|
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| Miscellaneous :
|
| Rodriguez et al. 2003: NH=2.1 x 1023 cm-2 |
|
| Lutovinov et al. 2005: Soft X-ray pulsations at 1309
+-40s in XMM, and 1295 +-50 s in ASCA |
|
| Corbet et al. 2005: Orbital period of 8.96+/-0.01 days in Swift/BAT (ATel #649) |
|
Rodriguez et al. 2006: - Confirm the presence of X-ray pulsations
at ~1300 s, detected above 20 keV with INTEGRAL
- Pulse fraction = constant with energy, <=> model of polar accretion by a pulsar
- Phase resolved spectroscopy =>, pulse solely due to
variations of X-ray flux & not to variations of spectral parameters
- Soft excess (blackbody) with kT~0.07 keV
- Narrow iron line at ~6.4 keV
- Hard X-rays = Compton emission from close vicinity of pulsar
- Soft excess = emission by a collisionally energised cloud in which compact object
is embedded
|
|
Negueruela & Schurch 2006: - 2MASS J16320215-4752289 is indeed the counterpart
- if OB supergiant then extremely reddened
|
|
Chaty et al. 2008: - Optical and infrared observations
- B>22.8, V>24.7, R>22.1, I>22.3, Z>21.7
- J=17.24, H=13.28, Ks=11.21
- Very red Near IR spectrum with absorption and emission lines
- The brackett serie has a P-Cygni profile=>luminous OB sg
|
|
Rahoui et al. 2008: - Medium infrared observations
- SED fitting => AV=35.4, Tstar=33000 K =>
O8 I
- Obscuring material contributes little to MIR spectrum
- Suggested distance 3.5 kpc
|
|
Coleiro et al. (2013) :
- NTT/Sofi NIR Spectroscopy
- Br(7-4) clearly detected with a possible P-Cygni profile. Faint broad He I emission, and another in absorption
- Several absorption lines not associated with physiocal transitions in spectrum
- Stellar companion is a BN0.5 Ia star
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