SRG/eROSITA discovery of 164 s pulsations from the SMC Be/X-ray binary XMMU J010429.4-723136

TL;DR

This paper reports the first detection of 164-second pulsations from the SMC Be/X-ray binary XMMU J010429.4-723136 using eROSITA data, along with spectral analysis and a revised orbital period of 22.3 days.

Contribution

First-time detection of pulsations and spectral analysis of XMMU J010429.4-723136, and a revised orbital period based on combined X-ray and optical data.

Findings

Detected 164 s pulsations, confirming the source as SXP 164.

Derived a consistent X-ray flux and luminosity for the source.

Revised the orbital period to 22.3 days, shorter than previous estimates.

Abstract

Context. The Small Magellanic Cloud (SMC) hosts many known high-mass X-ray binaries (HMXBs), and all but one (SMC X-1) have a Be companion star. Through the calibration and verification phase of eROSITA on board the Spektrum-Roentgen-Gamma (SRG) spacecraft, the Be/X-ray binary XMMU J010429.4-723136 was in the field of view during observations of the supernova remnant, 1E0102.2-7219, used as a calibration standard. Aims. We report timing and spectral analyses of XMMU J010429.4-723136 based on three eROSITA observations of the field, two of which were performed on 2019 November 7-9, with the third on 2020 June 18-19. We also reanalyse the OGLE-IV light curve for that source in order to determine the orbital period. Methods. We performed a Lomb-Scargle periodogram analysis to search for pulsations (from the X-ray data) and for the orbital period (from the OGLE data). X-ray spectral parameters and fluxes were retrieved from the best-fit model. Results. We detect, for the first time, the pulsations of XMMU J010429.4-723136 at a period of ~164 s, and therefore designate the source as SXP 164. From the spectral fitting, we derive a source flux of ~1x10e-12 erg s-1 cm-2 for all three observations, corresponding to a luminosity of ~4x10e35 erg s-1 at the distance of the SMC. Furthermore, reanalysing the OGLE light curve, including the latest observations, we find a significant periodic signal that we believe is likely be the orbital period; at 22.3d, this is shorter than the previously reported values. The Swift/XRT light curve, extracted from two long monitorings of the field and folded at the same period, suggests that a modulation is also present in the X-ray data.