ROSAT HRI catalogue of X-ray sources in the SMC region

Sasaki, M.; Haberl, F.; Pietsch, W.

doi:10.1051/aas:2000290

Cited by 51 publications

(64 citation statements)

References 16 publications

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“…XMMU J010137.4−720418 = RX J0101.6−7204 − This source is located close to the XMM-Newton calibration target 1E 0102.2−7219 and was detected more than 30 times. The error-weighted X-ray position is incompatible with that of the emission-line star [MA93]1277 (Meyssonnier & Azzopardi 1993), which was proposed by Sasaki et al (2000) as possible counterpart in a BeXRB. The source appears as entry 21 in Shtykovskiy & Gilfanov (2005).…”

Section: Rejected Candidates From Previous Workmentioning

confidence: 99%

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

Haberl

Sturm

2016

A&A

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149

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: Rejected Candidates From Previous Workmentioning

confidence: 99%

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

Haberl

Sturm

2016

A&A

Self Cite

149

176

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“…We refer to the SMC X-ray Pulsar (SXP) compilation for RXTE monitoring results , the ROSAT source catalogs of and Sasaki et al (2000) (for the PSPC and HRI instruments, respectively), and the catalog of Yokogawa et al (2003, hereafter Y03) for ASCA results. Published observations with XMM-Newton of HMXBs in the SMC Bar were also consulted, principally Haberl et al (2008) which became available while the present work was in progress.…”

Section: High-mass X-ray Binaries and Candidatesmentioning

confidence: 99%

“…The PSPC, HRI, and Remarks columns are drawn directly from the Yokogawa et al (2003) catalog, modified in the case of Part 1, with the SXP designation added if known. The PSPC and HRI source numbers derive from and Sasaki et al (2000) and can be compared with Tables 7 and 6. and the PF must therefore be very small at this time. The orbital phase (G08 ephemeris, Table 5) was 0.82, outside the range of the normal outbursts seen in SXP9.13, and therefore presumably far from periastron, which can account for the lack of pulsations.…”

Section: Cxou J0049135-731138-sxp913mentioning

confidence: 99%

Exploring the Small Magellanic Cloud to the Faintest X-Ray Fluxes: Source Catalog, Timing, and Spectral Analysis

Laycock

Zezas

Hong

et al. 2010

ApJ

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We present the results of a pair of 100 ks Chandra observations in the Small Magellanic Cloud (SMC) to survey high-mass X-ray binaries (HMXBs), stars, and low-mass X-ray binaries (LMXBs)/cataclysmic variables down to L x = 4.3 × 10 32 erg s −1 . The two SMC Deep Fields (DFs) are located in the most active star-forming region of the bar, with Deep Field-1 positioned at the most pulsar-rich location identified from previous surveys. Two new pulsars were discovered in the outburst: CXOU J004929.7-731058 (P = 892 s), CXOU J005252.2-721715 (P = 326 s), and three new HMXB candidates were identified. Of the 15 Be-pulsars now known in the field, 13 were detected, with pulsations seen in 9 of them. Ephemerides demonstrate that 6 of the 10 pulsars known to exhibit regular outbursts were seen outside their periastron phase, and quiescent X-ray emission at L X = 10 33 -10 34 erg s −1 is shown to be common. Comparison with ROSAT, ASCA, and XMM-Newton catalogs resulted in positive identification of several previously ambiguous sources. Bright optical counterparts exist for 40 of the X-ray sources, of which 33 are consistent with early-type stars (M V < −2, B −V < 0.2), and are the subject of a companion paper. The results point to an underlying HMXB population density up to double that of active systems. The full catalog of 394 point sources is presented along with detailed analyses of timing and spectral properties.

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“…The object showed a period of 15.3 s (Kahabka 1998(Kahabka , 1999Sasaki et al 2000; for PSPC data analysis see also Haberl et al 2000) and a flux in the 0.1-2 keV band of 2.6 × 10 −11 erg s −1 cm −2 .…”

Section: Rx J00521-7319mentioning

confidence: 99%

The discovery and study of the optical counterparts of the transient X-ray pulsars RX J0052.1-7319 and XTE J0111.2-7317 in the SMC

Covino

Negueruela

Campana

et al. 2001

A&A

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Abstract. We report on the discovery and confirmation of the optical counterparts of the two transient X-ray pulsars, RX J0052.1-7319 and XTE J0111.2-7317. In the narrow (∼3 radius) X-ray error circle of RX J0052.1-7319 we found a V = 14.6 (B − V = 0.1) 09.5IIIe (a classification as a B0Ve star is also possible, since the luminosity class depends on the uncertainty on the adopted reddening). Medium resolution spectra for this object show Balmer lines in emission with an equivalent width of Hα = −12 ÷ −16Å. In the X-ray error box of XTE J0111.2-7317 we found a relatively bright object (V = 15.4, B − V = 0.06) which has been classified as a B0.5-B1Ve star and that was later confirmed by Coe et al. (2000) as the most plausible counterpart for XTE J0111.2-7317. Also in this case we easily detect Balmer emission lines with an Hα equivalent width of about −21Å. There is also evidence for the presence of a surrounding nebula, possibly a supernova remnant. A further bright B0Ve star was found just outside the X-ray error circle of XTE J0111.2-7317. We discuss the implication of these results in the light of the current knowledge of Be/X-ray binary systems in the Magellanic Clouds and within our Galaxy.

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ROSAT HRI catalogue of X-ray sources in the SMC region

Cited by 51 publications

References 16 publications

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

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

Exploring the Small Magellanic Cloud to the Faintest X-Ray Fluxes: Source Catalog, Timing, and Spectral Analysis

The discovery and study of the optical counterparts of the transient X-ray pulsars RX J0052.1-7319 and XTE J0111.2-7317 in the SMC

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