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See detailK voprosou bidelenii fatsii zoubtchatogo moustié na materialakh pamyatnikov sredneï azii
Krivoshapkin, A.; Kolobova, K.; Pavlenok, K. et al

Scientific conference (2011)

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See detailK+ Production in a Cascade Model for High Energy Nucleus-Nucleus Collisions
Cugnon, Joseph ULiege; Lombard

in Nuclear Physics A (1984), 422

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See detailLe K-ABC utilisé avec des enfants trisomiques 21 : Un essai d’adaptation
Frenkel, Stéphanie ULiege; Bourdin, Béatrice; Vandromme, Luc

Conference (2001)

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See detailLe K-ABC utilisé avec des enfants trisomiques 21 : Un essai d’adaptation
Frenkel, Stéphanie ULiege; Bourdin, Béatrice; Vandromme, luc

in Vivicorsi, Bruno; Collet, R. (Eds.) Handicap, cognition et prise en charge individuelle : des aspects de la recherche au respect de la personne (2005)

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See detailK-excess, an unexploited method for discovering red quasars
Nakos, T.; Willis, J.; Andreon, S. et al

Conference (2006, May 19)

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See detailK-shell photoabsorption and photoionization of trace elements. I. Isoelectronic sequences with electron number 3 <= N <= 11
Palmeri, P.; Quinet, Pascal ULiege; Bautista, M.A. et al

in Astronomy and Astrophysics (2016), 589

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See detailK-shell photoabsorption and photoionization of trace elements: II. Isoelectronic sequences with electron number 12 ≤ N ≤ 18
Mendoza, C.; Bautista, M. A.; Palmeri, P. et al

in Astronomy and Astrophysics (2017), 604

Context. We are concerned with improving the diagnostic potential of the K lines and edges of elements with low cosmic abundances, namely F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn, that are ... [more ▼]

Context. We are concerned with improving the diagnostic potential of the K lines and edges of elements with low cosmic abundances, namely F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn, that are observed in the X-ray spectra of supernova remnants, galaxy clusters, and accreting black holes and neutron stars. Aims. Since accurate photoabsorption and photoionization cross sections are needed in their spectral models, they have been computed for isoelectronic sequences with electron number 12 ≤ N ≤ 18 using a multi-channel method. Methods. Target representations are obtained with the atomic structure code autostructure, and ground-state cross sections are computed with the Breit-Pauli R-matrix method (bprm) in intermediate coupling, including damping (radiative and Auger) effects. Results. Following the findings in our earlier work on sequences with 2 ≤ N ≤ 11, the contributions from channels associated with the 2s-hole [2s]μ target configurations and those containing 3d orbitals are studied in the Mg (N = 12) and Ar (N = 18) isoelectronic sequences. Cross sections for the latter ions are also calculated in the isolated-resonance approximation as implemented in autostructure and compared with bprm to test their accuracy. Conclusions. It is confirmed that the collisional channels associated with the [2s]μ target configurations must be taken into account owing to significant increases in the monotonic background cross section between the L and K edges. Target configurations with 3d orbitals give rise to fairly conspicuous unresolved transition arrays in the L-edge region, but to a much lesser extent in the K-edge that is our main concern; therefore, they have been neglected throughout owing to their computationally intractable channel inventory, thus allowing the computation of cross sections for all the ions with 12 ≤ N ≤ 18 in intermediate coupling with bprm. We find that the isolated-resonance approximations performs satisfactorily and will be our best choice to tackle the systems with ground configuration 3p63dm (3 ≤ m ≤ 8) in isoelectronic sequences with N > 20. © ESO 2017. [less ▲]

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See detailK-shell photoabsorption and photoionization of trace elements: III. Isoelectronic sequences with electron number 19 ≤ N ≤ 26
Mendoza, C.; Bautista, M. A.; Palmeri, P. et al

in Astronomy and Astrophysics (2018), 616

Context. This is the final report of a three-paper series on the K-shell photoabsorption and photoionization of trace elements (low cosmic abundance), namely F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu ... [more ▼]

