IGR J17098-3628

Type Mass Radio Counterpart Infrared Counterpart Optical Counterpart
R.A. (J2000) Dec. (J2000) References R.A. (J2000) Dec. (J2000) References R.A. (J2000) Dec. (J2000) References
X-ray nova
Black Hole candidate
17h 09m 45.934s +/- 0.011s -36d 27' 57.30" +/- 0.55" Rupen et al. Atel 490 2MASS J17094612-3627573 !!! But see Steeghs et al Atel 478, Rupen et al. Atel 490 Kong 2005 Atel 477 17h 09m 45.93s (+-0.2") -36d 27' 58.2" (+-0.2") Steeghs et al. 2005 Atel 494
Published Papers
Miscellaneous :

Grebenev et al. 2005 (Atel 447) :
  • NH<~1022 cm-2
  • Gamma~1.81 evolving to 2.10 at high energy
  • Gamma ~2.5, black body ~ 1 keV, in RXTE
  • Lightcurves and Images here (Courtesy S. Grebenev).
Mowlavi et al. 2005 (Atel 453) : Variability in hard X-rays, decrease of 20-60 and 60-150 keV flux.
Kong. 2005 (Atel 477) :
  • J=14.69, H=13.66, and K=13.37, and the couterpart position is at 2.7" from the Swift position
  • B=21.16, R=19.43, and I=18.75, and the couterpart position is at 3.25" from the Swift position
Steeghs et al. 2005 (Atel 478) :
  • Proposed optical counterpart is a blend of several point sources
  • Comparison between the SuperCOSMOS sky survey image and the 360s IMACS image is available here (courtesy D. Steeghs)
Blustin et al. (Atel 479) :
  • Swift/UVOT detects a V=19.3 +/- 0.1 source at a position ~ identical to the SuperCOSMOS candidate counterpart
  • An image of the Swift-UVOT source is available here (courtesy A. Blustin)
Rupen et al. (Atel 490) :
  • Radio counterpart evolution is consistent with X-ray history of the source
  • The radio source is at 0.8" from the Swift best position
  • the two last points render very likely the association of the radio source and IGR J17098-3628
  • Radio position inconsistent with the counterparts of Kong 2005 and Blustin et al. 2005.
  • VLA images are available here (courtesy M. Rupen)
Kennea & Capitanio 2007 ATel 1140:
  • Swift observation => absorbed disk blackbody model, whith Nh=0.89e22 cm-2 and kT = 0.89
  • 0.2-10 keV unabsorbed flux ~9 E-10 erg/s/cm2
Chen et al. 2008:
  • Analyse of RXTE/ASM and INTEGRAL data
  • Focus on a period during which the source underwent a hard outburst (March 2005)
  • Soft X-rays lag the hard ones by about 2 days, ie the hard peak occurs before the soft one.
  • cut-off pl gives a slightly better representation of the ISGRI spectra during the outburst
  • JEM-X ISGRI spectrum of the decaying phase well modeled with a broken power law
  • Further confirm that the source is a probable Black hole in a LMXB
Capitanio et al. 2009:
  • Regularly detected by INTEGRAL and RXTE over the period 2005-2007
  • Showed slight variations of the flux
  • Spectra show that the soft component (disc black body) remained essentially the same over the entire 2.5 years period
  • Hard tail fell below detection threshold of IBIS 3 months after the begining of the source outburst.
Kotze et al. 2009:
  • Long term analysis of ASM light curve
  • Quasi-period of 163 d during active states of the source
  • Light curve not typical of transient, source dubbed it "pseudo-transient"
  • Suggest source is an LMXB in a short (<1d) orbital period

Last updated 2 April 2009

Jerome Rodriguez