Discovery of the neutron star spin and a possible orbital period from the Be/X-ray binary IGR J05414-6858 in the LMC

Sturm, R.; Haberl, F.; Rau, A.; Bartlett, E. S.; Zhang, X.-L.; Schady, P.; Pietsch, W.; Greiner, J.; Coe, M. J.; Udalski, A.

doi:10.1051/0004-6361/201219093

Cited by 16 publications

(14 citation statements)

References 43 publications

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“…As done in our previous papers, we give an update of the statistics concerning the identifications of new hard X-ray INTEGRAL sources including the results of this work and those in Lutovinov et al (2012), Smith et al (2012), Sturm et al (2012), and Ratti et al (2013). Up to now, 240 INTEGRAL objects have been identified through optical or NIR spectroscopy; their separation into the main classes reported in Papers VI-IX is the following: 147 (61.2%) are AGNs, 60 (25.0%) are X-ray binaries, 29 (12.1%) are CVs, and 4 cases (1.7%) are likely identified as active stars.…”

Section: Statisticsmentioning

confidence: 94%

“…Among them, we selected unidentified or unclassified hard X-ray sources containing a single bright soft X-ray object within the IBIS 90% confidence level error box. The latter information was obtained from either the ROSAT all-sky bright source catalogue (Voges et al 1999), Swift/XRT pointings (from Krivonos et al 2009;Rodriguez et al 2009;Maiorano et al 2010;Sturm et al 2011;Kennea 2011;Landi et al 2012a;Luna et al 2012;Molina et al 2012a;Parisi et al 2012, and from the XRT archive 3 ), or Chandra observations (Kaur et al 2010;Tomsick et al 2008). As stressed and demonstrated (see Stephen et al 2006 and Papers I-IX), this procedure is extremely effective in substantially reducing the search area and in pinpointing a putative optical counterpart within the corresponding (sub)arcsecond-sized soft X-ray error box.…”

Section: Sample Selectionmentioning

confidence: 99%

“…When not indicated otherwise, X-ray luminosities in Table 7 were calculated using the fluxes extracted from Wang & Wu (1992), Voges et al (2000), Landi et al (2007Landi et al ( , 2013, Tomsick et al (2008), , Kennea (2011), Sturm et al (2011, Krivonos et al (2012), and Esposito et al (2013). Constraints on distance, reddening, spectral type, and X-ray luminosity shown in Table 7 for the identified HMXBs were derived by considering the absolute magnitudes of early-type stars and by applying the method described in Papers III and IV for the classification of this type of X-ray sources.…”

Section: X-ray Binariesmentioning

confidence: 99%

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Unveiling the nature of INTEGRAL objects through optical spectroscopy

Chavushyan¹

2013

A&A

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Within the framework of our program (running since 2004) of identification of hard X-ray INTEGRAL sources through optical spectroscopy, we present the results concerning the nature of 33 high-energy objects. The data were acquired with the use of six telescopes of different sizes and from one on-line archive. The results indicate that the majority of these objects (23 out of 33) are active galactic nuclei (AGNs), whereas 10 are sources in the local Universe with eight of which in the Galaxy and two in the Small Magellanic Cloud (SMC). Among the identified AGNs, 13 are of Type 1 (i.e., with broad emission lines), eight are of Type 2 (with narrow emissions only), and two are X-ray bright, optically normal galaxies with no apparent nuclear activity in the optical. Six of these AGNs lie at high redshift (z > 0.5). Concerning local objects, we found that five of them are Galactic cataclysmic variables, three are high-mass X-ray binaries (two of which lying in the SMC), one is a low-mass X-ray binary, and one is classified as a flare star that is likely of RS CVn type. The main optical properties and inferred physical characteristics of these sources are presented and discussed.

