|
|
| Miscellaneous :
|
Stephen et al. 2006 :
- B=13.6-14.0, J=8.3, H=7.3, K=7
|
|
Masetti et al. 2007:
- Multiwavelength studies of this object => Swift/XRT observations allowing refinement
of the X-ray position
- Identify USNO A2.0 U0600-20227091 as the optical counterpart to
the X-ray source.
- Optical spectrum shows several lines => they identify it as a M2 III star
- They can set an upper limit on the distance to the source of 3.7 kpc.
- IGR J16194-2810 a new symbiotic X-ray binary.
- Typical X-ray spectral parameters are an absorption column density of
NH= 1.6 10 21 cm-2, + comptt model
with kT0=0.63 keV, kTe=7.6 keV, Τ=6.8 => more typical of
a neutron star primary.
|
|
Ratti et al. 2010 (MNRAS):
- Chandra + optical observations
- Confirm the optical counterpart previously suggested
- Also present in 2MASS with J=8.268, H=7.333, K=6.984
- apparent magnitude r'=10.98
- Confirm the source is a Symbiotic XRB
- d=3.0 kpc
|
|
Kitamura et al. 2013 (PASJ):
- Analysis of Suzaku observations in the low hard state
- Two emission components in the source spectra
- Below 2 keV: either a raw black body 0.4 keV and R~1.7 km or
Comptonized emission with kT 0.1 keV and R~ 75 km
- Above 2 keV: Comptonized black body emissoin with kTseded~ 1.0 keV and R~700m
- Power spectrum has a continuum in f-1.04 with no significant periodic features
- Smaller radius and higher temp of hard component (compared to other LMXB) might be due to stronger magnetic field
|
|
|