XMMU J174716.1–281048: a “quasi-persistent” very faint  X-ray transient?

Santo, M. Del; Sidoli, L.; Mereghetti, S.; Bazzano, A.; Tarana, A.; Ubertini, P.

doi:10.1051/0004-6361:20077536

Cited by 61 publications

(85 citation statements)

References 19 publications

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“…At a distance of 8.4 kpc (inferred from a type-I X-ray burst analysis; Degenaar et al 2011b, see below for more information about the bursts seen in this source), the corresponding X-ray luminosity of the source is ∼ 3 × 10 34 erg s −1 . The source was not visible in the previous XMM-Newton and Chandra observations performed between September 2000 and July 2001 which implied that the quiescent X-ray luminosity of the source was 10 32 erg s −1 (Del Santo et al 2007b). The rise in flux by a factor more than 100 and the low peak X-ray luminosity classifies the source as a very faint X-ray transient (Del Santo et al 2007b).…”

Section: Introductionmentioning

confidence: 82%

“…The source was not visible in the previous XMM-Newton and Chandra observations performed between September 2000 and July 2001 which implied that the quiescent X-ray luminosity of the source was 10 32 erg s −1 (Del Santo et al 2007b). The rise in flux by a factor more than 100 and the low peak X-ray luminosity classifies the source as a very faint X-ray transient (Del Santo et al 2007b). …”

Section: Introductionmentioning

confidence: 82%

“…This classifies XMM1747 as a neutron star low mass X-ray binary. On the basis of the properties of the X-ray burst observed by INTEGRAL, it was suggested that the source was likely continuously active between 2003 and 2005 and was undergoing a long-term outburst (Del Santo et al 2007b). Another type-I X-ray burst was observed from this source on August 13, 2010 ) using the Swift/Burst Alert Telescope (BAT).…”

Section: Introductionmentioning

confidence: 98%

“…The source had an X-ray flux of 3.7 × 10 −12 erg cm −2 s −1 in 2-10 keV energy band (Sidoli and Mereghetti 2003, Sidoli et al 2004, Del Santo et al 2007b). The source X-ray spectrum was best fitted with an absorbed powerlaw model with photon index Γ of 2.1 and a hydrogen column density NH of 8.9 × 10 22 cm −2 .…”

Section: Introductionmentioning

confidence: 99%

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A search for near-infrared counterparts of two faint neutron star X-ray transients: XMMU J174716.1−281048 and SAX J1806.5−2215

Kaur

Wijnands

Kamble

et al. 2016

Mon. Not. R. Astron. Soc.

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We present our near-infrared (NIR) imaging observations of two neutron star low mass X-ray binaries XMMU J174716.1-281048 and SAX J1806.5-2215 obtained using the PANIC instrument on the 6.5-meter Magellan telescope and the WHIRC instrument on the 3.5-meter WIYN telescope respectively. Both sources are members of the class of faint to very-faint X-ray binaries and undergo very long X-ray outburst, hence classified as 'quasi persistent X-ray binaries'. While XMMU J174716.1-281048 was active for almost 12 years between 2003 and 2015, SAX J1806.5-2215 has been active for more than 5 years now since 2011. From our observations, we identify two NIR stars consistent with the Chandra X-ray error circle of XMMU J174716.1-281048. The comparison of our observations with the UKIRT Galactic plane observations taken during the same outburst, color-color diagram analysis and spectral energy distribution suggest that both stars are probably a part of the field population and are likely high mass stars. Hence possibly neither of the two stars is a true NIR counterpart. For the faint X-ray binary SAX J1806.5-2215 during its current outburst, we detected a NIR star in our K band WIYN observations consistent with its Chandra error circle. The identified NIR star was not detected during the UKIRT observations taken during its quiescent state. The comparison of two observations suggest that there was an increase in flux by at least one magnitude of the detected star during our observations, hence suggests the detection of the likely counterpart of SAX J1806.5-2215.

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Section: Introductionmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 82%

Section: Introductionmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

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A search for near-infrared counterparts of two faint neutron star X-ray transients: XMMU J174716.1−281048 and SAX J1806.5−2215

Kaur

Wijnands

Kamble

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The hypothesis that a significant fraction of the lowluminosity transients are X-ray binaries, gains credence by the detection of thermonuclear X-ray bursts from several of these systems (e.g., in 't Zand et al 1991;Maeda et al 1996;Cocchi et al 1999;Cornelisse et al 2002;Chelovekov & Grebenev 2007;Del Santo et al 2007;Wijnands et al 2009). This establishes that these objects harbor accreting neutron stars, most likely in an LMXB configuration.…”

Section: Introductionmentioning

confidence: 99%

A four-year baselineSwiftstudy of enigmatic X-ray transients located near the Galactic center

Degenaar

Wijnands

2010

A&A

108

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We report on continued monitoring observations of the Galactic center carried out by the X-ray telescope aboard the Swift satellite in 2008 and 2009. This campaign revealed activity of the five known X-ray transients AX J1745.6-2901, CXOGC J174535.5-290124, GRS 1741-2853, XMM J174457-2850.3 and CXOGC J174538.0-290022. All these sources are known to undergo very faint X-ray outbursts with 2-10 keV peak luminosities of L X,peak ∼ 10 34−36 erg s −1 , although the two confirmed neutron star low-mass X-ray binaries AX J1745.6-2901 and GRS 1741-2853 can also become brighter (L X,peak ∼ 10 36−37 erg s −1 ). We discuss the observed longterm lightcurves and X-ray spectra of these five enigmatic transients. In 2008, AX J1745.6-2901 returned to quiescence following an unusually long accretion outburst of more than 1.5 years. GRS 1741-2853 was active in 2009 and displayed the brightest outburst ever recorded for this source, reaching up to a 2-10 keV luminosity of L X ∼ 1 × 10 37 (D/7.2 kpc) 2 erg s −1 . This system appears to undergo recurrent accretion outbursts approximately every 2 years. Furthermore, we find that the unclassified transient XMM J174457-2850.3 becomes bright only during short episodes (days) and is often found active in between quiescence (L X ∼ 10 32 erg s −1 ) and its maximum outburst luminosity of L X ∼ 10 36 erg s −1 . CXOGC J174535.5-290124 and CXOGC J174538.0-290022, as well as three other veryfaint X-ray transients that were detected by Swift monitoring observations in 2006, have very low time-averaged mass-accretion rates of Ṁ long < ∼ 2 × 10 −12 M yr −1 . Despite having obtained two years of new data in 2008 and 2009, no new X-ray transients were detected.

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