Fast X-ray transients towards the Galactic bulge with the Rossi X-ray Timing Explorer

In X-ray binaries, rapid variability in X-ray flux of greater than an order of magnitude on time-scales of a day or less appears to be a signature of wind accretion from a supergiant companion. When the variability takes the form of rare, brief, bright outbursts with only faint emission between them, the systems are called supergiant fast X-ray transients (SFXTs). We present data from twice-weekly scans of the Galactic bulge by the Rossi X-ray Timing Explorer that allow us to compare the behaviour of known SFXTs and possible SFXT candidates with the persistently bright supergiant X-ray binary 4U 1700−377. We independently confirm the orbital periods reported by other groups for SFXTs SAX J1818.6−1703 and IGR J17544−2619. The new data do not independently reproduce the orbital period reported for XTE J1739−302, but slightly improve the significance of the original result when the data are combined. The bulge source XTE J1743−363 shows a combination of fast variability and a long-term decline in activity, the latter behaviour not being characteristic of supergiant X-ray binaries. A far-red spectrum of the companion suggests that it is a symbiotic neutron star binary rather than a high-mass binary, and the reddest known of this class: the spectral type is approximately M8 III.

Luminosity dependent accretion state change in GRO J1008–57

In a former publication, we have analyzed the transient neutron star X-ray binary GRO J1008–57 using all available RXTE-, Swift-, and Suzaku-data. As we have found, the source’s spectral components, i.e., a power-law with high exponential cutoff and a black-body, are strongly correlated with the hard X-ray flux (15–50 keV). We update the analytical description of these dependence, including a change in the photon index behaviour from a flat to a logarithmic function. The flux, where the change occurs, is consistent with the onset of the black-body emission. Thus, a change of the accretion state always occurs in GRO J1008–57 at a particular flux level.

The accretion environment in Vela X-1 during a flaring period using XMM-Newton

We present analysis of 100 ks contiguous XMM-Newton data of the prototypical wind accretor Vela X-1. The observation covered eclipse egress between orbital phases 0.134 and 0.265, during which a giant flare took place, enabling us to study the spectral properties both outside and during the flare. This giant flare with a peak luminosity of 3.92+0.42-0.09 × 1037 erg s-1 allows estimates of the physical parameters of the accreted structure with a mass of ~1021 g. We have been able to model several contributions to the observed spectrum with a phenomenological model formed by three absorbed power laws plus three emission lines. After analysing the variations with orbital phase of the column density of each component, as well as those in the Fe and Ni fluorescence lines, we provide a physical interpretation for each spectral component. Meanwhile, the first two components are two aspects of the principal accretion component from the surface of the neutron star, the third component seems to be the X-ray light echo formed in the stellar wind of the companion.

Pulse phase-coherent timing and spectroscopy of CXOU J164710.2−45521 outbursts

We present a long-term phase-coherent timing analysis and pulse-phase resolved spectroscopy for the two outbursts observed from the transient anomalous X-ray pulsar CXOU J164710.2−455216. For the first outburst we used 11 Chandra and XMM–Newton observations between 2006 September and 2009 August, the longest baseline yet for this source. We obtain a coherent timing solution with P = 10.61065583(4) s, Ṗ = 9.72(1) × 10−13 s s−1 and P̈ = –1.05(5) × 10−20 s s−2. Under the standard assumptions this implies a surface dipolar magnetic field of ∼1014 G, confirming this source as a standard B magnetar. We also study the evolution of the pulse profile (shape, intensity and pulsed fraction) as a function of time and energy. Using the phase-coherent timing solution we perform a phase-resolved spectroscopy analysis, following the spectral evolution of pulse-phase features, which hints at the physical processes taking place on the star. The results are discussed from the perspective of magnetothermal evolution models and the untwisting magnetosphere model. Finally, we present similar analysis for the second, less intense, 2011 outburst. For the timing analysis we used Swift data together with 2 XMM–Newton and Chandra pointings. The results inferred for both outbursts are compared and briefly discussed in a more general framework.

An XMM-Newton view of FeKα in high-mass X-ray binaries

We present a comprehensive analysis of the whole sample of available XMM-Newton observations of high-mass X-ray binaries (HMXBs) until August 2013, focusing on the FeKα emission line. This line is key to better understanding the physical properties of the material surrounding the X-ray source within a few stellar radii (the circumstellar medium). We collected observations from 46 HMXBs and detected FeKα in 21 of them. We used the standard classification of HMXBs to divide the sample into different groups. We find that (1) different classes of HMXBs display different qualitative behaviours in the FeKα spectral region. This is visible especially in SGXBs (showing ubiquitous Fe fluorescence but not recombination Fe lines) and in γ Cass analogues (showing both fluorescent and recombination Fe lines). (2) FeKα is centred at a mean value of 6.42 keV. Considering the instrumental and fits uncertainties, this value is compatible with ionization states that are lower than Fe xviii. (3) The flux of the continuum is well correlated with the flux of the line, as expected. Eclipse observations show that the Fe fluorescence emission comes from an extended region surrounding the X-ray source. (4) We observe an inverse correlation between the X-ray luminosity and the equivalent width of FeKα (EW). This phenomenon is known as the X-ray Baldwin effect. (5) FeKα is narrow (σline< 0.15 keV), reflecting that the reprocessing material does not move at high speeds. We attempt to explain the broadness of the line in terms of three possible broadening phenomena: line blending, Compton scattering, and Doppler shifts (with velocities of the reprocessing material V ~ 1000 km s-1). (6) The equivalent hydrogen column (NH) directly correlates to the EW of FeKα, displaying clear similarities to numerical simulations. It highlights the strong link between the absorbing and the fluorescent matter. (7) The observed NH in supergiant X-ray binaries (SGXBs) is in general higher than in supergiant fast X-ray transients (SFXTs). We suggest two possible explanations: different orbital configurations or a different interaction compact object – wind. (8) Finally, we analysed the sources IGR J16320-4751 and 4U 1700-37 in more detail, covering several orbital phases. The observed variation in NH between phases is compatible with the absorption produced by the wind of their optical companions. The results clearly point to a very important contribution of the donor’s wind in the FeKα emission and the absorption when the donor is a supergiant massive star.

