Tracing a Z-track in the M 31 X-ray binary RX J0042.6+4115

Barnard, R.; Kolb, U.; Osborne, J. P.

doi:10.1051/0004-6361:20031513

Cited by 23 publications

(29 citation statements)

References 21 publications

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“…Due to the much better spatial resolution of Chandra compared to ROSAT, Kong et al (2002b) showed that source r2-26 does not correlate with the globular cluster NB 21. Barnard et al (2003) identified this source as the first Z-source in M 31. The nature of source No.…”

Section: Integrated Colour Distribution Of Globular Clustersmentioning

confidence: 96%

“…The source with the highest XID Flux (No. 966, XID band flux of 3.75 × 10 −12 erg cm −2 s −1 ) is located in the centre of M 31 and identified as a Z-source LMXB ( Barnard et al 2003). This source has a mean absorbed XID luminosity of 2.74 × 10 38 erg s −1 .…”

Section: Flux Distributionmentioning

confidence: 97%

“…At least 15% of these sources appear to be variable on a time scale of several months. Barnard et al (2003) used XMM-Newton to study the X-ray binary RX J0042.6+4115 and suggested it as a Z-source. Orio (2006) studied the population of SSSs and QSSs with XMM-Newton.…”

Section: Introductionmentioning

confidence: 99%

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The deepXMM-NewtonSurvey of M 31

Stiele

Pietsch

Haberl

et al. 2011

A&A

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150

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Aims. The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, obtaining a luminosity lower limit ∼10 35 erg s −1 in the 0.2-4.5 keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from The main goal of the paper is to study the X-ray source population of M 31.Methods. An X-ray catalogue of 1897 sources was created, with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared, and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Results. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as is expected for an HMXB containing a neutron star primary. Conclusions. While our survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help classify these sources.

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Section: Integrated Colour Distribution Of Globular Clustersmentioning

confidence: 96%

Section: Flux Distributionmentioning

confidence: 97%

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The deepXMM-NewtonSurvey of M 31

Stiele

Pietsch

Haberl

et al. 2011

A&A

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150

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show abstract

“…XMM-Newton has observed M31 extensively, and Barnard et al [4,10,3,11,6] have conducted a survey of bright sources in the central region, over four observations. For each observation of every source, 0.3-10 keV lightcurves were obtained from source and background regions in the MOS1, MOS2 and pn images, using 2.6 second binning.…”

Section: Xmm-newton Lightcurvesmentioning

confidence: 99%

Artificial variability in XMM‐Newton observations of X‐ray sources: M31 as a case study

Barnard¹,

Trudolyubov²,

Haswell³

et al. 2007

AIP Conference Proceedings

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Abstract. Power density spectra (PDS) that are characteristic of low mass X-ray binaries (LMXBs) have been previously reported for M31 X-ray sources observed by XMM-Newton. However, we have recently discovered that these PDS are false positives resulting from the improper manipulation of non-simultaneous lightcurves. The lightcurves produced by the XMM-Newton Science Analysis Software (SAS) are non-synchronised by default. This affects not only the combination of lightcurves from the three EPIC detectors (MOS1, MOS2 and pn), but also background subtraction in the same CCD. It is therefore imperative that all SAS-generated lightcurves are synchronised by time filtering, even if the whole observation is to be used. We combined simulated lightcurves at various intensities with various offsets and found that the artefact is more dependent on the offset than the intensity. While previous timing results from M31 have been proven wrong, and also the broken power law PDS in NGC 4559 ULX-7, XMM-Newton was able to detect aperiodic variability in just 3 ks of observations of NGC 5408 ULX1. Hence XMM-Newton remains a viable tool for analysing variability in extra-galactic X-ray sources.

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“…Regarding X-ray binaries, most sources have been classified based on correlations with lists of globular clusters, fewer through the detection of long-term variability (e. g. Trudolyubov et al 2006;Stiele et al 2008;Hofmann et al 2013), and only a few sources through the detection of short-term variability features, characteristic for X-ray binaries (Barnard et al 2003;.…”

Section: Introductionmentioning

confidence: 99%

NuSTAR view of the central region of M31

Stiele

Kong

2018

Monthly Notices of the Royal Astronomical Society

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Our neighbouring large spiral galaxy, the Andromeda galaxy (M 31 or NGC 224), is an ideal target to study the X-ray source population of a nearby galaxy. NuSTAR observed the central region of M 31 in 2015 and allows studying the population of X-ray point sources at energies higher than 10 keV. Based on the source catalogue of the large XMM-Newton survey of M 31, we identified counterparts to the XMM-Newton sources in the NuSTAR data. The NuSTAR data only contain sources of a brightness comparable (or even brighter) than the selected sources that have been detected in XMM-Newton data. We investigate hardness ratios, spectra and long-term light curves of individual sources obtained from NuSTAR data. Based on our spectral studies we suggest four sources as possible X-ray binary candidates. The long-term light curves of seven sources that have been observed more than once show low (but significant) variability.

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Tracing a Z-track in the M 31 X-ray binary RX J0042.6+4115

Cited by 23 publications

References 21 publications

The deepXMM-NewtonSurvey of M 31

The deepXMM-NewtonSurvey of M 31

Artificial variability in XMM‐Newton observations of X‐ray sources: M31 as a case study

NuSTAR view of the central region of M31

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