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Classifying IGR J18007−4146 as an intermediate polar using XMM and NuSTAR.
Classifying IGR J18007−4146 as an intermediate polar using XMM and NuSTAR.
- Source :
- Monthly Notices of the Royal Astronomical Society; Apr2022, Vol. 511 Issue 3, p4582-4589, 8p
- Publication Year :
- 2022
-
Abstract
- Many new and unidentified Galactic sources have recently been revealed by ongoing hard X-ray surveys. A significant fraction of these have been shown to be the type of accreting white dwarfs known as cataclysmic variables (CVs). Follow-up observations are often required to categorize and classify these sources, and may also identify potentially unique or interesting cases. One such case is IGR J18007−4146, which is likely a CV based on follow-up Chandra observations and constraints from optical/IR catalogues. Utilizing simultaneous XMM–Newton and NuSTAR observations, as well as the available optical/IR data, we confirm the nature of IGR J18007−4146 as an intermediate polar type CV. Timing analysis of the XMM data reveals a periodic signal at 424.4 ± 0.7 s that we interpret as the spin period of the white dwarf. Modelling the 0.3–78 keV spectrum, we use a thermal bremsstrahlung continuum but require intrinsic absorption as well as a soft component and strong Fe lines between 6 and 7 keV. We model the soft component using a single-temperature blackbody with |$kT = 73^{+8}_{-6}$| eV. From the X-ray spectrum, we are able to measure the mass of the white dwarf to be |$1.06^{+0.19}_{-0.10}$|   |$\mathrm{ M}_{\mathord \odot }$| , which means IGR J18007−4146 is more massive than the average for magnetic CVs. [ABSTRACT FROM AUTHOR]
- Subjects :
- HARD X-rays
BREMSSTRAHLUNG
X-ray spectra
X-ray binaries
ACCRETION disks
DATA analysis
Subjects
Details
- Language :
- English
- ISSN :
- 00358711
- Volume :
- 511
- Issue :
- 3
- Database :
- Complementary Index
- Journal :
- Monthly Notices of the Royal Astronomical Society
- Publication Type :
- Academic Journal
- Accession number :
- 156006845
- Full Text :
- https://doi.org/10.1093/mnras/stac263