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| Miscellaneous :
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Masetti et al. 2010 (A&A):
- Optical spectroscopy of the counterpart
- R=16, Av ~ 0
- Balmer emission lines up to Hδ at z=0
- Strength of He II emission line => CV of probable IP type
- d ~ 250 pc
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Bernardini et al. 2013(MNRAS):
- XMM-Newton & Swift broad band spectral and timing analysis+Optical and IR
analysis
- Variable X-ray source: 1.69 h and 1.38h periodic variabilities, plus large
amplitude variability on timescale 11h
- X-ray spectrum well fitted by multi-temperature plasma, with kT=36 keV
- Interstellar and local absorption + partial absorber with covering factor 53%
- MWD=0.8 Msun with very low accretion rate below the
orbital period gap
- Magnetic CV, pre-polar or IP
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Thornstensen & Halpern 2013 (ApJ):
- Optical observations => spectra generally similar to those of Masetti
- Possible short but ambiguous orb. period at ~84 min
- No pulse period detected
- Source could be a polar
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