| Miscellaneous :
| Fillipova et al. 2005:
NH <1024, power law with Gamma=3.5
| Zurita Heras et al.
- Persistent, heavily-absorbed, wind-accreting pulsar
- NH = 1.5 x 1023 cm-2
- Pulse period = 413.7 s
- Orbital period= 9.72 days
- Iron line at 6.4 keV
- Continuum modeled by absorbed comptt (kTe~5.5 keV, tau~7.8) or an absorbed flat power law (Gamma~0.02,Ecut~8.2 keV).
- Spectral shape not modified by pulse
- Associated with EXO 1722-363 due to similar timing and spectral properties
| Thompson et al.
- Refine the orbital period to P=9.7403 days with
data collected over more than 7 years.
- Limit on the eccentricity to e< 0.19 which shows
it is consistent with being circular.
- They also report the observation of a torque reversal
between 1998 and 2006.
- Mass function of the system is 11.7 solar masses => source is a HMXB.
- Radius of 21 to 37 solar radius and a mass
not greater than 22 solar masses.
- Inclination of the system is
greater than 61 degrees.
- The star is in the range of BO I to B5 I spectral type (SEE HOWEVER RAHOUI ET
between 5.3 and 8.7 kpc.
- The spectral analysis reveal a variable Nh and Fe Kalpha
line and photon spectal index.
| Chaty et al. 2008:
- Position in Corbet diagram Optical and infrared observations
- 3 fainter IR counterpart candidate in addition to 2MASS source,
the latter is however favoured as the true counterpart
- J=14.19, H=11.90, Ks=10.67
- Very red Near IR spectrum with absorption and emission lines
- Paschen and Brackett H-lines , and HeI and He II in emission
- Likely P-Cygni profile
- Probable O/B star, and likely sg HMXB
| Rahoui et al. 2008:
- Medium infrared observations, and GLIMPSE data
- SED fitting => AV=20.8, Tstar=32600 K =>
O8.5 I companion
- No need for an additional model to fit model
- Suggested distance 6.1 kpc
| Mason et al. 2009:
- VLT/ISAAC IR spectrometry => companion is a B0-B1 Ia
- d=8 kpc
- Source has luminosities
in a range typical of those found in other sg HMXBs.
| Manousakis et al. 2010:
- XMM monitoring of IGR J17252-3616, re-analysis of INTEGRAL and RXTE data
- Refined orbital solution for the system: e>0.15, Porb=9.76 d, αx sin i= 102 lt-s.
- Significant variations of NH and the eq width of the iron line observed near eclipse of the source
- The variations of NH compatible with model of dense end extended hydrodynamical tail trailing NS
- This structure extends along most of orbit => estimate wind velocity vinf~400 km.s-1
- Most of the Fe emission generated in inner region of the tail, and does not contribute to the X-ray absorption.
| Manousakis et al. 2012:
- Modeling of the flow of the stellar wind
- Study the dependence of the absorbing column
density on the orbital phase
- Comparison of simulations with observations => mass of 1.75 to 2.15 solar masses for the neutron star
and a wind terminal velocity of 500-600 km.s-1
- Confirm previous conclusions of a slow velocity wind in this source
| Falanga et al. 2015 (A&A):
- Use of RXTE/ASM and INTEGRAL/ISGRI long term light curve to update ephemeris,
refine orbital period decay
- T0, ecl. = 53761.695 (MJD), POrb., ecl=9.74079, dot(P)/P=-21e-6/yr