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We present results from our  Chandra  and  XMM–Newton  observations of two low‐luminosity X‐ray pulsators  SAX J1324.4−6200  and  SAX J1452.8−5949  which have spin periods of 172 and 437 s, respectively. The  XMM–Newton  spectra for both sources can be fitted well with a simple power‐law model of photon index,  Γ∼ 1.0 . A blackbody model can equally well fit the spectra with a temperature,   kT ∼  2 keV, for both sources. During our  XMM–Newton  observations,  SAX J1324.4−6200  is detected with coherent X‐ray pulsations at a period of 172.86 ± 0.02 s while no pulsations with a pulse fraction greater than 18 per cent (at 95 per cent confidence level) in 0.2–12 keV energy band are detected in  SAX J1452.8−5949 . The spin period of  SAX J1324.4−6200  is found to be increasing on a time‐scale of  which would suggest that the accretor is a neutron star and not a white dwarf. Using subarcsec spatial resolution of the  Chandra  telescope, possible counterparts are seen for both sources in the near‐infrared images obtained with the son of infrared spectrometer and array camera (SOFI) instrument on the New Technology Telescope. The X‐ray and near‐infrared properties of  SAX J1324.4−6200  suggest it to be a persistent high‐mass accreting X‐ray pulsar at a distance  ≤8 kpc . We identify the near‐infrared counterpart of  SAX J1452.8−5949  to be a late‐type main‐sequence star at a distance ≤10 kpc, thus ruling out  SAX J1452.8−5949  to be a high‐mass X‐ray binary. However, with the present X‐ray and near‐infrared observations, we cannot make any further conclusive conclusion about the nature of  SAX J1452.8−5949 .

Chandra and XMM–Newton observations of the low‐luminosity X‐ray pulsators SAX J1324.4−6200 and SAX J1452.8−5949