (LMXB) system with an accretion disk seen nearly edge on. We identify a multi-wavelength counterpart to the X-ray source in UVW1 and g, r, i, and z images obtained by the optical/UV monitor on XMM-Newton and the Dark Energy Camera at the Cerro Tololo Inter-American Observatory. (abbreviated) Comment: Accepted for publication in Astronomy & Astrophysics. 10 pages, 13 figures |
| Databáze: | OpenAIRE |
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