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(abridged) We analysed eight XMM-Newton observations toward the SmallMagellanic Cloud (SMC), performed between October 2006 and June 2007, toinvestigate high mass X-ray binary systems. We found new X-ray binary pulsarswith periods of 202 s (XMMU J005929.0-723703), 342 s (XMMU J005403.8-722632),645 s (XMMU J005535.2-722906) and 325 s (XMMU J005252.1-721715), in the lattercase confirming the independent discovery in Chandra data. In addition wedetected sixteen known Be/X-ray binary pulsars and six ROSAT-classifiedcandidate high mass X-ray binaries. From one of the candidates, RXJ0058.2-7231, we discovered X-ray pulsations with a period of 291 s which makesit the likely counterpart of XTE J0051-727. From the known pulsars, we revisethe pulse period of CXOU J010206.6-714115 to 967 s, and we detected the 18.37 spulsar XTE J0055-727 (= XMM J004911.4-724939) in outburst, which allowed us tolocalise the source. The pulse profiles of the X-ray pulsars show a largevariety of shapes from smooth to highly structured patterns and differingenergy dependence. For all the candidate high mass X-ray binaries opticalcounterparts can be identified with magnitudes and colours consistent with Bestars. Twenty of the Be/X-ray binaries were detected with X-ray luminosities inthe range 1.5x10^35 erg/s - 5.5x10^36 erg/s. The majority of the spectra iswell represented by an absorbed power-law with an average power-law index of0.93. The absorption (in addition to the Galactic foreground value) varies overa wide range between a few 10^20 H cm^-2 and several 10^22 H cm^-2. An overallcorrelation of the absorption with the total SMC HI column density suggeststhat the absorption seen in the X-ray spectra is often largely caused byinterstellar gas.

XMM-Newton observations of the Small Magellanic Cloud: Be/X-ray binary pulsars active between October 2006 and June 2007