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X-ray observations: light curves XMM Feng & Kaaret 2006
X-ray observations: spectroscopy • light curves • observed since EINSTEIN • variability on time scales from days to months to years • maximum Lx up to 3x10 40 erg/s • X-ray spectra • can be fitted with a power-law (Γ~2.3, 63%) plus a cool accretion disk (~160 eV, 37%) suggestive of a IMBH of ~10 3 Ms (Miller et al. 2003) • but the cool accretion disk component is dominated by the power-law component, and the fit is not unique • it can also be fitted with a power-law (Γ~2.9,64%) plus a hot disk (~2.7 keV, 36%). (Stobbart et al. 2006)
Page 1 and 2: Optical studies of an ultraluminous
Page 3 and 4: ultraluminous X-ray sources
Page 5 and 6: ultraluminous X-ray sources • ULX
Page 7 and 8: ultraluminous X-ray sources • ULX
Page 9 and 10: ULXs in NGC1313 • a barred SB(s)d
Page 11: X-ray observations: light curves Za
Page 15 and 16: optical observations ESO 3.6m R cou
Page 17 and 18: optical observations
Page 19 and 20: optical observations: astrometry
Page 21 and 22: optical observations: astrometry x3
Page 23 and 24: optical observations: astrometry
Page 25 and 26: optical observations: environments
Page 27 and 28: optical observations: photometry
Page 29 and 30: optical observations: variability
Page 31 and 32: color-magnitude diagrams • two po
Page 33 and 34: spectral energy distribution
Page 35 and 36: spectral energy distribution
Page 37 and 38: IMBH formation
Page 39 and 40: IMBH formation • if an IMBH, cann
Page 41 and 42: IMBH formation • if an IMBH, cann
Page 43 and 44: adial velocity
Page 45 and 46: adial velocity Pakull et al. 2006 H
Page 47 and 48: adial velocity • if He II line fr
Page 49 and 50: adial velocity • if He II line fr
Page 51: adial velocity • if He II line fr

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