The high mass X-ray binary population of the Small Magellanic Cloud
The high mass X-ray binary population of the Small Magellanic Cloud |
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| The numerous high mass X-ray binaries (HMXBs) are marked on the EPIC mosaic image (see below) of the SMC region. The known pulsars are labeled with their pulse periods in seconds. Green and blue circles indicate the positions of other (candidate) HMXBs. The size of the circles indicates the positional uncertainty (or the size of the field-of-view for pulsars only detected through their pulsations by RXTE). |
| A catalogue paper with 148 HMXBs and candidates was submitted to A&A on Sept. 8, 2015. ADS private libraries collected by Frank Haberl with notes are available for each of the (candidate) HMXBs. A short HTML summary of the SMC HMXB catalogue is also provided. |
An X-ray survey of the Small Magellanic Cloud with XMM-Newton |
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| Full XMM-Newton, EPIC PN+MOS mosaic image of the SMC region including all observations available as of December 2013. The red, green and blue images are produced from ata in the energy bands 0.2-1.0 keV, 1.0-2.0 keV and 2.0-4.5 keV. The images are detector-background subtracted, exposure and vignetting corrected (and out-of-time event subtracted for PN). |
| ADS list of SMC publications based on XMM-Newton data. |
XMM-Newton AO8 - the proposalA complete survey of the Small Magellanic Cloud |
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PI: Frank Haberl, MPE Garching CoIs: Jean Ballet Dominik Bomans David A.H. Buckley Malcolm J. Coe Robin Corbet Matthias Ehle Miroslav D. Filipovic Marat Gilfanov Frank Haberl Despina Hatzidimitriou Sandro Mereghetti Wolfgang Pietsch Steve Snowden Andrea Tiengo |
Abstract:We propose EPIC observations to obtain a complete survey of the SMC down to a limiting point source luminosity of 2 x 10^33 erg/s. Its proximity makes the SMC the ultimate target for obtaining a complete inventory of SSSs, HMXBs and SNRs and to study the diffuse emission of the hot ISM. Most importantly, the high throughput of XMM-Newton will allow us to perform detailed spectral and temporal analyses of a large fraction of the sources. We will identify and/or classify fainter sources using hardness ratios, long-term variability, and source extent, together with information from other wavelength bands. Including the existing XMM-Newton data our observations will create a unique data set to study the star-formation history and its implications on the morphology of the ISM in the SMC. |
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XMM-Newton, EPIC PN+MOS mosaic image of the SMC region. The RGB colour image is composed of archival data (as of September 2008) from the three energy bands 0.2-1.0 keV, 1.0-2.0 keV and 2.0-4.5 keV (exposure corrected and out-of-time event subtracted for PN). The brightest source in the NE is the SNR 1E0102.2-7219 which is regularly observed as XMM-Newton routine calibration target. The observations accumulate to a maximum exposure of 264 ks (PN) and 338 ks (MOS) west of the SNR where observations of neighboring fields overlap. The other areas have average exposures of 16.6 ks and 19.1 ks for PN and MOS, respectively. |
Internal project pages.
Last update: Frank Haberl, 2015-08-26