Peering through the stellar wind of IGR J19140+0951 with simultaneous<i>INTEGRAL</i>/<i>RXTE</i>observations

Prat, L.; Rodríguez, J.; Hannikainen, D. C.; Shaw, S. E.

doi:10.1111/j.1365-2966.2008.13558.x

Cited by 23 publications

(24 citation statements)

References 25 publications

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“…This source was first reported in the second IBIS/ISGRI catalog and detected consistently by INTEGRAL with a flux of 1-2 mCrab in the 20-40 keV band Bird et al 2016 Although the Chandra data suffered from photon pile-up, since the photon indices derived by Chandra and Swift are so similar, it is unlikely that the large difference in the derived N H values is simply a result of the photon pile-up in Chandra. Thus, the large variability of N H is likely real and associated with material local to the source; similar N H variations have been seen in other Sg HMXBs (e.g., IGR J19140+0951; Prat et al 2008). The hard power-law index measured in the soft X-ray band suggests that the compact object in IGR J18214-1318 is more likely to be an NS than a BH, but it does not constitute strong or definitive evidence.…”

Section: Introductionmentioning

confidence: 85%

“…Another non-pulsating Sg HMXB that is similar to IGR J18214-1318 is IGR J19140+0951, except for the fact that IGR J19140+0951 exhibits a soft excess modeled by a lower temperature (kT=0.3 keV) blackbody, which is attributed to a shock formed between the ionized gas around the NS and the stellar wind (Prat et al 2008). The N H variations measured in the spectrum of IGR J19140+0951 are related to its orbital phase and are even larger than those observed for IGR J18214-1318.…”

Section: Comparison To Other Hxmbsmentioning

confidence: 99%

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An XMM-Newton and NuSTAR Study of IGR J18214-1318: A Non-pulsating High-mass X-Ray Binary with a Neutron Star

Fornasini

Tomsick

Bachetti

et al. 2017

ApJ

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IGR J18214-1318, a Galactic source discovered by the International Gamma-Ray Astrophysics Laboratory, is a high-mass X-ray binary (HMXB) with a supergiant O-type stellar donor. We report on the XMM-Newton and NuSTAR observations that were undertaken to determine the nature of the compact object in this system. This source exhibits high levels of aperiodic variability, but no periodic pulsations are detected with a 90% confidence upper limit of 2% fractional rms between 0.00003-88 Hz, a frequency range that includes the typical pulse periods of neutron stars (NSs) in HMXBs (0.1-10 3 s). Although the lack of pulsations prevents us from definitively identifying the compact object in IGR J18214-1318, the presence of an exponential cutoff with e-folding energy 30 keV in its 0.3-79 keV spectrum strongly suggests that the compact object is an NS. The X-ray spectrum also shows a Fe Kα emission line and a soft excess, which can be accounted for by either a partial-covering absorber with » N 10, which could be due to the inhomogeneous supergiant wind, or a blackbody component with = -+ kT 1.74 0.05 0.04 keV and » R 0.3 BB km, which may originate from NS hot spots. Although neither explanation for the soft excess can be excluded, the former is more consistent with the properties observed in other supergiant HMXBs. We compare IGR J18214-1318 to other HMXBs that lack pulsations or have long pulsation periods beyond the range covered by our observations.

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Section: Introductionmentioning

confidence: 85%

Section: Comparison To Other Hxmbsmentioning

confidence: 99%

An XMM-Newton and NuSTAR Study of IGR J18214-1318: A Non-pulsating High-mass X-Ray Binary with a Neutron Star

Fornasini

Tomsick

Bachetti

et al. 2017

ApJ

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“…4. The Comptonisation parameter, y = k T τ 2 /(m e c 2 ), determines the efficiency of the Comptonisation process (Titarchuk 1994;Prat et al 2008), and we derived its value from the six orbital phase ranges (see Table 2). This indicates an efficient process that corresponds to a moderate accretion rate, which is higher in the orbital phase ranges just before and after the eclipse than in the mid-orbital phase ranges.…”

