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| Miscellaneous :
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Kuulkers et al. 2006 ATel 888:
- JEMX+ISGRI spectrum => absorbed power law, Gamma=1.93,
NH < 6
x 1022 cm-2
- Typical hard state of XRBs
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Walter et al. 2006ATel 889:
- NH < 3.5
x 1022 cm-2
- source detected up to 200 keV
- two IR objects in 2MASS archives in Swift error circle
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Markwardt & Swank 2006ATel 891:
- No QPO
- Strong red noise dominated by periods > 1s
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Chaty et al. 2006ATel 897:
- 3 candidate IR counterparts
- 2MASS 17493780-2821181 and 2MASS 17493774-2821173 are blended in 2MASS
- 2MASS 17493780-2821181 is blended in J H Ks, and one of its constituent
(src3) is more reddened
- src3 is the real counterpart.
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Kennea et al. 2006ATel 900:
- refined position
- 2MASS 17493780-2821181 is the only counterpart in the Swift error
- NH = (4.8 +/- 0.3) x 1022 cm-2,
Gamma = 1.6 +/- 0.1,
Flux = 3.3 e-10erg/s/cm2 (absorbed 0.3-10.0 keV).
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Paizis et al. 2006ATel 907:
- refined position with Chandra
- Candidate 1 from Chaty et al. ATel 906 is the counterpart
- NH = (4.2 +/- 0.1) x 1022 cm-2,
Gamma = 1.15 +/- 0.05,
Flux = 3.1 e-10erg/s/cm2 (absorbed 1-8 keV).
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Torres et al. 2006ATel 909:
- Candidate 1 is blended
- Faintest object likely counterpart
- Ks=15.9
- Finding Chart here
(courtesy Torres et al.)
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Itoh et al. 2006ATel 914:
- source is detected from 0.5 to 300 keV
- 1-60 keV spectrum well fitted by an absorbed
power law with NH = 4.6 x 1022 cm-2, Gamma=1.6
- gradual cut-off above 100 keV.
- hint for some structures in the Fe region
- Some variations of flux and spectral hardness
along the observation.
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Walter et al. 2007, A&A:
- IR/optical source located at RA=17h 49m 38.11s Dec=-28O 21' 17.2"
associated with the X-ray source
- No Type I X-ray burst in 995 ks of data down to 0.1-0.2 Ledd.
- Power law with a high energy cut-off (Gamma=1.67), or Comptonised spectrum,
with kT=35 keV and Tau= 1.45
- New X ray nova harbouring a black hole.
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Rodriguez et al. 2007, ApJL:
- 3~200 keV spectral analysis => very little variations over a period of 10 days
around the maximum of the outburst.
- typical Low Hard State of X-ray binaries
- Absorbed Comptonization with Nh~3.3-4e22 cm-2, kT~35-40 keV and Tau~1.6-2 + iron edge at about 6.6-7.1 keV
- Timing analysis: no particular features. Shape of the power density spectra typical of LHS of XRBs
(flat top noise + ~power law decay above<=>sum of 3 Lorentzians) with ~36% RMS variability
- 3-sigma upper limits of 2% on the presence of a 2Hz FWHM QPO.
- 3 sigma upper limits ranging from 2.4% to 0.9% for coherent pulsations between 4mHz and 4096 Hz.
- No radio counterpart with limit of 0.21 mJy at 4.80 GHz and 8.64 GHz.
- IGR J17497-2821 in the radio to X-ray flux diagram is well below
the correlation usually observed in the LHS of black holes
- X-ray spectral properties make it black hole candidate.
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Paizis et al. 2007, ApJL:
- X-ray spectrum well fitted by an absorbed (NH=5.6 x 1022
cm-2) power-law (gamma=1.5)
- disk emission with kTin=0.2 keV.
- Optical and near infra-red photometric follow-up observations (mag Ks=16).
- source is a LMXB, hosting a
black hole, with a red giant K-type companion
- Possible first "symbiotic" LMXB hosting a black hole.
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| Torres et al. 2007, ATel 1002:
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Paizis et al. 2009, :
- Broad-band X-ray spectrum as observed by Suzaku eight days after its
discovery (September 2006)
- Very bright, with L(1-300 keV) = 2 10^37 erg/sec at 8 kpc, + very hard spectrum.
- Simple phenomenological model => high energy cut-off around 150 keV
- physical scenario fits with diskbb+compps, kTdisc=0.25 keV, kTe=85 keV ,
τ=1.42
- A very mild reflection component is seen for the first time in the spectrum
- Hint of spectral hardening about 10 days after the peak
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Shah Alam et al. 2015 (MNRAS), :
- Analysis of XMM observations
- Source spectra compatible with a hard (Γ=1.5) power law and cold (kT~0.2 keV) disk
- Broad Kα iron line with 27000 km.s-1 compatible with disk truncated at large radius
- Source behaviour = BH hard state
- PDS modeled with 3 broad Lorentzians
- RMS higher in the softest energy range(0.1-2 keV), but otherwise increases with energy (>2 keV), which is
not typical of a BH in a hard state
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