IGR J08408-4503: A New Recurrent Supergiant Fast X-Ray Transient

Götz, D.; Falanga, M.; Senziani, F.; Luca, A. De; Schanne, S.; Kienlin, A. von

doi:10.1086/511818

Cited by 25 publications

(30 citation statements)

References 30 publications

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“…The quiescent level in these systems is of the order 10 32−33 erg s −1 (e.g. IGR J08408−4503 Götz et al 2007;Leyder et al 2007). The X-ray luminosity increases up to 10 36 erg s −1 (as observed in known SGXBs) only during periods of short and luminous flares.…”

Section: Introductionmentioning

confidence: 99%

Discovery of an eccentric 30 day period in the supergiant X-ray binary SAX J1818.6–1703 with INTEGRAL

Heras

Chaty²

2008

A&A

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Context. SAX J1818.6−1703 is a flaring transient X-ray source serendipitously discovered by BeppoSAX in 1998 during an observation of the Galactic centre. The source was identified as a high-mass X-ray binary with an OB supergiant companion (SGXB). Displaying short and bright flares and an unusually very low quiescent level implying an intensity dynamical range as large as 10 3−4 , the source was classified as a supergiant fast X-ray transient (SFXT). Aims. The mechanism triggering the different temporal behaviour observed between the classical SGXBs and the recently discovered class of SFXTs is still debated. The discovery of long orbits (>15 d) should help to discriminate between emission models and bring constraints. Methods. We analysed archival INTEGRAL data on SAX J1818.6−1703. We built short-and long-term light curves and performed a timing analysis in order to study the temporal behaviour of SAX J1818.6−1703 on different time scales. Results. INTEGRAL revealed an unusually long orbital period of 30.0 ± 0.2 d and an elapsed accretion phase of ∼6 d in the transient SGXB SAX J1818.6−1703. This implies an elliptical orbit and constraints the possible supergiant spectral type between B0.5−1I with eccentricities e ∼ 0.3−0.4 (for the average fundamental parameters of supergiant stars). During the accretion phase, the source behaved like a classical SGXB. The huge variations of the observed X-ray flux can be explained through accretion of macro-clumps formed within the stellar wind. Our analysis strengthens the model which predicts that SFXTs behave as SGXBs but with different orbital parameters, thus different temporal behaviour.

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Section: Introductionmentioning

confidence: 99%

Discovery of an eccentric 30 day period in the supergiant X-ray binary SAX J1818.6–1703 with INTEGRAL

Heras

Chaty²

2008

A&A

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“…Discovered by INTEGRAL and identified as HMXB with a supergiant companion through multi-wavelength observations in X-rays, optical and infrared, these sources are rarely detected with ISGRI except during short and bright flares. Their quiescent emission reaching levels as low as 10 32−33 erg s −1 [14,15], one needs observatories such as XMM-Newton or Swift to observe such low emission. We show 2 ISGRI light curves of one SGXB and one SFXT in Fig.…”

Section: Resultsmentioning

confidence: 99%

Observational properties of candidate supergiant fast X-ray transients

Heras¹,

Chaty²,

Walter³

2009

Proceedings of 7th INTEGRAL Workshop — PoS(Integral08)

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INTEGRAL allowed the discovery of several new SuperGiant X-ray Binaries of which very few were known before its launch. Among them, INTEGRAL has unveiled a new sub-class: galactic X-ray sources with a supergiant companion and displaying a transient behaviour, namely Supergiant Fast X-ray Transient. Most of the time in quiescence with a luminosity of 10 33 erg s −1 (if not totally absent), these sources display rare episodes of short (few ks) and bright (up to ∼ 10 36 erg s −1 as in other SGXB) flares. Several scenarii have been proposed to explain the atypical temporal behaviour of the SFXT among the SGXB: a different separation/geometry of their orbits, accretion of dense structures/clumps formed in the stellar wind that would produce these huge flares, magnetic centrifugal barrier and variation of the local stellar wind density and/or sources hosting a magnetar. We present a systematic study, based on ISGRI observations from 2 ks-bin lightcurves to deep mosaics, of the observational properties (flares, duration, fluxes, etc.) of two SFXT candidates in order to bring constraints, to be able to distinguish between these different models of emission. Finally, this study will allow to better understand the overall characteristics of different classes of high-mass X-ray binaries. 7th INTEGRAL Workshop

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“…They differ from persistent High Mass X-ray Binaries (HMXBs) because (i) they have blue OB supergiant companion stars, (ii) they show very high dynamical range in outbursts (3−5 orders of magnitude). IGR J08408−4503 is an SFXT discovered in 2006 with a confirmed association with a O8.5Ib(f) supergiant star, HD 74194 [1]. Two outbursts have been caught by Swift/BAT on 2006 October 4 [2] and 2008 July 5 [3], and followed-up at softer energies with Swift/XRT.…”

Section: The History Of Swift Detected Outburst Of Igr J08408−4503mentioning

confidence: 99%

“…Luminosity of the source in the 0.5−10 and 0.5−100 keV bands for the four time intervals described in the text in units of 10 37 erg s −1 derived assuming a distance of 3 kpc[1] …”

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confidence: 99%

IGR J08408–4503 in outburst observed by Swift

Mangano

Romano²,

Ceccobello³

et al. 2012

AIP Conference Proceedings

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Supergiant Fast X-ray Transients (SFXTs) are accreting high mass X-ray binaries (HMXBs) with OB supergiant companions showing outbursts in the soft and hard X-rays. SFXT outbursts are charachterized by an increase of 3−5 orders of magnitudes in the luminosity for a few hours usually followed by smaller amplitude flaring activity. We report on the analysis of the outburst of the IGR J08408−4503 caught by Swift/BAT (in the 15−150 keV band) on 2011 August 25 and followed up at softer energies (0.2−10 keV) with Swift/XRT. The spacecraft automatic slew and BAT/XRT simultaneous observations allowed us for the first time resolved broadband spectral analysis of the outburst emission for this source. We searched for spectral evolution with different spectral models. We compare our results with those obtained from time resolved spectral analysis of the 2008 March 19 outburst of IGR J16479−4514.

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IGR J08408-4503: A New Recurrent Supergiant Fast X-Ray Transient

Cited by 25 publications

References 30 publications

Discovery of an eccentric 30 day period in the supergiant X-ray binary SAX J1818.6–1703 with INTEGRAL

Discovery of an eccentric 30 day period in the supergiant X-ray binary SAX J1818.6–1703 with INTEGRAL

Observational properties of candidate supergiant fast X-ray transients

IGR J08408–4503 in outburst observed by Swift

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