Period-luminosity relation for persistent low-mass X-ray binaries in the near-infrared

Revnivtsev, M.; Zolotukhin, I.; Meshcheryakov, A. V.

doi:10.1111/j.1365-2966.2012.20511.x

Cited by 17 publications

(34 citation statements)

References 57 publications

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“…The existence of such a correlation has been demonstrated by Revnivtsev et al (2012), analogously to the work by van Paradijs & McClintock (1994) for the case of the optical emission of X-ray binaries. We have used their empirical formula to constrain the orbital period of GX 9+1 based on its X-ray luminosity and estimated absolute K s magnitude.…”

Section: The Origin Of the Nir Emission In Gx 9+1mentioning

confidence: 51%

On the Origin of the Near-Infrared Emission From the Neutron-Star Low-Mass X-Ray Binary Gx 9+1*

Berg

Homan

2017

ApJ

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We have determined an improved position for the luminous persistent neutron-star low-mass X-ray binary and atoll source GX 9+1 from archival Chandra X-ray Observatory data. The new position significantly differs from a previously published Chandra position for this source. Based on the revised X-ray position we have identified a new near-infrared (NIR) counterpart to GX 9+1 in K s -band images obtained with the PANIC and FourStar cameras on the Magellan Baade Telescope. NIR spectra of this =  K 16.5 0.1 s mag star, taken with the FIRE spectrograph on the Baade Telescope, show a strong Br γ emission line, which is a clear signature that we discovered the true NIR counterpart to GX 9+1. The mass donor in GX 9+1 cannot be a late-type giant, as such a star would be brighter than the estimated absolute K s magnitude of the NIR counterpart. The slope of the dereddened NIR spectrum is poorly constrained due to uncertainties in the column density N H and NIR extinction. Considering the source's distance and X-ray luminosity, we argue that N H likely lies near the high end of the previously suggested range. If this is indeed the case, the NIR spectrum is consistent with thermal emission from a heated accretion disk, possibly with a contribution from the secondary. In this respect, GX 9+1 is similar to other bright atolls and the Z sources, whose NIR spectra do not show the slope that is expected for a dominant contribution from optically thin synchrotron emission from the inner regions of a jet.

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Section: The Origin Of the Nir Emission In Gx 9+1mentioning

confidence: 51%

On the Origin of the Near-Infrared Emission From the Neutron-Star Low-Mass X-Ray Binary Gx 9+1*

Berg

Homan

2017

ApJ

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“…This suggests the presence of a Brγ absorption feature in the NIR spectrum of SAX1806 and, though the derived EW of ∼ 120 seems rather large, is indicative of hydrogen present in the system. This, coupled with an estimate of P orb ≈ 4 ± 1h from the Revnivtsev et al (2012) relations provides significant evidence against an ultracompact nature. We require NIR spectroscopy to confirm the absorption in the Brγ -band, and SAX1806 is bright and isolated enough to be targeted for spectroscopy with the current generation of 8m class telescopes.…”

Section: Discussionmentioning

confidence: 69%

“…If we assume that the secondary star fills its Roche lobe, then we can use the NIR magnitude from the 2010 outburst to constrain the orbital period of the system using the relationship between K-band magnitude, L X and P orb derived by Revnivtsev et al (2012). Assuming a distance of 8 kpc, a luminosity of L X ≈ 0.02L Edd (for a 1.4M NS) at the peak of the outburst (Del Santo et al 2010) and K = 15.63 (Torres et al 2010) we estimate P orb ≈ 15h with a typical propagated uncertainty of ±4h.…”

Section: Sax J17535-2349mentioning

confidence: 99%

“…10), so the quiescent magnitude of this source remains unknown. Zolotukhin & Revnivtsev (2015) provided a constraint of P orb < 9h using the Revnivtsev et al (2012) relations, based on an upper limit to the NIR brightness, as the source has not been detected in archival images. We can provide a more accurate estimate using the measured Ks-band magnitude.…”

Section: Ax J17542-2754mentioning

confidence: 99%

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Near-infrared counterparts of three transient very faint neutron star X-ray binaries

Shaw

Heinke

Degenaar

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present near-infrared (NIR) imaging observations of three transient neutron star X-ray binaries, SAX J1753.5-2349, SAX J1806.5-2215 and AX J1754.2-2754. All three sources are members of the class of 'very faint' X-ray transients which exhibit X-ray luminosities L X 10 36 erg s −1 . The nature of this class of sources is still poorly understood. We detect NIR counterparts for all three systems and perform multi-band photometry for both SAX J1753.5-2349 and SAX J1806.5-2215, including narrowband Br γ photometry for SAX J1806.5-2215. We find that SAX J1753.5-2349 is significantly redder than the field population, indicating that there may be absorption intrinsic to the system, or perhaps a jet is contributing to the infrared emission. SAX J1806.5-2215 appears to exhibit absorption in Br γ , providing evidence for hydrogen in the system. Our observations of AX J1754.2-2754 represent the first detection of a NIR counterpart for this system. We find that none of the measured magnitudes are consistent with the expected quiescent magnitudes of these systems. Assuming that the infrared radiation is dominated by either the disc or the companion star, the observed magnitudes argue against an ultracompact nature for all three systems.

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“…The criterion for this type of instability is still debated, the critical mass ratio could be q ≃ 12 (for The dashed-dotted line denotes the L X ∝ P orb line obtained in (Iben & Tutukov 1984;Revnivtsev et al 2012). …”

Section: Resultsmentioning

confidence: 99%

The nature of donors in ultraluminous X-ray binaries powered by neutron stars

Karino

2017

Monthly Notices of the Royal Astronomical Society

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In this study, we examine the properties of donor stars of the three recently discovered ultraluminous X-ray sources (ULXs) powered by rotating neutron stars. For this purpose, we constructed a theoretical relation between the X-ray luminosity (L X ) and the orbital period (P orb ) suitable for ULXs with neutron stars. By using this new L X − P orb relation, we attempt to determine the currently unknown nature of donor stars in ULXs associated with neutron stars. Especially, comparing the observed properties with the stellar evolution tracks, we suggest that the donor star in the NGC5907 ULX-1 system is a moderately massive star with 6 − 10M ⊙ , just departing from the main sequence phase. The results of our models for the other two ULX systems (M82 X-2 and NGC7793 P-13) are consistent with those in previous studies. Although there are only a few samples, observed ULX systems with neutron stars seems to involve relatively massive donors.

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Period-luminosity relation for persistent low-mass X-ray binaries in the near-infrared

Cited by 17 publications

References 57 publications

On the Origin of the Near-Infrared Emission From the Neutron-Star Low-Mass X-Ray Binary Gx 9+1*

On the Origin of the Near-Infrared Emission From the Neutron-Star Low-Mass X-Ray Binary Gx 9+1*

Near-infrared counterparts of three transient very faint neutron star X-ray binaries

The nature of donors in ultraluminous X-ray binaries powered by neutron stars

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