Section: Orbital Phase-resolved Spectramentioning

confidence: 99%

Orbital phase-resolved spectroscopy of 4U 1538−52 with MAXI

Roca

Mihara

Nakahira

et al. 2015

A&A

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Context. 4U 1538−52, an absorbed high mass X-ray binary with an orbital period of ∼3.73 days, shows moderate orbital intensity modulations with a low level of counts during the eclipse. Several models have been proposed to explain the accretion at different orbital phases by a spherically symmetric stellar wind from the companion. Aims. The aim of this work is to study both the light curve and orbital phase spectroscopy of this source in the long term. In particular, we study the folded light curve and the changes in the spectral parameters with orbital phase to analyse the stellar wind of QV Nor, the mass donor of this binary system. Methods. We used all the observations made from the Gas Slit Camera on board MAXI of 4U 1538−52 covering many orbits continuously. We obtained the good interval times for all orbital phase ranges, which were the input for extracting our data. We estimated the orbital period of the system and then folded the light curves, and we fitted the X-ray spectra with the same model for every orbital phase spectrum. We also extracted the averaged spectrum of all the MAXI data available. Results. The MAXI spectra in the 2-20 keV energy range were fitted with an absorbed Comptonisation of cool photons on hot electrons. We found a strong orbital dependence of the absorption column density but neither the fluorescence iron emission line nor low energy excess were needed to fit the MAXI spectra. The variation in the spectral parameters over the binary orbit were used to examine the mode of accretion onto the neutron star in 4U 1538−52. We deduce a best value ofṀ/v ∞ = 0.65 × 10 −9 M yr −1 /(km s −1 ) for QV Nor.

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“…We estimated the level of emission using the results from Valinia & Marshall (1998), and first corrected the spectra from the Galactic ridge emission in a similar way as done for IGR J19140+0951 by Prat et al (2008), i.e.…”

Section: X-ray Spectral Analysismentioning

confidence: 99%

The nature of the X-ray binary IGR J19294+1816 fromINTEGRAL,RXTE, andSwiftobservations

Rodríguez

Tomsick

Bodaghee

et al. 2009

A&A

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We report the results of a high-energy multi-instrumental campaign with INTEGRAL, RXTE, and Swift of the recently discovered INTEGRAL source IGR J19294+1816. The Swift/XRT data allow us to refine the position of the source to RA J2000 = 19 h 29 m 55.9 s Dec J2000 = +18 • 18 38.4 (±3.5 ), which in turn permits us to identify a candidate infrared counterpart. The Swift and RXTE spectra are well fitted with absorbed power laws with hard (Γ ∼ 1) photon indices. During the longest Swift observation, we obtained evidence of absorption in true excess to the Galactic value, which may indicate some intrinsic absorption in this source. We detected a strong (P = 40%) pulsation at 12.43781(±0.00003) s that we interpret as the spin period of a pulsar. All these results, coupled with the possible 117 day orbital period, point to IGR J19294+1816 being an HMXB with a Be companion star. However, while the long-term INTEGRAL/IBIS/ISGRI 18−40 keV light curve shows that the source spends most of its time in an undetectable state, we detect occurrences of short (∼2000−3000 s) and intense flares that are more typical of supergiant fast X-ray transients. We therefore cannot make firm conclusions on the type of system, and we discuss the possible implications of IGR J19294+1816 being an SFXT.

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Peering through the stellar wind of IGR J19140+0951 with simultaneousINTEGRAL/RXTEobservations

Cited by 23 publications

References 25 publications

An XMM-Newton and NuSTAR Study of IGR J18214-1318: A Non-pulsating High-mass X-Ray Binary with a Neutron Star

An XMM-Newton and NuSTAR Study of IGR J18214-1318: A Non-pulsating High-mass X-Ray Binary with a Neutron Star

Orbital phase-resolved spectroscopy of 4U 1538−52 with MAXI

The nature of the X-ray binary IGR J19294+1816 fromINTEGRAL,RXTE, andSwiftobservations

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