Detection of a cyclotron line in SXP 15.3 during its 2017 outburst

Maitra, Chandreyee; Paul, Biswajit; Haberl, F.; Vasilopoulos, Georgios

doi:10.1093/mnrasl/sly141

Cited by 25 publications

(21 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…s −1 ). A cyclotron feature was detected at 5 keV from AstroSAT and NuSTAR observations during this outburst with an estimated surface magnetic field of 6 × 10 11 G for the neutron star (Maitra et al 2018). A series of three outbursts followed, with a recurring timescale of ∼ 150 days at peak flux levels of ∼ 4×10 −11 erg.…”

Section: X-ray Variabilitymentioning

confidence: 87%

Disentangling the neighbouring pulsars SXP 15.3 and SXP 305

Monageng,

Coe,

Townsend

et al. 2022

Preprint

View full text Add to dashboard Cite

SXP 15.3 and SXP 305 are two Be X-ray binaries in the Small Magellanic Cloud that are spatially separated by ∼7 arcsec. The small separation between these sources has, in the past, resulted in confusion about the origin of the emission from the combined region. We present long-term optical and X-ray monitoring results of both sources, where we study the historic and recent behaviour. In particular, from data collected as part of the S-CUBED project we see repeating X-ray outbursts from the combined region of the two sources in the recent lightcurve from the Neil Gehrels Swift Observatory, and we investigate the origin of this emission. Using the H𝛼 emission line from the Southern African Large Telescope (SALT) and photometric flux from the Optical Gravitational Lensing Experiment (OGLE) to study the changes in the size and structure of the Be disc, we demonstrate that the X-ray emission likely originates from SXP 15.3. Timing analysis reveals unusual behaviour, where the optical outburst profile shows modulation at approximately twice the frequency of the X-ray outbursts. We consider either of these periodicities being the true orbital period in SXP 15.3 and propose models based on the geometric orientations of the Be disc and neutron star to explain the physical origin of the outbursts.

show abstract

Section: X-ray Variabilitymentioning

confidence: 87%

Disentangling the neighbouring pulsars SXP 15.3 and SXP 305

Monageng,

Coe,

Townsend

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Events were re-binned for plotting purposes only. cretion column (e.g., Tsygankov et al 2017;Maitra et al 2018). In many cases BeXRB spectra show residuals at soft energies.…”

Section: Spectral Propertiesmentioning

confidence: 99%

The 2019 super-Eddington outburst of RX J0209.6−7427: detection of pulsations and constraints on the magnetic field strength

Vasilopoulos

Ray

Gendreau

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

In November 2019, MAXI detected an X-ray outburst from the known Be X-ray binary system RX J0209.6−7427 located in the outer wing of the Small Magellanic Cloud. We followed the outburst of the system with NICER which led to the discovery of X-ray pulsations with a period of 9.3 s. We analyzed simultaneous X-ray data obtained with NuSTAR and NICER allowing us to characterize the spectrum and provide an accurate estimate of its bolometric luminosity. During the outburst the maximum broadband X-ray luminosity of the system reached 1-2×10 39 erg s −1 , thus exceeding by about one order of magnitude the Eddington limit for a typical 1.4 M ⊙ mass neutron star (NS). Monitoring observations with Fermi/GBM and NICER allowed us to study the spin evolution of the NS and compare it with standard accretion torque models. We found that the NS magnetic field should be of the order of 3×10 12 G. We conclude that RX J0209.6−7427 exhibited one of the brightest outbursts observed from a Be X-ray binary pulsar in the Magellanic Clouds, reaching similar luminosity level to the 2016 outburst of SMC X-3. Despite the super-Eddington luminosity of RX J0209.6−7427, the NS appears to have only a moderate magnetic field strength.

show abstract

“…In November 2017 Ducci et al (2017) observed the source in outburst. Maitra et al (2018) observed the source in late 2017 with both NuSTAR and Swift-XRT simultaneously and measured a 3-80 keV luminosity of ∼ 10 38 erg s −1 . We obtained three NuSTAR observations of this source in March, July, and August 2017, respectively (see Table 3).…”

Section: Source 1705 -Detection Of Two Be-xrbsmentioning

confidence: 99%

Neutron Stars and Black Holes in the Small Magellanic Cloud: The SMC NuSTAR Legacy Survey

Lazzarini

Williams

Hornschemeier

et al. 2019

ApJ

View full text Add to dashboard Cite

We present a source catalog from the first deep hard X-ray (E > 10 keV) survey of the Small Magellanic Cloud (SMC), the NuSTAR Legacy Survey of the SMC. We observed three fields, for a total exposure time of 1 Ms, along the bar of this nearby star-forming galaxy. Fields were chosen for their young stellar and accreting binary populations. We detected 10 sources above a 3σ significance level (4-25 keV) and obtained upper limits on an additional 40 sources. We reached a 3σ limiting luminosity in the 4-25 keV band of ∼ 10 35 erg s −1 , allowing us to probe fainter X-ray binary (XRB) populations than has been possible with other extragalactic NuSTAR surveys. We used hard X-ray colors and luminosities to constrain the compact-object type, exploiting the spectral differences between accreting black holes and neutron stars at E > 10 keV. Several of our sources demonstrate variability consistent with previously observed behavior. We confirmed pulsations for seven pulsars in our 3σ sample. We present the first detection of pulsations from a Be-XRB, SXP305 (CXO J005215.4−73191), with an X-ray pulse period of 305.69 ± 0.16 seconds and a likely orbital period of ∼1160-1180 days. Bright sources ( 5 × 10 36 erg s −1 ) in our sample have compact-object classifications consistent with their previously reported types in the literature. Lower luminosity sources ( 5 × 10 36 erg s −1 ) have X-ray colors and luminosities consistent with multiple classifications. We raise questions about possible spectral differences at low luminosity between SMC pulsars and the Galactic pulsars used to create the diagnostic diagrams.

show abstract

Detection of a cyclotron line in SXP 15.3 during its 2017 outburst

Cited by 25 publications

References 26 publications

Disentangling the neighbouring pulsars SXP 15.3 and SXP 305

Disentangling the neighbouring pulsars SXP 15.3 and SXP 305

The 2019 super-Eddington outburst of RX J0209.6−7427: detection of pulsations and constraints on the magnetic field strength

Neutron Stars and Black Holes in the Small Magellanic Cloud: The SMC NuSTAR Legacy Survey

Contact Info

Product

Resources

About