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| Miscellaneous :
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Barlow et al. 2005 :
- 20-150 keV flux of 1.1 10-10 erg s-1 cm-2 during outburst
- Γ=2.1
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Tomsick et al. 2008:
- Chandra reveals 6 sources within INTEGRAL error box.
- Upper limit on the 0.3-10 keV source flux 5.5-6.4e-14 erg/s/cm2 assuming Γ=2.1
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Markwardt et al. 2010 ATel 2823:
- RXTE/PCA detection of an outburst from a source dubbed XTE J1728-295, during scans on 2010-08-28
- Rose to a 2-10 keV flux of 6.5 mCrab.
- RXTE/PCA position consistent with IGR J17285-2922
- IGRJ17285-2922 and the XTE source are very likely to be the same source.
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Yang et al. 2010 ATel 2824:
- Swift follow up ToO
- X-ray position not consistent with any of the 6 chandra sources => source probably in quiescence
at time of Chandra obs.
- Spectrum best fitted with an absorbed power-law model with NH =5.4 x1021
cm-2, &Gamma= 2.23;
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Tuerler et al. 2010 ATel 2825:
- INTEGRAL detection of IGR J17285-2922 in the 20-40 keV band on several occasions
- Source is detected at 40-80 keV in combined pointings
- INTEGRAL position consistent with Swift => Strengthens the association of the XTE and IGR sources.
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Russel et al. 2010 ATel 2827:
- Search for optical counterpart => 3 faint sources within XRT error circle
- Only 3 star detected in the H-alpha image, none show evidence for variability
- No further conclusions on the association of one of the star with the IGR
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Torres et al. 2010 ATel 2870:
- Optical observation => refine position of previously suggested optical
counterpart
- Remark the presence of at least two other point-like sources within
Chandra error
- Lack of variability of source
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Russel et al. 2010 ATel 2997:
- Optical monitoring
- confirm their source 3 is the optical counterpart due to 0.4 mag
variability
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Kong et al. 2010 ATel 3011:
- Non detection of source 3 in the R band => source 3 is the optical
counterpart
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Sidoli et al. 2011 (MNRAS) :
- Broad band (INTEGRAL+XMM) spectrum: absorbed
power law , NH=0.5 x 1022 cm-2 and Γ=1.61
- No cut off Ec > 50 keV
- No type I X-ray bursts or coherent pulsations are found.
- Power spectrum: shape typical
of that of LMXBs in the low hard state and a level of variability (20% between
0.1 and 1 Hz) also compatible with this..
- LMXB, possibly hosting a black hole, but true nature of primary uncertain
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