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

Carpano, S.; Haberl, F.; Maitra, Chandreyee; Freyberg, M. J.; Dennerl, K.; Schwope, A. D.; Buckley, Alex; Monageng, I. M.

doi:10.1051/0004-6361/202141082

Cited by 5 publications

(6 citation statements)

References 31 publications

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“…Figure 9 shows the location of SXP 182 when placed on the Corbet diagram with all BeXRBs in the SMC that have known spin and orbital periods (Haberl & Pietsch 2005;Coe & Kirk 2015;Haberl & Sturm 2016;Carpano et al 2017Carpano et al , 2022McBride et al 2017;Kennea et al 2018Kennea et al , 2020Lazzarini et al 2019;Maitra et al 2023). The location of SXP 182 is consistent with the trend shown by other SMC BeXRBs.…”

Section: Corbet Diagramsupporting

confidence: 58%

“…A radius of this size rules out the NS, a large planet, or a Sun-like tertiary star as the cause of the eclipsing behavior. Therefore, it can be concluded that the McBride et al 2017;Kennea et al 2018Kennea et al , 2020Lazzarini et al 2019;Carpano et al 2022;Maitra et al 2023). SXP 182 is plotted alongside these data and is shown to demonstrate the same correlation between X-ray pulsar spin period and NS orbital period that is seen in the rest of the SMC BeXRB population.…”

Section: Eclipsing Behaviormentioning

confidence: 69%

“…Figure 9. Corbet diagram for all BeXRBs in the SMC with known orbital periods and spin periods (Haberl & Pietsch 2005; Coe & Kirk 2015; CarpanoMcBride et al 2017;Kennea et al 2018Kennea et al , 2020Lazzarini et al 2019;Carpano et al 2022;Maitra et al 2023). SXP 182 is plotted alongside these data and is shown to demonstrate the same correlation between X-ray pulsar spin period and NS orbital period that is seen in the rest of the SMC BeXRB population.…”

mentioning

confidence: 99%

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Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182

Gaudin,

Kennea,

Coe

et al. 2024

ApJL

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We report on the discovery of Swift J010902.6-723710, a rare eclipsing Be/X-ray Binary system by the Swift SMC Survey (S-CUBED). Swift J010902.6-723710 was discovered via weekly S-CUBED monitoring observations when it was observed to enter a state of X-ray outburst on 2023 October 10. X-ray emission was found to be modulated by a 182 s period. Optical spectroscopy is used to confirm the presence of a highly inclined circumstellar disk surrounding a B0-0.5Ve optical companion. Historical UV and IR photometry is then used to identify strong eclipse-like features reoccurring in both light curves with a 60.623 day period, which is adopted as the orbital period of the system. Eclipsing behavior is found to be the result of a large accretion disk surrounding the neutron star. Eclipses are produced when the disk passes in front of the OBe companion, blocking light from both the stellar surface and circumstellar disk. This is only the third Be/X-ray binary to have confirmed eclipses. We note that this rare behavior provides an important opportunity to constrain the physical parameters of a Be/X-ray binary with greater accuracy than is possible in noneclipsing systems.

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Section: Corbet Diagramsupporting

confidence: 58%

Section: Eclipsing Behaviormentioning

confidence: 69%

mentioning

confidence: 99%

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Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182

Gaudin,

Kennea,

Coe

et al. 2024

ApJL

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“…In the SMC, the eROSITA observations covered 16 BeXRB pulsars, including XMMU J010429.4−723136, from which 164 s pulsations were discovered in eROSITA data (Carpano et al 2022;Haberl et al 2019). We present detailed spectral and temporal analyses for SXP 304, SXP 455, SXP 522, SXP 726, and SXP 1323.…”

Section: Discussionmentioning

confidence: 99%

“…All these are known to be BeXRB pulsars: RX J0101.0−7206, also known as SXP 304; RX J0101.3−721, also known as SXP 455; AX J0103−722, also known as SXP 522; RX J0105.9−720, also known as SXP 726,; and RX J0103.6−7201, also known as SXP 1323. The results from the HMXB XMMU J010429.4−723136, from which 164 s pulsations were discovered in the eROSITA CalPV data (Haberl et al 2019), are presented in Carpano et al (2022). The results from the other sources are described below.…”

