| Miscellaneous :
| Fillipova et al. 2005:
- NH = 5.8 x 1023 cm-2
- Ecut=11+/-1 keV
| Bodaghee et al. 2006:
- Persistent, heavily-absorbed, wind-accreting pulsar
- NH = 2.5 x 1023 cm-2
- Pulse period = 912.0+/-0.1 s
- Gamma = 0.8+/-0.2
- Ecut = 10+/-1 keV
- Iron lines at 6.4 and 7.1 keV, with an absorption edge > 7.1 keV
- Soft excess emission
- Continuum modeled by absorbed comptt or an absorbed cutoff power law
- Spectral shape not modified by pulse
- Crowded field => 3EG association might be due to chance
| Thompson et al. 2006:
- Orbital period from RXTE data is 3.688+/-0.001 days.
- This implies a stellar mass of 6.5+/-1.1 solar masses.
| Thompson et al. 2006, ApJ:
- Orbital period from RXTE data is 3.6875+/-0.0006 days.
- pulse period of 911.3 s => may imply spin up since measure by Bodaghee et al. 2005
| Chaty et al. 2008:
- Optical and infrared observations
- 3 additional counterparts to 2MASS source, however 2MASS considered as
the likely candidate
- B>24.97, V=21.53, R=19.62, I=17.92, Z=16.99
- J=17.24, H=13.28, Ks=11.21
- SED fitting => Tstar=24400 K, typical of B star
- SED fitting => d=10.6 kpc for a BIV-V star, and 20.4kpc at least for a
supergiant. BIV-V favoured
| Nespoli et al. 2008:
- Prominent CO absorption features between 2.29 and 2.40 Ám,
<=> late type stars.
- Presence of metallic lines.
- Presence of He I 20581 A and Br-gamma =>circumstellar disk around a compact object,
but warning is given
- HXMB ruled out, companion very probablyof K or M spectral type =>
system is Symbiotic X-ray binaries
| Nespoli et al. 2010 (A&A):
- Prominent CO absorption features => late type stars.
- HXMB ruled out, companion very probably K or M Giant/Supergiant =>
system is Symbiotic X-ray binaries
- Select mass function of 0.092 Msun and orbit of 52 days.
- Companion mass < 5 Msun
- All conclusions valid if the counterpart considered is the true one
| Corbet et al. 2010 ATel 2570:
- Swift/BAT and RXTE/PCA monitoring
- None of the previously reported period in the long term light curves.
- Highly significant modulation at 4.2 days in both light curves.
- fits with sine wave to the LCs
Tmax (BAT) = MJD 54,352.50 (+/- 0.09) + n x 4.2368 (+/- 0.0007)
Tmax (PCA) = MJD 54,352.39 (+/- 0.11) + n x 4.2371 (+/- 0.0007)
- Semi-amplitude of the modulation divided by the mean flux is approximately 25%.
- Modulation likely being orbital period of the system
- Source lies in the Sg-HMXB region of the Corbet diagram =>IGR J16393-4643 very probably sg HMXB
- Not a symbiotic system.
| Bodaghee et al. 2012 (ApJ):
- Chandra observation => refined X-ray position
- 2MASS J16390535-4642137 excluded as IR counterpart
- New candidate IR counterpart blended with the 2 MASS star
- Large distance (>12 kpc) to the source suggested
| Corbet & Krimm 2013 (ApJ):
- Search for periodicities in BAT light curves
- possible identification of a super orbital period due to coincidence of peaks from the BAT, RXTE,
INTEGRAL light curves
- possible Super orbital period at 14.98 days
| Islam et al. 2015 (MNRAS):
- SUzaku broad band pulsation and spectral analysis
- Swift light curve => evidence for an eclipsing system
- Short eclipse semi-angle ~ 17o
- Change of photon index during high and low phase of pulse
| Bodaghee et al. 2016 (ApJ):
- Nustar+Swift observations
- Discovery of a cyclotron resonant scattering feature @ 29.3 keV
- B~2.5e12 G
- Neutron star spin period measured at 904 s => dν/dt=3 e-14 Hz
- Addition of angular momentum either due to accretion of quasi spherical wind or
transient appearance of accretion disk