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ABSTRACT  IGR J16493−4348 was one of the first new sources to be detected by the  INTErnational Gamma‐Ray Astrophysics Laboratory  ( INTEGRAL ) γ‐ray telescope in the 18–100 keV energy band. Based on spatial coincidence, the source was originally associated with the free radio pulsar PSR J1649−4349. Presented here are the results of 2.8 Ms of observations made by the  INTEGRAL  mission and a 5.6‐ks observation with the  Swift /X‐ray Telescope (XRT). Spectral analysis indicates that the source is best modelled by an absorbed power law with a high energy cut‐off at  E  cut ∼ 15 keV and a hydrogen absorbing column of   N  H = 5.4 +1.3  −1 × 10 22  cm −2  . Analysis of the light curves indicates that the source is a weak, persistent γ‐ray emitter showing indications of variability in the 2–9 and 22–100 keV bands. The average source flux is  ∼1.1 × 10 −10  erg cm −2  s −1   in the 1–100 keV energy band. No coherent timing signal is identified at any time‐scale in the  INTEGRAL  or  Swift  data.  The refined source location and positional uncertainty of IGR J16493−4348 places PSR J1649−4349 outside the 90 per cent error circle. We conclude that IGR J16493−4348 is not associated with PSR J1649−4349. Combining the  INTEGRAL  observations with  Swift /XRT data and information gathered by  RXTE  and  Chandra , we suggest that IGR J16493−4348 is an X‐ray binary, and that the source characteristics favour a high‐mass X‐ray binary although a low‐mass X‐ray binary nature cannot be ruled out.

Probing the nature of IGR J16493−4348: spectral and temporal analysis of the 1–100 keV emission