EDP Sciences
Free access
Volume 483, Number 1, May III 2008
Page(s) 249 - 251
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:200809397
Published online 11 March 2008

A&A 483, 249-251 (2008)
DOI: 10.1051/0004-6361:200809397

Research Note

Swift observations of the X-ray pulsar SAX J1324-6200

S. Mereghetti1, P. Romano2, and L. Sidoli1

1  INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, via E. Bassini 15, 20133 Milano, Italy
    e-mail: sandro@iasf-milano.inaf.it
2  INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica Palermo, via U. La Malfa 153, 90146 Palermo, Italy

(Received 15 January 2008 / Accepted 21 February 2008)

We present recent observations of the X-ray pulsar SAX J1324-6200  obtained in December 2007 with the Swift satellite, significantly improving the source localization over previous data and providing a new measurement of the spin period P=172.84 s. A single object that is consistent in colors with a highly reddened early type star is visible in the X-ray error box. The period is significantly longer than what was obtained in 1997, indicating that SAX J1324-6200  has been spinning down at an average rate of ${\sim}$ $6 \times 10^{-9}$ s s-1. We discuss the possible nature of the source, showing that it most likely belongs to the class of low-luminosity, persistent Be/neutron star binaries.

Key words: X-rays: binaries

© ESO 2008