6533b856fe1ef96bd12b26ec
RESEARCH PRODUCT
IGR J17451-3022: a dipping and eclipsing low mass X-ray binary
Patryk PjankaAlessandro PapittoSara MottaAndrzej A. ZdziarskiDavide LazzatiFabio PintoreFabio PintoreCarlo FerrignoLuciano BurderiEnrico BozzoLucia PavanGabriele PontiT. Di SalvoP. Romanosubject
PhysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)010308 nuclear & particles physicsAstrophysics::High Energy Astrophysical PhenomenaX-ray binaryFOS: Physical sciencesX-rays: individuals: IGR J17451-3022Astronomy and AstrophysicsAbsorption columnAstrophysicsAstronomy and AstrophysicOrbital periodX-rays: binarie01 natural sciencesSettore FIS/05 - Astronomia E AstrofisicaAccretion discSpace and Planetary ScienceIonization0103 physical sciencesThermalbinaries; X-rays: individuals: IGR J17451-3022; Astronomy and Astrophysics; Space and Planetary Science [X-rays]Astrophysics - High Energy Astrophysical PhenomenaLow MassAbsorption (electromagnetic radiation)010303 astronomy & astrophysicsdescription
In this paper, we report on the available X-ray data collected by INTEGRAL, Swift, and XMM-Newton during the first outburst of the INTEGRAL transient IGR J17451-3022, discovered in 2014 August. The monitoring observations provided by the JEM-X instruments on-board INTEGRAL and the Swift/XRT showed that the event lasted for about 9 months and that the emission of the source remained soft for the entire period. The source emission is dominated by a thermal component (kT~1.2 keV), most likely produced by an accretion disk. The XMM-Newton observation carried out during the outburst revealed the presence of multiple absorption features in the soft X-ray emission that could be associated to the presence of an ionized absorber lying above the accretion disk, as observed in many high-inclination low mass X-ray binaries. The XMM-Newton data also revealed the presence of partial and rectangular X-ray eclipses (lasting about 820 s), together with dips. The latter can be associated with increases in the overall absorption column density in the direction of the source. The detection of two consecutive X-ray eclipses in the XMM-Newton data allowed us to estimate the source orbital period at 22620.5(-1.8,+2.0) s (1{\sigma} c.l.).
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2016-03-10 |