IGR J16358-4726

Type Spectral Type
Radio Counterpart Infrared Counterpart
R.A. (J2000) Dec. (J2000) References (position) R.A. (J2000) Dec. (J2000) References (position)
Symbotic X-ray Binary x Candidate = 2MASS J16355369-4725398 Koveliotou et al. 2003 IAUC 8109
16h 35m 53.69s -47° 25' 39.8"
Published Papers
Miscellaneous :
Patel et al 2004 :
  • NH=3.3 x 1023 cm-2
  • X-ray pulsations at 5850 +-50 s
Lutovinov et al 2005 :
  • X-ray pulsations at 5980 +-22s in INTEGRAL (20-60 keV)
Mereghetti et al. 2006 :
  • Source detected by XMM on two occasions: spectra are well described with an absorbed power law with Gama=1.5 and Nh=2e23 cm-2 (for the brightest observation)
  • 5880s pulsation is present although the source flux is 200 times dimmer than when discovered with Chandra
  • when source not detected upper limit on the 2-10 keV flux is 4e-14 erg/cm2/s
Patel et al. 2007, ApJ :
  • Any periodic outburst cannot occur on period > 400 days
  • Joint Chandra and INTEGRAL spectrum fitted with absorbed cut off powerlaw (or equivalently model of comptonisation)
  • Gamma=0.4, Ecut=19 keV, Efold=12 keV
  • 1.6 hour pulsation confirmed in INTEGRAL data
  • spin up rate of 1.9e-4s/s
  • B~1e13-1e15 G
Chaty et al. 2008:
  • Optical and infrared observations
  • B>23.42, V>23.67, R=23.75, I=20.49, Z=18.59
  • J=15.46, H=13.57, Ks=12.60
  • IR counterpart could be a blend of sources
  • Very faint and absorbed near IR spectrum
  • Tentative P-cygni profile for some lines and HeI and HeII absorption=>typical of O/B Sg
  • Forbidden FeII line => SgB[e]
Rahoui et al. 2008:
  • Medium infrared observations
  • SED fitting => AV=17.6, Tstar=24500 K
  • Obscuring material possibly contributes to MIR spectrum with T=810 K at 10.1 Rstar
  • SgB[e] possibly confirmed, and suggested distance 18.5 kpc
Nespoli et al. 2008: ATel 1450
  • Prominent CO absorption features between 2.29 and 2.40 µm, <=> 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):
  • CO absorption features => late type star
  • HXMB ruled out, companion very probably of K or M Giant/Supergiant => system is Symbiotic X-ray binaries
Bodaghee et al. 2012 (ApJ) :
  • Non detection with Chandra => 2-10 keV 3-σ upper limit = 1.8E-12 erg/cm2/s

Last updated 12 April 2010

Jerome Rodriguez