High-mass X-ray binaries in the Magellanic Clouds

Liu, Q.Z.; Paradijs, J. van; Heuvel, E. P. J. van den

doi:10.1051/0004-6361:20053718

Cited by 99 publications

(130 citation statements)

References 26 publications

(36 reference statements)

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“…Description Liu et al (2005) HMXB catalogue of the Magellanic Clouds Coe et al (2005) Optical properties of HMXBs in the SMC Shtykovskiy & Gilfanov (2005) HMXBs in archival XMM-Newton data McGowan et al (2008b) Chandra SMC Wing survey Galache et al (2008) RXTE observations of SMC pulsars McBride et al (2008) Optical spectroscopy of BeXRB pulsars in the SMC New BeXRBs from XMM-Newton observations in Antoniou et al (2009b Optical identification of Chandra sources Antoniou et al (2009a) Optical spectroscopy of BeXRBs in the SMC Laycock et al (2010) Catalogue of SMC sources from deep Chandra observations a Rajoelimanana et al (2011b) Long-term optical variability of HMXB pulsars in the SMC Sturm et al (2013c) XMM-Newton survey of the SMC Coe & Kirk (2015) BeXRB pulsars in the SMC Notes. (a) Includes detections down to two net counts.…”

Section: Referencementioning

confidence: 99%

“…The compact object is in most cases a neutron star (NS), but it can also be a black hole (see e.g. for the Magellanic Clouds, Liu et al 2005) or a white dwarf (Sturm et al 2012, and references therein). Many of the HMXBs show pulsations in their X-ray flux, which indicate the spin period of the NS.…”

Section: Introductionmentioning

confidence: 99%

“…So far, the optical counterpart is only in one (well-confirmed) case a super-giant star (SMC X-1), while for all other identified cases a Be star (with Balmer emission lines) was found, forming a Be/X-ray binary (BeXRB). The last comprehensive catalogue of HMXBs in the SMC was published by Liu et al (2005). In the meantime, new multiwavelength data were collected, and many new objects were found with Chandra, RXTE, Swift, and XMM-Newton observations of the SMC, which can at least be treated as candidates for this class of X-ray binaries.…”

Section: Introductionmentioning

confidence: 99%

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High-mass X-ray binaries in the Small Magellanic Cloud

Haberl

Sturm

2016

A&A

157

176

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Aims. The last comprehensive catalogue of high-mass X-ray binaries in the Small Magellanic Cloud (SMC) was published about ten years ago. Since then new such systems were discovered, mainly by X-ray observations with Chandra and XMM-Newton. For the majority of the proposed HMXBs in the SMC no X-ray pulsations were discovered as yet, and unless other properties of the X-ray source and/or the optical counterpart confirm their HMXB nature, they remain only candidate HMXBs. Methods. From a literature search we collected a catalogue of 148 confirmed and candidate HMXBs in the SMC and investigated their properties to shed light on their real nature. Based on the sample of well-established HMXBs (the pulsars), we investigated which observed properties are most appropriate for a reliable classification. We defined different levels of confidence for a genuine HMXB based on spectral and temporal characteristics of the X-ray sources and colour-magnitude diagrams from the optical to the infrared of their likely counterparts. We also took the uncertainty in the X-ray position into account. Results. We identify 27 objects that probably are misidentified because they lack an infrared excess of the proposed counterpart. They were mainly X-ray sources with a large positional uncertainty. This is supported by additional information obtained from more recent observations. Our catalogue comprises 121 relatively high-confidence HMXBs (the vast majority with Be companion stars). About half of the objects show X-ray pulsations, while for the rest no pulsations are known as yet. A comparison of the two subsamples suggests that long pulse periods in excess of a few 100 s are expected for the "non-pulsars", which are most likely undetected because of aperiodic variability on similar timescales and insufficiently long X-ray observations. The highest X-ray variability together with the lowest observed minimum fluxes for short-period pulsars indicate that in addition to the eccentricity of the orbit, its inclination against the plane of the Be star circum-stellar disc plays a major role in determining the outburst behaviour. Conclusions. The large population of HMXBs in the SMC, in particular Be X-ray binaries, provides the largest homogeneous sample of such systems for statistical population studies.

