IGR J17451-3022

Other name =

Type Spin P. / Orb. P. Radio Counterpart Infrared/Optical Counterpart
R.A. (J2000) Dec. (J2000) References R.A. (J2000) Dec. (J2000) References
LMXB / 6.28 hr
Published Papers
Miscellaneous :
Heinke et al. 2014 ATel 6459 :
  • Analysis of Swift observations
  • Spectrum poorly represented by an absorbed power law, and best represented by black body (kT~0.8 keV, NH to vary between ~5 and ~7 x 1022 cm-2
  • High absorption consistent with location near or beyond Galactic centre
Altamirano et al. 2014 ATel 6469 :
  • Analysis of further Swift observations
  • Spectra broadly consistent with previous analysis
  • Search for pulsations unsuccessful with a typical upper limit of 10% in the range 0.01-280 Hz
Bahramian et al. 2014, 2015 ATel 6486
ATel 7028 :
  • Analysis of further Swift observations
  • Spectra of first two observations (Sept. 15 and 19 2014)consistent with being soft and thermal
  • Spectrum of the Sept. 21 observation has become harder => Power law (Γ~2.2) gives a better fit
  • Spectral hardening favours an LMXB (with d> 8kpc)
  • In Feb, 2015 outburst continues with parameters consistent with those obtained before sun constrained period.
  • No significant variation over 4-5 months during which the source remained in a bright soft state
Homan et al. 2015 ATel 7361
  • Suzaku observation on 2014 Sept. 23/24
  • Strong dipping activity in 0.5-10 keV light curves
  • Identification of eclipses with recurrence period 22623s identified as orbital period
  • Difficulty to estimate true duration of eclipses but constrained to be < 2600s
  • => Strongly inclined system > 70 degrees
Bahramian et al. 2015 ATel 7570
  • Swift observation durin 2015 May =>decline of brightness until marginal detection
  • Spectral analysis of the most recent obs. => consistent with kT=0.6 black body
  • => Source is returning to quiescence
Bozzo et al. 2015 (A&A)
  • INTEGRAL, Swift and XMM observations
  • OUtburst lasted 9 months with source remaining soft over the entire period
  • Source spectra dominated by thermal (kT~1.2 keV) emission attributed to accretion disk
  • Presence of multiple absorption features with potential presence of ionized absorber above the disk
  • Partial and rectangular X-ray eclipse (820s) and dips => source orbital period 22620.5 s (~6.28 hr)

Last updated 18 Apr. 2016

Jerome Rodriguez