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Register a new userIGR J19140+098, a new INTEGRAL transient
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Authors
Juho Schultz
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IGR J19140+098 (SIMBAD corrected name IGR J19140+0951) is a new X-ray transient, discovered by INTEGRAL during an observation of GRS 1915+015. The source presents strong variations on timescales from seconds to days. We present results of multiwavelength observations, including spectral analysis of INTEGRAL observations, and propose that IGR J19140+098 is a Galactic X-ray binary. Further classification of the source is also discussed.
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IGR J19140+0951 (formerly known as IGR J19140+098) was discovered with the INTEGRAL satellite in March 2003. We report the details of the discovery, using an improved position for the analysis. We have performed a simultaneous study of the 5-100 keV JEM-X and ISGRI spectra from which we can distinguish two different states. From the results of our analysis we propose that IGR J19140+0951 is a persistent Galactic X-ray binary, probably hosting a neutron star although a black hole cannot be completely ruled out.
The INTEGRAL observatory has been (re-)discovering new X-ray sources since the beginning of nominal operations in early 2003. These sources include X-ray binaries, Active Galactic Nuclei, cataclysmic variables, etc. Amongst the X-ray binaries, the true nature of many of these sources has remained largely elusive, though they seem to make up a population of highly absorbed high-mass X-ray binaries. One of these new sources, IGR J19140+0951, was serendipitously discovered on 2003 Mar 6 during an observation of the galactic microquasar GRS 1915+105. We observed IGR J19140+0951 with UKIRT in order to identify the infrared counterpart. Here we present the H- and K-band spectra. We determined that the companion is a B0.5-type bright supergiant in a wind-fed system, at a distance $la$ 5 kpc.
Following an extensive survey of the galactic plane by the INTEGRAL satellite, new hard X-ray sources are discovered with a significant fraction of Cataclysmic Variables (CVs) among them. We report here the identification of one of these hard X-ray sources, IGR J00234+6141, as an accreting magnetic white dwarf of intermediate polar type. We analyse the high energy emission of the INTEGRAL source using all available data and provide complementary optical photometric and spectroscopic data obtained respectively in August and October 2006. Based on a refined INTEGRAL position, we confirm the proposed optical identification. We clearly detect the presence of a 564 s periodic optical modulation that we identify as the rotation of the white dwarf. The analysis of the optical spectrum also demonstrates that the emission lines show a modulation in radial velocity with an orbital period of Porb = (4.033 +/- 0.005) hr. The two periodicities indicate that IGR00234+6141 is a magnetic CV of the intermediate polar type. This is one of the faintest and hardest sources of this type detected by INTEGRAL. This confirms earlier conclusions that IPs contribute significantly to the population of galactic X-ray sources and represent a significant fraction of the high energy background.
Of the 21 new sources that INTEGRAL discovered up to Feb. 1, 2004, five were detected with the BeppoSAX Wide Field Cameras at earlier times. IGR J16320-4751 appears to be a persistently active X-ray source which hints at a supergiant Roche-lobe overflowing companion star in this proposed high-mass X-ray binary. IGR J17091-3624 is a transient source that was detected in 1996 and 2001 with a maximum flux of 20 mCrab (2-28 keV). It is either a Be X-ray binary or a low mass X-ray binary transient. IGR J18483-0311 may be a high-mass X-ray binary, because it is located in a region rich of such objects, just like IGR J19140+098. IGR J17544-2619 appears to be a frequently active X-ray source whose hours-long flares, of which WFC detected five, are reminiscent of the stellar black hole source V4641 Sgr. We discuss this source in detail.
We report on the discovery of two Fast X-ray Transients (FXTs) from analysis of archival INTEGRAL data. Both are characterized by a remarkable hard X-ray activity above 20 keV, in term of duration (about 15 and 30 minutes, respectively), peak-flux (about 10^-9 erg cm^-2 s^-1) and dynamic range (about 2400 and 1360, respectively). Swift/XRT follow-up observations failed to detect any quiescent or low level soft X-ray emission from either of the two FXTs, providing an upper limit of the order of a few times 10^-12 erg cm^-2 s^-1. The main spectral and temporal IBIS/ISGRI characteristics are presented and discussed with the aim of infering possible hints on their nature.
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