IGR J16318-4848

Type Mass Radio Counterpart Infrared/Optical Counterpart
R.A. (J2000) Dec. (J2000) References R.A. (J2000) Dec. (J2000) References
sgB[e]/HMXB ? 1 sig. upper limits 0.1 mJy (4.8 and 8.6 GHz) Walter et al. 2003 Preprint Images here Filliatre & Chaty 2004 Preprint
16h 31m 48.31s -48° 49' 00.7"
Published Papers
Miscellaneous :
  • NH=~1 x 1024 cm-2
  • Prominent X-ray lines around 6.4 keV
  • XMM quick look results here
  • Distance between 0.9 and 6.2 kpc
Kaplan et al. (2006):
  • long wavelength excess
  • SED is higher in Mid IR than expected from pure stellar emission
  • warm circumstellar dust at 1000 K possibly responsible for X-ray absorption
Ibarra et al. (2007 A&A, 465, 501):
  • source always remains bright => very probable persistent source
  • variations of the absorbing column density (1.38e24 to 2.16e24 cm-2), but always remains compton thick
  • Variations of the Fe Kalpha emission line follow variations of the source flux (even on short time scales) => lines produced by the illumination of small-scale optically thick matter surounding the high energy source.
  • Evidence for a Compton shoulder in the spectra.
  • Obscuring matter is in a flattened configuration around the source, IGR J16318-4848 almost edge-on
Moon et al. (2007 ApJL):
  • Spitzer observations
  • Two continuum component a hot (1040 K) and a warm (190 K) one =>two circumstellar dust components, one warm and one hot.
  • Many emission lines: majority are HI lines
  • Also metallic forbidden lines (Ne II, Ne III, S III, Si II, Ni II, Fe II), pure rotational H2 lines, and PAH emission .
  • Deduce the presence of ionized stellar wind, an extended low density ionized region, and a photo dissociation region.
  • X-ray source is not the primarily responsible for the emission of forbidden lines although it can have some contribution.
  • Both dust components contibute very little to the total Optical extinction.
  • Highly obscured X-ray binaries could represent an unknown evolutionary phase of XRBs with early type Optical companions.
Rahoui et al. 2008:
  • Medium infrared observations
  • SED fitting => AV=17, T*=22200 K
  • Need for additional component to fit SED. T=1100 K, confirm results of Kaplan et al. 2006
  • Suggested distance 1.6 kpc
Pacciani et al. 2008 ATel 1713:
  • Hard X-ray bright state caught with super Agile
  • 20-60 keV flux (of 300 mCrab) 10 times higher than its average flux reported in the 3rd IBIS catalogue.
Barragán et al. 2010 (A&A):
  • Hard X-ray bright state caught with super Agile
  • 20-60 keV flux (of 300 mCrab) 10 times higher than its average flux reported in the 3rd IBIS catalogue.
Krimm et al. 2010 Atel 3051 :
  • Observation of renewed hard X-ray activity with Swift/BAT
  • 3rd large outburst seen with Swift since 2004
  • Earlier outbursts each lasted ~20 days
  • Time between outburst = multiple of the 80.2-day orbital period proposed
Chaty & Rahoui 2012 (ApJ):
  • New VLT/VISIR Mid IR observations
  • Broad band SED (with NTT and Spitzer) => star surrounded by irradiated rim at T~ 3800-5500 K
  • Presence of viscous disc component Tin~ 750 K
  • Spherical geometry excluded for dust component.
Coleiro et al. (2013) :
  • NTT/Sofi NIR Spectroscopy
  • Many intense and broad emission lines
  • Two He I lines with P-Cygni profile => Strong stellar wind. Velocity ~400 km.s-1
  • Possible presence of an H2 line => either shock heating high enough, or sufficiently low temperature region
  • Confirm sgB[e] HMXB

Last updated 10 October 2013

Jerome Rodriguez