| Miscellaneous :
| Zand & Heise 2004 (Atel 362) & Swank and Markwardt
2004 (Atel 359)
- NH~9 X 1022 cm-2
- Gamma ~1.9 - 2.3
- Pulsations at 161.76 ± 0.01 sec
- possible orbital period of 52.5d (Atel 362)
| Torrejon & Negueruela (Atel 370)
- Not associated with 1RXS J114358.1-610736
- Magnitudes of USNO-B1.0 0288-0337948 (Be star of spectral type ~B3): B2=13.17, R2=12.95, I=11.61
| Corbet & Remillard (Atel 377)
Orbital period confirmed at 52.46 ± 0.06 days with RXTE/ASM
| Wen et al. 2006 (ApJS)
Orbital period confirmed at 52.36 days with RXTE/ASM
| Tomsick et al. 2007 (ATel 1231)
- Chandra observations:
- Energy spectrum consistent with an absorbed power-law, Γ=~1.0,
NH~10 e22 cm-2
- 0.3-10 keV flux 4.8e-12 ergs/cm2/s.
- USNO-B1.0 0288-0337502 = UCAC 04813819 = 2MASS J11440030-6107364 = DENIS J114400.2-610736 very probable counterpart.
- B = 16.6, R = 15.7, and I = 14.8 in USNO, J = 13.00 , H = 12.34, and K = 11.852 in 2MASS
and I = 14.5, J = 13.02, and K = 11.81 in DENIS
- Counterpart is an HMXB
- Significant amount of the absorption is intrinsic to the source.
- USNO-B1.0 0288-0337948 is not the counterpart, no X-ray emission is found
in the chandra observation at this position
| Negueruela et al. 2007 (ATel 1239)
- confirm the identification of 2MASS J11440030-6107364
= USNO-B1.0 0288-0337502 as the correct counterpart.
- Spectroscopic SAAO 1.9-m telescope observations of
- Below 5000A the source is too faint to be detected. The
5000-7800A spectrum shows a strong H-alpha emission line on top of a reddened
- -26A EW and lack of any other obvious stellar
features => source is an obscured
Be star, compatible with the position of IGR J11435-6109 in the Corbet diagram.
- NTT=>B=17.71, V=16.43, R=15.44.
- Even for a B2Ve counterpart the source is at least at 6 kpc.
| Tomsick et al. 2008:
- Absorbed power law, NH=15x1022 cm-2,
Γ= 1.1, Unabs. 0.3-10 keV flux=9.1 e-12 erg/cm2/s
- if d>6kpc => L0.3-10 keV > 3e34 erg/s
| Masetti et al. 2009:
- Optical spectroscopy
- Av~5.7, d~8.6 kpc
- B2 III or B0 V counterpart
| Coleiro et al. (2013) :|
- NTT/Sofi NIR Spectroscopy
- Several lines in spectra among which possible He I, Mg II, He II, and possibly N III, CIII and Fe II in emission
- Possible [Fe II] line in H-band spectrum
- Spectrum similar to IGR J10101-5654, but fewer lines, and not some typical lines of B[e] star are not observed
- Companion star suggested to be a B0.5Ve
- Broad band SED fitted with 2 black bodies => Av=7.98, Tdust=925.6 K
- Relatively weak mIR excess probably due to bremsstrahlung coming decretion disk of Be star