With these properties, the XRT imaging locates the position of the burst with 5 arcsec accuracy within ten seconds of the target acquisition (for a typical GRB) and then continues

(2007) suggested (based on observations of two ULXs in NGC 1313) that the PL-type state may be representative of the very high state observed in Galactic black hole X-ray

The first X-ray observation of IC342 from Einstein (Fabbiano & Trinchieri 1987) showed that the X-ray emission was dominated by three ultraluminous X-ray sources (ULXs) which

The discovery of the long sought powerful winds in ULXs provides further sup- port to the scenario of super-Eddington accretion and in this paper we discuss the relevance of

We perform a Gaussian line search in SPEX to find any spectral lines, both absorption and emission, that a possible outflow might have imprinted on the X-ray continuum of the

For cos( i ) = 0.0, in the Galactic extinction corrected case the mass and radius constraints listed in Table 7 constrain the allowable companion star types to O V, OB III, or early

have shown that the neutron star accretion rate expected from Be-type mass ejection is large enough to power the observed X-ray luminosity. Corbet (1984, 1986) has shown that

But as more observations were made, the data did not appear consistent with this scenario, and instead, lower-mass black holes accreting at super-Eddington luminosities were favored

Additionally, Feng & Kaaret (2010) (here- after F10) observed the source with XMM-Newton and Chandra over the course of a flaring episode and fitted the spectra with the

This sample shows a large deficit in the number of ULXs detected per unit SFR (0.2 versus 2 ULXs, per M  yr −1 ) compared to the detection rate in nearby (D L < 14.5 Mpc)

Soft, potentially thermal spectral components observed in some ultra-luminous X-ray sources (ULXs) can be fit with models for emission from cool, optically thick accretion disks..

Simultaneous broadband observations with XMM-Newton and NuSTAR will permit us to better constrain the source nature by, for example, testing the existence of a third,

We study the spectra mainly in terms of a two-component model consisting of a cool multi-colour disc blackbody and a hotter Comptonised medium (diskbb + comptt in xspec), but

Given that the numbers of massive star-forming systems similar to LIRGs increase to peak at redshifts ∼ 1, this implies that understanding the concealment of X-ray source populations

We study the spectra mainly in terms of a two-component model consisting of a cool MCD blackbody and a hotter Comptonized medium ( DISKBB + COMPTT in XSPEC ), but the requirement for

The search for a wind in this object is highly motivated by the detection of soft X-ray residuals in the EPIC spectra of NGC 55 ULX that are simi- lar in both shape and energy ( ∼1

Using all the archival XMM-Newton X-ray (3–10 keV) observations of the ultraluminous X-ray source (ULX) M82 X−1, we searched for a correlation between its variable mHz

Background AGN or Star Clusters Candidates 16 of the 96 ULXs in this search for Spitzer /IRAC mid-IR ULX counterparts were detected with absolute magnitudes brighter than expected