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| Miscellaneous :
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Sidoli et al. 2005 :
- NH=~12 x 1022 cm-2
- Hard X-ray spectrum (photon index~0.6) as ssen by ASCA
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Sguera et al. 2006:
- Behaviour similar to Fast X-ray Transient
- Suggest High mass companion
- peak flux 17-35 mCrab (20-40 keV)
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Tomsick et al. 2006 :
- Chandra position rules out association with HD 146628 (1.2' away).
- Column density is ~7x1022 at/cm2 and Gamma~0.5.
- Spectral type of optical companion (J-band magnitude of 13.57(3)) is compatible with an O, B or A giant so the system is a HMXB.
- Distance estimated at 3-15 kpc, so 0.3-10 keV luminosity is ~1.4x1034 ergs/s (for d=5kpc).
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Tovmassian et al.
2006 ATel 804:
- Spectrum is consistent with that of a late F-type star, and shows absorption lines but none of the emission lines that are
expected from an X-ray binary system.
- Source reddening is too low to be compatible with the large extinction that was recently reported by Tomsick et al. (2006).
- Therefore, this object is a foreground dwarf star and not the giant star that is expected to be the likely counterpart.
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Rahoui et al. 2008: - Not detected in medium infrared observations
- SED fitting based on 2MASS and GLIMPSE data => AV=15.5,
T*=23800 K
- Need for an additional component to sit spectra: T=1160K
- Temperature of star compatible with an O/B sg, best fit => B1 distance
from 3.1 to 9.8 kpc if source is main seq, sub giant or super giant
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Morris et al. 2009: - Suzaku observations
- Observation is separated into several intervals due to flare
- Heavily absorbed HMXB
- Mention the possible presence of a disk around the donor star through
models of accretion=>they can estimate a tentative orbital period
of about 16 days from modelisation.
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Coleiro et al. (2013) :
- NTT/Sofi NIR Spectroscopy
- H-band spectrum shows very few lines => consistent with Sg late O-type star
- Analysis of other lines => ON9.7 Iab
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Cusumano et al. (2016) :
- Analysis of long term Swift monitoring
- BAT ligth curve => modulation at 3.945d interpreted as the orbital period of the system
- Folded light curve shows narrow eclipse lasting 3.5% of the orbit. => semi-major orbital axis 31 RSun, inclination 55-60°
- XRT+BAT spectrum => absorbed (NH=7e22 cm-2) power law (Γ=0.5) with high energy cut-off (14 keV)
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