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| Miscellaneous :
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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).
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| Mowlavi et al. 2005 (Atel
453) : Variability in hard X-rays, decrease of
20-60 and 60-150 keV flux. |
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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
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| 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)
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| 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) |
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| 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) |
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| 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
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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
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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.
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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
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