The Ultraluminous X‐Ray Source NGC 1313 X‐2 (MS 0317.7−6647) and Its Environment

Zampieri, L.; Mucciarelli, P.; Falomo, R.; Kaaret, Philip; Stefano, Rosanne Di; Turolla, R.; Chieregato, M.; Treves, A.

doi:10.1086/381541

Cited by 66 publications

(89 citation statements)

References 41 publications

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“…Further attention should be paid to minimize the effects of possible absolute calibration uncertainties. We then decided to perform differential photometry of the target with respect to a nearby field star (star D in Zampieri et al 2004), located on the same chip in both instruments. The reference star is brighter than the target and has a low root mean square variability (∼ 0.05 mag in the VLT and < ∼ 0.02 mag in the HST exposures).…”

Section: Vlt and Hst Observationsmentioning

confidence: 99%

Optical variability of the ultraluminous X‐ray source NGC 1313 X‐2

Impiombato¹,

Zampieri²,

Falomo³

et al. 2011

Astron Nachr

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Section: Vlt and Hst Observationsmentioning

confidence: 99%

Optical variability of the ultraluminous X‐ray source NGC 1313 X‐2

Impiombato¹,

Zampieri²,

Falomo³

et al. 2011

Astron Nachr

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“…Pakull & Mirioni (2002) observed 15 ULXs in 11 galaxies, and found 13 ULXs associated with well-defined H ii regions and emission nebulae. With the superb spatial resolution and sensitivity of HST, some ULXs have been identified to young massive stars in star-forming regions, e.g., the ULX in M81 to an O8 V star (Liu et al 2002b), the ULX in NGC 5204 to a B0 Ib supergiant (Liu et al 2004), the ULX in Holmberg II to a young star with spectral type between O4 V and B3 Ib (Kaaret et al 2004), the ULX in NGC 1313 to a star of 15-20 M (Zampieri et al 2004), and the ULX in NGC 4559 to four young supergiants (Soria et al 2005). In comparison, only a few ULXs are reported to associate with globular clusters, e.g., the ULX in NGC 4565 (Wu et al 2002), and the two ULXs in NGC 1399 (Angelini et al 2001).…”

Section: Young and Old Ulx Populationsmentioning

confidence: 99%

Ultraluminous X‐Ray Sources in Nearby Galaxies fromROSATHRI Observations. II. Statistical Properties

Liu

Bregman

Irwin

2006

ApJ

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The statistical properties of the nonnuclear X-ray point sources from the ROSAT HRI survey of nearby galaxies in Paper I are studied, with particular attention to the contamination from background and/or foreground objects. This study reveals a statistical preference for the ultraluminous X-ray sources (ULXs) to occur in late-type galaxies over early-type galaxies, and in starburst/H ii galaxies over nonstarburst galaxies. There is a trend of greater occurrence frequencies and ULX rates for galaxies with increasing star formation rates, confirming the connection between the ULX phenomenon and the star formation. A nonlinear correlation is found between the number of ULXs and the star formation rate, with significantly more ULXs at low star formation rates than the ULX population expected from the high-mass X-ray binaries (HMXBs) as an indicator of the star formation and the accompanying young stellar population, suggestive of another population of ULXs associated with the low-mass X-ray binaries (LMXBs) and the old stellar population. There are no breaks around 10 39 ergs s À1 in the luminosity functions of ULXs in all galaxies or in late-type galaxies, suggesting the regular ULXs below 10 40 ergs s À1 are a high-luminosity extension of the ordinary HMXB/LMXB populations below 10 39 ergs s À1 . There is evidence that the extreme ULXs above 10 40 ergs s À1 might be a different ULX class from the regular ULXs below 10 40 ergs s À1 , although a larger sample with more ULXs is needed to establish the statistical properties of the extreme ULXs as a class.

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“…Left: Multicolor image (including Hα) of the 400 pc diameter bubble around the ULX NGC 1313 X-2. The Chandra error circle includes a close pair of stars (star C in Zampieri et al 2004). The N-W component is the optical counterpart.…”

Section: Clustersmentioning

confidence: 99%

Ultraluminous X-ray Sources: Bubbles and Optical Counterparts

2005

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Abstract. Optical studies of ultraluminous X-ray sources (ULX) in nearby galaxies have turned out to be instrumental in discriminating between various models including the much advertised intermediate mass black hole hypothesis and various beaming scenarios. Here we report on ESO VLT and SUBARU observations of ULX that have revealed the parent stellar clusters with ages of some 60 million years in two cases. Thus we are able to derive upper limits of about 8 M for the mass donors in these systems. The optical counterparts are dominated by X-ray heated accretion disks, and the discovery of the He II λ4686 emission line now allows to derive dynamical masses in these systems. Apparent radial velocity variations of 300 km/s have been detected in NGC 1313 X-2 which, if confirmed by further observations, would exclude the presence of IMBH in these systems.

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The Ultraluminous X‐Ray Source NGC 1313 X‐2 (MS 0317.7−6647) and Its Environment

Cited by 66 publications

References 41 publications

Optical variability of the ultraluminous X‐ray source NGC 1313 X‐2

Optical variability of the ultraluminous X‐ray source NGC 1313 X‐2

Ultraluminous X‐Ray Sources in Nearby Galaxies fromROSATHRI Observations. II. Statistical Properties

Ultraluminous X-ray Sources: Bubbles and Optical Counterparts

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