IGR J18410-0535

Other name = AX J1841.0-0536

Type Companion Radio Counterpart Infrared Counterpart
R.A. (J2000) Dec. (J2000) References (position) R.A. (J2000) Dec. (J2000) References (position)
Be X-ray Binary


Superfast X-ray transient
B0 I (see also Nespoli et al. 2008) 18h 41m 0s.43 -05° 35' 46".5 Halpern & Gotthelf 2004 Atel 341
Published Papers
Miscellaneous :

Halpern et al. 2004 Atel 289:
  • Chandra and DSS image available here (Courtesy J. Halpern)
  • B=15.91, R=12.78, I=10.90, J= 9.74, H=9.22, K= 8.93 (USNO B1 and 2MASS, Atel 289)
  • Nh=6.1*1022cm-2 (Chandra),
Bamba et al.:
  • Nh=3 *1022cm-2 (ASCA)
  • Coherent pulsation at 4.7394+- 0.0008 s
Sguera et al. 2006 :
    20-80 keV peak flux of 120 mCrab
Nespoli et al. 2007 ATel 983:
  • HeI, NIII/CIII, and CIV in emission (weak for the later),
  • HeI and Br-gamma in absorption
  • Supergiant B0 with uncertainty of 2 subtypes
Sidoli et al. 2008 :
  • Swift study of the "out-of-outburst" periods
  • Swift=> pulsation at 4.7008s
  • Spin up trend
  • Absorbed pl or bbody fits the data well
  • Γ= 1.6 and NH=4.2x1022cm-2 or kT=1.5 keV and NH=2.0x1022cm-2
Nespoli et al. 2008 :
  • Infrared spectroscopy
  • BI Ib suggested
  • Distance 3.2 (-1.5 +2.0) kpc
  • Local absorption comes from material concentrated around the compact object
Sguera et al. 2009 :
  • study possible association with either 3EG J1837-0423 or HESS J1841-055.
  • Good positional match with HESS src but HESS source extended and non-variable => AX/IGR source cannot be responsible for the entire TeV emission.
  • Marginally positionally consistent with Egret one. The variability and behavior of the 2 sources => suggest a possible association
  • Theoretical scenario where the AX/IGR source contains a pulsar with a low B undergoing sporadic changes to transient Atoll-states. There a magnetic tower could produce transient jets and high-energy emission.
Romano et al. 2009 (MNRAS):
  • Swift analysis of the first year of monitoring
  • Complete spectral analysis of the data => spectra well fitted with either an absorbed power law or an absorbed black body
  • Study of UVOT light curves
  • duty cycle of inactivity = 28% => true quiescence is a rare state
Romano et al. 2010 (MNRAS):
  • Swift monitoring
  • Typical properties of SFXTs during its 2010-June outburst:
    • dynamical range of ~1600 in its flux variations
    • hard power law index, high energy cut off in its spectra
    • harder spectra for brighter states
  • B field < 3e12 G based on the constraint they get on the high energy cut-off.
Bozzo et al. 2011 (A&A):
  • long XMM-Newton observation + re-analysis of previous Swift and ASCA data
  • Bright flare in XMM observation
  • Full time-resolved spectral analysis => X-ray flare probably due to accretion of a massive clump
  • Mass and radius of clump = 1.4 x 1022g and 8 x 1011 cm
  • Temporal analysis of XMM data do not reveal the presence of the previously reported ~4.7s pulsation
  • Re-analysis archival ASCA and Swift data => the pulsation was in fact due in one case to statistical fluctuations and instrumental effects in the other case.

Last updated 30 june 2011

Jerome Rodriguez