IGR J17252-3616

Other name = EXO 1722-363

Type Mass
type of companion
Radio Counterpart Infrared Counterpart
R.A. (J2000) Dec. (J2000) References (position) R.A. (J2000) Dec. (J2000) References (position)
pulsar/HMXB <22 Msun
B0-B1 Ia
2MASS J17251139-3616575 Cutri et al. 2003
17h 25m 11.39s (+-0.06" 1sig) -36o 16' 57.5" (+-0.06" 1sig)
Published Papers
Miscellaneous :

Fillipova et al. 2005: NH <1024, power law with Gamma=3.5
Zurita Heras et al. 2006:
  • 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. 2007:
  • 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 AL. 2008)
  • Distance 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

Last updated 4 March 2015

Jerome Rodriguez