XMM-Newton survey of the Local Group galaxy M 33

Pietsch, W.; Misanovic, Zdenka; Haberl, F.; Hatzidimitriou, D.; Ehle, M.; Trinchieri, G.

doi:10.1051/0004-6361:20047068

Cited by 70 publications

(123 citation statements)

References 48 publications

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“…In this way, we selected 22 SNRs: the data sample is shown in Table 2. The first 3 columns report the SNR identification numbers in the various catalogs, respectively, Gordon et al (1998, labeled by "opt" in the table), Gordon et al (1999, labeled by "rad"), and Pietsch et al (2004; labeled by "xray"), while the next 3 columns show, respectively, the published linear (optical) diameters, 20 cm fluxes, and measured (i.e., absorbed) 0.2-4.5 keV fluxes.…”

Section: Results From An Independent Sample: M 33mentioning

confidence: 99%

A statistical approach to radio emission from shell-type SNRs

Bandiera¹,

Petruk

2009

A&A

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Context. Shell-type supernova remnants (SNRs) exhibit correlations between radio surface brightness, SNR diameter, and ambient medium density, that between the first two quantities being the well known Σ-D relation. Aims. We investigate these correlations, to extract useful information about the typical evolutionary stage of radio SNRs, as well as to obtain insight into the origin of the relativistic electrons and magnetic fields responsible for the synchrotron emission observed in radio.Methods. We propose a scenario, according to which the observed correlations are the combined effect of SNRs evolving in a wide range of ambient conditions, rather than the evolutionary track of a "typical" SNR. We then develop a parametric approach to interpret the statistical data, and apply it to the data sample previously published by Berkhuijsen, as well as to a sample of SNRs in the galaxy M 33. Results. We find that SNRs cease to emit effectively in radio at a stage near the end of their Sedov evolution, and that models of synchrotron emission with constant efficiencies in particle acceleration and magnetic field amplification do not provide a close match to the data. We discuss the problem of the cumulative distribution in size, showing that the slope of this distribution does not relate to the expansion law of SNRs, as usually assumed, but only to the ambient density distribution. This solves a long-standing paradox: the almost linear cumulative distribution of SNRs led several authors to conclude that these SNRs are still in free expansion, which also implies very low ambient densities. Within this framework, we discuss the case of the starburst galaxy M 82. Conclusions. Statistical properties of SNR samples may be used to shed light on both the physics of electron acceleration and the evolution of SNRs. More precise results could be obtained by combining data of several surveys of SNRs in nearby galaxies.

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Section: Results From An Independent Sample: M 33mentioning

confidence: 99%

A statistical approach to radio emission from shell-type SNRs

Bandiera¹,

Petruk

2009

A&A

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“…If we assume that we have identified all foreground star candidates from the optical correlation and inspection of the optical images, the remaining sources can be classified as SNR candidates using the criteria given in Table 6. Similar criteria were used to select supernova remnant candidates in XMM-Newton observations of M 33 (Pietsch et al 2004;Misanovic et al 2006). Ghavamian et al (2005) and Long et al (2010) confirmed the supernova remnant nature of many of these candidates based on optical and radio follow-up observations.…”

Section: Supernova Remnantsmentioning

confidence: 99%

“…The image bin size is 2 . The same procedure was applied in our previous M 31 and M 33 studies (PFH2005 and Pietsch et al 2004).…”

Section: Imagesmentioning

confidence: 99%

“…Source identification and classification were based on hardness ratios, and correlations with sources in other wavelength regimes. In follow-up work, (i) Pietsch & Haberl (2005) searched for X-ray burst sources in globular cluster (GlC) sources and candidates and identified two X-ray bursters and a few more candidates; while (ii) Pietsch et al (2005a searched for correlations with optical novae. They identified seven SSSs and one symbiotic star from the catalogue of PFH2005 with optical novae, and identified anadditional XMM-Newton source with an optical nova.…”

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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“…This pipeline was already used for the surveys of M31 (Pietsch et al 2005;Stiele et al 2011) and M33 (Pietsch et al 2004;Misanovic et al 2006). It was then enhanced for the analysis of the SMC survey by Richard Sturm (2012).…”

Section: Data Reductionmentioning

confidence: 99%

The population of X-ray supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2016

A&A

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156

205

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Aims. We present a comprehensive X-ray study of the population of supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). Using primarily XMM-Newton observations, we conduct a systematic spectral analysis of LMC SNRs to gain new insight into their evolution and the interplay with their host galaxy. Methods. We combined all the archival XMM-Newton observations of the LMC with those of our Very Large Programme LMC survey. We produced X-ray images and spectra of 51 SNRs, out of a list of 59 objects compiled from the literature and augmented with newly found objects. Using a careful modelling of the background, we consistently analysed all the X-ray spectra and measure temperatures, luminosities, and chemical compositions. The locations of SNRs are compared to the distributions of stars, cold gas, and warm gas in the LMC, and we investigated the connection between the SNRs and their local environment, characterised by various star formation histories. We tentatively typed all LMC SNRs, in order to constrain the ratio of core-collapse to type Ia SN rates in the LMC. We also compared the column densities derived from X-ray spectra to H i maps, thus probing the three-dimensional structure of the LMC. Results. This work provides the first homogeneous catalogue of the X-ray spectral properties of SNRs in the LMC. It offers a complete census of LMC remnants whose X-ray emission exhibits Fe K lines (13% of the sample), or reveals the contribution from hot supernova ejecta (39%), which both give clues to the progenitor types. The abundances of O, Ne, Mg, Si, and Fe in the hot phase of the LMC interstellar medium are found to be between 0.2 and 0.5 times the solar values with a lower abundance ratio [α/Fe] than in the Milky Way. The current ratio of core-collapse to type Ia SN rates in the LMC is constrained to N CC /N Ia = 1.35( +0.11 −0.24 ), which is lower than in local SN surveys and galaxy clusters. Our comparison of the X-ray luminosity functions of SNRs in Local Group galaxies (LMC, SMC, M31, and M33) reveals an intriguing excess of bright objects in the LMC. Finally, we confirm that 30 Doradus and the LMC Bar are offset from the main disc of the LMC to the far and near sides, respectively.

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XMM-Newton survey of the Local Group galaxy M 33

Cited by 70 publications

References 48 publications

A statistical approach to radio emission from shell-type SNRs

A statistical approach to radio emission from shell-type SNRs

The deepXMM-NewtonSurvey of M 31

The population of X-ray supernova remnants in the Large Magellanic Cloud

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