|
|
| 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.
|
|
|