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| Miscellaneous :
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Gibaud et al. 2011ATel 3551:
- INTEGRAL discovery. IBIS spectrum => power law Γ=1.9
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Bozzo et al. 2011ATel 3555:
- Swift/XRT observations => pile up corrected spectrum absorbed power law, NH=3 x 1022 cm-2,
Γ=1.9
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Papitto et al. 2011ATel 3556:
- RXTE Observation => detection of a 401 Hz oscillation => source possibly a ms accreting pulsar
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Jonker et al. 2011ATel 3559:
- Chandra observation => detection of quiescent counterpart at Fx=2.5e 14 erg/cm2/s
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Ferrigno et al. 2011ATel 3560:
- Detection of a type I X-ray burst from INTEGRAL/JEM-X
- Burst is 15s long and has a decay time of 6s
- Burst is well fitted by black body kT~1.4 keV and R~19 km (at 10 kpc)
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Markwardt et al. 2011ATel 3561:
- Two candidates orbital solutions at 3.8432 hr and 4.0834 hr from an RXTE observation
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Greiss et al. 2011ATel 3562:
- NIR source has J = 17.45, H = 15.73 and Ks = 15.10
- Extinction lower than that obtained from fits to the X-ray spectra
- De-reddened magnitudes are consistent with a late K or early M type star => source is an LMXB
- If NIR and X-ray sources are associated then system much closer than Galactic bulge
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Papitto et al. 2011ATel 3563:
- Several RXTE obs => orbital solution is 3.84281hr
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Linares et al. 2011ATel 3568:
- RXTE obs => Type I X-ray burst + burst oscillations
- Burst:
- total duration (PCA) 30s
- Absorbed black body model with cooling tail (kT from 2.6 keV to 1.4 keV)
- Moderate photospheric expansion during burst rise and peaks
- Burst oscillations at ~401 Hz detected during 2-3 s in the tail after PRE episode
- Distance estimated to 7.6kpc
- Total radiated energy = 3.2e39 erg
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Markwardt & Strohmayer 2011ATel 3601:
- Refined orbital solution
- Coherent pulsation at 400.990187287 Hz (non corrected for
the RXTE orbit and without clock correction applied)
- Orbital period 13865.615 s
- Projected semi major axis 0.365108 lt-sec
- Masses between 0.17 and 0.22 Solar masses
for the companion depending of the NS mass
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Russell et al. 2011ATel 3622:
- Optical observations with Faulkes telescope
- 4σ source detected at position consistent with X-ray and
quiescent IR counterparts=> likely optical counterpart
- i'~ 22.5
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van der Berg et al. 2011ATel 3634:
- Optical and NIR observations
- Optical source consistent with Chandra position and associated
to Faulkes counterpart
- Estimate of i' consistent with no variation between quiescence and outburst =>
source probably not counterpart to the IGR, probable chance alignment
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Torres et al. 2011ATel 3638:
- NIR and Chandra observations
- IR counterpart has H~16.0 consistent with pre-outburst value=> not related to
X-ray source
- Chandra spectra => power law with Γ=1.75 and
NH=2.87x1022
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Chakraborty et al. 2011ATel 3643:
- Detection and analysis of 10 X-ray bursts
- One shows photospheric radius expansion
- burst oscillations detected in the tail of the PRE X-ray flare
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Linares et al. 2011 ATel 3661 (see also Chakraborty et al. 2012 for detailed analysis and discussion):
- Swift monitoring
- Two X-ray burst were detected two X-ray bursts on Aug. 18 and
28 (2011)
- The source count rate remained ~constant until Aug. 24
- The count rate then started to decrease slowly until Sep. 18
- In the last two observations of this period (Sep. 17 and 18) the source
spectrum was soft => fitted with an absorbed blackbody with kT~ 0.6 keV Nh fixed at 3e22 cm-2
(a very soft absorbed power law also fits the data well)
- Not detected during five Swift-XRT observations on Sep. 19, 20, 22, 24 and 26 => has returned to quiescence
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Papitto et al. 2011 (A&A):
- Analysis of RXTE and Swift observations
- Coherent pulsation at 400.99018734 Hz,
- Analysis the modulations of pulsation=> orbital period of ~3.84 hr
- Mass of the donor between 0.17 Msun (lower limit) and 0.48 Msun (upper limit)
- Spectra well modeled with absorbed power law with Γ comprised between 1.7 and 2
- Close to quiescence Γ softer.
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Falanga et al. 2012 (A&A):
- Analysis of simultaneous Swoft, RXTE and INTEGRAL observations
- Broad band 0.6-300 keV spectrum well described by thermal Comptonisation
with kTe~50 keV, kTbb~1 keV and τ=1 in a
slab geometry with an area ~ 9 km
- No spetral variations during outburst => X-ray emission originate above
the surface in hot slab (heated NS surface or accretion shock)
- 2.5ms pulsation detected up to 65 keV
- Pulsed fraction is energy independent and is found around 6-7%
- Analysis of burst => hydrogen poor material at ignition => material
hydorgen deficient or CNO metallicity up to twice the solar values
- Burst recurrence time smaller than predicted by He-ignition models
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