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| Miscellaneous :
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Keek et al. 2006 ATel 810:
- 20-60 keV Flux = 0.97 mCrab
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Malizia et al. 2007:
- Swift observations
- NH=1.3 1022 cm-2, Γ=2.2
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Tomsick et al. 2009:
- Chandra observation => 1.5 arcmin extended source
- source is a SNR. significant structure at the centre of the SNR => PWN. At the
centre lies a point source that could be the putative neutron star.
- Emission detected by INTEGRAL =likely the PWN or the SNR
- Spectra extracted from a 1.5' circular region centred on the point source
well fitted with absorbed power law: NH=3.1 x1022
cm-2 Γ=1.83
- Non detection at TeV energies
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Renaud et al. 2010:
- RXTE, Chandra, INTEGRAL, Radio observations
- RXTE => pulsation at 31.18 ms source iss a ms pulsar
- The pulsar at the centre of a G310.6-1.6 classified as a PWN.
- Pulsar detected in radio band, pulsed emission as well
- MGPS 140045-632542 is the radio counterpart of the PWN
- Not detected by Fermi
- Spin down luminosity of 5.1x1037 erg/s => surface magnetic field 1.1 1012 G.
- Source lies at about 7 kpc, and quite young (<~1000 yr).
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Curran et al. 2011:
- ESO NIR/Optical observations of the field
- No counterpart detected down to Ks>17.2, H>18.0, J>19.2, i>21.2, R>21.0, V>21.8, B>22.3
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