A ROSAT PSPC catalogue of X-ray sources in the SMC region

Haberl, F.; Filipović, Miroslav; Pietsch, W.; Kahabka, P.

doi:10.1051/aas:2000136

Cited by 103 publications

(103 citation statements)

References 6 publications

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“…For these observations, no detection at the position of SXP 1062 is reported in the catalogue of Haberl et al (2000). Assuming 10 counts as a typical detection limit and the same spectral shape as measured in the recent XMM-Newton observation, we derive upper limits of 1.4, 2.7, and 2.1 × 10 −13 erg cm −2 s −1 , respectively, which are the lowest limits for the X-ray flux reported so far.…”

Section: Long-term X-ray Light Curvementioning

confidence: 54%

Long-term evolution of the neutron-star spin period of SXP 1062

Sturm

Haberl

Oskinova

et al. 2013

A&A

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Context. The Be/X-ray binary SXP 1062 is of especial interest owing to the large spin period of the neutron star, its large spin-down rate, and the association with a supernova remnant constraining its age. This makes the source an important probe for accretion physics. Aims. To investigate the long-term evolution of the spin period and associated spectral variations, we performed an XMM-Newton target-of-opportunity observation of SXP 1062 during X-ray outburst. Methods. Spectral and timing analysis of the XMM-Newton data was compared with previous studies, as well as complementary Swift/XRT monitoring and optical spectroscopy with the SALT telescope were obtained. Results. The spin period was measured to be P s = (1071.01 ± 0.16) s on 2012 Oct. 14. The X-ray spectrum is similar to that of previous observations. No convincing cyclotron absorption features, which could be indicative for a high magnetic field strength, are found. The high-resolution RGS spectra indicate the presence of emission lines, which may not completely be accounted for by the SNR emission. The comparison of multi-epoch optical spectra suggest an increasing size or density of the decretion disc around the Be star. Conclusions. SXP 1062 showed a net spin-down with an average ofṖ s = (2.27 ± 0.44) s yr −1 over a baseline of 915 days.

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Section: Long-term X-ray Light Curvementioning

confidence: 54%

Long-term evolution of the neutron-star spin period of SXP 1062

Sturm

Haberl

Oskinova

et al. 2013

A&A

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“…For comparison, the 90% c.l. error radius obtained for RX J0059.6−7138 with ROSAT was 14.5 (Haberl et al 2000). The EPIC and ROSAT count rates, considering the uncertainties caused by the small number statistics and poorly constrained spectral properties, are consistent with a constant source flux.…”

Section: Search For X-ray Emission From Other Smc Planetary Nebulaementioning

confidence: 59%

An XMM-Newton view of planetary nebulae in the Small Magellanic Cloud

Mereghetti¹,

Krachmalnicoff

Palombara³

et al. 2010

A&A

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During an X-ray survey of the Small Magellanic Cloud, carried out with the XMM-Newton satellite, we detected significant soft X-ray emission from the central star of the high-excitation planetary nebula SMP SMC 22. Its very soft spectrum is reproduced well with a non-local thermodynamical equilibrium model atmosphere composed of H, He, C, N, and O, with abundances equal to those inferred from studies of its nebular lines. The derived effective temperature of 1.5 × 10 5 K is in close agreement with that found from the optical/UV data. The unabsorbed flux in the 0.1-0.5 keV range is ∼3 × 10 −11 erg cm −2 s −1 , corresponding to a luminosity of ∼1.2 × 10 37 erg s −1 at a distance of 60 kpc. We also searched for X-ray emission from a large number of SMC planetary nebulae, confirming the previous detection of SMP SMC 25 with a luminosity of (0.2−6) × 10 35 erg s −1 (0.1-1 keV). For the remaining objects that were not detected, we derived flux upper limits corresponding to luminosity values from several tens to hundreds times lower than that of SMP SMC 22. The exceptionally high X-ray luminosity of SMP SMC 22 is probably due to the high mass of its central star, which is rapidly evolving toward the white dwarf's cooling branch, and to a small amount of intrinsic absorption in the nebula itself.

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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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A ROSAT PSPC catalogue of X-ray sources in the SMC region

Cited by 103 publications

References 6 publications

Long-term evolution of the neutron-star spin period of SXP 1062

Long-term evolution of the neutron-star spin period of SXP 1062

An XMM-Newton view of planetary nebulae in the Small Magellanic Cloud

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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