IGR J16465-4507


Other name =

Type Orb. Period/Spin Period Radio Counterpart Infrared Counterpart
R.A. (J2000) Dec. (J2000) References (position) R.A. (J2000) Dec. (J2000) References (position)
HMXB Pulsar
SFXT
B0.5I (see however Nespoli et al. 2008)
30.32d / 228.5 s 2MASS J16463526-4507045 Zurita & Walter 2004 Atel 336
Published Papers
Miscellaneous :
2 MASS J image+XMM error available here (Courtesy J. Zurita)
Zurita & Walter 2004 : J=10.54
Smith 2004, ATEL 338 :
  • Optical magnitudes (USNO B1.0): B2=15.2, R2=13.0
  • (possible) Distance 12.5 kpc
Neguerela et al. 2005 Atel 429 :
  • reddened early-type B0.5I supergiant,
  • H-alpha line shows a broad emission component on top of the photospheric profile
Lutovinov et al. 2005:
  • pulsations at 228 +- 6s
  • NH=72x 1022 cm-2, Gamma~1.0, Ec~30 keV
Walter et al. 2006:
  • pulse period of 227+-5 s in XMM (not seen in ISGRI)
  • large soft excess (not described by partial-covering absorber) and marginal K-alpha line (EW < 60 eV)
  • NH = 60(+-10)x1022 at/cm2
  • IR counterpart (2.6 arcsec away) has a K-band magnitude of 9.8
  • unabsorbed flux (2-100 keV) is 2.8x10-10 ergs/cm2/s
Rahoui et al. 2008:
  • Medium infrared observations
  • SED fitting => AV=5.9, T*=25000 K
  • Obscuring material contributes little to MIR spectrum
  • Suggested distance 9.4 kpc
Nespoli et al. 2008:
  • Infrared spectroscopy
  • Suggest companion is O9.5 Ia
  • The X-ray nature => SFXT nature
  • Distance 9.5 (-5.7 +14.1) kpc
  • Local absorption comes from material concentrated around the compact object
Morris et al. 2009:
  • Suzaku observations
  • confirm the source is an heavily absorbed HMXB
La Parola et al. 2010 (MNRAS):
  • Significant periodicity in Swift/BAT at P=30.243 d
  • Observation of a wide phase of 0 intensity at T(MJD)=54180.5+- nPorb
  • Semi-major orbital axis a~125 Rsun (150 Rsun)~6 Rstar (5 Rstar) for a typical 09.5 I (B0.5 Ib) star
  • Do not favour an eclipse as the origin of the minimum phase
Clark et al. 2010 (MNRAS):
  • Periodicity in Swift/BAT and INTEGRAL/IBIS at P=30.32 d
  • Semi-major orbital axis a~121.9--126.3 Rsun according to the mass of the donor
  • e either <0.6 or <0.8 depending on the exact mass of the donor.
  • Source is an intermediate SFXT
Wang & Chang 2012 (A&A):
  • Study retrograde wind accretion scenario
  • => spin and orbital period => R corrotation ~ 3.7e9 cm and source is a pure propeller
Romano et al. 2014(A&A):
  • Study of long term Swift/XRT monitoring
  • Low ~5% inactivity duty cycle, and a dynamic range of ~40 during bursts
  • Low inactivity duty cycle and dynamic range compared to (other) SFXTs is rather reminiscent of classical sg-HMXBs
  • No correlation between duty cycle and orbital period

Last updated 4 March 2015

Jerome Rodriguez