Context. This is the final report of a three-paper series on the K-shell photoabsorption and photoionization of trace elements (low cosmic abundance), namely F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, and Zn. K lines and edges from such elements are observed in the X-ray spectra of supernova remnants, galaxy clusters, and accreting black holes and neutron stars, their diagnostic potential being limited by poor atomic data. Aims. We here complete the previously reported radiative datasets with new photoabsorption and photoionization cross sections for isoelectronic sequences with electron number 19 = N = 26. We also describe the access to and integrity and usability of the whole resulting atomic database. Methods. Target representations were obtained with the atomic structure code AUTOSTRUCTURE. Where possible, cross sections for ground-configuration states were computed with the Breit Pauli R-matrix method (BPRM) in either intermediate or LS coupling including damping (radiative and Auger) effects; otherwise and more generally, they were generated in the isolated-resonance approximation with AUTOSTRUCTURE. Results. Cross sections were computed with BPRM only for the K (N = 19) and Ca (N = 20) isoelectronic sequences, the latter in LS coupling. For the remaining sequences (21 = N = 26), AUTOSTRUCTURE was run in LS-coupling mode taking into account damping effects. Comparisons between these two methods for K-like Zn xii and Ca-like Zn xi show that to ensure reasonable accuracy, the LS calculations must be performed taking into account the non-fine-structure relativistic corrections. The original data structures of the BPRM and AUTOSTRUCTURE output files, namely photoabsorption and total and partial photoionization cross sections, are maintained but supplemented with files detailing the target (NT-electron system, where NT = N-1) representations and photon states (N-electron system). Conclusions. We conclude that because of the large target size, the photoionization of ions with N > 20 involving inner-shell excitations rapidly leads to untractable BPRM calculations, and is then more effectively treated in the isolated resonance approximation with AUTOSTRUCTURE. This latter approximation by no means involves small calculations as Auger damping must be explicitly specified in the intricate decay routes. © 2018 ESO. [less ▲]

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See detailK-shell photoionization and photoabsorption of Ne, Mg, Si, S, Ar and Ca
Witthoeft, M; Bautista, M A; Mendoza, C et al

in Astrophysical Journal Supplement Series (2009), 182

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See detailK-shell photoionization of highly-charged iron ions under high-density astrophysical plasma conditions
Deprince, J.; Bautista, M.A.; Fritzsche, S. et al

Poster (2019)

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See detailK-shell photoionization of Na-like to Cl)like ions of Mg, Si, S, Ar and Ca
Witthoeft, M; Garcia, J; Kallman, T R et al

in Astrophysical Journal Supplement Series (2011), 192

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See detailK-shell photoionization of Nickel ions using R-matrix
Witthoeft, M C; Bautista, M A; Garcia, J et al

in Astrophysical Journal Supplement Series (2011), 196

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See detailK-Stacker: an algorithm to hack the orbital parameters of planets hidden in high-contrast imaging. First applications to VLT/SPHERE multi-epoch observations
Le Coroller, H.; Nowak, M.; Delorme, P. et al

in Astronomy and Astrophysics (2020), 639

Context. Recent high-contrast imaging surveys, using the Spectro- Polarimetic High contrast imager for Exoplanets REsearch (SPHERE) or the Gemini Planet Imager in search of planets in young, nearby ... [more ▼]

