IGR J17195-4100

Other name = 1RXS J171935.6-410054

Type Orb. P. / Spin P. Radio Counterpart Optical Counterpart
R.A. (J2000) Dec. (J2000) References (position) R.A. (J2000) Dec. (J2000) References (position)
4.005 h / 18.9925 min USNO B1, A2 catalogues U0450_27095307
USNO-B1.0 0489-0511283
17h 19m 35.91s -41deg 00' 53.7"
Published Papers
Miscellaneous :
Stephen et al. 2005: :
  • B~15
  • Possible extended or unresolved IR source within 2.2" of the optical counterpart
Masetti et al. 2006Atel 783:
  • Balmer and He emissions at z = 0
  • possible CV
Tomsick et al. 2006 :
  • Chandra position is 0.7" away from USNO-B1.0 0489-0511283, and therefore (along with supplemental IR/optical analysis) the USNO source must be considered as the optical counterpart.
  • Column density is ~8x1020 (low) at/cm2 and Gamma~1.1.
  • Some variability present in Chandra lightcurve.
  • Spectral type of optical companion is no later than A3 which along with distance estimations and extinction measurements is incompatible with a supergiant or OB main sequence star, so the system can not be a HMXB.
  • Maximum distance is 2.6 kpc, so 0.3-10 keV luminosity is <2.0x1034 ergs/s.
Barlow et al. (2006) :
  • 20-100 keV Power law photon index 2.9, or bremsstrahlung kT=27.0 keV
Masetti et al. (2006) :
  • Halpha, Hbeta, He II emission lines
  • R=14.3
  • d~110 pc
Butters et al. (2008) :
  • RXTE analysis
  • 2 equally possible periods in the periodogram at 1842.4s and 2645.0s
  • Typical of spin periods for Intermediate Polar
  • If longer=spin, and other=beat period => orbital period=1.7 hr.
  • Source is a likely IP although no definitive classification
Pretorius 2009:
  • Optical observations: Phase resolved spectroscopy => Orb. period 4.005h
  • Spin period of 18.9925 min
  • Source is a confirmed IP
Revnivtsev et al. (2010) :
  • Study of optical aperiodic variability
  • νbreak~2 x Spin period
  • If break freq <=> inner disc radius then inner radius close to corotation with WD magnetosphere
Bernardini et al. 2012 (A&A):
  • Multi-wavelengths observations
  • Pulse period = 1062s
  • Broad band spectral analysis
  • Disc overflow accretion mode
  • MWD~0.86 Msun at d~130 pc
Girish & Singh 2012 (MNRAS):
  • XMM-Newton and Suzaku observations
  • New period 1053.7 s and new binary orbital period of 3.52 h
  • Soft X-rays (<3keV) dominate variability
  • Spectral fitting with plasma emission, cooling flow models (apec, mkcflow), plus Gaussian, partial covering
  • Presence of a soft excess attributed to varying coverage of accretion curtains

Last updated 22 Aug. 2012

Jerome Rodriguez