IGR J11215-5952

Other name =

Type Pulse/Orb. Period Radio Counterpart Infrared/Optical Counterpart
R.A. (J2000) Dec. (J2000) References R.A. (J2000) Dec. (J2000) References
HMXB, Fast X-ray transient 195 sec. / 165 days HD 306414 Neguerela 2005

Masetti et al. 2006
Published Papers
Miscellaneous :
Neguerela et al. 2005 Atel 470:
  • Possible association with HD 306414, B supergiant
  • V=9.98, (B-V)=0.59, (U-B)=-0.45, AV 2.42
  • distance to the supergiant ~8 kpc
Masetti et al. 2006:
    Fast X-ray transient?
Sidoli et al. 2006:
  • discover two new outbursts of longer duration than typical outbursts from other Supergiant Fast X-ray Transients
  • periodicity of 330 days (or half of it).
  • confirm the association with HD 306414
  • confirm Supergiant Fast X-ray Transients.
Smith et al. 2006 ATel 766:
  • outburst observed with RXTE.
  • periodicity of 329.0 days.
  • gamma=-1.7(2), nH=11(2)e22.
  • extreme variability.
  • confirm Supergiant Fast X-ray Transient.
Steeghs et al. 2006 ATel 768:
    Swift XRT position confirms the association with HD 306414.
Smith et al. 2006 ATel 773:
  • End of the outburst as predicted.
  • .RXTE follow ups => lower and upper limits to the total duration of the outburst of 2.0 and 3.4 days.
  • possible pulsation at 195 s
  • relative constancy of spectra along outburst
Sguera et al. 2006 :
    20-40 keV peak flux of 40 mCrab
Romano et al. 2007: ATel 994
  • New outburst seen with Swift starting exactly 328 days after the last one
  • Confirm the periodicity of the outbursts
Mangano et al. 2007: ATel 995:
Sidoli et al. 2007: ATel 997
  • Confirm pulsation at 180.4 +-1 s, with Swift/XRT
Swank et al. 2007: ATel 999
  • Pulsation at 186.78 +-0.3 s with RXTE/PCA
  • Spectrum typical of that of a power law and high energy cut-off. Gamma=1.07 and Ecut=5.8 keV, Efold=15 keV
  • Light curves available at http://scipp.ucsc.edu/~dsmith/atel/atel0999/
Romano et al. 2007(A&A):
  • Monitoring of an entire outburst with Swift
  • outburst lasted 23 days
  • peak luminosity (6.2 kpc, 1-10 keV) 1.1 x 1036 erg/s
  • minutes to hours flares (SFXT definition) are part of longer episode of outburst.
  • flares due to episodic accretion from wind of companion
  • outburst due to accretion near periastron
  • hard spectrum at maximum, softening towards quiescence
Romano et al. 2007: ATel 1151
  • Detection of an outburst with Swift XRT
  • The 1-10 keV unabsorbed flux reached 1.4e-10 erg/cm2/s, for a spectrum that is well represented by a power law with Gamma=0.87 absorbed with Nh=1.08 E22 cm-2
  • Occurs 165 days after the preceding outburst at half the period reported previously.
Sidoli et al. 2007 (A&A):
  • Swift, XMM and INTEGRAL observations
  • Detection of a pulse period at 186.9 s compatible with that found with RXTE.
  • Outburst could be divided in two intervals: a bright and a faint one, both well fitted with absorbed cut-off power-laws.
  • Purely spherical and symmetric wind accretion is excluded in this system.
  • Either the neutron star crosses a dense equatorial wind of the secondary once per orbit, and then the true period is 165 days, or the orbit is circular and the NS crosses the equatorial wind of the secondary twice per orbit, and the period is ~330 days.
Sidoli et al. 2008 ATel 1444:
  • Swift observations at P329/4
  • Not detected with 3-σ upper limits (unabsorbed) 1-10 keV flux of 1.7E-12 and 2.3E-12 erg/cm2/s <=> 3-σ upper of 1.1E-12 erg/cm2/s wile cumulating the two obs
Romano et al. 2009 ApJ:
  • Results of Swift monitoring observations
  • 164.6 days periodic outburst =>orbital period of the system
  • system is eccentric
  • no evolution of NH during the outburst, nor in comparison to previous outbursts
  • Favour the presence of a strong equatorial wind from the companion
  • Period of 165/2 is excluded
Wang & Chang 2012 (A&A):
  • Study retrograde wind accretion scenario
  • => spin and orbital period => R corrotation ~ 3.3e9 cm and source is a pure propeller
Lorenzo et al. 2014 (A&A):
  • High resolution spectroscopy of HD 306414 at different epochs
  • Companion classified as B0.5 Ia with Teff~24700K
  • Distance d>~7 kpc => Mspec~30 Msun
  • Not a typical SFXT but flares driven by close approach to companion during periastron

Last updated 24 April 2014

Jerome Rodriguez