IGR J17285-2922

Other name = XTE J1728-295 (probably)

Type Mass Radio Counterpart Infrared/Optical Counterpart
R.A. (J2000) Dec. (J2000) References R.A. (J2000) Dec. (J2000) References
BH transient (?)
17h 28m 38.86s -29 o 21' 44.0" Torres et al. 2010 ATel 2870
Miscellaneous :

Barlow et al. 2005 :
  • 20-150 keV flux of 1.1 10-10 erg s-1 cm-2 during outburst
  • Γ=2.1
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
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.
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;
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.
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
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
Russel et al. 2010 ATel 2997:
  • Optical monitoring
  • confirm their source 3 is the optical counterpart due to 0.4 mag variability
Kong et al. 2010 ATel 3011:
  • Non detection of source 3 in the R band => source 3 is the optical counterpart
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

Last updated 24 November 2010

Jerome Rodriguez