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| Miscellaneous :
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Bozzo et al. 2009 ATel
2079:
- INTEGRAL discovery => source is compatible with being in the SMC
- IBIS/ISGRI spectrum => power law Γ=2.5
- Rosat source in error box not counterpart unless IGR strongly variable
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Coe et al. 2009 ATel 2088:
- Swift observations
- [M2002] SMC 59977 a V=14.8 star could be the counterpart
- Star variable in I typical of Be in SMC
- Periodicity at 17.49 s
- HMXB in SMC
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Corbet et al. 2009 ATel 2092:
- RXTE observations => pulse at 11.483s and harmonics
- Pulse profile complex with multiple peaks
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Townsend et al. 2009 ATel 2202:
- Doppler modulation of the 11.48s pulse period and
a spin-up of this modulation.
- Orbital period = 36.3 days
- Average spin-up rate = 4.7 E-10 s/s.
- Orbit is eccentric with e~0.28
- Results => source lying in the Be region of the
Corbet diagram
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Masetti et al. 2010(A&A):
- Optical spectroscopy of the counterpart
- R=14.81, Av ~ 0.7
- Balmer emission lines at z=0, intrinsically blue spectrum => XRB
- d=60 kpc (SMC)
- Early type star spectral appearance => HMXB
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Townsend et al. 2010(MNRAS):
- X-ray/Optical/IR analysis
- Optical/IR observations =>orbital period =36.70 days
- Spectral class constrained to O9.5-B0 luminosity class of IV-V rather than III as previously proposed
- Distance to the source ~71 kpc
- RXTE => Orb. period consistent with that of IR/Optical, semi-major axis of 167 lt-s, and eccentricity of 0.28(3)
- Spin period=11.48143 s , spin-up rate of -4.67e-10 s/s, satisfying theoretical relation between luminosity, spin period, and spin-period derivative
- Absorbed cutoff power law fits combined RXTE/XMM spectra with NH=2.3x1021 cm-2, Γ=1.06,
Ecut=9 keV, and Efold=22 keV.
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