An X-ray spectral survey of the disc of M 31 with XMM-Newton

Greening, L. Shaw; Barnard, R.; Kolb, U.; Tonkin, C.; Osborne, J. P.

doi:10.1051/0004-6361/200809864

Cited by 19 publications

(17 citation statements)

References 35 publications

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“…for variability >3; 6 new X-ray binary candidates, 3 supernova remnant classifications were rejected Shaw Greening et al (2009 X 335 ∼10 34 -∼10 39 5 fields along background subtracted spectra and lightcurves for (0.3-10 keV) major axis each source; 18 HMXB candidates, selected from their power law photon index Stiele et al (2010) X 40 whole galaxy supersoft sources; comparing ROSAT, Chandra and XMM-Newton catalogues Notes. (+) X-ray satellite(s) on which the study is based: E for Einstein, R for ROSAT, C for Chandra, and X for XMM-Newton (EPIC).…”

Section: Screening For High Backgroundmentioning

confidence: 99%

“…One of these sources ([SBK2009] 123) correlates with a globular cluster, and hence it is rather an LMXB in a very hard state rather than an HMXB (cf. Trudolyubov & Priedhorsky 2004 Eger (2008) developed a selection algorithm for HMXBs in the SMC, which also uses properties of the optical companion.…”

Section: Detection Of High Mass X-ray Binariesmentioning

confidence: 99%

“…Recently, Trudolyubov & Priedhorsky (2008) reported the discovery of 217s pulsations in the bright persistent SSS XMMU J004252.5+411540. Shaw Greening et al (2009 presented the results of a complete spectral survey of the 335 X-ray point sources they detected in five XMM-Newton observations located along the major axis of M 31. They obtained background subtracted spectra and lightcurves for each of the 335 X-ray sources.…”

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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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: Screening For High Backgroundmentioning

confidence: 99%

Section: Detection Of High Mass X-ray Binariesmentioning

confidence: 99%

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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“…The disk XLFs of M31 are more difficult to compare as studies of the M31 disk return different results (Kong et al 2003, Shaw Greening et al 2009). Although the XLFs in each of the disk regions are consistent with single, unbroken power law, as expected, the power-law slopes measured by each group are significantly different.…”

Section: Comparisons With M31mentioning

confidence: 99%

LUMINOSITY FUNCTIONS AND POINT-SOURCE PROPERTIES FROM MULTIPLECHANDRAOBSERVATIONS OF M81

Sell

Pooley

Zezas

et al. 2011

ApJ

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We present an analysis of 15 Chandra observations of the nearby spiral galaxy M81 taken over the course of six weeks in May-July 2005. Each observation reaches a sensitivity of ∼ 10 37 erg s −1 . With these observations and one previous deeper Chandra observation, we compile a master source list of 265 point sources, extract and fit their spectra, and differentiate basic populations of sources through their colors. We also carry out variability analyses of individual point sources and of X-ray luminosity functions in multiple regions of M81 on timescales of days, months, and years. We find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the X-ray luminosity function of M81. We also fit the X-ray luminosity functions for multiple regions of M81 and, using common parametrizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way.

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“…Among dozens of new X-ray pulsators found so far with periodic signals at high confidence (>4.5σ ), there is 3XMM J004301.4+413017 (3X J0043) in M 31. 3X J0043 (Supper et al 2001;Kaaret 2002) lies in the direction of an external arm to the north-east of the galaxy, and was proposed as a high-mass X-ray binary (HMXB) by Shaw Greening et al (2009). The suggestion was based on its hard X-ray spectrum and the coincidence (within 0.7 arcsec) with a V = 17.2 object found in the optical catalogue by Massey et al (2006).…”

Section: Introductionmentioning

confidence: 99%

EXTraS discovery of an 1.2-s X-ray pulsar in M 31

Esposito

Israel

Belfiore

et al. 2015

Monthly Notices of the Royal Astronomical Society: Letters

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During a search for coherent signals in the X-ray archival data of XMM-Newton, we discovered a modulation at 1.2 s in 3XMM J004301.4+413017 (3X J0043), a source lying in the direction of an external arm of M 31. This short period indicates a neutron star (NS). Between 2000 and 2013, the position of 3X J0043 was imaged by public XMM-Newton observations 35 times. The analysis of these data allowed us to detect an orbital modulation at 1.27 d and study the long-term properties of the source. The emission of the pulsar was rather hard (most spectra are described by a power law with < 1) and, assuming the distance to M 31, the 0.3-10 keV luminosity was variable, from ∼3 × 10 37 to 2 × 10 38 erg s −1 . The analysis of optical data shows that, while 3X J0043 is likely associated to a globular cluster in M 31, a counterpart with V 22 outside the cluster cannot be excluded. Considering our findings, there are two main viable scenarios for 3X J0043: a peculiar low-mass X-ray binary, similar to 4U 1822−37 or 4U 1626−67, or an intermediate-mass X-ray binary resembling Her X−1. Regardless of the exact nature of the system, 3X J0043 is the first accreting NS in M 31 in which the spin period has been detected.Key words: galaxies: individual: M 31 -X-rays: binaries -X-rays: individual: 3XMM J004301.4+413017. I N T RO D U C T I O NEXTraS (Exploring the X-ray Transient and variable Sky) is a project to explore systematically the serendipitous content of the XMM-Newton European Photon Imaging Camera (EPIC) pn (Strüder et al. 2001) and MOS (Turner et al. 2001) data in the temporal domain. The results will be released to the astronomical community in an easy-to-use form. The project includes a search for fast transients missed by standard image analysis, as well as the search and characterization of variability (both periodical and aperiodical) in hundreds of thousands of sources, spanning more than nine orders of magnitude in time-scale (from <1 s to >10 yr) and

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An X-ray spectral survey of the disc of M 31 with XMM-Newton

Cited by 19 publications

References 35 publications

The deepXMM-NewtonSurvey of M 31

The deepXMM-NewtonSurvey of M 31

LUMINOSITY FUNCTIONS AND POINT-SOURCE PROPERTIES FROM MULTIPLECHANDRAOBSERVATIONS OF M81

EXTraS discovery of an 1.2-s X-ray pulsar in M 31

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