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| Miscellaneous :
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- NH=~1 x 1024 cm-2
- Prominent X-ray lines around 6.4 keV
- XMM quick look results here
- Distance between 0.9 and 6.2 kpc
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Kaplan et al. (2006):
- long wavelength excess
- SED is higher in Mid IR than expected from pure stellar emission
- warm circumstellar dust at 1000 K possibly responsible for X-ray absorption
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Ibarra et al. (2007 A&A,
465, 501):
- source always remains bright => very probable persistent source
- variations of the absorbing column density (1.38e24 to 2.16e24 cm-2), but
always remains compton thick
- Variations of the Fe Kalpha emission line follow variations of
the source flux (even on short time scales) => lines produced by the
illumination of small-scale optically thick matter surounding the high energy source.
- Evidence for a Compton shoulder in the spectra.
- Obscuring matter is in a flattened configuration around the source, IGR J16318-4848 almost
edge-on
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Moon et al. (2007 ApJL):
- Spitzer observations
- Two continuum component a hot (1040 K) and a warm (190 K)
one =>two circumstellar dust components, one warm and one hot.
- Many emission lines: majority are HI lines
- Also metallic forbidden lines (Ne II, Ne III, S III, Si II,
Ni II, Fe II), pure rotational H2 lines, and PAH emission .
- Deduce the presence of ionized stellar wind, an
extended low density ionized region, and a photo dissociation region.
- X-ray source is not the primarily responsible for the emission
of forbidden lines although it can have some contribution.
- Both dust components contibute very little to the total Optical
extinction.
- Highly obscured X-ray binaries could represent an
unknown evolutionary phase of XRBs with early type Optical companions.
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Rahoui et al. 2008:
- Medium infrared observations
- SED fitting => AV=17, T*=22200 K
- Need for additional component to fit SED. T=1100 K, confirm results of
Kaplan et al. 2006
- Suggested distance 1.6 kpc
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Pacciani et al. 2008
ATel 1713:
- Hard X-ray bright state caught with super Agile
- 20-60 keV flux (of 300 mCrab)
10 times higher than its average flux reported in the 3rd IBIS catalogue.
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Barragán et al. 2010 (A&A):
- Hard X-ray bright state caught with super Agile
- 20-60 keV flux (of 300 mCrab)
10 times higher than its average flux reported in the 3rd IBIS catalogue.
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Krimm et al. 2010 Atel 3051
:
- Observation of renewed hard X-ray activity with Swift/BAT
- 3rd large outburst seen with Swift since 2004
- Earlier outbursts each lasted ~20 days
- Time between outburst = multiple of the 80.2-day orbital period proposed
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Chaty & Rahoui 2012 (ApJ):
- New VLT/VISIR Mid IR observations
- Broad band SED (with NTT and Spitzer) => star surrounded by irradiated rim at T~
3800-5500 K
- Presence of viscous disc component Tin~ 750 K
- Spherical geometry excluded for dust component.
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Coleiro et al. (2013) :
- NTT/Sofi NIR Spectroscopy
- Many intense and broad emission lines
- Two He I lines with P-Cygni profile => Strong stellar wind. Velocity ~400 km.s-1
- Possible presence of an H2 line => either shock heating high enough, or sufficiently low temperature region
- Confirm sgB[e] HMXB
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