An X‐Ray Investigation of the NGC 346 Field in the Small Magellanic Cloud. III.<i>XMM‐Newton</i>Data

Nazé, Yaël; Manfroid, Jean; Stevens, I. R.; Corcoran, M. F.; Flores, Aaron

doi:10.1086/386323

Cited by 16 publications

(22 citation statements)

References 22 publications

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“…In the centre of the star cluster NGC 346 we see an unresolved convolution of X-ray bright stars (see Nazé et al 2002Nazé et al , 2004, which is source № 535 in our catalogue. Source № 2706 has similar X-ray colours and correlates with the star cluster Lindsay 66.…”

Section: Stars Within the Smcmentioning

confidence: 84%

TheXMM-Newtonsurvey of the Small Magellanic Cloud: The X-ray point-source catalogue

Sturm

Haberl

Pietsch

et al. 2013

A&A

164

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Context. Local-Group galaxies provide access to samples of X-ray source populations of whole galaxies. The XMM-Newton survey of the Small Magellanic Cloud (SMC) completely covers the bar and eastern wing with a 5.6 deg 2 area in the (0.2−12.0) keV band. Aims. To characterise the X-ray sources in the SMC field, we created a catalogue of point sources and sources with moderate extent. Sources with high extent (≥40 ) have been presented in a companion paper. Methods. We searched for point sources in the EPIC images using sliding-box and maximum-likelihood techniques and classified the sources using hardness ratios, X-ray variability, and their multi-wavelength properties. Results. The catalogue comprises 3053 unique X-ray sources with a median position uncertainty of 1.3 down to a flux limit for point sources of ∼10 −14 erg cm −2 s −1 in the (0.2−4.5) keV band, corresponding to 5 × 10 33 erg s −1 for sources in the SMC. We discuss statistical properties, like the spatial distribution, X-ray colour diagrams, luminosity functions, and time variability. We identified 49 SMC high-mass X-ray binaries (HMXB), four super-soft X-ray sources (SSS), 34 foreground stars, and 72 active galactic nuclei (AGN) behind the SMC. In addition, we found candidates for SMC HMXBs (45) and faint SSSs (8) as well as AGN (2092) and galaxy clusters (13). Conclusions. We present the most up-to-date catalogue of the X-ray source population in the SMC field. In particular, the known population of X-ray binaries is greatly increased. We find that the bright-end slope of the luminosity function of Be/X-ray binaries significantly deviates from the expected universal high-mass X-ray binary luminosity function.

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Section: Stars Within the Smcmentioning

confidence: 84%

TheXMM-Newtonsurvey of the Small Magellanic Cloud: The X-ray point-source catalogue

Sturm

Haberl

Pietsch

et al. 2013

A&A

164

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“…We constructed this image from observations of the general area around NGC 346/N66 with XMM-Newton in X-rays (blue), ESO New Technology Telescope (NTT) in [O iii] (green), and Spitzer Infrared Array Camera (IRAC) in the 8 m band (red). The XMM-Newton observations have ID 0110000201 (PI: J. Bleeker), and they have been used in variability studies of X-ray sources (Nazé et al 2004) and in the investigation of high-mass X-ray binaries (Sasaki et al 2003;Shtykovskiy & Gilfanov 2005) (Simon et al 2007).…”

Section: Star Formation Away From the Bar Of N66mentioning

confidence: 99%

NGC 346 in The Small Magellanic Cloud. IV. Triggered Star Formation in the HiiRegion N66

Gouliermis

Chu

Henning

et al. 2008

Astrophysical Journal

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Stellar feedback, expanding H ii regions, wind-blown bubbles, and supernovae are thought to be important triggering mechanisms of star formation. Stellar associations, being hosts of significant numbers of early-type stars, are the loci where these mechanisms act. In this part of our photometric study of the star-forming region NGC 346/N66 in the Small Magellanic Cloud, we present evidence based on previous and recent detailed studies that it hosts at least two different events of triggered star formation, and we reveal the complexity of its recent star formation history. In our earlier studies of this region (Papers I and III) we find that besides the central part of N66, where the bright OB stellar content of the association NGC 346 is concentrated, an arclike nebular feature, north of the association, hosts recent star formation. This feature is characterized by a high concentration of emission-line stars and young stellar objects, as well as embedded sources seen as IR emission peaks that coincide with young compact clusters of low-mass pre-mainsequence stars. All these objects indicate that the northern arc of N66 encompasses the most current star formation event in the region. We present evidence that this star formation is the product of a different mechanism than that in the general area of the association, and that it is triggered by a wind-driven expanding H ii region (or bubble) blown by a massive supernova progenitor, and possibly other bright stars, a few megayears ago. We propose a scenario according to which this mechanism triggered star formation away from the bar of N66, while in the bar of N66 star formation is introduced by the photoionizing OB stars of the association itself.

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“…SNRs and SNR candidates in the SMC. The radio spectral index (α) is taken from Filipović et al (2005) Payne et al 2007;van der Heyden et al 2004;Dickel et al 2001;Mathewson et al 1984;Mills et al 1982;Hughes & Smith 1994;Nazé et al 2004, and references therein). Thirteen of the remnants were covered by early XMM-Newton observations and a comprehensive study was presented by van der Heyden et al (2004).…”

Section: Introductionmentioning

confidence: 99%

New XMM-Newton observations of supernova remnants in the Small Magellanic Cloud

Filipović

Haberl

Winkler³

et al. 2008

A&A

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Context. A complete overview of the supernova remnant (SNR) population is required to investigate their evolution and interaction with the surrounding interstellar medium in the Small Magellanic Cloud (SMC). Aims. Recent XMM-Newton observations of the SMC cover three known SNRs (DEM S5, SNR B0050−72.8, and SNR B0058−71.8), which are poorly studied and are X-ray faint. We used new multi-frequency radio-continuum surveys and new optical observations at H α , [S ii], and [O iii] wavelengths, in combination with the X-ray data, to investigate their properties and to search for new SNRs in the SMC. Methods. We used X-ray source selection criteria and found one SMC object with typical SNR characteristics (HFPK 334), that was initially detected by ROSAT. We analysed the X-ray spectra and present multi-wavelength morphological studies of the three SNRs and the new candidate. Results. Using a non-equilibrium ionisation collisional plasma model, we find temperatures kT around 0.18 keV for the three known remnants and 0.69 keV for the candidate. The low temperature, low surface brightness, and large extent of the three remnants indicates relatively large ages. The emission from the new candidate (HFPK 334) is more centrally peaked and the higher temperature suggests a younger remnant. Our new radio images indicate that a pulsar wind nebulae (PWN) is possibly associated with this object. Conclusions. The SNRs known in the SMC show a variety of morphological structures that are relatively uncorrelated in the different wavelength bands, probably caused by the different conditions in the surrounding medium with which the remnant interacts.

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An X‐Ray Investigation of the NGC 346 Field in the Small Magellanic Cloud. III.XMM‐NewtonData

Cited by 16 publications

References 22 publications

TheXMM-Newtonsurvey of the Small Magellanic Cloud: The X-ray point-source catalogue

TheXMM-Newtonsurvey of the Small Magellanic Cloud: The X-ray point-source catalogue

NGC 346 in The Small Magellanic Cloud. IV. Triggered Star Formation in the HiiRegion N66

New XMM-Newton observations of supernova remnants in the Small Magellanic Cloud

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