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| Miscellaneous :
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| Masetti et al.
2006: Is HD 146803 the counterpart? then source is
HMXB |
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Masetti et al.
2006 Atel 783:
- Halpha emission at redshift 0 superimposed on a reddened continuum
- HD 146803 not counterpart
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Tomsick et al.
2006:
- Chandra position rejects association with HD 146803.
- Gamma~0.5 and nH~3.7x1022 at/cm2 (slightly higher than galactic absorption alone), with a high-energy cutoff.
- Variability evident in the Chandra lightcurve.
- Optical counterpart has J-band magnitude of 10.44(2), and a stellar temperature > 18,000 K which indicates that the system is a HMXB.
- Distance estimated to be between 3 and 10 kpc which, if assuming d=5 kpc, gives a 0.3-10 keV luminosity of ~1.3x1035 ergs/s.
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Negueruela and Schurch 2006:
- New supergiant XRB (wind accretor)`
- Possible B0 spectral type of the companion, but earlier than B1 in any case.
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Masetti et al. 2006:
- Halpha, EW=5.0 Angstrom
- R~15.6
- d~4.6 kpc
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Rahoui et al. 2008: - Medium infrared observations
- SED fitting => AV=10.5, Tstar=33800 K
- O/B massive star, 07.5 favoured, distance between 1.8 and 4.1 kpc if source
is main sequence, sub giant or supergiant
- No need for additional component in SED fitting
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Nespoli et al. 2008: - Infrared spectroscopy
- Rather a B1 Ia companion
- d~6.1 (-3.5+8.9) kpc
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Tomsick et al. 2009: - XMM-Newton observations
- Spectrum typical of HMXB with neutron star
- Absorbed HMXB, confirmed by re analysis of Chandra data
- Short term var. not only due to variations of Nh
- No pulsations between 0.005 and 88 Hz with upper limit of 2.3 % (@ 90%) nor
between 0.000023 and 0.05 Hz with upper limit of 1.7% (@90%)
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Bodaghee et al. 2010:
- Suzaku observation
- Cutoff energy constrained for the first time at ~19 keV.
- Cutoff E argues in favour of a neutron star primary
- Spectrum strongly absorbed NH=16.2x1022 cm-2
- ~30 ks epoch with source flux is extremely low (no change in nH or Γ)
- Several mechanisms explored to explain diminished flux
- Possible scenario of partial or full eclipse
- If eclipse is real=> orbital period (4d <= P <= 9 d) and inclination angle (i >= 50 degs).
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Jain et al. 2011 ATel 3785:
- Detection of sporadic intensity modulation in the BAT 15-50 keV light curve
- Period of of 9.726 d possible orbital period of the X-ray binary
- Possible eclipse seen with Suzaku does not coincide with the phase at which the Swift-BAT light
shows lowest intensity
- If orbital period the suzaku event would likely be an absorption event
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