Identifying IGR J14091−6108 as a magnetic CV with a massive white dwarf using X-ray and optical observations. Issue 1 (14th April 2016)

• Record Type: Journal Article
• Authors: Tomsick, John A.; Rahoui, Farid; Krivonos, Roman; Clavel, Maïca; Strader, Jay; Chomiuk, Laura
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 460:Issue 1(2016)
• Page Start: 513
• Page End: 523
• Publication Date: 2016-04-14
• Subjects: stars: individual: IGR J14091−6108 -- novae, cataclysmic variables -- white dwarfs -- X-rays: stars; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stw871
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: INTEGRAL Gamma-Ray (IGR) J14091−6108 is a Galactic X-ray source known to have an iron emission line, a hard X-ray spectrum, and an optical counterpart. Here, we report on X-ray observations of the source with XMM–Newton and NuSTAR as well as optical spectroscopy with European Southern Obseratory/Very Large Telescope and National Optical Astronomy Observatory/Southern Astrophysical Research Telescope. In the X-rays, this provides data with much better statistical quality than the previous observations, and this is the first report of the optical spectrum. Timing analysis of the XMM data shows a very significant detection of 576.3 ± 0.6 s period. The signal has a pulsed fraction of 30 ± 3 per cent in the 0.3–12 keV range and shows a strong drop with energy. The optical spectra show strong emission lines with significant variability in the lines and continuum, indicating that they come from an irradiated accretion disc. Based on these measurements, we identify the source as a magnetic cataclysmic variable of intermediate polar (IP) type where the white dwarf spin period is 576.3 s. The X-ray spectrum is consistent with the continuum emission mechanism being due to thermal bremsstrahlung, but partial covering absorption and reflection are also required. In addition, we use the IP mass model, which suggests that the white dwarf in this system has a high mass, possibly approaching the Chandrasekhar limit.