Abstract:
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, ∼ 1.0. A blackbody model can equally well fit the
spectra with a temperature, kT ∼ 2 keV, for both sources. During our XMM–Newton observa-
tions, 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 confi-
dence 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 P = (6.34±0.08)×10−9 s s−1
̇
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.
