IGR J00234+6141

Other name = 1RXS J002258.3+614111(?)

Type Mass/distance Radio Counterpart Infrared/Optical Counterpart
R.A. (J2000) Dec. (J2000) References R.A. (J2000) Dec. (J2000) References
CV Int. Polar 0.91 Msun/ 500 pc
00h 22m 57.6s +61o 41' 08" Bikmaev et al. (2006)
Published Papers
Miscellaneous :

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
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.
Masetti et al. (2006) :
  • Confirm source is a CV, probably Intermediate Polar
  • Source caught in quiescence, likely distance 300 pc
Barlow et al. (2006) :`
  • Power law index 3.1, or bremsstrahlung kT=15.9 keV
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.
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
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.
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
Butters et al. (2011) :
  • Modulation detected at 563.5s.
  • Amplitude increasing with energy
  • Hard spectrum + iron line

Last updated 6 Dec. 2010

Jerome Rodriguez