XMM-Newton observations of the isolated neutron star RX J0806.4-4123

Haberl, F.; Zavlin, V. E.

doi:10.1051/0004-6361:20020778

Cited by 32 publications

(32 citation statements)

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“…We used a Bayesian odds ratio (Gregory & Loredo 1996;Haberl et al 2008) and a Rayleigh Z 2 1 (Buccheri et al 1983;Haberl & Zavlin 2002) Since this period has a significance of 3.3σ and could not be confirmed in the other observations, probably owing to the lower number of detected counts, the spin period needs further confirmation.…”

Section: Analyses and Results Of X-ray Observationsmentioning

confidence: 99%

RX J0123.4-7321, a Be/X-ray binary in the wing of the Small Magellanic Cloud

Sturm

Haberl

Pietsch

et al. 2013

A&A

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Aims. To confirm faint Be/X-ray binary candidates from the XMM-Newton survey of the Small Magellanic Cloud, we searched for X-ray outbursts in archival ROSAT observations. We found that RX J0123.4-7321 was much brighter when detected with ROSAT than seen 16 years later by XMM-Newton. Methods. We analysed the ROSAT observations and the OGLE I-band light curve of the optical counterpart to investigate the nature of the system. Results. High long-term variability in the X-ray flux of a factor of ∼150 was found between the ROSAT and XMM-Newton detections, indicating strong outburst activity during the ROSAT observations. The I-band light curve reveals long-term variability and regular outbursts with a period of (119.9 ± 2.5) days, indicating the orbital period of the binary system. Conclusions. The large X-ray flux variations and the properties of the optical counterpart confirm RX J0123.4-7321 as a new Be/X-ray binary in the wing of the Small Magellanic Cloud.

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Section: Analyses and Results Of X-ray Observationsmentioning

confidence: 99%

RX J0123.4-7321, a Be/X-ray binary in the wing of the Small Magellanic Cloud

Sturm

Haberl

Pietsch

et al. 2013

A&A

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“…The same holds for the Swift data (2.5 s frame time). A χ 2 test, a Bayesian odds ratio (Gregory & Loredo 1996), and a Rayleigh Z 2 test for one harmonic (Haberl & Zavlin 2002;Buccheri et al 1983) around the periodicity signal are shown in Fig. 5.…”

Section: Pulsationsmentioning

confidence: 99%

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

Sturm

Haberl

Rau

et al. 2012

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Context. The number of known Be/X-ray binaries in the Large Magellanic Cloud is small compared to the observed population of the Galaxy or the Small Magellanic Cloud. The discovery of a system in outburst provides the rare opportunity to measure its X-ray properties in detail. Aims. IGR J05414-6858 was discovered in 2010 with INTEGRAL and was found in another outburst with the Swift satellite in 2011.To characterise the system, we analysed the data from a follow-up XMM-Newton target of opportunity observation of the 2011 outburst and investigated the stellar counterpart with photometry and spectroscopy. Methods. We modelled the X-ray spectra from the EPIC instruments on XMM-Newton and compared them with Swift archival data. We searched for periodicities and variability in the X-ray and optical light curves. The optical counterpart was classified using spectroscopy obtained with ESO's Faint Object Spectrograph at NTT. Results. The X-ray spectra as seen in 2011 are relatively hard with a photon index of ∼0.3−0.4 and show only low absorption. They deviate significantly from earlier spectra of a probable type-II outburst in 2010. The neutron star spin period of P spin = 4.4208 s was discovered with EPIC-pn. The I-band light curve revealed a transition from a low to a high state around MJD 54 500. The optical counterpart is classified as B0-1 IIIe and shows Hα emission and a variable near-infrared excess that vanishes during the 2010 outburst. In the optical high state, we found a periodicity at 19.9 days, probably caused by binarity and indicating the orbital period.

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“…In particular, a substantial contribution of ROSAT to this field has been the discovery of a group of seven radioquiet, close-by, thermally-emitting INSs, dubbed ROSAT INSs (RINSs) and sometimes referred to as the "magnificent seven" (see for recent references Treves et al 2000;Zampieri et al 2001;Haberl & Zavlin 2002; see also Popov & Prokhorov 2003). The nature of these sources has been controversial and two interpretations were proposed, either as conventional middle-aged cooling NSs or as very old NSs accreting the Send offprint requests to: S. B. Popov, e-mail: polar@sai.msu.ru interstellar gas (see again Treves et al 2000).…”

Section: Introductionmentioning

confidence: 99%

Young isolated neutron stars from the Gould Belt

Попов¹,

Colpi²,

Прохоров³

et al. 2003

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Abstract. The origin of the local population of young, cooling neutron stars is investigated with a population synthesis model taking into account the contribution of neutron stars born in the Gould Belt, in addition to those originating in the Galactic disk. We estimate their emission in the soft X-ray band as a function of distance and age and construct the Log N-Log S distribution. It is shown that the inclusion of neutron stars from the Gould Belt provides a good fit to the observed Log NLog S distribution. As the Sun is situated inside the Gould Belt, one can naturally explain the comparative local overabundance of massive progenitors and can remove the difficulty of the deficit of relatively bright ( > ∼ 0.1 ROSAT PSPC cts s −1 ) cooling neutron stars previously reported from models where only neutron stars from the Galactic disk were accounted for.Key words. stars: neutron -stars: evolution -stars: statistics -X-rays: stars IntroductionObservations of isolated neutron stars (INSs) are important for gaining deeper insight on their structure and thermal evolution and ultimately might prove decisive in unveiling the physical properties of matter at ultra-high densities. Up to a decade ago, the only known INSs were active radio pulsars, with the addition of the γ-ray pulsar Geminga. Despite the fact that X-ray emission from some radio pulsars was already detected by Einstein, it was in the 90's that ROSAT, thanks to its sensitivity in the 0.1−2 keV band, gave a clearer picture of the faint X-ray emission produced by the cooling surface of the closest INSs. ROSAT, supplemented by more recent observations by Chandra and XMM-Newton, revealed a variety of types of behavior in the X-ray emission from INSs and its relation with radio activity.In particular, a substantial contribution of ROSAT to this field has been the discovery of a group of seven radio- Since the seven RINSs have remarkably similar observed properties, it is quite natural to assume that they belong to the same class, i.e. all of them are close-by, cooling NSs. This, however, poses a major problem. A useful and standard way to study a population of sources is to compute the Log N-Log S distribution starting from a model, and then compare it with observations. This has been done for RINSs by Neuhäuser & Trümper (1999) and Popov et al. (2000b). The main conclusion of the latter investigation is that the typical spatial density of radio pulsars in our Galaxy is too low to explain RINSs. In other words, the assumption that RINSs and ordinary radio pulsars derive from the same parent population underpredicts the number of observed "coolers", i.e. NSs which are hot and close enough for their thermal emission to be detected in X-rays.An obvious solution is to invoke a local (both in space and time) overabundance of NSs with respect to those originating in the Galactic disk and seen now as radio pulsars. The main goal of this paper is to investigate the possible origin of these objects. Here we suggest that the likely birthplace for many of the INSs in th...

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XMM-Newton observations of the isolated neutron star RX J0806.4-4123

Cited by 32 publications

References 26 publications

RX J0123.4-7321, a Be/X-ray binary in the wing of the Small Magellanic Cloud

RX J0123.4-7321, a Be/X-ray binary in the wing of the Small Magellanic Cloud

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

Young isolated neutron stars from the Gould Belt

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