La tagatose-1,6-bisphosphate aldolase et la fructose-1,6-bisphosphate aldolase de classe I : mécanisme et stéréospécificité

La tagatose-1,6-biphosphate aldolase de Streptococcus pyogenes est une aldolase qui fait preuve d'un remarquable manque de spécificité vis à vis de ses substrats. En effet, elle catalyse le clivage réversible du tagatose-1,6-bisphosphate (TBP), mais également du fructose-1,6-bisphosphate (FBP), du sorbose-1,6-bisphosphate et du psicose-1,6-bisphosphate, quatre stéréoisomères, en dihydroxyacétone phosphate (DHAP) et en glycéraldéhyde-3-phosphate (G3P). Aldolase de classe I, qui donc catalyse sa réaction en formant un intermédiaire covalent obligatoire, ou base de Schiff, avec son susbtrat, la TBP aldolase de S. pyogenes partage 14 % d’identité avec l’enzyme modèle de cette famille, la FBP aldolase de muscle de mammifère. Bien que le mécanime catalytique de la FBP aldolase des mammifères ait été examiné en détails et qu’il soit approprié d’en tirer des renseignements quant à celui de la TBP aldolase, le manque singulier de stéréospécificité de cette dernière tant dans le sens du clivage que celui de la condensation n’est toujours pas éclairci. Afin de mettre à jour les caractéristiques du mécanisme enzymatique, une étude structurale de la TBP aldolase de S. pyogenes, un pathogène humain extrêmement versatile, a été entreprise. Elle a permis la résolution des structures de l’enzyme native et mutée, en complexe avec des subtrats et des inhibiteurs compétitifs, à des résolutions comprises entre 1.8 Å et 2.5 Å. Le trempage des cristaux de TBP aldolase native et mutante dans une solution saturante de FBP ou TBP a en outre permis de piéger un authentique intermédiaire covalent lié à la Lys205, la lysine catalytique. La determination des profils pH de la TBP aldolase native et mutée, entreprise afin d'évaluer l’influence du pH sur la réaction de clivage du FBP et TBP et ìdentifier le(s) résidu(s) impliqué(s), en conjonction avec les données structurales apportées par la cristallographie, ont permis d’identifier sans équivoque Glu163 comme résidu responsable du clivage. En effet, le mode de liaison sensiblement différent des ligands utilisés selon la stéréochimie en leur C3 et C4 permet à Glu163, équivalent à Glu187 dans la FBP aldolase de classe I, d’abstraire le proton sur l’hydroxyle du C4 et ainsi d’amorcer le clivage du lien C3-C4. L’étude du mécanimse inverse, celui de la condensation, grâce par exemple à la structure de l’enzyme native en complexe avec ses substrats à trois carbones le DHAP et le G3P, a en outre permis d’identifier un isomérisme du substrat G3P comme possible cause de la synthèse des isomères en C4 par cette enzyme. Ce résultat, ainsi que la decouverte d’un possible isomérisme cis-trans autour du lien C2-C3 de la base de Schiff formée avec le DHAP, identifié précedemment, permet de cerner presque complètement les particularités du mécanisme de cette enzyme et d’expliquer comment elle est capable de synthétiser les quatres stéréoisomères 3(S/R), 4(S/R). De plus, la résolution de ces structures a permis de mettre en évidence trois régions très mobiles de la protéine, ce qui pourrait être relié au rôle postulé de son isozyme chez S. pyogenes dans la régulation de l’expression génétique et de la virulence de la bactérie. Enfin, la résolution de la structure du mutant Lys229→Met de la FBP aldolase de muscle en complexe avec la forme cyclique du FBP, de même que des études cristallographiques sur le mutant équivalent Lys205→Met de la TBP aldolase de S. pyogenes et des expériences de calorimétrie ont permis d’identifier deux résidus particuliers, Ala31 et Asp33 chez la FBP aldolase, comme possible cause de la discrimination de cette enzyme contre les substrats 3(R) et 4(S), et ce par encombrement stérique des substrats cycliques. La cristallographie par rayons X et la cinétique enzymatique ont ainsi permis d'avancer dans l'élucidation du mécanisme et des propriétés structurales de cette enzyme aux caractéristiques particulières.

International Conference on the Physics of X-Ray Spectra program and extended abstracts.

Mode of access: Internet.

Course manual for X-ray measurements (GS-462).

Mode of access: Internet.

Nationwide evaluation of X-ray trends : NEXT.

Mode of access: Internet.

Surgery, its principles and practice,

"The first six volumes of this work recorded the progress of Surgery down to 1913. Then came the Great War ... Hence, immediately after the Armistice ... I began to assemble a full staff of experts, whose work appears in Volumes VII and VIII."--Preface, v.7, 1921.

BRH routine compliance testing for diagnostic x-ray systems or components of diagnostic x-ray systems to which 21 CFR subchapter J is applicable.

Supersedes HEW publication (FDA) 75-8012.

Evaluation of MDH model 1015 x-ray monitor /

Mode of access: Internet.

A study of fluorescent excitation using isotopic X-ray emission /

"ORO-627; Isotopes - Industrial technology; (TID-4500, 43rd. ed)."

X ray wavelengths /

"Contract No. AT(30-1)-2543."

The negation of squid embryo tropisms by x-radiation /

"3-20-50--525-A201183."