Rubens C. Reis

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Substance P (SP) is a neuropeptide that can modulate inflammatory mediator release through activation of NK(1) receptors (NK(1)R). Some studies have also suggested the involvement of SP in lipopolysaccharide (LPS)-induced fever. However, the precise contribution of this neuropeptide to the pathways activated during fever is unknown. In this study we(More)
We present a systematic study of GX 339-4 in both its very high and low hard states from simultaneous observations made with XMM-Newton and RXTE in 2004 and 2006. The X-ray spectra of both these extreme states exhibit strong reflection signatures, with a broad, skewed Fe-Kα line clearly visible above the continuum. Using a newly developed, self-consistent(More)
We have compared the 2001 XMM–Newton spectra of the stellar mass black hole binary XTE J1650−500 and the active galaxy MCG–6-30-15, focusing on the broad, excess emission features at ∼4–7 keV displayed by both sources. Such features are frequently observed in both low-mass X-ray binaries and active galactic nuclei (AGN). For the former case it is generally(More)
The spin of Cygnus X-1 is measured by fitting reflection models to Suzaku data covering the energy band 0.9–400 keV. The inner radius of the accretion disc is found to lie within 2 gravitational radii (rg = GM/c2), and a value of 0.97+0.014 −0.02 is obtained for the dimensionless black hole spin. This agrees with recent measurements using the continuum(More)
We report on the detection of a thermal disc component from the stellar-mass black hole binary XTE J1118+480 in the canonical low/hard state. The presence of a thermal component with a temperature of approximately 0.21 keV in the Chandra spectra of XTE J1118+480 is found at more than the 14σ confidence level. Based on this evidence, we argue that the(More)
Observations over the past 20 years have revealed a strong relationship between the properties of the supermassive black hole (SMBH) lying at the center of a galaxy and the host galaxy itself. The magnitude of the spin of the black hole will play a key role in determining the nature of this relationship. To date, direct estimates of black hole spin have(More)
The XMM–Newton spectrum of the black hole candidate XTE J1652−453 shows a broad and strong Fe Kα emission line, generally believed to originate from reflection of the inner accretion disc. These data have been analysed by Hiemstra et al. using a variety of phenomenological models. We re-examine the spectrum with a self-consistent relativistic reflection(More)
Soft, potentially thermal spectral components observed in some ULXs can be fit with models for emission from cool, optically-thick accretion disks. If that description is correct, the low temperatures that are observed imply accretion onto “intermediate-mass” black holes. Subsequent work has found that these components may follow an inverse relationship(More)
In the microquasar V4641 Sgr the spin of the black hole is thought to be misaligned with the binary orbital axis. The accretion disc aligns with the black hole spin by the Lense-Thirring effect near to the black hole and further out becomes aligned with the binary orbital axis. The inclination of the radio jets and the FeKα line profile have both been used(More)
We have analysed all the good quality XMM–Newton data publicly available for the bright ultraluminous X-ray sources Holmberg IX X-1 and NGC 1313 X-1, with the aim of searching for discrete emission or absorption features in the Fe K band that could provide observational evidence for the massive outflows predicted if these sources are accreting at(More)