Description
SXP$\,$1323 is a Be/X-ray binary pulsar discovered in 2005 with a pulse period of 1323$\,$s, making the source one of the longest period pulsar known in the Small Magellanic Cloud. Being very close to the bright supernova remnant 1E 0102-72.3, it is often observed for calibration purposes and a large number of observations are therefore available from several X-ray observatories. A period of 26.2$\,$d was observed in the X-ray wavelengths, that was associated with the orbital period, visible as well in the optical OGLE data. Furthermore, a rapid spinning-up of the source was noted in the period from 2006 to 2016, where the pulse period dropped from 1340 to 1100$\,$s, with a |$\dot{P}/P$| of 0.0172$\,$yr$^{-1}$.
We report here the results from the analysis of the recent eROSITA and ART-XC observations of the source performed during the CalPV phase in November 2019. The pulse period, detected with both instruments, is now around 1005$\,$s confirming that the source continues to spin-up at a similar rate. The eROSITA spectral model (an absorbed power-law with a power-law index around 0.5-1) is also consistent with what has been reported in the literature from XMM-Newton data.