Section: Smc Fieldmentioning

confidence: 96%

eROSITA calibration and performance verification phase: High-mass X-ray binaries in the Magellanic Clouds

Haberl

Maitra

Carpano

et al. 2022

A&A

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Context. During its performance verification phase, the soft X-ray instrument eROSITA on board the Spektrum-Roentgen-Gamma (SRG) spacecraft observed large regions in the Magellanic Clouds in which almost 40 known high-mass X-ray binaries (HMXBs, including candidates) are located. Aims. We looked for new HMXBs in the eROSITA data, searched for pulsations in HMXB candidates, and investigated the long-term behaviour of the full sample using archival X-ray and optical data. Methods. For sufficiently bright sources, we performed a detailed spectral and temporal analysis of their eROSITA data. A source detection analysis of the eROSITA images in different energy bands provided count rates and upper limits for the remaining sources. Results. We report the discovery of a new Be/X-ray binary in the Large Magellanic Cloud. The transient SRGEt J052829.5–690345 was detected with a 0.2–8.0 keV luminosity of~1035 erg s−1. It exhibits a hard X-ray spectrum, typical for this class of HMXBs. The OGLE I-band light curve of the V~15.7mag counterpart shows large variations up to 0.75 mag, which occur with a quasi-period of~511 days. The eROSITA observations of the Small Magellanic Cloud covered 16 Be/X-ray binary pulsars, 5 of which were bright enough for an accurate determination of their current pulse period. The pulse periods for SXP 726 and SXP 1323 measured from eROSITA data are~800 s and~1006 s, respectively, which is very different from their discovery periods. Including archival XMM-Newton observations, we update the spin-period history of the two long-period pulsars, which have shown nearly linear trends in their period evolution for more than 15 yr. The corresponding average spin-down rate for SXP 726 is 4.3 s yr−1, while SXP 1323 has a spin-up rate of –23.2 s yr−1. We discuss the spin evolution of the two pulsars in the framework of quasi-spherical accretion.

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Broadband study and the discovery of pulsations from the Be/X-ray binary eRASSU J052914.9−662446 in the Large Magellanic Cloud

Maitra¹,

Kaltenbrunner²,

Haberl³

et al. 2023

A&A

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Context. The Magellanic Clouds are our nearest star-forming galaxies. While the population of high-mass X-ray binaries (HMXBs) in the Small Magellanic Cloud (SMC) is relatively well studied, our knowledge about the Large Magellanic Cloud (LMC) is far from complete given its large angular extent and the insufficient coverage with X-ray observations. Aims. We conducted a search for new HMXBs in the LMC using data from eROSITA, the soft X-ray instrument on board the Spektrum-Roentgen-Gamma (SRG) satellite. Methods. After confirming the nature of eRASSU J052914.9−662446 as a hard X-ray source that is positionally coincident with an early-type star, we followed it up with optical spectroscopic observations from the South African Large Telescope (SALT) and a dedicated NuSTAR observation.Results. We study the broadband timing and spectral behaviour of the newly discovered HMXB eRASSU J052914.9−662446 through eROSITA, Swift, and NuSTAR data in X-rays and the Optical Gravitational Lensing Experiment (OGLE) and SALT RSS data at the optical wavelength. We report the detection of a spin period at 1412 s and suggest that the orbital period of the system is ∼151 days. We thereby establish that eRASSU J052914.9−662446 is an accreting pulsar. Furthermore, through optical spectroscopic observations and the detection of Hα emission, the source is identified as a Be X-ray binary pulsar in the LMC. We also investigated the variability of the source in the optical and X-ray regime over the past decades and provide estimates of the possible magnetic field strength of the neutron star.

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

Cited by 5 publications

References 31 publications

Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182

Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182

eROSITA calibration and performance verification phase: High-mass X-ray binaries in the Magellanic Clouds

Broadband study and the discovery of pulsations from the Be/X-ray binary eRASSU J052914.9−662446 in the Large Magellanic Cloud

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