IGR J16207-5129

Other name = (?)

Type Spectral type
Radio Counterpart Infrared/Optical Counterpart
R.A. (J2000) Dec. (J2000) References R.A. (J2000) Dec. (J2000) References
/ Supergiant XRB
early supergiant
O7.5 (see however Nespoli et al. 2008)
33800 K
14h53m41.16s -55021' 37.4"
Published Papers
Miscellaneous :

Masetti et al. 2006: Is HD 146803 the counterpart? then source is HMXB
Masetti et al. 2006 Atel 783:
  • Halpha emission at redshift 0 superimposed on a reddened continuum
  • HD 146803 not counterpart
Tomsick et al. 2006:
  • Chandra position rejects association with HD 146803.
  • Gamma~0.5 and nH~3.7x1022 at/cm2 (slightly higher than galactic absorption alone), with a high-energy cutoff.
  • Variability evident in the Chandra lightcurve.
  • Optical counterpart has J-band magnitude of 10.44(2), and a stellar temperature > 18,000 K which indicates that the system is a HMXB.
  • Distance estimated to be between 3 and 10 kpc which, if assuming d=5 kpc, gives a 0.3-10 keV luminosity of ~1.3x1035 ergs/s.
Negueruela and Schurch 2006:
  • New supergiant XRB (wind accretor)`
  • Possible B0 spectral type of the companion, but earlier than B1 in any case.
Masetti et al. 2006:
  • Halpha, EW=5.0 Angstrom
  • R~15.6
  • d~4.6 kpc
Rahoui et al. 2008:
  • Medium infrared observations
  • SED fitting => AV=10.5, Tstar=33800 K
  • O/B massive star, 07.5 favoured, distance between 1.8 and 4.1 kpc if source is main sequence, sub giant or supergiant
  • No need for additional component in SED fitting
Nespoli et al. 2008:
  • Infrared spectroscopy
  • Rather a B1 Ia companion
  • d~6.1 (-3.5+8.9) kpc
Tomsick et al. 2009:
  • XMM-Newton observations
  • Spectrum typical of HMXB with neutron star
  • Absorbed HMXB, confirmed by re analysis of Chandra data
  • Short term var. not only due to variations of Nh
  • No pulsations between 0.005 and 88 Hz with upper limit of 2.3 % (@ 90%) nor between 0.000023 and 0.05 Hz with upper limit of 1.7% (@90%)
Bodaghee et al. 2010:
  • Suzaku observation
  • Cutoff energy constrained for the first time at ~19 keV.
  • Cutoff E argues in favour of a neutron star primary
  • Spectrum strongly absorbed NH=16.2x1022 cm-2
  • ~30 ks epoch with source flux is extremely low (no change in nH or Γ)
  • Several mechanisms explored to explain diminished flux
  • Possible scenario of partial or full eclipse
  • If eclipse is real=> orbital period (4d <= P <= 9 d) and inclination angle (i >= 50 degs).
Jain et al. 2011 ATel 3785:
  • Detection of sporadic intensity modulation in the BAT 15-50 keV light curve
  • Period of of 9.726 d possible orbital period of the X-ray binary
  • Possible eclipse seen with Suzaku does not coincide with the phase at which the Swift-BAT light shows lowest intensity
  • If orbital period the suzaku event would likely be an absorption event

Last updated 30 Nov 2011o1

Jerome Rodriguez