BeppoSAX observations of the young pulsar in the Kes 75 Supernova Remnant

Details BeppoSAX observations of the young pulsar in the Kes 75 Supernova Remnant BeppoSAX observations of the young pulsar in the Kes 75 Supernova Remnant

2002-04-03

arxiv.org/abs/astro-ph/0204050v1

Astronomy and Astrophysics

Astrophysics

17 pages, latex, 5 figures, Accepted for publication on The Astrophysical Journal Part 1

Scientific paper

10.1086/340976

We present the results of BeppoSAX observations of the young X-ray pulsar PSR J1846-0258, recently discovered at the center of the composite supernova remnant Kes 75. The pulsar (plus nebula) spectrum can be fitted by an absorbed power law with photon index alpha_ph=2.16+/-0.15, N_H=(4.7+/-0.8) x 10^22 cm^-2, and unabsorbed flux ~3.9x10^-11 erg cm^-2 s^-1 (2-10 keV). By joining two observations taken at an interval of two weeks we have been able to obtain a precise measurement of the spin period (P=324.818968+/-0.000006 ms). This value, when combined with previous measurements, cannot be fitted by a smooth frequency evolution with a canonical braking index n=3. With the hypothesis of no glitches and/or significant timing noise, the braking index would be n=1.86+/-0.08 and, assuming a short initial period, the pulsar age would be \~1700 years, closer to that of the supernova remnant than the simple estimate \tau=P/2\pdot=723 years. Other likely possibilities involve the presence of glitches and lead to a wide range of acceptable ages. For example, we obtain n in the range 1.8-2.5, if a glitch occurred near MJD 51500, while for a glitch between October 1993 and March 1999 we can only get a lower limit of n>1.89.

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