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| Miscellaneous :
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Kuiper et al. (2006) Atel 684:
- Flux of ~1.4 mCrab in the 20-65 keV band.
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| Masetti et al. (2006):
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Tomsick et al. (2008) :
- Chandra position confirms all proposed associations
- Absorbed power law, NH=3.2x1022 cm-2,
Γ= 1.0, Unabs. 0.3-10 keV flux=2.0 e-12 erg/cm2/s
- Not a high level of local absorption
- Chandra spectrum significantly lower than INTEGRAL=> significant change
in mass accretion rate
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Rodriguez et al. (2009) :
- Swift Results compatible with Chandra
- Further confirmation of source being an HMXB
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Coleiro et al. (2013) :
- NTT/Sofi NIR Spectroscopy
- Several lines in spectra among which He I, Mg II, He II, Na I and Fe II in emission
- Possible [Fe II] lines in H-band spectrum
- NaI => mow excitation region not directly exposed to radiation of star and compact object
- source surrounded by highly stratified environment with region shielded form direct stellar radiation
- Clear mIR excess compatible wih 1016 K dust around the system
- Possible sgB[e]
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