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|Title:||Swift J174540.7-290015: a new accreting binary in the Galactic Centre||Authors:||PONTI, GABRIELE
De Marco, B.
Coti Zelati, F.
Bower, G. C.
|Issue Date:||2016||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||461||Issue:||3||First Page:||2688||Abstract:||We report on the identification of the new Galactic Centre (GC) transient Swift J174540.7-290015 as a likely low-mass X-ray binary located at only 16 arcsec from Sgr A<SUP>⋆</SUP>. This transient was detected on 2016 February 6, during the Swift GC monitoring, and it showed long-term spectral variations compatible with a hard- to soft-state transition. We observed the field with XMM-Newton on February 26 for 35 ks, detecting the source in the soft state, characterized by a low level of variability and a soft X-ray thermal spectrum with a high energy tail (detected by INTEGRAL up to ∼50 keV), typical of either accreting neutron stars or black holes. We observed: (I) a high column density of neutral absorbing material, suggesting that Swift J174540.7-290015 is located near or beyond the GC and; (II) a sub-Solar iron abundance, therefore we argue that iron is depleted into dust grains. The lack of detection of Fe K absorption lines, eclipses or dipping suggests that the accretion disc is observed at a low inclination angle. Radio (Very Large Array) observations did not detect any radio counterpart to Swift J174540.7-290015. No evidence for X-ray or radio periodicity is found. The location of the transient was observed also in the near-infrared (near-IR) with gamma-ray burst optical near-IR detector at MPG/European Southern Observatory La Silla 2.2 m telescope and VLT/NaCo pre- and post-outburst. Within the Chandra error region, we find multiple objects that display no significant variations.||URI:||http://hdl.handle.net/20.500.12386/26485||URL:||https://academic.oup.com/mnras/article/461/3/2688/2608489||ISSN:||0035-8711||DOI:||10.1093/mnras/stw1382||Bibcode ADS:||2016MNRAS.461.2688P||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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