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Section: Referencementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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High-mass X-ray binaries in the Small Magellanic Cloud

Haberl

Sturm

2016

A&A

157

176

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“…Binder et al (2016) propose the interesting hypothesis that the initial outburst of SN2010da marked the onset of the HMXB phase based on the recurring X-ray bursts and the presumed quiescence of the progenitor, where L X <(3-9)×10 36 erg s −1 at fourepochs. HMXBs are accretion-powered binary systems with an NS or black hole orbiting an O-or B-type companion and are subdivided into two subclasses depending on the evolutionary status of the optical companion (Liu et al 2005;Reig 2011). The most common types of HMXBs (∼60%; Liu et al 2006) are known as Be/X-ray binaries (BeXBs) and host a rapidly rotating, non-supergiant B-type star with low-ionization emission lines attributed to an equatorial "excretion" disk of material ejected from the star.…”

Section: Introductionmentioning

confidence: 99%

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

Lau

Kasliwal

Bond

et al. 2016

ApJ

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We present multi-epoch mid-infrared (IR) photometry and the optical discovery observations of the "impostor" supernova (SN) 2010da in NGC300 using new and archival Spitzer Space Telescope images and ground-based observatories. The mid-infrared counterpart of SN2010da was detected as Spitzer Infrared Intensive Transient Survey (SPIRITS)14bme in the SPIRITS, an ongoing systematic search for IR transients. Before erupting on 2010 May 24, the SN2010da progenitor exhibited a constant mid-IR flux at 3.6 and only a slight ∼10% decrease at 4.5 μm between 2003 November and 2007 December. A sharp increase in the 3.6 μm flux followed by a rapid decrease measured ∼150 days before and ∼80 days after the initial outburst, respectively, reveal a mid-IR counterpart to the coincident optical and high luminosity X-ray outbursts. At late times, after the outburst (∼2000 days), the 3.6 and 4.5 μm emission increased to over a factor of twotimes the progenitor flux and is currently observed (as of 2016 Feb) to be fading, but still above the progenitor flux. We attribute the re-brightening mid-IR emission to continued dust production and increasing luminosity of the surviving system associated with SN2010da. We analyze the evolution of the dust temperature (T d ∼700-1000 K), mass (M d ∼0.5-3.8×10 −7 M e ), luminosity (L IR ∼1.3-3.5×10 4 L e ), and the equilibrium temperature radius (R eq ∼6.4-12.2 au) in order to resolve the nature of SN2010da. We address the leading interpretation of SN2010da as an eruption from a luminous blue variable high-mass X-ray binary (HMXB) system. We propose that SN2010da is instead a supergiant (sg)B[e]-HMXB based on similar luminosities and dust masses exhibited by two other known sgB[e]-HMXB systems. Additionally, the SN2010da progenitor occupies a similar region on a mid-IR color-magnitude diagram (CMD) with known sgB[e] stars in the Large Magellanic Cloud. The lower limit estimated for the orbital eccentricity of the sgB[e]-HMXB (e>0.82) from X-ray luminosity measurements is high compared to known sgHMXBs and supports the claim that SN2010da may be associated with a newly formed HMXB system.

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“…Among the 68 objects with identified primaries ∼ 60% are Be/X-ray binaries, ∼15% are classified as giants, and ∼22% are supergiant/X-ray binaries. The catalogue of HMXRBs in the Magellanic Clouds contains 128 binaries (Liu, van Paradijs & van den Heuvel 2005), where most of the objects (76%) are known or suspected Be/X-ray binaries.…”

Section: Introductionmentioning

confidence: 99%

Tidal interaction in High‐Mass X‐ray Binaries

Stoyanov

Zamanov

2009

Astron Nachr

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Our aim is to investigate tidal interaction in High-Mass X-ray Binary stars in order to determine in which objects the rotation of the mass donors is synchronized or pseudosynchronized with the orbital motion of the compact companion. We calculate the pseudosynchronization period (Pps) and compare it with the rotational period of the mass donors (Prot). We find that (1) the Be/X-ray binaries are not synchronized, the mass donors rotate faster than the orbital period and the ratio Pps/Prot is 2 -300; (2) the giant and supergiant systems are close to synchronization and for them the ratio Pps/Prot is 0.3 -2.

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High-mass X-ray binaries in the Magellanic Clouds

Cited by 99 publications

References 26 publications

High-mass X-ray binaries in the Small Magellanic Cloud

High-mass X-ray binaries in the Small Magellanic Cloud

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

Tidal interaction in High‐Mass X‐ray Binaries

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