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| Miscellaneous :
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Halpern & Mirabal (2006 ATel 709):
- Optical counterpart only 6" from Rosat source
- B=18.01, R=16.34, I=15.63, J=15.12, H=15.05, K=14.77
- Emission lines in Balmer series
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Bikmaev et al. (2006) :
- Optical counterpart is a CV star based on its strong emission lines and zero redshift.
- Spin period of the white dwarf is 570 s.
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Masetti et al. (2006) :
- Confirm source is a CV, probably Intermediate Polar
- Source caught in quiescence, likely distance 300 pc
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Barlow et al. (2006) :`
- Power law index 3.1, or bremsstrahlung kT=15.9 keV
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Bonnet-Bideau et al. (2007) :
- Identification of IGR J00234+6141 as an intermediate polar (INTEGRAL and
optical observations)
- ISGRI spectrum <=> thermal bremsstrahlung
with kT=31.3 keV, 20-100 keV flux is 8.3E-12 erg/cm2/s
- Optical observations => spin period of 563.5s for the compact object,
& orbital period of 4.033 hours.
- The mean Optical spectrum typical of magnetic CVs
with strong emission lines of the Balmer series, HeII, HeI and CIII-NIII
- Suggest that the surface magnetic field of the WD is 2.4e5 G making
the source a low accreting IP with a low B.
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Tomsick et al. (2008) :
- Chandra position confirms all proposed associations
- Source is indeed a CV
- Absorbed power law, NH=0.17x1022 cm-2,
Γ= 0.87, Unabs. 0.3-10 keV flux=8.6 e-12 erg/cm2/s
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Anzolin et al. (2009) :
- Updated spin period of 561.64(56)s for the white-dwarf
- Pulsation detected only below 2 keV + significant signal at 2P
- ~1hr pseudo-periodic variation also seen in optical data
- 0.3--100 keV broadband spectrum <=> multi-temperature
plasma-emission model with maximum temperature is ~50 keV.
- Iron line detected at 6.4 keV
- Absorption consistent with interstellar value, dense intrinsic
absorber partially covering the source can not be ruled out
- Mass of the white dwarf ~0.91 solar masses witha distance of 500 pc
- Lower limit for the
magnetic dipole moment ~10^32 G cm^3, suggesting the WD not strongly
magnetized and not spinning at its equilibrium period.
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Revnivtsev et al. (2010) :
- Study of optical aperiodic variability
- νbreak~1 x Spin period
- If break freq <=> inner disc radius then inner radius at corotation with WD
magnetosphere
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Butters et al. (2011) :
- Modulation detected at 563.5s.
- Amplitude increasing with energy
- Hard spectrum + iron line
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