|
|
| Miscellaneous :
|
Frankowski et al. 2011 ATel 3223:
- IBIS/ISGRI spectrum well fitted with a power law with Γ=1.8
|
|
Zhang et al. 2011 ATel 3226:
- Swift pointing => exclude 1st proposed optical counterpart
- Spectral analysis of two pointings which show no significant
evolution of the parameters.
- Absorbed powerlaw fits the data well: NH = 3.7 x1022 cm-2 and Γ=1.45
- 2MASS J17174269-3656039 has J=15.2, H=13.9 and K=12.9 and is present in the NOMAD and
GLIMPSE catalogs
- NVSS J171743-365606 is also found at a position consistent
with that of the X-ray source
|
|
Paizis et al. 2011 ATel 3236:
- Chandra pointing => exclude all previously proposed optical counterparts
- Spectral analysis => NH=5.9 x1022 /cm2 (larger than the expected absorption through the Galaxy) and Γ=1.2
|
|
Torres et al. 2011 ATel 3241:
- no counterpart within the Chandra error box
- 2MASS source at 1" => Not associated (colour)
- Faint source in their images at 1" =>rule it out based on the separation
to the X-ray source.
- Counterpart to the IGR not brighter than 17.5 mag (in Ks band) at the time of their
observations.
|
|
Corbel and Tzioumis ATel 3246:
- Discovery of a radio source within the Chandra error box
- Flux densities ~0.24 mJy at 5500 MHz and ~0.20 mJy at 9000 MHz
- Spectral index poorly constrained (alpha = -0.37+/- 0.79)
- Radio spectrum either compact jet or a discrete ejection event
- Could be a BH in a hard state, or radio = resudual
radio emission from a discrete ejection.
|
|
Rojas ATel 3275:
- No detection any IR source within the Chandra error with limits of J~19.5, H~18.0 and K~18.0
- Presence of two sources just outside the Chandra error box=> from possible variations of the magnitudes of
one, possible association to the IGR is mentioned
|
|
Paizis et al. 2011 (ApJ):
- Chandra and multiwavelengths observations
- Time resolved X-ray spectroscopy => variations of NH
- Position of source in radio-X-ray diagram compatible with H1743-322 if at 8 kpc
- Discussion on the type of source=> LMXB favoured, Black Hole candidate suggested
|
|
Ma 2012 (MNRAS):
- Nearly-simultaneous broadband energy spectrum=> input to an accretion-jet model
- Results indicate that the accretion is probably driven by luminous hot
accretion flow (LHAF)
- Distance of between 21 and 25 kpc is proposed (assuming
a 10 Msun black hole
- The results lend credence to the view that the LHAF can
explain the steep correlation between the radio and X-ray luminosity
|
|