Context. Recent high-contrast imaging surveys, using the Spectro- Polarimetic High contrast imager for Exoplanets REsearch (SPHERE) or the Gemini Planet Imager in search of planets in young, nearby systems, have shown evidence of a small number of giant planets at relatively large separation beyond 10-30 au, where those surveys are the most sensitive. Access to smaller physical separations between 5 and 30 au is the next step for future planet imagers on 10 m telescopes and the next generation of extremely large telescopes in order to bridge the gap with indirect techniques such as radial velocity, transit, and soon astrometry with Gaia. In addition to new technologies and instruments, the development of innovative observing strategies combined with optimized data processing tools is participating in the improvement of detection capabilities at very close angular separation. In that context, we recently proposed a new algorithm, Keplerian-Stacker, which combines multiple observations acquired at different epochs and takes into account the orbital motion of a potential planet present in the images to boost the ultimate detection limit. We showed that this algorithm is able to find planets in time series of simulated images of the SPHERE InfraRed Dual-band Imager and Spectrograph (IRDIS) even when a planet remains undetected at one epoch. <BR /> Aims: Our goal is to test and validate the K-Stacker algorithm performances on real SPHERE datasets to demonstrate the resilience of this algorithm to instrumental speckles and the gain offered in terms of true detection. This will motivate future dedicated multi-epoch observation campaigns of well- chosen, young, nearby systems and very nearby stars carefully selected to search for planets in emitted and reflected light, respectively, to open a new path concerning the observing strategy used with current and future planet imagers. <BR /> Methods: To test K-Stacker, we injected fake planets and scanned the low signal-to-noise ratio (S/N) regime in a series of raw observations obtained by the SPHERE/IRDIS instrument in the course of the SPHERE High-contrast ImagiNg survey for Exoplanets. We also considered the cases of two specific targets intensively monitored during this campaign: β Pictoris and HD 95086. For each target and epoch, the data were reduced using standard angular differential imaging processing techniques and then recombined with K-Stacker to recover the fake planetary signals. In addition, the known exoplanets β Pictoris b and HD 95086 b previously identified at lower S/N in single epochs have also been recovered by K-Stacker. <BR /> Results: We show that K-Stacker achieves a high success rate of ≈100% when the S/N of the planet in the stacked image reaches ≈9. The improvement of the S/N is given as the square root of the total exposure time contained in the data being combined. At S/N < 6-7, the number of false positives is high near the coronagraphic mask, but a chromatic study or astrophysical criteria can help to disentangle between a bright speckle and a true detection. During the blind test and the redetection of HD 95086 b, and β Pic b, we highlightthe ability of K-Stacker to find orbital solutions consistent with those derived by the current Markov chain Monte Carlo orbital fitting techniques. This confirms that in addition to the detection gain, K-Stacker offers the opportunity to characterize the most probable orbital solutions of the exoplanets recovered at low S/N. <P />Based on observations collected at the European Southern Observatory under programs: 095.C-0298, 096.C-0241, 097.C-0865, 198.C-0209, 099.C-0127. [less ▲]

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See detailK-type geomagnetic index nowcast with data quality control
Stankov, Stanimir; Stegen, Koen; Warnant, René ULiege

in Annals of Geophysics (2011), 54(3), 285-295

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See detailThe K1 beta-lactamase of Klebsiella pneumoniae.
Joris, Bernard ULiege; De Meester, F; Galleni, Moreno ULiege et al

in Biochemical Journal (1987), 243(2), 561-7

beta-Lactamase K1 was purified from Klebsiella pneumoniae SC10436. It is very similar to the enzyme produced by Klebsiella aerogenes 1082E and described by Emanuel, Gagnon & Waley [Biochem. J. (1986) 234 ... [more ▼]

beta-Lactamase K1 was purified from Klebsiella pneumoniae SC10436. It is very similar to the enzyme produced by Klebsiella aerogenes 1082E and described by Emanuel, Gagnon & Waley [Biochem. J. (1986) 234, 343-347]. An active-site peptide was isolated after labelling of the enzyme with tritiated beta-iodopenicillanate. A cysteine residue was found just before the active-site serine residue. This result could explain the properties of the enzyme after modification by thiol-blocking reagents. The sequence of the active-site peptide clearly established the enzyme as a class A beta-lactamase. [less ▲]

