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| Miscellaneous :
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| 2 MASS J image+XMM error available here (Courtesy J. Zurita) |
| Zurita & Walter 2004
: J=10.54 |
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Smith
2004, ATEL 338 : - Optical magnitudes (USNO B1.0): B2=15.2, R2=13.0
- (possible) Distance 12.5 kpc
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Neguerela et al. 2005
Atel 429 : - reddened early-type B0.5I supergiant,
- H-alpha line shows a
broad emission component on top of the photospheric profile
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Lutovinov et al. 2005:
- pulsations at 228 +- 6s
- NH=72x 1022 cm-2, Gamma~1.0, Ec~30 keV
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Walter et al. 2006:
- pulse period of 227+-5 s in XMM (not seen in ISGRI)
- large soft excess (not described by partial-covering absorber) and marginal K-alpha line (EW < 60 eV)
- NH = 60(+-10)x1022 at/cm2
- IR counterpart (2.6 arcsec away) has a K-band magnitude of 9.8
- unabsorbed flux (2-100 keV) is 2.8x10-10 ergs/cm2/s
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Rahoui et al. 2008: - Medium infrared observations
- SED fitting => AV=5.9, T*=25000 K
- Obscuring material contributes little to MIR spectrum
- Suggested distance 9.4 kpc
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Nespoli et al. 2008: - Infrared spectroscopy
- Suggest companion is O9.5 Ia
- The X-ray nature => SFXT nature
- Distance 9.5 (-5.7 +14.1) kpc
- Local absorption comes from material concentrated around the compact object
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Morris et al. 2009: - Suzaku observations
- confirm the source is an heavily absorbed HMXB
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La Parola et al. 2010 (MNRAS):
- Significant periodicity in Swift/BAT at P=30.243 d
- Observation of a wide phase of 0 intensity at T(MJD)=54180.5+- nPorb
- Semi-major orbital axis a~125 Rsun (150 Rsun)~6 Rstar (5 Rstar)
for a typical 09.5 I (B0.5 Ib) star
- Do not favour an eclipse as the origin of the minimum phase
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Clark et al. 2010 (MNRAS):
- Periodicity in Swift/BAT and INTEGRAL/IBIS at P=30.32 d
- Semi-major orbital axis a~121.9--126.3 Rsun according to the
mass of the donor
- e either <0.6 or <0.8 depending on the exact mass of the donor.
- Source is an intermediate SFXT
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Wang & Chang 2012 (A&A):
- Study retrograde wind accretion scenario
- => spin and orbital period => R corrotation ~ 3.7e9 cm and source is a pure propeller
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Romano et al. 2014(A&A):
- Study of long term Swift/XRT monitoring
- Low ~5% inactivity duty cycle, and a dynamic range
of ~40 during bursts
- Low inactivity duty cycle and dynamic range compared to (other) SFXTs is rather reminiscent
of classical sg-HMXBs
- No correlation between duty cycle and orbital period
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