|
|
| Miscellaneous :
|
|
| Halpern & Gotthelf (2006, ATel:688): identify AX J1845.0-0433 as
the likely counterpart.
|
|
Sguera et al. (2007, A&A): - INTEGRAL and Swift observations
- fast flaring activity on timescale few tens of minutes
- 2 outbursts seen by INTEGRAL
- 2 other outbursts seen by Swift
- refined Swift position confirms associations with the ASCA source
- COnfirmation of HMXB nature => SFXT, and recurrent transient behaviour
|
|
Zurita Heras & Walter (2009, A&A): - INTEGRAL and Swift observations
- INTEGRAL and XMM-Newton observations
- Confirm the O9.5 I nature of the companion
- Quiescent luminosity L(0.2-100 keV) ~ 1e35 erg/s seen with both satellites
- Binary separation of ~3 Rstar (higher than in other known supergiant HMXB)
- 2 bright and short flares (XMM) reaching L~1e36 erg/s => maximum variability factor of 50
on time scale ~few hundreds of seconds
- Broad-band spectrum typical of wind-fed accreting pulsars: absorbed cut-off power law with
NH= 2.6 x 1022 cm-2, Γ=0.7-0.9 and Ecut=16 keV
- Soft excess fitted with a black body kT=0.18 keV
- Optically-thin and highly-ionised iron (Fe XVIII-XIX) detected during quiescence.
- Flare characteristics suggest massive clumps are formed within the stellar wind of Sg companion
|
|
|