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See detailThe K2-ESPRINT Project I: Discovery of the Disintegrating Rocky Planet K2-22b with a Cometary Head and Leading Tail
Sanchis-Ojeda, R.; Rappaport, S.; Pallé, E. et al

in Astrophysical Journal (2015), 812(2), 112

We present the discovery of a transiting exoplanet candidate in the K2 Field-1 with an orbital period of 9.1457 hr: K2-22b. The highly variable transit depths, ranging from ∼0% to 1.3%, are suggestive of ... [more ▼]

We present the discovery of a transiting exoplanet candidate in the K2 Field-1 with an orbital period of 9.1457 hr: K2-22b. The highly variable transit depths, ranging from ∼0% to 1.3%, are suggestive of a planet that is disintegrating via the emission of dusty effluents. We characterize the host star as an M-dwarf with Teff ≃ 3800 K. We have obtained ground-based transit measurements with several 1-m class telescopes and with the GTC. These observations (1) improve the transit ephemeris; (2) confirm the variable nature of the transit depths; (3) indicate variations in the transit shapes; and (4) demonstrate clearly that at least on one occasion the transit depths were significantly wavelength dependent. The latter three effects tend to indicate extinction of starlight by dust rather than by any combination of solid bodies. The K2 observations yield a folded light curve with lower time resolution but with substantially better statistical precision compared with the ground-based observations. We detect a significant “bump” just after the transit egress, and a less significant bump just prior to transit ingress. We interpret these bumps in the context of a planet that is not only likely streaming a dust tail behind it, but also has a more prominent leading dust trail that precedes it. This effect is modeled in terms of dust grains that can escape to beyond the planet's Hill sphere and effectively undergo “Roche lobe overflow,” even though the planet's surface is likely underfilling its Roche lobe by a factor of 2. [less ▲]

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See detailKaberdoes
Vromans, Joseph ULiege

in Nederlands Van Nu (1993), 41(5),

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See detailThe Kačák event (late Eifelian, Middle Devonian) on the Belgian shelf and its effects on rugose coral palaeobiodiversity
Jamart, Valentin ULiege; Denayer, Julien ULiege

in Bulletin of Geosciences (2020), 95(3), 279-311

The Devonian is a period that recorded many biocrises. One of them, known as the Kačák event ranges through the Polygnathus ensensis Zone immediately before the Eifelian-Givetian boundary (Middle Devonian ... [more ▼]

The Devonian is a period that recorded many biocrises. One of them, known as the Kačák event ranges through the Polygnathus ensensis Zone immediately before the Eifelian-Givetian boundary (Middle Devonian). This crisis has been identified in many localities worldwide, mostly in bathyal settings. The event, divided into two phases (otomari event and Kačák event s.s.), is typically marked by a turnover among pelagic faunas, especially conodonts, dacryoconarids and ammonoids. This turnover result from a transgression associated with anoxia that generally corresponds to the deposition of black shale in deep-water settings. In Belgium, the Kačák event s.s. corresponds to a time window equivalent to the deposition of the Lomme and Hanonet formations. New stratigraphic and palaeontological (rugose corals) data show that the Kačák event had a moderate to weak impact on the Belgian carbonate shelf ecosystem. The Old World Realm faunal assemblages show no significant variation in diversity across the Kačák event. Nevertheless, the remarkable and unexpected occurrence of some rugose corals typical of the East American Realm (siphonphrentids and heliophyllids) in the lower part of the Hanonet Formation helps identify the event as the latter is also marked by a short phase of cosmopolitanism of benthic fauna. This is a proposed criterion useful to recognize the Kačák event where the typical pelagic guides are missing. [less ▲]

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See detail"Kadenzen des ganzen Körpers" - Das Sich-Bewegen des Musikers.
Viehöver, Vera ULiege; Wunsch, Stephan

in Görling, Reinhold; Skrandies, Timo; Trinkaus, Stephan (Eds.) Geste - Bewegungen zwischen Film und Tanz (2009)

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