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| Miscellaneous :
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| Stephen et al. 2005: :
B~15
Possible extended or unresolved IR source within 2.2" of the optical
counterpart |
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Masetti et al.
2006Atel 783:
- Balmer and He emissions at z = 0
- possible CV
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Tomsick et al. 2006 :
- Chandra position is 0.7" away from USNO-B1.0 0489-0511283, and therefore (along with
supplemental IR/optical analysis) the USNO source must be considered as the optical counterpart.
- Column density is ~8x1020 (low) at/cm2 and Gamma~1.1.
- Some variability present in Chandra lightcurve.
- Spectral type of optical companion is no later than A3 which along with distance estimations and extinction measurements is incompatible with a
supergiant or OB main sequence star, so the system can not be a HMXB.
- Maximum distance is 2.6 kpc, so 0.3-10 keV luminosity is <2.0x1034 ergs/s.
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Barlow et al. (2006) :
- 20-100 keV Power law photon index 2.9, or bremsstrahlung kT=27.0 keV
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Masetti et al. (2006) :
- Halpha, Hbeta, He II emission lines
- R=14.3
- d~110 pc
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Butters et al. (2008) :
- RXTE analysis
- 2 equally possible periods in the periodogram at 1842.4s and 2645.0s
- Typical of spin periods for Intermediate Polar
- If longer=spin, and other=beat period => orbital period=1.7 hr.
- Source is a likely IP although no definitive classification
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Pretorius 2009:
- Optical observations: Phase resolved spectroscopy => Orb. period 4.005h
- Spin period of 18.9925 min
- Source is a confirmed IP
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Revnivtsev et al. (2010) :
- Study of optical aperiodic variability
- νbreak~2 x Spin period
- If break freq <=> inner disc radius then inner radius close to corotation with WD
magnetosphere
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Bernardini et al. 2012 (A&A):
- Multi-wavelengths observations
- Pulse period = 1062s
- Broad band spectral analysis
- Disc overflow accretion mode
- MWD~0.86 Msun at d~130 pc
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Girish & Singh 2012 (MNRAS):
- XMM-Newton and Suzaku observations
- New period 1053.7 s and new binary orbital period of 3.52 h
- Soft X-rays (<3keV) dominate variability
- Spectral fitting with plasma emission, cooling flow models (apec, mkcflow), plus Gaussian, partial covering
- Presence of a soft excess attributed to varying coverage of accretion curtains
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