|
|
| Miscellaneous :
|
|
|
Rodriguez et al. 2008:
- Refined X-ray position
- K=14.159, V> 20.2
- Absorbed power law fits 0.5-9 keV spectra well, Γ= 1.8
NH=5 x1022cm-2; F2-10 keV=6.4 x 10-12 erg/s/cm2
- Galactic source, possible XRB reinforced by position in Sagittarius arm
|
|
Ratti et al. 2010:
- Chandra and Optical observations
- Chandra refined position => refute the previously suggested IR counterpart
- Identify a faint candidate in handra error box, with Ks=16.4 but association with IGR/Chandra source is
discussed
- Chandra source is extended
- Source is a PWN (see also Terrier et al. 2008 AIP vol 1085, p312)
|
|
Gotthelf et al. 2010
ATel 3057 Gotthelf et al. 2011 (ApJ):
- Discovery of 38.52 ms pulsar with RXTE => name PSR J1849-0001
- Association with IGR source based on location and compatibility of X-ray flux
- Confirm the previously proposed pulsar/PWN nature
- Barycentric P = 0.03851893151s and P-dot ~1.40E-14 s/s at epoch MJD 55525.62.
- Spin-down power 9.8E36 erg/s, surface dipole magnetic
field strength 7.5E11 G, and characteristic age 42.9 kyr.
- XMM observation => extended source
- Spectral analysis => NH=4.3 x 1022 cm-2, Γpulsar=1.1, Γnebula=2.1
|
|
Curran et al. 2011(A&A):
- ESO NIR observations
- confirm magnitude (Ks=16.4) of previously suggested counterpart
- Probability of chance superposition 5%
- Source significantly brighter than any other isolated pulsar, hence possibility
of unrelated star cannot be firmly rejected
|
|