Discovery of a 30-d period in the supergiant fast X-ray transient SAX J1818.6–1703

Bird, A. J.; Bazzano, A.; Hill, A. B.; McBride, V. A.; Sguera, V.; Shaw, S. E.; Watkins, H. J.

doi:10.1111/j.1745-3933.2008.00583.x

Cited by 40 publications

(55 citation statements)

References 23 publications

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“…The estimated source distance is 2.1 ± 0.1 kpc (Torrejón et al 2010). An in-depth study of the X-ray activity of the source was carried out by Bird et al (2009) andChaty (2009). The first investigation determined the best orbital period of SAX J1818.6−1703 at 30 ± 0.1 d (in the following we also consider the reference phase 0 at 53 671 MJD, as reported by Bird et al 2009).…”

Section: Igr J16328−4726mentioning

confidence: 99%

“…An in-depth study of the X-ray activity of the source was carried out by Bird et al (2009) andChaty (2009). The first investigation determined the best orbital period of SAX J1818.6−1703 at 30 ± 0.1 d (in the following we also consider the reference phase 0 at 53 671 MJD, as reported by Bird et al 2009). Zurita Heras & Chaty (2009) also found that most of the discovered outbursts took place when the NS passed close to the periastron, and that the source usually remains relatively bright in X-rays (a few times 10 −11 erg/cm 2 /s) for about ∼6 d around this orbital phase.…”

Section: Igr J16328−4726mentioning

confidence: 99%

“…IGR J17354−3255 was discovered with INTEGRAL in 2006 during a monitoring observation of the Galactic bulge region (Kuulkers et al 2006), and is reported in the fourth IBIS catalogue (Bird et al 2009) and in the 54 months Swift/BAT hard X-ray catalogue (Cusumano et al 2010). The average X-ray fluxes in the 20-40 keV and 15-150 keV energy band are 1.1 × 10 −11 erg/cm 2 /s and 2.1 × 10 −11 erg/cm 2 /s, respectively.…”

Section: Igr J17354−3255mentioning

confidence: 99%

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XMM-Newtonobservations of four high mass X-ray binaries and IGR J17348−2045

Bozzo¹,

Pavan²,

Ferrigno³

et al. 2012

A&A

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We present the results of the XMM-Newton observations of five hard X-ray emitters: IGR J08262−3736, IGR J17354−3255, IGR J16328−4726, SAX J1818.6−1703, and IGR J17348−2045. The first source is a confirmed supergiant high mass X-ray binary, the following two are candidates supergiant fast X-ray transients, SAX J1818.6−1703 is a confirmed supergiant fast X-ray transient and IGR J17348−2045 is one of the still unidentified objects discovered with INTEGRAL. The XMM-Newton observations permitted the first detailed soft X-ray spectral and timing study of IGR J08262−3736 and provided further support in favor of the association of IGR J17354−3255 and IGR J16328−4726 with the supergiant fast X-ray transients. SAX J1818.6−1703 was not detected by XMM-Newton, thus supporting the idea that this source reaches its lowest X-ray luminosity ( 10 32 erg s −1 ) around apastron. For IGR J17348−2045 we identified for the first time the soft X-ray counterpart and proposed the association with a close-by radio object, suggestive of an extragalactic origin.

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Section: Igr J16328−4726mentioning

confidence: 99%

Section: Igr J16328−4726mentioning

confidence: 99%

Section: Igr J17354−3255mentioning

confidence: 99%

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XMM-Newtonobservations of four high mass X-ray binaries and IGR J17348−2045

Bozzo¹,

Pavan²,

Ferrigno³

et al. 2012

A&A

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“…This source is SAX J1818.6-1703 (in't Zand et al 1998), a high-mass X-ray binary with an OB supergiant companion in a 30 day orbit (Bird et al 2009;Zurita Heras & Chaty 2009). This source was previously observed for 9.8 ks using the ACIS-S array (in 't Zand et al 2006), and while its distance is not known, its strongly absorbed, power-law spectrum suggests that it is a background object observed through the outer envelope of M17 SWex.…”

Section: Nvmentioning

confidence: 99%

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

Povich

Townsley

Robitaille

et al. 2016

ApJ

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We present a catalog of 840 X-ray sources and first results from a 100 ks Chandra X-ray Observatory imaging study of the filamentary infrared (IR) dark cloud G014.225-00.506, which forms the central regions of a larger cloud complex known as the M17 southwest extension (M17 SWex). In addition to the rich population of protostars and young stellar objects with dusty circumstellar disks revealed by archival data from the Spitzer Space Telescope, we discover a population of X-ray-emitting, intermediate-mass pre-main-sequence stars that lack IR excess emission from circumstellar disks. We model the IR spectral energy distributions of this source population to measure its mass function and place new constraints on the destruction timescales for the inner dust disk for 2-8 M ☉ stars. We also place a lower limit on the star formation rate (SFR) and find that it is quite high (  M 0.007 M ☉ yr −1 ), equivalent to several Orion Nebula Clusters in G14.225-0.506 alone, and likely accelerating. The cloud complex has not produced a population of massive, O-type stars commensurate with its SFR. This absence of very massive (20 M ☉ ) stars suggests that either (1) M17 SWex is an example of a distributed mode of star formation that will produce a large OB association dominated by intermediate-mass stars but relatively few massive clusters, or (2) the massive cores are still in the process of accreting sufficient mass to form massive clusters hosting O stars.

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“…Additionally, it is said that also IGR J08408-4503 (P orb = 35 d, e is unknown) has large eccentricities (Leyder et al 2007;Romano et al 2009a;Bird et al 2009;Sidoli et al 2009b). Although precise measurements have not been reported, this system may enter the SFXT window, or locate around the boundary.…”

Section: Resultsmentioning

confidence: 99%

Orbital parameters of supergiant fast X-ray transients

Karino

2010

A&A

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Context. Supergiant fast X-ray transient (SFXT) is a new class of the high-mass X-ray binary that shows short X-ray flares. The physical mechanism of SFXT short flares is still open for discussion. The accretion process of dense clumps in stellar wind onto neutron star (NS) has been proposed as the origin of such short flares. Aims. In order to examine the applicability of the clumpy wind scenario, we focus on the accretion mode that depends on orbital parameters. Our goal is to impose restrictions on the orbital parameters of SFXT. Methods. Assuming a simple analytic model of clumpy wind, we investigate the condition where the size of accretion cylinder overcomes the clump size. Results. The allowed parameter region for SFXT is restricted in a relatively narrow window in P orb − e diagram. Conclusions. Binary systems with large eccentricities (e > ∼ 0.4) and moderate orbital periods (P orb ∼ 10 d) are prone to show periodic X-ray outbursts, which are characteristic for SFXT. We confirm that systems with a long orbital period of more than 100 days cannot produce bright X-ray flares in the simple clumpy wind scenario.

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Discovery of a 30-d period in the supergiant fast X-ray transient SAX J1818.6–1703

Cited by 40 publications

References 23 publications

XMM-Newtonobservations of four high mass X-ray binaries and IGR J17348−2045

XMM-Newtonobservations of four high mass X-ray binaries and IGR J17348−2045

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

Orbital parameters of supergiant fast X-ray transients

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