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Section: Statisticsmentioning

confidence: 94%

Section: Sample Selectionmentioning

confidence: 99%

Section: X-ray Binariesmentioning

confidence: 99%

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Unveiling the nature of INTEGRAL objects through optical spectroscopy

Chavushyan¹

2013

A&A

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“…2010). Using data of the XMM-Newton observations of this source carried out during its outburst in 2011, Sturm et al (2012) revealed X-ray pulsations with a period of ∼ 4.4 s in its light Table 2. Fluxes in the 20-60 keV energy band from the known hard X-ray sources in the LMC field not included in Table 1 curve and classified the source as a X-ray pulsar in a highmass X-ray binary system.…”

Section: High-mass X-ray Binariesmentioning

confidence: 99%

Deep hard X-ray survey of the Large Magellanic Cloud

Гребенев¹,

Lutovinov²,

Tsygankov³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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Results of the deep survey of the Large Magellanic Cloud (LMC), performed with the INTEGRAL observatory, are presented. The long exposure (∼ 7 Ms) allowed us to detect twenty one sources in this sky region: ten belonging to the LMC itself (7 HMXBs, 2 PSRs, 1 LMXB), six of extragalactic origin and three belonging to other galaxies from the Local Group -the Milky Way (2 sources) and Small Magellanic Cloud (1 source). Four new hard X-ray sources of these 21 ones were discovered during the survey in addition to IGR J05414-6858 reported earlier; two of them were identified with extragalactic objects. We report also for the first time the detection of a hard Xray emission from the Crab-like pulsar PSR J0537-6910 and identification of the hard X-ray source IGR J05305-6559 with the high-mass X-ray binary EXO 053109-6609.

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“…About 45 candidates have also been identified during the XMM-Newton survey of the SMC (Sturm et al 2013). While the LMC is about ten times as massive as the SMC, it contains only A&A 554, A1 (2013) 14 confirmed BeXRBs so far (Liu et al 2005;Masetti et al 2006;Sturm et al 2012;Klus et al 2013). This discrepancy is possibly explained by different star formation histories (SFHs).…”

Section: Introductionmentioning

confidence: 99%

Discovery of a 168.8 s X-ray pulsar transiting in front of its Be companion star in the Large Magellanic Cloud

Maggi

Haberl

Sturm

et al. 2013

A&A

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Aims. We report the discovery of LXP 169, a new high-mass X-ray binary in the Large Magellanic Cloud. The optical counterpart has been identified and appears to exhibit an eclipsing light curve. We performed follow-up observations to clarify the eclipsing nature of the system. Methods. Energy spectra and time series were extracted from two XMM-Newton observations to search for pulsations, characterise the spectrum, and measure spectral and timing changes. Long-term X-ray variability was studied using archival ROSAT data. The XMM-Newton positions were used to identify the optical counterpart. We obtained ultraviolet to near-infrared photometry to characterise the companion, along with its 4000 d I-band light curve and colour-magnitude variability. We observed LXP 169 with Swift at two predicted eclipse times. Results. We found a spin period of 168.8 s that did not change between two XMM-Newton observations. The X-ray spectrum, well characterised by a power law, was harder when the source was brighter. The X-ray flux of LXP 169 is found to be variable by a factor of at least 10. The counterpart is highly variable on short and long timescales, and its photometry is that of an early-type star with an ouflowing circumstellar disc producing a near-infrared excess. This classifies the source as a Be/X-ray binary pulsar. We observe a transit in the ultraviolet, thereby confirming that the companion star itself is eclipsed. We give an ephemeris for the transit of MJD 56 203.877 +0.934−0.197 + N × (24.329 ± 0.008). We propose and discuss the scenario where the matter captured from the companion's equatorial disc creates an extended region of high density around the neutron star, which partially eclipses the companion as the neutron star transits in front of it. Conclusions. This is most likely the first time the compact object in an X-ray binary is observed to eclipse its companion star. LXP 169 would be the first eclipsing Be/X-ray binary, and a wealth of important information might be gained from additional observations, such as a measure of the possible Be disc/orbital plane misalignment, or the mass of the neutron star.

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Discovery of the neutron star spin and a possible orbital period from the Be/X-ray binary IGR J05414-6858 in the LMC

Cited by 16 publications

References 43 publications

Unveiling the nature of INTEGRAL objects through optical spectroscopy

Unveiling the nature of INTEGRAL objects through optical spectroscopy

Deep hard X-ray survey of the Large Magellanic Cloud

Discovery of a 168.8 s X-ray pulsar transiting in front of its Be companion star in the Large Magellanic Cloud

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