| Miscellaneous :
| Tomsick et al. 2008 ATel 1649:
Extremely hard Chandra spectrum Γ=0.68
NH=2.1 x1021 cm-2
USNO-B1.0 and 2MASS counterparts with B = 17.7, R = 16.0 ,
I= 15.1 , J = 14.94 , H = 14.46 , and Ks = 14.10
| Steeghs et al. 2008 ATel 1653:
IPHAS frames => modest variability in the
r', i', and H-alpha band.
r'=17.70, i'=16.74 and significant H-alpha excess with (r' - H-alpha) = 1.1-1.2 mag.
Presence of strong and broad lines from the Balmer
and Paschen series as well as HeI and HeII in emission. from
EW of the H-alpha emission line is ~120 A.
Spectrum typical of a cataclysmic variable
Presence of significant HeII emission at a
strength comparable to the higher Balmer lines is suggestive of a CV
containing a magnetic white dwarf.
| Evans et al. 2008 ATel 1669:
- Swift => pulsation at 938.6s with 25% rms amplitude
- Other possible periods one of which (4.58 hours) associated with orbit.
- 938s pulsation seen in UVOT data
- confirm the source is an CV/IP
| Rodriguez et al. 2009:
Swift Analysis => absorbed power law acceptable (but not perfect) fit
NH <0.6 x1022 cm-2 Γ=1.1
No evidence for a bbody emission in spectrum
Possible significant variation of flux
| Masetti et al. 2009:
- Optical spectroscopy
| Butler et al. 2009:
Cnfirm the CV and magnetic nature of this source=> IP
V=17.4, R=16.7 and I=15.8
Distance of ~250 pc
| Tomsick et al. 2009:
NH=0.3 x1022 cm-2 Γ=0.75
| Thornstensen & Halpern 2013 (ApJ):
- Optical observations => red sloping continuum with strong single peaked emission lines (Hα, Hβ He II)
- Unambiguous 3.4 hr orbital period => 16500s period previously reported unrelated to orbit
- Spin period in R filter = 931.5s consistent with X-ray
- Possible Polar