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| Miscellaneous :
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Paizis et al. 2005 Atel 458 :
X-ray flux increase by factor of ~2 in ~5 days |
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Kennea et al. 2005 Atel 459 : Highly absorbed in X-rays, no detected flux below 1.5 keV |
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Rodriguez & Paizis 2005 Atel 460
: - Ks = 13.95 +- 0.058,J > 16.8 , H > 15.8 (95% lower limits)
- Infrared image can be found here (courtesy
J. Rodriguez)
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Markwardt et al. 2005 Atel 465:
- RXTE spectra absorbed NH~4-5 1022 cm-2
- Γ = 0.8-1.1
- No pulsations
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Steeghs et al. 2005 Atel 478:
- several sources in the Swift error circle
- 2 MASS candidate counterpart is a blend of sources
- Preliminary relative photometry -> K~14.1 for the brightest source resolved in
Magellan/PANIC images, consistent with the K=14 2MASS source
- A comparison between the 2MASS field and the 300s PANIC K-band image is available
here (courtesy D.
Steeghs)
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Beckmann et al. 2005 (ApJ):
- Variable absorption NH~4-1722 cm-2
- Flat spectrum Γ = 1
- New member of highly absorbed HMXB
- 3-σ upper limit on the flux of a 6.4 keV line is 3 x 10-4
ph/cm2 with an EW < 600 eV
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Pelizza et al. 2011 (A&A):
- optical/IR observations with the ESO-NTT.
- 3 candidate counterparts are located within the Swift error circle
- Brightest (2MASS J16281083-4838560) is the most likely counterpart
has parameters typical of supergiant O or B stars.
- Distance to the source estimated to be in the range of 13.6 to 21.6 kpc.
- Source is a member of the highly-obscured HMXBs with supergiant companions.
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Cusumano et al. 2013 (ApJ):
- Analysis of Swift BAT monitoring and Swift XRT pointings
- Discovery of orbital period P=287.6 days in BAT data
- Broad band X-ray spectral analysis of 2 different phases=> absorbed cut-off power law
NH=11-18 x 1022 cm-2, Γ=0-1.3, Ecut=12-27 keV
- Source is an HMXB, probably with Be companion
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